Sixth Catalog of Orbits of Visual Binary Stars: Notes


                                                                                                                             
00000-1930   LTT 9831    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
00002+0146   WEI  45     HWE 64 is certainly identical with Weisse 45 = ADS 17156. Howe misread          
                         the sign of the declination. This was already stated in Cin. Pub v 6,           
                         nos 748 and 749, and the mean of the two measures is given in the mean          
                         results, assigned to Weisse 45. Nevertheless the pair was given                 
                         separately in the BDS and 12692 and taken over as ADS 17168. ADS 17156          
                         is misidentified. It is BD+00 5079 (9.1), 9.5, G0, with the position            
                         for 1900 (1950) as 23 55.1 (57.6) +01 13 (30).                          B__1950c
00003+1642   HJ  318     A component is PPM 116047. In Tycho catalog magnitude of A is 9.46; in          
                         Guide Star Catalogue B is GSC 1178 1031 with magnitude 12.77. Spectral          
                         types are K for A component, G5-K0 for B component. Annual proper               
                         motion for B: AR= -0.013" and DEC=-0.0005"                              FMR1999c
00006-5238   FIN 294     Spectrum: K1/2III+A/F.                                                          
00008+0630   GWP   2     XMI 101.                                                                Tob2012b
00011+6935   STTA253     B is BD+68@1417.                                                                
00011-2326   LDS2070     B is CD-24@17944.                                                               
00012-0005   TOK 359     Long-period SB.                                                         Tok2013b
00012-0312   LDS9082     Old LDS6082.                                                                    
00013+6021   STTA254     A is the semiregular variable WZ Cas.                                           
00013+0742   DU    4     HJL 325.                                                                HJL1986 
00013-7012   GLI 290     B is CPD-70@3035.                                                               
00014+3937   HLD  60     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.67 +/- 0.29, 1.79, and 1.65 Msun, respectively.             Mlk2012 
00016+6437   MLR  79     Misidentified by Muller as BD +63@2093.                                         
00016+3714   ES 2444     Aka ALI 472.                                                                    
00018-0322   LDS9083     Old LDS6083.                                                                    
00018-2548   B   630     Measures uncertain, too close.                                                  
                         G266-029. Not resolved in our images                                    Oso2004 
                         HIP 146. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
00019-0952   LDS5157     NLTT 58812/58813                                                        Chm2004 
00020+4530   J   864     BRT 1164.                                                                       
                         -22s and +2.4' from BD+44 4541.                                         J__1955 
                         AC: CPM pair.                                                           J__1955 
00022+5958   BU 1337     STI 1256.                                                                       
00022+2705   BU  733     85 Peg. Spectral types and masses of primary and secondary assigned by          
                         ten Brummelaar et al., based on adaptive optics observations.           TtB2000 
                         AB: Additional notes may be found in Baize (1945).                      Baz1945b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.49 +/- 0.81, 1.58, and 1.56 Msun, respectively.  Mlk2012 
                         Soderhjelm notes poor Hipparcos solution.                               Sod1999 
                         A third star has been detected by infrared speckle interferometry.      Mcy1983 
                         HIP 171. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AC and AD: Additional notes may be found in Burnham (1894).             Bu_1894 
00023+1609   BPM   1     [PM2000]    1692 + [PM2000]    1685.                                    Gvr2010 
00023+0732   LDS9084     Old LDS6084.                                                                    
00023-2943   B   631     zet Scl. The companion is very faint and not accurately measured. A             
                         is a spectroscopic binary.                                                      
00024+1429   GWP   4     XMI 102.                                                                Tob2012b
00024+1047   BGH   1     AB,C: HJL 326.                                                          HJL1986 
                         AB,C: SHY 377. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
00025-0826   LDS5255     NLTT 2/3                                                                Chm2004 
00026+6606   STF3053     B is BD+65@1988.                                                                
00026+1841   SHY 378     AB: HIP    201 + HIP    206.                                                    
00028+1647   BPM   2     [PM2000]    2010 + [PM2000]    1993.                                    Gvr2010 
00028+0208   HJ  998     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00031+0816   STF3054     B component is eclipsing binary of Algol-type, period 2.2604 d.         Zas2012 
00032+4508   HJ 1927     Unless the separation has decreased greatly, the measures given in the          
                         ADS would seme to refer to the nearby pair ADS 108.                     B__1963b
00032+3315   ES 2400     Pair long unconfirmed due to 1m error in published epoch-1900                   
                         coordinates (thanks to Rafael Caballero, private communication)                 
00034+1839   GWP   6     XMI 103.                                                                Tob2012b
00034-2430   LDS2076     NLTT 53/54                                                              Chm2004 
00037+1851   GWP   7     XMI 104.                                                                Tob2012b
00037+1134   BPM   3     [PM2000]    2710 + [PM2000]    2680.                                    Gvr2010 
00037-2824   CRZ   1     BDK   1. G 266-33 + 2MASS J00034227-2822410. Distance 39.5 +1.8/-1.6            
                         pc for primary, 26 +/- 3 pc for secondary. Estimated age of system              
                         0.9-1.4 Gyr. Mass of secondary estimated at 0.100-0.103 Msun.           Fah2010 
00042+6217   H 5  79     9 Cas.                                                                          
00042-1008   LDS3116     NLTT 86/84                                                              Chm2004 
00044+5804   OSO   1     G217-030. No common proper motion pairs, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
00045+0045   GWP  10     XMI 106.                                                                Tob2012b
00045+1851   GWP   9     XMI 105.                                                                Tob2012b
00046+4206   CHR 122     B is a spectroscopic binary. Hence the system is quadruple.                     
00046-4044   GKI   2     Ba,Bb. GJ 1001BC = LHS 102BC. Spectral types L4.5 and L4.5              Red2006b
00049+5832   STF3057     Called a two-spectrum SB in the Bright Star Catalog Supplement.                 
                         H 1  39.                                                                MEv2010 
00049-1320   GAL 295     Object #1 in Gallo's original list.                                     Gal1912a
00050+0835   GWP  11     XMI 107.                                                                Tob2012b
00051+6323   HJ 1933     STI 1265.                                                                       
00052+4514   ES 9001     Previously known as ES 1293a.                                                   
             BU 9001     Previously known as BU  997a.                                                   
00053-0542   33 Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1926).                                                          Hrp1926 
00054+1620   STTA255     B is BD+15@4934.                                                                
00054-2559   LDS3119     NLTT 158/159                                                            Chm2004 
00055+3406   HU 1201     A possible close approach about 1980.                                           
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.09 +/- 0.63, 2.52, and 1.10 Msun, respectively.  Mlk2012 
00056-0141   LDS3012     NLTT 176/175                                                            Chm2004 
00057+4549   STT 547     Premature orbits have been computed. Motion direct.                             
                         Both A and B have variable RV (ranges 45 and 25 km/s, respectively).            
                         Another star (9.9, 330") has common proper motion.                              
                         AB: Bolometric corrections and component masses determined from                 
                         M-L relation. A family of possible orbits were determined by Kiyaeva    Kiy2001 
                         (2001) for the F component relative to AB pair (Note: only the                  
                         shortest-period solution is presented in orbit catalog.)                        
                         AB: NLTT 172/173                                                        Chm2004 
                         AD and AE: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AF: HIP    473 + HIP    428.                                                    
00057+0626   BFR   1     NLTT 182 + 2MASS J00054171+0626300. Baron et al. (2015) estimate                
                         spectral types M4.5 +/- 0.5 and L0 +/- 1, distances 62 +38/-23 and              
                         69 +5/-22 pc, masses 0.157-0.181 and 0.079-0.085 Msun.                  BFr2015 
00059+1805   STF3060     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Aka J  3330.                                                                    
             HD    108   Hutchings (1975 ApJ 200, 122) presented a preliminary orbit with a              
                         period of 4.6d, but subsequent  work has cast doubt on the reality of           
                         the orbit (Underhill 1994 ApJ 420, 869).                                Msn1998a
             LEP   1     AD: HJL1001.                                                            HJL1986 
                         AD: SHY 112. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AD: the visual binary at 573" is co-moving, same parallax. The D                
                         component is ~1.3m below the main sequence in the (K, V-K) color-               
                         magnitude diagram.                                                      Tok2012a
00063+5826   STF3062     One component, designated V640                                                  
                         Cas, is variable, probably due to partial eclipses. P = 1.08 d.                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Secondary is SB, P=47.685d                                              Tok2014d
00063-4905   HDO 180     A is a spectroscopic binary.                                                    
                         Primary is planet host star, P=339d. B comp is LHS 1021. Pair bound.            
                         Photometry suggests companion K8.5-M1.5 with mass 0.59 +/- 0.02 Msun.   Egn2007 
00064+4501   UC  320     Aka BVD 170.                                                            Skf2013 
00066+2901   STT 549     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             ENG   1     A,CD: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
             BU 1338     CD: J 866.                                                                      
00066+1554   GWP  12     XMI 108.                                                                Tob2012b
                         Aka GRV1158 with quadrant flip.                                                 
00067-0706   JNN  11     Estimated age 1000-10000 Myr; masses 0.35 +/- 0.09 and 0.21 +/- 0.05            
                         Msun; a ~5.6 AU.                                                        Jnn2014 
00068-2106   RSS  41     CPD-21@1                                                                        
00068-0853   BUG  15     Burgasser et al. (2012) determine that the pair comprised of LP 704-48          
                         and SDSS J000649.16-085246.3 share cpm, at a projected separation of            
                         820 +/- 120 AU, based on a derived distance 30 +/- 3pc. Spectral type           
                         of the primary is M7. From near-IR spectroscopy they determine the              
                         secondary is SB, orbital period 147.6 +/- 1.5d, e = 0.10 +/- 0.07;              
                         spectral types of Ba and Bb are M8.5 +/- 0.5 and T5 +/- 1. Estimated            
                         ages of A and B are >8 and >3-4 Gyr; masses 0.092 Msun for A,                   
                         0.082-0.083 and 0.049-0.064 Msun for the M8.5 and T5 stars.             Bug2012 
                         NLTT 251 + 2MASS J00064916-0852457. Baron et al. (2015) estimate                
                         spectral types M6.0 +/- 0.5 and M9.0 +/- 0.5, distances 25 +7/-11 and           
                         37 +5/-11 pc, masses 0.102-0.133 and 0.079-0.085 Msun.                  BFr2015 
00070+0303   GWP  14     XMI 109.                                                                Tob2012b
00071+6309   MLR 105     No significant movement since first resolution.                         Drd2009 
00074-2936   LDS2088     NLTT 296/295                                                            Chm2004 
00076+4009   STF3064     Taken to be the same as H 4  69 (= H IV 69). With error of 1deg in              
                         declination it would be the same as STF 3064 rej.                               
                         BDS 8.                                                                          
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00076-2718   LDS2089     NLTT 307/308                                                            Chm2004 
00077+6022   JNN 247     G 217-32. Estimated age 35-300 Myr; masses 0.17 +/- 0.07 and 0.12 +/-           
                         0.06 Msun; a ~9.8 AU.                                                   Jnn2014 
00078+5723   HJ 3241     HJ 1935.                                                                        
00079+0317   J   301     BAL 1606.                                                                       
00079-2727   LDS   5     Also known as CHM   1. WDS designation in error, apparently due to              
                         confusion between CD-28 11 and CPD-28 11.                                       
00079-3005   LDS2092     NLTT 319/320                                                            Chm2004 
00080+3123   STTA256     B is BD+30@3.                                                                   
00082+6217   HJ 1936     Optical pair, since relative motion reflects the proper motion of               
                         component A relative to B to high accuracy.                             Kiy2012 
00082+5933   STI   8     AB: 00083+5934SMA   3                                                           
00082+0937   LDS9085     Old LDS6085.                                                                    
00083+1329   GWP  17     XMI 110.                                                                Tob2012b
00084+2905   H 5  32     21 And = alp And                                                                
                         AB: H V 32. STFB 15. A is spectroscopic binary, P = 96.7d.                      
                         AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             MKT  11     Aa,Ab: Separations and magnitude differences derived by model fitting           
                         to calibrated squared visibilities, using measurements with the Mark            
                         III interferometer. Spectroscopic and photometric data are combined             
                         with astrometry from the Mark III interferometer to derive orbital              
                         elements for the SB1 by Pan et al.                                      MkT1992a
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Pan et al. (1992).                                                      MkT1992a
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 4.05 +/- 0.50 and                
                         1.71 +/- 0.20 Msun.                                                     Ren2010 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 5.19 +/- 0.18, 4.10, and 3.09 Msun, respectively.  Mlk2012 
                         Aa,Ab: Docobo et al. (2014) use the spectroscopic elements of Pourbaix          
                         (2000), together with speckle data and the Hipparcos parallax, to       Pbx2000b
                         derive the remaining orbital elements. The resulting masses are                 
                         3.84 +/- 0.29 and 1.63 +/- 0.26 Msun.                                   Doc2014h
00085+3456   HDS  17     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.78 +/- 0.89, 2.67, and 1.10 Msun, respectively.             Mlk2012 
00085-7134   HLN  18     Also known as TDS1309.                                                          
00085-0419   GWP  19     AB and BC were originally listed as the triple 00086-0418; now are              
                         merged with GWP 18 at the correct WDS designation.                              
00087+5006   ES  443     Identical to ES 744.                                                            
00088+8647   NLTT 324    Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Latham             
                         et al. (2002). They derived component masses 1.06 and 0.59 Msun and an  Lat2002 
                         estimated semimajor axis of 7.00 mas.                                   Ren2013 
00088+0801   HDO   2     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00089+3257   SEI   1     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00089+2050   BEU   1     GJ 3010. Estimated age 30-300 Myr; masses 0.20 +/- 0.09 and 0.11 +/-            
                         0.06 Msun; a ~2.0 AU.                                                   Jnn2014 
00090+2738   GIC   1     AB = G130-046/G130-045.                                                         
00090-5400   HDO 181     Spectroscopic binary.                                                           
                         Quoted errors in P and a are +116/-40y, +0".20/-0".06, respectively.    Ary2002b
00092+5909   AGC  15     bet Cas = 11 Cas = Caph                                                         
                         The primary is a Delta Scuti-type variable.                                     
                         Spectroscopic binary, P = 27 d.                                                 
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00092-3035   LDS2093     NLTT 410/401                                                            Chm2004 
00093+7943   STF   2     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.97 +/- 2.24, 3.22, and 2.02 Msun, respectively.             Mlk2012 
00093+5324   FYM   4     The EF pair reported by Fay (2013) is not seen in Aladin; probably an   FyM2013d
                         erroneous identification of their CG pair.                                      
             BVD  11     CD: Originally listed as separate pair (00096+5325), aka FYM 4CD.               
00093+2517   GIC   2     LDS 859 = G130-048/G130-047.                                                    
                         HIP 754. See Allen et al. (2000) for information on metallicity,        AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         A companion is a close astrometric binary.                              HIP1997d
                         AB: Primary is SB2, P=463.250d                                          Tok2014d
                         Spectroscopic orbit P=463.44d and radial velocity of B consistent       Grf2015b
                         with physicality.                                                               
00094+6357   BUP   1     V641 Cas, a VV Cep-type system.                                                 
00094+4819   LDS3128     NLTT 412/405                                                            Chm2004 
00094+1415   CHE   1     Due to poor published coordinates, identification with the coordinates          
                         in the WDS is uncertain. Chevalier’s measure does not agree well with   Che191
                         others for this pair.                                                   Hrt2012b
00094-2759   BU  391     kap 1 Scl                                                                       
00096+3826   PTT   1     This appears to be the same as ALI 473. PTT position 00 10.0 +38 23.            
00096+0148   GWP  22     XMI 113.                                                                Tob2012b
00096+1047   GWP  21     XMI 112.                                                                Tob2012b
00096+1052   GWP  20     XMI 111.                                                                Tob2012b
00097+3107   GIC   3     G130-050/G130-049.                                                              
                         NLTT 433/431                                                            Chm2004 
00100+4623   STF   3     A small star in field: 1831.33 133.0@ 4.57"; Possibly an illusion.      Bu_1906 
                         H 2  83.                                                                MEv2010 
                         Primary is V342 And, an Algol type eclipsing binary, P = 2.63934d.      Zas2012 
00100+1109   STF   5     34 Psc.                                                                         
00101+5847   STI1287     SMA.                                                                            
                         Daley (Dal2002c) finds a large B-V for the secondary of 1.52.                   
00101+3825   HDS  23     Da,Db: Cvetkovic et al. (2014) derive spectral types K3 and  K4,                
                         masses 0.79 and 0.72 Msun. Dynamical parallax is 11.42 +/- 0.70 mas.    Cve2014 
00103+7231   HJ 1941     See note to 00138+7233BUP   2.                                                  
00104+4952   ES 2576     B is BD+49@17.                                                                  
00105+1716   ALP   1     2MASSI J0010325+171549                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00106-7313   I    43     There is a long gap (1931-1977) in the observations.                            
00107+5453   WOR  37     SX Cas, an eclipsing and spectroscopic binary, P = 36.6d.                       
                         Spectral types A6shell and K3III.                                               
00108-5729   HJ 3350     Primary is BL Phe, a Beta Lyr type eclipsing binary, P = 0.81035d.      Zas2012 
00109+4807   LEP   2     NI    1.                                                                        
00109+1705   GWP  24     XMI 114.                                                                Tob2012b
00110+0058   SKF1821     Initial WDS designation (00110+0913) garbled - dec portion copied from          
                         SKF1820.                                                                        
00111+5755   HJ 1003     STI 1291.                                                                       
00112+4933   ES 2577     B is BD+48@28.                                                                  
00113+1435   LDS1072     NLTT 521/522                                                            Chm2004 
00113+0625   GWP  27     XMI 115.                                                                Tob2012b
00113-2045   LDS   1     G266-060. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 525/526                                                            Chm2004 
00114+5850   SKW   1     Aa,Ab. Primary of the Herbig Ae/Be pair LkHa 198. A family of possible  SKW2005 
                         orbits are calculated, based on various choices for initial parameters          
                         (luminosities, component masses, etc.). Neither a" nor T0 was                   
                         provided. a" was calculated from other published parameters and T0 was          
                         determined by trial and error with comparison to their Figure 3.                
00116-0305   STF   8     H 2  55.                                                                MEv2010 
00116-2748   LDS2099     kap 2 Scl                                                                       
00117+0323   FMR  29     aka UC  332.                                                                    
00121+5337   BU 1026     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.13 +/- 1.26, 3.41, and 3.01 Msun, respectively.  Mlk2012 
             CHR   1     AC: Rapid motion, particularly in separation.                                   
00121+3327   GII  13     Aka ITF  31.                                                                    
00122+4647   A   802     Not seen 1950-1976. Possibly a whole revolution.                                
00125+1434   LN Peg      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
00126+2143   LDS 861     NLTT 589/592                                                            Chm2004 
00126+1118   BPM   4     [PM2000]    8713 + [PM2000]    8668.                                    Gvr2010 
00130+0257   A  2001     Apparent motion in a highly-inclined orbit.                                     
00132+1511   BUP   3     gam Peg = 88 Peg = Algenib                                                      
                         Beta CMa variable and spectroscopic binary.                                     
00132+0536   PLQ   3     Possibly same star as HDO   5 (Doolittle).                                      
00132-1711   HJ 1944     B is BD-17@16.                                                                  
00133+6919   KUI   1     AB: Nechville 6.                                                                
             JNN 248     BC: GJ 11 B. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.10 and             
                         0.26 +/- 0.06 Msun; a ~17.2 AU.                                         Jnn2014 
00134+3859   BRT2196     ALI 718, J 2709.                                                                
00134+3801   ES 2445     ALI 474.                                                                        
00134+2659   STT   2     Hipparcos parallax of 0".00808 yields a mass sum of 1.9 Msun,                   
                         slightly underestimated for a double star of spectral type F8V.                 
                         Dynamic parallax is 0".0053, considerably different from the                    
                         measured one.                                                           Sca2000b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.36 +/- 1.29, 4.23, and 1.10 Msun, respectively.  Mlk2012 
                         Star C (mag. 10.37, 18") is physical, according to Le Beau.             LBu1990c
00135-0009   HJ  618     BAL 641 = LDS   4.                                                              
00136+1356   LDS1073     LDS6086 = LDS9086.                                                              
00137+7702   MLR 283     Aka TDS1350.                                                                    
00137+4934   STF   9     B is BD+48@42.                                                                  
00137+1537   BPM   5     [PM2000]    9457 + [PM2000]    9535.                                    Gvr2010 
00138+7233   BUP   2     Misinterpretation of a note in Bu_1913 resulted in these three BUP              
                         components being associated with 00103+7231HJ 1941, when all three              
                         were actually measured relative to a planetary nebula (NGC 40) about            
                         3m following the HJ pair. Since one BUP component was also the primary          
                         of the MLR 282 triple system, the BUP component designations were               
                         changed to become part of the MLR multiple. The planetary nebula is             
                         now the D component in this system.                                             
00138+3612   BU 1341     AC: This is a measure of A and BD+35@27.                                        
00138+0812   TOK 360     Likely triple system.                                                   Tok2013b
                         Primary is unresolved Hipparcos acceleration solution (G-code) binary.  Tok2014d
00138-7442   HJ 3353     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00139+6323   BU 1309     AB: The star is 63@703-62@1909 in Vat. Astrog. Cat. (Van Biesbroeck).   VBs1954 
                         AD: D is 63@656-62@1910.                                                        
00139+1518   LDS1074     NLTT 667/666                                                            Chm2004 
00139-0429   LDS9087     Old LDS6087.                                                                    
00140+2837   BRT 117     MLB 554.                                                                        
00140-1815   BFR   2     NLTT 687 + 2MASS J00135882-1816462. Baron et al. (2015) estimate                
                         spectral types M3.0 +/- 0.5 and L1.0 +/- 0.5, distances 42 +26/-16 and          
                         83 +7/-27 pc, masses 0.389-0.412 and 0.072-0.078 Msun.                  BFr2015 
00141+7601   STTA  1     B is BD+75@5.                                                                   
00141+3957   ES 2544     ALI 1008.                                                                       
00142-0712   MSH   1     Meshkat et al (2015) resolved a faint companion to HD 984. They derive          
                         a system age in the range 30-200 Myr. Teff for the primary is 6315 +/-          
                         89K; temperature for the secondary is 2777 +127/-130K or 2900 +/- 200K,         
                         depending on adopted scale and synthetic spectra. Spectral types are            
                         F7V and M6.0 +/- 0.5. Primary mass is 1.20 +/- 0.06 Msun; secondary             
                         mass estimates range from 74 - 90 Mjup, depending on adopted models.    Msh2015 
00143-0535   OSO   2     G031-036. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00144+3609   LDS3140     NLTT 703/704                                                            Chm2004 
00144+1643   BPM   6     [PM2000]    9941 + [PM2000]    9955.                                    Gvr2010 
00144-1424   GAL 296     Object #7 in Gallo's original list.                                     Gal1912a
00145-0747   BU  486     Irregular variable, AD Cet.                                                     
00148-2859   RSS   1     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
00150+0849   STF  12     35 Psc. A is an Algol-type system, UU Psc, P = 0.84d. Also known as             
                         CHE   2.                                                                        
                         HJL   2.                                                                HJL1986 
                         H 3  62.                                                                MEv2010 
00150-7251   BRG   1     The AstraLux PSF was strongly asymmetric for this target, hence in              
                         addition to the usual PSF fitting, we also performed a customized               
                         aperture photometry scheme in order to ensure that the PSF fitting did          
                         not provide a biased result (see paper for details). We adopt the               
                         aperture photometry values for the differential photometry, and let             
                         the errors be represented by the scatter between PSF fitting results            
                         and the aperture photometry. Note that the photometry values presented  Brg2010 
                         here should replace those in Bergfors et al. (2010).                    Jnn2012 
00152+5947   FYM 153     Purported AJ pair removed on request of author.                         FyM2014b
00152+2717   KUI   2     A is a spectroscopic binary.                                                    
00152+2722   J   868     Despite having an orbit, this pair determined to be optical.            FMR2014d
00152+2454   GIC   4     G130-059/G130-060.                                                              
00153+5304   GIC   5     G217-041/G217-040.                                                              
                         NLTT 739/738                                                            Chm2004 
00153+4412   A  1256     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.79 +/- 3.58, 5.77, and 2.82 Msun, respectively.  Mlk2012 
                         Primary is the Algol-type eclipsing binary V348 And.                    Zas2009 
00153+1630   BPM   7     [PM2000]   10539 + [PM2000]   10566.                                    Gvr2010 
00153+0936   GWP  30     XMI 116.                                                                Tob2012b
00153-4006   WG    2     B is CPD-40@14.                                                                 
00154-1134   GAL 297     00153-1133SLE 251. Object #9 in Gallo's original list.                  Gal1912a
00155-1608   HEI 299     L722-22. Astrometric binary now resolved.                                       
                         Too poor astrometric orbit (Innes 1998) and too few resolved            Inn1988 
                         observations (cf. Heintz 1990) to give definite orbit. Present          Hei1990a
                         solution at least preferable to `X' HIP solution.                               
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.17 +/- 0.02, 0.39, and 0.50 Msun, respectively.             Mlk2012 
00157+3516   ALP   2     2MASSW J0015447+351603                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00159-0853   SHY 381     HIP   1266 + HIP    118.                                                        
00160+0415   NLS   1     Nielsen et al. (2012) discovered two low-mass companions to the young           
                         A0V star HD 1160. The B component is thought to be a brown dwarf,               
                         mass 33 +12/-9 Mjup. The C component is of spectral type M3.5 +/- 0.5,          
                         with estimated mass 0.22 +0.03/-0.04 Msun. The age of the system is             
                         roughly 50 +50/-40 Myr.                                                 Nls2012 
00161+0902   GWP  32     XMI 117.                                                                Tob2012b
00162+7657   STF  13     A premature orbit has been calculated.                                          
00162+1903   J   217     Measures scattered.                                                             
                         Additional notes may be found in Couteau (1952) and                     Cou1952a
                         Van Biesbroeck (1954).                                                  VBs1954 
00162-7951   GJ 3021     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
             CVN  14     Companion is a probable mid-M dwarf.                                    Cvn2006 
                         Spectral type of B component M4V +/- 1.                                 Cvn2007 
                         A second candidate companion at 39" is noted in UCAC2 as having much            
                         different proper motion, so has been ruled out as a companion. The              
                         measured proper motion of the companion between the two SofI observing          
                         epochs is (+368 +/- 68 mas, -48 +/- 68 mas). IR spectroscopy suggests           
                         a spectral type of M4-M5V for the B component.                          Mug2007b
                         Co-moving with HIP 107705 at 3.5pc.                                     Shy2001 
00164+5722   TDS1375     Aa,Ab: formerly 00165+5722, WDS designation changed when merged with            
                         HJ 1011 into triple                                                             
00164+1950   LDS 863     AB: NLTT 803/804                                                        Chm2004 
00165-2805   LDS2107     NLTT 834/835                                                            Chm2004 
00167+3910   ES 1936     ALI 719.                                                                        
00167+3638   STF  19     STT   3.                                                                        
00167+3629   STT   4     Hipparcos parallax of 0".01115 yields a mass sum of 2.75 Msun                   
                         with an uncertainty of 38% overestimated for a double star of                   
                         spectral type G0. Dynamic parallax is 0".0108, agreeing well with               
                         the measured parallax.                                                  Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.59, 2.35, and 1.05 Msun, respectively.             Mlk2012 
00169-5239   GC 333      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Bopp et al. (1970).                                                     Evn1970 
00171+3841   CHR 123     theta And = 24 And                                                              
00171-1205   CBL 202     GWP  34.                                                                Tob2012b
00171-1406   GAL 298     Object #12 in Gallo's original list.                                    Gal1912a
00172-1921   LDS   9     B is BD-20@34.                                                                  
00174+0853   A  1803     Too close 1932, 1946-47, 1965-72. Modern measures show a close                  
                         approach about 1985. While both 18- and 36-year period orbits                   
                         have been calculated for this pair, Griffin (Docobo, private                    
                         communication) determined spectroscopically that the shorter-period             
                         high-eccentricity orbit is the correct one.                                     
                         The measure reported for 1976.622 is spurious and has been deleted              
                         from the catalogs.                                                      McA1982b
                         Large and irregular residuals preclude the correction of an orbit.      Tok1985 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.02 +/- 0.02, 1.48, and 1.13 Msun, respectively.  Mlk2012 
             STF  22     AB,C: H 2  50.                                                          MEv2010 
00174+0221   STF  21     HJL   3.                                                                HJL1986 
00176+1300   HJ    3     HJL   4.                                                                HJL1986 
00176-1113   GAL 299     Object #13 in Gallo's original list.                                    Gal1912a
00177+5126   TRN   8     AO Cas.  Classification is from the UV tomographic analysis of          Bgn1991 
                         Bagnuolo & Gies (1991).                                                 Msn1998a
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7341 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
00178+1620   TOK 646     Primary is 39 Psc. B is likely physical, as it moves in the same                
                         direction as A in DSS2 image.                                           Tok2014d
00180+2057   LDS 864     NLTT 912/910                                                            Chm2004 
00180+0931   AG    1     HJL   5.                                                                HJL1986 
00182+7257   A   803     Quadrant uncertain.                                                     Wor1967b
00182+1209   GWP  38     XMI 118.                                                                Tob2012b
00183+1646   BPM   8     [PM2000]   12613 + [PM2000]   12602.                                    Gvr2010 
00184+4401   GRB  34     AB: Proper motion of A +2860 +390. Proper motion of B +2884 +410.               
                         Premature orbits have been calculated. RV of star A possibly variable.          
                         B component is the BY Dra-type variable CQ And and a SB.                        
                         AB: NLTT 919/923                                                        Chm2004 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00184+0344   HDO  12     AB: Appears to be same pair as HDO 13.                                          
00185-2757   HJ 1949     B is CD-28@75.                                                                  
00187+4347   STT   5     26 And.                                                                         
00188+5923   HJ 1012     STI 1320.                                                                       
00188-1217   GAL  15     Incorrectly entered in WDS as GAL   5.                                          
00188-1258   GIC   6     G158-057/G158-054.                                                              
00189+5923   HJ 1013     STI 1322.                                                                       
00189-1135   GAL  16     Originally entered with incorrect RA, so also known as                          
                         10187-1239GAL 422                                                               
00190+4301   ES 1483     J 1359.                                                                         
00192+5942   KR    4     A is an irregular variable, V377 Cas.                                           
00192+4330   ES 1484     BRT 67. Djurkovic calls this ES 1484BC.                                 Dju1954c
00192+0827   GWP  39     XMI 119.                                                                Tob2012b
00194-0849   HJ 1953     iot Cet = 8 Cet.  Variable?                                                     
00196-2808   LDS  12     Proper motion -275 -1292.                                                       
00197+6046   LDS9088     Old LDS6088.                                                                    
00197+1951   GWP  40     XMI 120.                                                                Tob2012b
                         2MASS J00193931+1951050 and J00194303+1951117 are separated by only             
                         53", have very similar proper motions (e.g. Roser et al. 2010) and      Rsr2010 
                         have similar estimated spectroscopic distances (23 and 21 pc,                   
                         respectively) in Riaz et al. (2006), hence it is highly likely that     Ria2006 
                         they form a physical pair.                                              Jnn2012 
00197+0624   ZUC   5     Primary is white dwarf PG 0017+061 = PHL 790.                           Zuc1992 
00199+2633   CHE   4     Chevalier's measure was correct, but his published (dx,dy) predict      Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dy, which was printed as -0'.0317 rather than              
                         -0'.0617. There is also an apparent trigonometric error in his value            
                         for position angle. Chevalier gives a value for theta of 154.62 deg,            
                         but all later measures in the WDS give values of about 204.0 deg. It            
                         appears his value should be 360−154.62 = 205.38 deg instead.            Hrt201
00200+3814   S   384     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 5  85.                                                            MEv2010 
00201+4244   OSO   3     G171-050. AB is not a common proper motion pair, based on astrometry            
                         and color.                                                              Oso2004 
             LDS3151     AC: NLTT 1038/1036                                                      Chm2004 
00203-3246   B  1025     Considerable motion, but no measures for more than 30 years.                    
00204+1757   OSO   4     G032-012. Not a common proper motion pair.                              Oso2004 
00206+1219   BU 1015     Hipparcos parallax of 0".00883 yields a mass sum of 2.87 Msun                   
                         with an uncertainty of 75% slightly in excess for a binary of                   
                         spectral type F5. The great uncertainty concerning the sum of                   
                         masses is largely due to the consistent error in the measured                   
                         parallax. The dynamical parallax is 0".0085, agreeing well with                 
                         the observed parallax.                                                  Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.44 +/- 1.04, 2.58, and 1.20 Msun, respectively.             Mlk2012 
00207+3159   CCA   1     WSP   1. WASP-1.  Duplicity discovered based on low-amplitude radial            
                         velocity variation. Spectral analysis plus transit light curves yields          
                         an orbital period of 2.520d. Given a spectral type for the primary of           
                         F7V, the planet has mass 0.80-0.98 +/- 0.11 Mjup and radius 1.33-2.53           
                         Rjup. Mass of the parent star is 1.06-1.39 Msun.                        CCA2007 
00207+0738   GWP  41     AB: XMI 121AB.                                                          Tob2012b
             GWP  42     AC: XMI 121AC.                                                          Tob2012b
00208+2737   CHE   7     MLB 674.  Also known as ROE 116.                                                
00210+6740   HJ 1018     STF 18.                                                                 Mlr1955c
00210+2647   CHE   9     Chevalier's measure was correct, but his published (dx,dy) predict      Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dx, which should be +0'.0708. Chevalier applied            
                         his declination offset from the plate center in the wrong direction,            
                         leading to an error of over 25' in the coordinates. The image for the           
                         pair at the corrected coordinates is elongated on the Aladin image;             
                         due to uncertain relative proper motion it's impossible to tell                 
                         whether his rho and theta values are correct.                           Hrt2012b
00210-7429   OGL   1     SMC139.6.72    + SMC139.6.636                                           Pli2012 
00211+6443   TDS  13     According to Milburn this pair was originally "found by Aitken          Mlb1925 
                         (private letter) in looking for MLB 244". This note went unnoticed      A__1925D
                         until long after the Tycho designation had come into usage, however;            
                         although the historical measures have been added the original TDS               
                         designation has been retained.                                                  
00212-4246   KO    1     A = LEHPM 494 (spec M6.0 +/0 1.0 V), B = DENIS-P J0021.0-4244 (spec             
                         M9.5 +/- 0.5 V). Data sources: UK Schmidt blue survey (1977.6), ESO             
                         Schmidt red (1984.8), DENIS I (1996.60), UK Schmidt red (1996.61), UK           
                         Schmidt near-IR (1999.6), 2MASS (1999.7). Mean separation (1974-1999)           
                         1.296 +/- 0.012 arcmin. The pair moved 5".7 over 22 years, 80 times             
                         the uncertainty in mean rho; concludes is CPM pair.                     Cab2007a
                         Additional 2003 measure from Spitzer Space Telescope.                   Cab2007b
00214+6700   STT   6     Orbit is very eccentric and very inclined. Scardia's geometrical                
                         elements do not differ much from those of Van Biesbroeck and Muller,            
                         but the orbit is more eccentric and has twice the period. An Hipparcos          
                         parallax of 0".00491 yields a mass sum of 6.6 Msun, overestimated for           
                         a binary system of spectral type B8.5V. The dynamical parallax is               
                         0".0054, in reasonable agreement with the measured one.                 Sca2000b
00214+2744   CHE  10     MLB 675.                                                                        
00214-7355   OGL   2     SMC138.6.56    + SMC138.6.104                                           Pli2012 
00215-6744   HJ 3361     CD-68@10.                                                                       
00215-7407   OGL   3     SMC138.8.18    + SMC138.6.78                                            Pli2012 
00216-7442   OGL   4     SMC139.8.20    + SMC139.8.81                                            Pli2012 
00217+1301   BPM   9     [PM2000]   14913 + [PM2000]   14833.                                    Gvr2010 
00218+6628   STT   7     CD: Previously listed incorrectly as AB,E, with quadrants flipped to            
                         275 deg.                                                                        
00219+1706   BPM  10     [PM2000]   15011 + [PM2000]   15046.                                    Gvr2010 
00219-2300   HJ 1957     Designated as HJ 3429 in BDS.                                           Bu_1906 
00220+4913   BWL   3     AC and AD: Colors and/or astrometry are inconsistent with a late-type           
                         common proper motion companion based on visual inspection of the field          
                         from 2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3030.                Bwl2015 
00220+4231   RAS  16     Poorly-studied silicon star with weak magnetic field.                   Ras2014 
00221+4822   J  9001     Was a measure of a new pair designated as J  2384.                              
00222-7439   OGL   5     SMC139.7.1570  + SMC139.7.1569                                          Pli2012 
00224+1329   STF  27     42 Psc.                                                                         
00225+4456   A   648     Measure very doubtful. Not seen double on two later nights.             B__1963b
00226+5033   KU   67     B is BD+49@62.                                                                  
00226-3111   LDS  14     NLTT 1165/1164                                                          Chm2004 
00229+6214   ES  115     Primary is V745 Cas, a W UMa type eclipsing binary, P = 1.41057d.       Zas2012 
00229+5420   ES   42     ES 154.                                                                         
00229-1213   BUP   6     9 Cet.                                                                          
00230+6112   STI  43     HJ 1023.                                                                        
00234+2624   CHE  17     AC: Chevalier's measure was correct, but his published (dx,dy) predict  Che1908 
                         different (rho,theta) than published. This was apparently due to a              
                         typographic error in dy, which should be -0'.2783.                      Hrt2012b
00234-0121   HJ 1961     J 1433.                                                                         
00235-0343   LDS3160     AB: NLTT 1213/1214                                                      Chm2004 
00236+0947   KUI   3     LDS3162                                                                         
00239+2930   STF  28     B is BD+28@55. The variable, double-lined spectroscopic binary                  
                         BD+28@54 may belong to the system. This was previously reported as              
                         BD+28@49, but was corrected by Weis{2002, "F.G.W. Struve's                      
                         Double Stars (STF2000.0)"}                                                      
                         SHY 383. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
00240+3835   BUP   7     A is a Mira-type variable, R And.                                               
00240-0329   BU 488      Due to poor published coordinates, Chevalier's measure of this pair     Che1910 
                         was originally added to the WDS as a new discovery: 00245−0327 CHE 23   Hrt201
00240-7300   OGL   6     SMC136.8.38    + SMC136.8.178                                           Pli2012 
00241-7300   OGL   7     SMC136.8.41    + SMC136.8.408                                           Pli2012 
00242+1505   GWP  44     XMI 122.                                                                Tob2012b
00242-1305   VOU  83     Also single in 1958. Star confused with HU 4 (00246).                   VBs9999 
00242-7349   OGL   8     SMC138.6.4018  + SMC138.6.246                                           Pli2012 
00243+5201   HU  506     A premature orbit has been computed.                                            
                         Single 1934, 1953. A is SB, P = 28d:.                                           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Additional notes may be found in van den Bos (1963).                    B__1963b
00244+1322   BPM  11     [PM2000]   16681 + [PM2000]   16731.                                    Gvr2010 
00245-1217   GIC   7     LDS 3163 = G158-073/G158-074.                                                   
                         NLTT 1262/1265                                                          Chm2004 
00247-2653   LEI   1     Paper includes orbit of BC pair and estimate of mass sum.               Lei2001a
                         HST WFPC2 photometry was also transformed to standard Johnson B and V           
                         and Cousins R and I filters, yielding the following magnitudes for the          
                         A, B, and C components:                                                 Lei2000 
                            ------ A -----  ------ B -----  ------ C -----  filt                         
                            17.17 +/- 0.05  20.57 +/- 0.07  21.48 +/- 0.11   B                           
                            15.35     0.04  18.68     0.06  19.07     0.07   V                           
                            13.63     0.04  16.30     0.05  16.65     0.05   R                           
                            11.66     0.04  14.01     0.05  14.43     0.05   I                           
                         Seifahrt et al. (2008) determine mass sum of BC pair to be 0.157 +/-    Sef2008 
                         0.009 Msun; mass of A 0.115 +/- 0.010 Msun. They find no sign of the            
                         fourth component reported by Henry et al. (1999).                       Hen1999 
                         Rajpurohit et al. (2012) derive Teff, log g, radius, luminosity, and    Raj2012 
                         spectral type for the components of LHS 1070 using various models.              
                         Mean values (assuming distance = 8.8pc) are:                                    
                                 Teff (K)   log g   radius (Rsun)   log(L/Lsun)   spec                   
                             A:    2950      5.3       0.136           -2.92      M5.5                   
                             B:    2400      5.5       0.102           -3.44      M9.5                   
                             C:    2300      5.5       0.099           -3.55      L0                     
                         Koehler et al. (2012) derive masses for the A, B, and C components of           
                         0.172+/-0.010, 0.077+/-0.005, and 0.071+/-0.004 Msun, respectively.     Koh2012 
00247-5359   HJ 3364     B is CPD-54@89.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00247-7240   OGL   9     SMC136.6.12    + SMC136.6.115                                           Pli2012 
00248+1925   BRT2296     J 2586.                                                                         
00249+1355   GWP  45     XMI 123. SLW  18.                                                       Tob2012b
00250+2726   CHE  24     There was a 1' error in Chevalier's determination of declination.       Che1908 
                         In addition, there was a trigonometric error in deriving theta; the             
                         correct value is 180deg - theta.                                        Hrt2012b
00250+0600   GWP  46     XMI 124.                                                                Tob2012b
00250-7244   OGL  10     SMC136.7.2977  + SMC136.7.2975                                          Pli2012 
00251+4803   CRZ   2     BDK   2. G 171-58 + 2MASS J00250365+4759191. Distance 42.2 +2.0/-1.8            
                         pc for primary, 31 +/- 6 pc for secondary. Estimated ages of                    
                         components are discrepant: 1.8-3.5 Gyr for primary, versus 0.1-0.5 Gyr          
                         for secondary. The primary is a spectroscopic binary resolved by        Hip1997a
                         Hipparcos, the secondary a close (~10AU) L4+L4 pair, resolved by Reid   Red2006b
                         (2006).                                                                 Fah2010 
             HDS  56     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.30 +/- 0.21, 1.85, and 1.10 Msun, respectively.  Mlk2012 
             RED  14     Ba,Bb: 2MASS J00250365+4759191. Spectral types L4 and L4                Red2006b
00251-3646   BRG   2     Like BRG 1, this stellar binary also had an asymmetric PSF, and we              
                         therefore calculated the photometry in the same way as for that case.           
                         Note that the photometry values presented here should replace those in  Brg2010 
                         Bergfors et al. (2010).                                                 Jnn2012 
00251-7432   OGL  11     SMC139.2.27    + SMC139.3.744                                           Pli2012 
00253-7446   OGL  12     SMC139.1.28    + SMC139.1.120                                           Pli2012 
00254+2036   A  2301     J 219.                                                                          
00254+0156   STT   8     44 Psc                                                                          
00254-7404   OGL  13     SMC138.2.19    + SMC138.7.4092                                          Pli2012 
00255-7334   OGL  14     SMC135.8.3096  + SMC135.8.3687                                          Pli2012 
00256+1536   LDS9089     Old LDS6089.                                                                    
00256-1849   HJ 1964     SEE 8.                                                                          
00257-5050   HJ 3365     B is CD-51@102.                                                                 
00259-0748   RIA   1     LHS 1074.                                                                       
00260+0027   GRV 974     Aka SLW  21.                                                                    
00260-0542   LDS3168     NLTT 1360/1359                                                          Chm2004 
00261-1037   GIC   8     LDS5273 = G158-077/G158-078.                                                    
                         NLTT 1370/1374                                                          Chm2004 
00261-7057   OGL  15     SMC137.5.17    + SMC137.5.19                                            Pli2012 
00262-4217   alp Phe     Alden's astrometric solution uses values of P, T, e adopted from the    Ald1938a
                         spectroscopic orbit (Lunt 1924).                                        Lun1924b
00266-1924   ARA 515     Aka ITF  33.                                                                    
00267-7220   OGL  16     SMC140.1.3576  + SMC140.1.3730                                          Pli2012 
00268+0722   DOO  23     Doolittle calls this HDO 21, BDS 210. However, this seems to be a       Doo1915b
                         different pair.                                                                 
00268-3220   LDS2121     LDS5274                                                                         
                         NLTT 1416/1412                                                          Chm2004 
00269-0531   SCJ   1     B is BD-06@72.                                                                  
00269-7123   OGL  17     SMC137.8.790   + SMC137.8.846   + SMC137.8.1090                         Pli2012 
00269-8308   I   177     Spectrum of B is F.                                                             
00270+1705   BFR   3     HD 2292 + 2MASS J00265989+1704463. Baron et al. (2015) estimate                 
                         spectral types G5 and M9 +/- 1, distances 42 +28/-14 and 65 +4/-20 pc,          
                         masses 1.05 -1.12 and 0.108-0.118 Msun.                                 BFr2015 
00270-7237   OGL  18     SMC136.3.1     + SMC136.6.2735                                          Pli2012 
00271-0628   LDS3169     NLTT 1426/1425                                                          Chm2004 
00272+4959   STF  30     B is BD+49@89.                                                                  
00274+3054   HDS  62     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1979).                                                         Grf1979c
00274+0124   GWP  51     XMI 125.                                                                Tob2012b
00276+5120   COU2252     Transcription error resulted in 10' error in WDS designation.                   
                         00274+5130TDS1470                                                               
00276+1616   GWP  52     XMI 126.                                                                Tob2012b
00276-7221   OGL  19     SMC140.1.4858  + SMC140.1.4878                                          Pli2012 
00277+0936   GIC   9     G001-005/G032-021.                                                              
00277-7228   OGL  20     SMC136.4.4     + SMC136.4.17    + SMC136.4.36                           Pli2012 
00277-7300   OGL  21     SMC136.1.16    + SMC136.1.168                                           Pli2012 
00278+1803   BPM  12     [PM2000]   18879 + [PM2000]   18873.                                    Gvr2010 
00278-7251   OGL  22     SMC136.2.4     + SMC136.2.19    + SMC136.2.207                          Pli2012 
00279+2220   FRV   1     LP 345-25. Assuming a parallactic distance of 13.19 +/- 0.28 pc                 
                         (Gatewood & Coban 2009), Konopacky et al. (2010) derive a system mass   Gat2009 
                         of 0.121 +/- 0.009 Msun.                                                Kon2010 
                         Dupuy et al. (2010) determine system mass 0.120 +0.008/-0.007 Msun;             
                         spectral types are  M7.5 +/- 1.0  and M8.0 +1.5/-1.0.                   LiM2010b
00280-2654   LDS2123     DEA  22.                                                                        
00281-0001   HJ 1970     Designated as HJ 1972 in BDS.                                           Bu_1906 
00281-2512   B     5     AC = LDS2124                                                                    
00281-7329   OGL  23     SMC135.1.4464  + SMC138.3.12                                            Pli2012 
00282-1030   GAL 300     Object #18 in Gallo's original list.                                    Gal1912a
00283+6344   HU 1007     A premature orbit has been calculated. Motion direct.                   B__1963b
00283+1131   BPM  13     [PM2000]   19197 + [PM2000]   19238.                                    Gvr2010 
00283-7339   OGL  24     SMC138.4.5573  + SMC138.4.5757                                          Pli2012 
00283-7427   OGL  25     SMC139.3.2443  + SMC139.3.2445                                          Pli2012 
00284-2020   B  1909     Difficult visual system, with two components remaining within 0".2              
                         of each other throughout the orbit.                                             
                         Two orbit solutions (van den Bos 1956, Soedehjelm 1999). High-          B__1956b
                         eccentricity, half-period solution fits equally well but gives          Sod1999 
                         too high mass-sum (with no third component allowed by q).                       
                         1982.7657 autocorrelogram remeasured; new results listed in catalog.    McA1987b
                         Martin et al. (1998) derive component masses 1.563 +/- 0.177 and                
                         1.238 +/- 0.151 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.14 +/- 0.32, 2.15, and 1.05 Msun, respectively.             Mlk2012 
00287+5801   MLB 107     WDS changed from 00293+5800, BC pair merged with STI1355                        
00287+1502   ALP   3     2MASSI J0028394+150141                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
00288+5756   OSO   5     G217-052. No common proper motion pairs, based on comparison with               
                         POSS2 red plates.                                                       Oso2004 
00288+0251   HJ  623     C component is galaxy NGC 125.                                                  
00289+5023   DAE   1     GJ 3036 = G172-001                                                              
                         Daemgen et al. derive a distance of 17.4 +/- 4.5 pc, a separation of    Dae2007 
                         7.4 +/- 2.2 AU, and a predicted orbital period of 40 +19/-18 yr.                
                         Spectral types are M4.0 +/- 0.5 and M4.5 +/- 0.5; masses are 0.24               
                         +0.11/-0.07 and 0.19 +0.07/-0.05 Msub.                                          
00289+1835   BPM  14     [PM2000]   19589 + [PM2000]   19539.                                    Gvr2010 
00290-0933   GIC  10     G158-086/G158-087.                                                              
                         NLTT 1529/1530                                                          Chm2004 
00291+5752   MLB  39     STI 1359.                                                                       
00291-0742   MLR   2     Speckle measures show rapid motion.                                             
00292+7646   HJ 1967     Aka PKO  19.                                                                    
00293-0555   SHY 384     AB: HIP   2292 + HIP   2350.                                                    
             RAO   1     BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral            
                         types of B and C as G8V and M1V.                                        Rbr2015a
00293-7244   OGL  26     SMC136.2.2867  + SMC136.2.2890                                          Pli2012 
00295+1413   BPM  15     [PM2000]   20020 + [PM2000]   19943.                                    Gvr2010 
00296-2845   LDS2130     NLTT 1581/1580                                                          Chm2004 
00297+5548   MLB 150     STI1361.                                                                        
00300-0357   HJ  322     12 Cet.                                                                         
00300-1058   GAL 301     Object #19 in Gallo's original list.                                    Gal1912a
00300-1657   CHM   2     NLTT  1595 +  1598.                                                             
00300-6023   JSP 855     00301-6027TDS1494                                                               
00300-7257   OGL  27     SMC136.1.2934  + SMC136.1.3498                                          Pli2012 
00301+2945   BU 1095     28 And. A is a Delta Scuti-type variable, GN And.                               
00301-3740   DAY   1     2MASS J0030-3739 + 2MASS J0030-3740. Dwarf / white dwarf binary.                
                         Spectral types M9+/-1 + DA, Teff 2000-2400 + 7600+/-175K, masses                
                         0.07-0.08 + 0.48-0.65 Msun. Minimum age of the system > 1.94 Gyr.       Day2008 
00302+5929   STI  79     Historical measures of STI1363 match STI  79 and have been included.            
00304-0947   CHE  27     This pair has opened considerably since its discovery (from 9".6 to     Che1910 
                         19"), due to the considerable proper motion of the primary. AC2000              
                         coordinates of both components from ~1901 are in good agreement with            
                         Chevalier measure, so identification with this pair appears probable.   Hrt2012b
00305-7237   OGL  28     SMC136.3.2481  + SMC136.3.2710                                          Pli2012 
00306+4919   OL   86     Aka TDS1492.                                                                    
00306+1442   OSO   6     G032-026. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00306-7358   OGL  29     SMC133.7.1599  + SMC138.1.5656                                          Pli2012 
00306-7242   OGL  30     SMC136.3.2599  + SMC136.2.3059                                          Pli2012 
00307+3208   STT  11     B is BD+31@66.                                                                  
00307-1545   HJ 1979     J 1435.                                                                         
00310+3817   ALI 480     Also known as ES 2447.                                                          
00311+5648   ES    2     BDS 269 same star.                                                              
00311-7239   OGL  31     SMC131.6.14    + SMC131.6.859   + SMC136.4.2269                         Pli2012 
00312+0631   GWP  57     XMI 127.                                                                Tob2012b
00312-3041   LDS2132     NLTT 1669/1668                                                          Chm2004 
00312-6102   HJ 3372     CD-61@81.                                                                       
00313-7311   OGL  32     SMC130.6.354   + SMC130.5.916                                           Pli2012 
00314+3335   HJ 5451     STTA  2. A is a spectroscopic binary. B is BD+32@81.                            
                         HJL1004.                                                                HJL1986 
00314+0158   LDS 865     Also known as GWP  59 or XMI 128.                                       Tob2012b
00314-1113   GAL 302     Object #21 in Gallo's original list.                                    Gal1912a
00314-4848   RST  11     lam 1 Phe. A is a spectroscopic binary.                                         
00315-6257   B     7     A: bet 1 Tuc. A is a spectroscopic binary.                                      
             I   260     C: bet 2 Tuc                                                                    
                         bet 1,2,3 Tuc form a sextuple system with cpm.                                  
                         bet 3 Tuc (mag. 5.14, A2) is the close binary B     8.                          
             SHY 114     AE: HIP   2484 + HIP   2578.                                                    
             SHY 114     AF: HIP   2484 + HIP   2729.                                                    
             SHY 114     AG: HIP   2484 + HIP   1481.                                                    
             SHY 113     FG: HIP   2729 + HIP   1481.                                                    
             SHY 117     FH: HIP   2729 + HIP   1993.                                                    
             SHY 117     FI: HIP   2729 + HIP   1910.                                                    
             SHY 113     GH: HIP   1481 + HIP   1993.                                                    
00316+1344   LDS9091     Old LDS6091.                                                                    
00317+5057   LDS3175     Coordinate correction and estimate of secondary's proper motion by              
                         Caballero (2013, private comm.)                                                 
00318+5431   STT  12     lam Cas = 14 Cas. A premature orbit has been computed.                          
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Corrections to Drummond et al. (2014) orbit: P=245.70 +/- 35.96y,               
                         T0=2025.54 +/- 4.65 (Drummond, private comm.)                                   
00319+3705   BRT2584     ALI 248.                                                                        
00319-2750   LDS2134     NLTT 1711/1713                                                          Chm2004 
00319-7318   OGL  33     SMC130.6.16    + SMC130.6.13                                            Pli2012 
00320+1426   GRV 975     Aka SLW  29.                                                                    
00321+6715   MCY   1     Aa,Ab: Discovery designation is per Todd Henry 03/02/98.                        
                         K-band magnitudes of components 6.42 and 8.44, derived masses are               
                         0.377 +/= 0.030 and 0.138 +/- 0.007 Msun.                               Doc2008d
             VYS   2     AB: ADS 433, MLB 377. The primary is an astrometric binary, P=16y.              
                         Proper motion +1.723 -0.242. A premature orbit has been computed for            
                         the visible pair.                                                               
                         Also a flare star, V547 Cas.                                                    
                         Woitas et al. (2003) give orbital solution and determination of         Woi2003 
                         dynamical masses for this low-mass M dwarf triple.                              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Solution includes mass determination.                                   Woi2003 
                         In the orbit catalog figure illustrating the Docobo et al. (2006)       Doc2006g
                         orbital solution, B is plotted relative to the center of mass. These            
                         adjusted measures were provided by Docobo (2007, private comm.) See             
                         also further analysis by Docobo et al. (2008), who derive a mass for    Doc2008d
                         the B component (K-band mag 7.88) of 0.177 +/- 0.014 Msun (see note to          
                         MCY 1 pair above for masses of Aa and Ab components.)                           
             GL 22       Ba,Bb: Andrade & Docobo detect a sinusoidal pattern in the motion of            
                         the B component, which they attribute to a possible 4th component of            
                         the system in a 15y orbit.  Masses under this scenerio are 0.162 +/-            
                         0.014 Msun for Ba and 0.0152 +/- 0.0053 Msun (16.0 +/- 5.6 Mjup) for            
                         Bb (assuming a circular solution) or 0.0147 +/- 0.0027 Msun (15.4 +/-   Ana2009 
                         2.8 Mjup) for Bb (assuming an elliptical solution). The Bb component            
                         may be either a giant planet or a brown dwarf.                          Ana2011 
00321+0155   GWP  60     XMI 129.                                                                Tob2012b
00321-0511   A   111     Elongations and quadrant of AB doubtful.                                B__1963b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.48 +/- 0.34, 1.75, and 0.85 Msun, respectively.  Mlk2012 
00321-1218   HDS  71     Cvetkovic et al. (2014) derive spectral types G2 and  G5, masses 1.11           
                         and 1.05 Msun. Dynamical parallax is 14.06 +/- 0.62 mas.                Cve2014 
00322-1050   LDS3176     NLTT 1727/1715                                                          Chm2004 
00322-7515   HJ 3374     B is CPD-75@48.                                                                 
00323-6304   LDS9092     Old LDS6092.                                                                    
00324+7335   LDS1509     NLTT 1681/1680.                                                                 
00324+0657   MCA   1     51 Psc. A is a triple occultation system, and a resolved                        
                         interferometric pair. B is BD+06@65.                                            
                         First detected as an occultation binary by Africano.                    Afr1976 
                         Mason et al. give Aa,Ab,B triple solution (double (Aa)-B in HIP).       Msn1997a
                         Orbit mostly dependent on Hershey pc obs; more IR speckle needed.       Hry1973 
                         The Aa,Ab components of ADS 449 apparently went through periastron              
                         some time during 1987-1990.                                             Hrt1992b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.08 +/- 0.46, 3.66, and 2.40 Msun, respectively.  Mlk2012 
             STF  36     AB: H 4  70.                                                            MEv2010 
00325+0101   GWP  61     XMI 130. GRV1160.                                                       Tob2012b
00326+5513   RAS  17     SrCrEu star at about 36 pc. Secondary likely close to solar (G2-G5).    Ras2014 
00326+2018   HJ 1982     52 Psc.                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00327+7807   STF  34     HJL   6.                                                                HJL1986 
00327+0732   GWP  62     XMI 131.                                                                Tob2012b
00327-6302   B     8     Aa,Ab: bet 3 Tuc. CPM with bet 1 and bet 2 Tuc = B     7.                       
             SHY 116     AB: HIP   2578 + HIP   2729. B component = F component of 00315-6257.           
             SHY 116     AC: HIP   2578 + HIP   1993. C component = H component of 00315-6257.           
00328+2817   STT  14     A is a spectroscopic binary. Aka H N  76.                                       
00329-7445   OGL  34     SMC134.1.90    + SMC134.8.2266                                          Pli2012 
00330+4442   LDS9093     Old LDS6093.                                                                    
                         NLTT 1759/1762                                                          Chm2004 
00330+0850   J  2710     -9s, -5' from BD+08   69.  Declinaison augmentee de 2'.                 J__1955 
00330-7335   OGL  35     SMC130.8.5777  + SMC130.8.5810                                          Pli2012 
00331-7446   OGL  36     SMC134.1.223   + SMC134.1.542                                           Pli2012 
00332+1902   GWP  63     XMI 132.                                                                Tob2012b
00332-7114   OGL  37     SMC132.7.12    + SMC132.7.25                                            Pli2012 
00334+1418   LDS9094     Old LDS6094.                                                                    
00334-7104   OGL  38     SMC132.6.11    + SMC132.6.191                                           Pli2012 
00334-7407   OGL  39     SMC133.8.4148  + SMC133.1.95                                            Pli2012 
00335+4006   HO    3     A premature orbit has been computed.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.60 +/- 0.55, 2.07, and 1.10 Msun, respectively.             Mlk2012 
00336+1712   GWP  64     XMI 133.                                                                Tob2012b
00336-0811   LDS 5280    B component of 00339-0813 LDS5281 found to be the A component of                
                         LDS5280; pairs merged, with LDS5281 made AC pair (with quadrant flip).          
00337-3500   HJ 3375     HIP 2663. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
00339+1748   GWP  65     XMI 134.                                                                Tob2012b
00340-7056   OGL  40     SMC132.5.883   + SMC132.5.916                                           Pli2012 
00344-7252   OGL  41     SMC131.7.3527  + SMC131.7.4371                                          Pli2012 
00346+6254   BU  108     AB: B component is SB, P=156.430d                                       Tok2014d
00345-0433   STF  39     AB,C: H 4  76.                                                          MEv2010 
00346-7105   OGL  42     SMC132.6.1065  + SMC132.6.1159                                          Pli2012 
00349+2627   COU 548     Originally entered as AG   4.                                                   
00350+5636   ES    3     BDS 326 identical.                                                              
00351+8337   MLR 481     00356+8338HDS  80                                                               
00351+0209   RST5182     J 3281.                                                                         
00352-0336   HO  212     13 Cet.                                                                         
                         Visual primary is 2.1d SB1 (#27 in Batten et al., 1989) and may be a    Bte1989 
                         Delta Scuti-type variable.                                                      
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1979.5326: This measure was incorrectly attributed to ADS 2200          McA1982d
             BU  490     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
00353-0942   CHE  28     J  1437 = 00358-0942CHE  28                                                     
00356-7342   OGL  43     SMC133.4.124   + SMC133.4.3322                                          Pli2012 
00357+0233   LAW   7     LSPM J0035+0233 = NLTT 1930. Law et al (2008) derive a distance of      Law2008 
                         14.5 +6.3/-2.4 pc and a projected separation of 6.8 +3.1/-1.0 AU.               
                         Estimated spectral types are M5 and M6.0.                                       
00357-7055   OGL  44     SMC132.5.871   + SMC132.5.912   + SMC132.5.1085                         Pli2012 
00358+5241   GIC  11     G172-011/G217-059.                                                              
                         NLTT 1920/1921                                                          Chm2004 
00359-7429   OGL  45     SMC134.3.2988  + SMC134.3.3515                                          Pli2012 
00360+2959   STF  42     Hyperbolic orbit by Hopmann.                                            Hop1967 
                         sigma = areal constant in the true orbit = 0.1432 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 6".123                              
                         Hopmann made small but unspecified corrections to the node and                  
                         inclination before computing residuals and ephemeris.                   Fin1970b
                         All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                         A is a spectroscopic binary.                                                    
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00360+0514   GWP  66     XMI 135.                                                                Tob2012b
00360+1040   GWP  67     XMI 136.                                                                Tob2012b
00361+3858   J  2711     ALI 723.                                                                        
00364-7313   OGL  46     SMC130.3.8754  + SMC130.3.8886                                          Pli2012 
00365-0639   LDS3183     NLTT 1976/1977                                                          Chm2004 
00365-7246   OGL  47     SMC131.2.1420  + SMC126.6.896                                           Pli2012 
00366-4908   LDS  21     A is a spectroscopic binary, P = 3.74d. B is CD-49@138.                         
                         SHY 118. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         B component is SB, P=22d                                                Tok2006 
00366-7435   OGL  48     SMC134.2.2429  + SMC134.2.2618                                          Pli2012 
00367+1542   GWP  68     XMI 137.                                                                Tob2012b
00368+1605   KU   69     HJL   7.                                                                HJL1986 
00369+3343   H 5  17     pi And = 29 And.  H V 17. STTA  4.  BDS 263, HJ 1030 identical.                 
                         A is a spectroscopic binary, P = 143.6d. B is BD +32@102.                       
             MKT   1     Aa,Ab: Hummel et al. (1995) visual orbit is based on astrometry from    MkT1995 
                         the Mark III interferometer. Additional spectroscopic data yield                
                         masses, luminosities, radii, effective temperatures, and distance.              
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 11.98 +/- 2.06, 11.18, 4.79 Msun, respectively.    Mlk2012 
             RBR   3     Aa,Ac: PA for 2001.7424 observation is measured in zenith mode. If              
                         data collected in equatorial mode, PA = 97.6. Confirmation of the pair          
                         should establish the proper value for theta.                            Rbr2007 
00372+7149   HDS  86     1997.7289: Large change in separation seen since Hipparcos epoch.       Msn1999b
00373+5801   BU 1097     Spectrum composite; A2+K.                                                       
00373-2446   BU  395     Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         HIP 2941. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.79 +/- 0.29, 1.92, and 0.91 Msun, respectively.             Mlk2012 
00374-2054   FAR  23     GJ 2010 = NLTT 2019. Primary is white dwarf WD 0034-211.                Far2006 
00374-3717   I   705     Many attempts, but only a few positive observations.                            
00374-3904   WHI   1     Other IDs uncertain; based on Simbad search using epoch-1950                    
                         coordinates 003456-392028 from White et al. (1991).                     Whi1991 
00374-7243   OGL  49     SMC131.3.3943  + SMC131.3.4041                                          Pli2012 
00376+1257   GWP  69     XMI 138.                                                                Tob2012b
00376+1547   GWP  70     XMI 139.                                                                Tob2012b
00378-7246   OGL  50     SMC131.2.5591  + SMC131.2.6860                                          Pli2012 
00378-7413   OGL  51     SMC128.8.65    + SMC128.8.358                                           Pli2012 
00379+1404   GWP  71     XMI 140. GRV1161.                                                       Tob2012b
00379-7256   OGL  52     SMC131.1.6657  + SMC126.7.785                                           Pli2012 
00381-7127   OGL  53     SMC132.1.1336  + SMC132.1.1337                                          Pli2012 
00381-7345   OGL  54     SMC128.5.115   + SMC128.5.276   + SMC128.7.9551                         Pli2012 
00382+0322   J  1042     BAL 1609.                                                                       
00383-7124   OGL  55     SMC132.1.1263  + SMC132.1.1284                                          Pli2012 
00384+0130   BAL 947     Probably ARG 47, BD+00@93.                                                      
00385+4300   LDS5176     old LDS6095.                                                                    
                         NLTT 2053/2057                                                          Chm2004 
00386+4738   OSO   7     G172-016. Common proper motion pair                                     Oso2004 
00386+1420   GWP  72     XMI 141.                                                                Tob2012b
00386-2118   LDS2140     NLTT 2075/2062                                                          Chm2004 
00386-3903   WHI   2     Other IDs uncertain; based on Simbad search using epoch-1950                    
                         coordinates 003609-391934 from White et al. (1991), where pair is       Whi1991 
                         listed as possibly resolved.                                                    
00387-7431   OGL  56     SMC129.7.14    + SMC129.7.603                                           Pli2012 
00388+3101   AG  430     B is BD+30@90.                                                                  
                         Not confirmed using images from the Digitized Sky Surveys               Oso2004 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00388-2506   HJ 1991     B is CD-25@235.                                                                 
00389-2536   HJ 1992     B is CD-26@195.                                                                 
00389-7248   OGL  57     SMC126.7.3     + SMC126.7.86                                            Pli2012 
00391-7313   OGL  58     SMC125.6.23680 + SMC125.6.24279                                         Pli2012 
00392+1329   GWP  73     XMI 142.                                                                Tob2012b
00393+3052   BU  491     del And = 31 And                                                                
                         A is a long-period spectroscopic binary, P = 15000d (?).                        
             BTM   1     Aa,Ab: Bottom et al. (2015) resolve the spectroscopic binary del And            
                         using the Palomar 5m and Stellar Double Coronograph. The physical               
                         separation is 11.55 +/- 0.13 AU; the spectral type of the companion is          
                         estimated at K4 +/- 2.                                                  Btm2015 
                         Aa,Ab: Gontcharov & Kiyaeva (2002) orbit based on combination of        Gon2002b
                         ground-based catalogs with Hipparcos. They quote masses of 1.3+/-0.4            
                         and 1.3 Msun for the two components, and estimate their spectral types          
                         as K3III and white dwarf.                                                       
00394+2115   STT 550     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             LUH   3     54 Psc. AC: Common proper motion for both components was determined             
                         through comparison of relative location with that obtained by 2MASS.            
                         The B component is determined to be a possible T dwarf (T7.5 +/- 0.5)           
                         based on mid-IR colors and magnitudes. Age is determined to be 7 +/-            
                         3 Gyr and mass of C component 0.051 +/- 0.014 Msun.                     Luh2007 
                         The T dwarf is referred to by Luhman et al. as the "B" component,               
                         either because the non-physical STT 550 was not considered, or the WDS          
                         was not consulted. In any event, this component referred to in the WDS          
                         hierarchy as "C" is sometimes called "B" in the literature.                     
00395+6151   STI 110     00394+6158MLB 378                                                               
00395+6002   HJ 1042     STI 111.                                                                        
00395+1454   GIC  12     AB: LDS 868 = G032-037/G032-038.                                                
                         NLTT 2126/2125                                                          Chm2004 
             JNN 249     Ba,Bb: G 32-37B. Estimated age 300-1000 Myr; masses 0.33 +/- 0.03 and           
                         0.19 +/- 0.01 Msun; a ~4.3 AU.                                          Jnn2014 
00396+8445   HJ 1986     STTA  3. B is BD+83@11.                                                         
00398+6157   LAM   1     MLB 379. STI 114AC.                                                             
                         BDS notes AB measure 357deg, 69".87 - Burnham was unable to find any            
                         pair that matched this separation - perhaps typo for 6".98?                     
             STI 113     BD: Previously 00399+6158STI 113AB.                                             
00398-1418   GAL 303     Object #23 in Gallo's original list.                                    Gal1912a
00399+2126   STF  46     55 Psc.                                                                         
00400+7652   STTA  5     B is BD+76@16.                                                                  
00400+1336   BPM  16     [PM2000]   26418 + [PM2000]   26431.                                    Gvr2010 
00400+0106   GWP  74     XMI 143.                                                                Tob2012b
00401+5014   V523 Cas    Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.130 Msun and the minimum             
                         mass of the wider component at 0.31 Msun.                                       
00403+2403   BU 1348     AC : Carries BU 1348 from ADS (562), despite earlier discovery by STF.          
                         BC : AD equated with this component.                                            
00403-0855   GAL 304     Object #24 in Gallo's original list.                                    Gal1912a
                         Also known as FAB   3.                                                          
00403-7241   OGL  59     SMC126.6.564   + SMC126.6.565                                           Pli2012 
00404+0722   OSO   8     G001-012. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00405+5632   BU 1349     alp Cas = 18 Cas = Schedar                                                      
             H 5  18     AD: H V 18. Also HJ 1993.                                                       
                         AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00405-1631   BU  109     B is BD-17@108.                                                                 
00405-4829   LDS9096     Old LDS6096.                                                                    
00405-7321   OGL  60     SMC125.7.29221 + SMC125.7.29234                                         Pli2012 
00406-0023   ARG  48     BAL 646.                                                                        
00406-1502   GAL 305     Object #26 in Gallo's original list.                                    Gal1912a
00407-0421   HJ  323     B is BD-05@100.                                                                 
00408+1618   GWP  76     XMI 144.                                                                Tob2012b
00408-7125   OGL  61     SMC127.8.10    + SMC127.8.21                                            Pli2012 
00409+0810   GWP  77     XMI 145.                                                                Tob2012b
00409-7320   OGL  62     SMC125.7.29414 + SMC125.7.30547                                         Pli2012 
00410+3257   SEI   8     Listed in ADS as both #565 and #580 (00420+3304POT   8)                         
00414-7124   OGL  63     SMC127.8.1547  + SMC127.8.2057  + SMC127.8.2076                         Pli2012 
00415+5550   GIC  13     G218-007/G218-008 = GJ 1015AB.                                                  
00416+2438   WRH  28     Hynek 1. Not certainly resolved by Wilson in 1949, but successfully             
                         resolved by McAlister in 1980.                                                  
                         1983.9362: this (and presumably other) negative results may be due              
                         to a delta m between 1.5 and 3.                                         Bnu1984 
00416-0934   GRV1162     SLW  36.                                                                        
00416-5621   RNR   1     2MASS J0041353-562112. Spectral types M6.5 +/- 1 and M9.0 +/- 1.                
                         Assuming age of ~10 Myr, component masses are ~30 and ~15 Mjup;                 
                         distance 50 +21/-10 pc, orbital period 126 +86/-37y.                    Rnr2010 
00417-4729   LDS9097     Old LDS6097.                                                                    
00417-7102   OGL  64     SMC127.6.1579  + SMC127.6.1681                                          Pli2012 
00418-5630   HJ 3387     xi Phe. Variable.                                                               
00419+1751   A  2303     J 585.                                                                          
00419+1341   JMS   1     BDK   3. NLTT 2274 + 2MASS J00415453+1341351. Distance 21 +/- 8 pc for          
                         the primary, 31 +/- 6 pc for the secondary. Estimated age of system             
                         4.5-8 Gyr. Mass of secondary estimated at 0.081-0.083 Msun.             Fah2010 
                         NLTT 2274 + 2MASS J00415453+1341351. Baron et al. (2015) estimate               
                         spectral types M4.0 +/- 0.5 and M9.5 +/- 0.5, distances 23 +14/-9 and           
                         40 +6/-12 pc, masses 0.207-0.272 and 0.076-0.083 Msun.                  BFr2015 
00420-7306   OGL  65     SMC125.5.32790 + SMC125.5.33233                                         Pli2012 
00422-7435   OGL  66     SMC129.2.448   + SMC129.2.992                                           Pli2012 
00424+1721   BPM  17     [PM2000]   27917 + [PM2000]   27832.                                    Gvr2010 
00424+0410   STT  18     AB: Visual orbit (Grade 4) gives too large mass sum of 52 Msun.         Tok2014d
00426-5407   HJ 3388     B is CPD-54@159.                                                                
00427-3828   HDO 182     lam 1 Scl                                                                       
00427-6537   I   440     Probable rapid motion, as yet undefined by the measures.                        
                         Derived orbital parallax 0".00685, mass sum 4.91 +/- 2.94 Msun          Lin2004a
00427-7409   OGL  67     SMC128.1.11    + SMC128.1.217                                           Pli2012 
00428+3533   TOK  10     FF And. Primary is 2.2d SB2. Estimated period of visual pair 4400y.             
                         G-solution in HIPPARCOS.                                                Tok2006 
                         This system is noted as being triple in Tokovinin et al. (2006),        Tok2006 
                         including a close spectroscopic binary pair with approximately 1.3 mas          
                         separation and a likely wider companion at 11" separation. Due to               
                         these separations however, it is counted as single for our purposes.    Jnn2012 
00429+2047   A  2205     A premature orbit has been calculated.                                          
00431+3913   MLB1054     ALI 727.                                                                        
00431+0707   OSO   9     G001-013. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates                                                        Oso2004 
00432+0128   GWP  80     XMI 146.                                                                Tob2012b
00432-2146   LDS1078     SLW  39.                                                                        
00432-3759   UC  427     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                         Spectral type of comoving secondary estimated as M0-1, mass 0.56 Msun.  Mug2014 
00434-0054   STF  53     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00434-5728   HJ 3391     eta Phe.                                                                        
             MRN   1     Aa,Ab: Marion et al. (2014) estimate the companion as K1V, at about             
                         6.8AU separation from the A0IV primary. They derive a minimum orbital           
                         period of ~9.5y, consistent with an astrometric companion reported by           
                         Makarov & Kaplan (2005). A followup K-band observation suggests         Mkr2005 
                         spectral type for the secondary of ~G5V.                                Mrn2014 
00435+3351   BUP 241     AB: B is BD+32@120.                                                             
             WEI  46     AC: Distances are 1321" and 1310".                                              
00436-2354   LDS2147     NLTT 2383/2381                                                          Chm2004 
00437+7211   OSO  10     G242-065. Neither is a common proper motion pair, based on comparison           
                         with POSS2 red plates                                                   Oso2004 
00439+0946   J  2712     Not found by Heintz at IDS position.                                    Hei1990b
00441+5655   MLR 625     Also known as TDS1589.                                                          
00441-7238   OGL  68     SMC126.3.2852  + SMC126.3.910                                           Pli2012 
00442+3122   GRV  40     Aka HJL1007                                                                     
00442+4614   STF  52     Primary is eclipsing binary V355 And (period 4.7184 day).               Zas2010 
00443-7439   OGL  69     SMC129.2.3173  + SMC129.1.2349                                          Pli2012 
00444+3332   STF  54     STF  56.                                                                        
00444+1235   HJ    6     AG 7.                                                                           
00445-1715   B  2513     Probably BD-18@118.                                                             
00445-3607   B   640     Primary is CR Scl, eclipsing binary of W UMa-type, period 0.246537d.    Zas2013 
00446+4341   LDS5177     old LDS6098.                                                                    
00446+2007   GWP  84     XMI 147.                                                                Tob2012b
00446-1856   LDS3195     AC: NLTT 2439/2437                                                      Chm2004 
00447+4817   BU  231     omi Cas = 22 Cas                                                                
                         Primary is a spectroscopic binary, P = 1033:d.                                  
             NOI   3     Aa,Ab: Hipparcos astrometric solution adopted some elements from the    HIP1997d
                         orbit of Abt & Levy (1978).                                             AbH1978 
                         Koubsky et al. (2010) combined solution uses NPOI astrometric data      NOI2010 
                         together with radial velocities from the Dominion Astrophysical and             
                         Ondrejov Observatories. The secondary appears to be of similar mass to          
                         the primary, although the magnitude difference is nearly 3 magnitudes.          
                         One possible explanation might be that the secondary is comprised of a          
                         close pair of similar stars, possible early A dwarfs.                           
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 6.12 +/- 2.94, 7.39, and 5.62 Msun, respectively.  Mlk2012 
00448+4202   LDS5178     old LDS6099.                                                                    
00448+3940   ALI1011     MLB 810.                                                                        
00450-7234   OGL  70     SMC126.4.9807  + SMC126.4.10299 + SMC126.4.10283                        Pli2012 
00451+0533   PLQ   8     BAL2993.                                                                        
                         HJL   8.                                                                HJL1986 
00451-7310   OGL  71     SMC125.4.14538 + SMC125.4.14830                                         Pli2012 
00452+0015   LDS 836     AB: Primary is SB1, P=11.439d (Griffin 2002 Obs 121, 221).              Tok2014d
00453+1019   STF  58     B is BD+09@85.                                                                  
00454+1422   LDS1079     G032-046. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
00454-7413   OGL  72     SMC128.1.8607  + SMC128.1.10178                                         Pli2012 
00455-1253   BUP   8     18 Cet.                                                                         
00456-7115   OGL  73     SMC127.2.1735  + SMC127.1.582                                           Pli2012 
00456-7331   OGL  74     SMC125.1.37411 + SMC125.1.37410                                         Pli2012 
00457+7459   H N 122     A: 21 Cas = YZ Cas                                                              
                         A is an Algol-type eclipsing and spectroscopic binary, P = 4.47d.               
00457-1625   MLF   1     aka HO  624                                                                     
00457-3510   LDS3191     LDS5294                                                                         
00457-7401   OGL  75     SMC128.2.9138  + SMC128.2.10100                                         Pli2012 
00458+5459   ARG   2     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00458-4733   HDO 183     AB: PMS star, X-ray source, rapid rotation, debris disk.                Tok2014d
00458-7242   OGL  76     SMC126.3.12924 + SMC126.3.13758                                         Pli2012 
00459+3347   LAW   8     LSPM J0045+3347 = NLTT 2511. Law et al (2008) derive a distance of      Law2008 
                         14.9 +7.0/-2.6 pc and a projected separation of 4.0 +2.1/-0.6 AU.               
                         Estimated spectral types are M4.5 and M5.5.                                     
00459-7359   OGL  77     SMC128.2.9204  + SMC128.2.11627                                         Pli2012 
00460+3626   HJ  627     ALI 22.                                                                         
00460-7108   OGL  78     SMC127.3.1324  + SMC127.2.2113                                          Pli2012 
00461-0539   LDS3199     NLTT 2540/2538                                                          Chm2004 
00462-7250   OGL  79     SMC126.2.15522 + SMC126.2.15521                                         Pli2012 
00463+6517   HJ 1052     STI 124.                                                                        
00463-0634   HDS 101     Cvetkovic et al. (2016) estimate spectral types F2 and F9, masses 1.56          
                         and 1.20 Msun. Dynamical parallax is 9.22 +/- 1.22 mas.                 Cve2016b
00464+3057   STFA  1     STTA  6. B is BD+30@114.                                                        
                         H 5 123.                                                                MEv2010 
00464-7332   OGL  80     SMC103.5.132   + SMC103.5.864                                           Pli2012 
00466-7334   OGL  81     SMC103.5.4     + SMC103.5.25                                            Pli2012 
00467+1335   BPM  18     [PM2000]   30523 + [PM2000]   30577.                                    Gvr2010 
00467-0426   LDS9100     Old LDS6100.                                                                    
                         NLTT 2582/2586                                                          Chm2004 
00467-7228   OGL  82     SMC101.6.16943 + SMC101.6.16996                                         Pli2012 
00468-5200   HJ 3398     B is CPD-52@91.                                                                 
00469+0533   GWP  86     XMI 148.                                                                Tob2012b
00470+3848   ES  223     00471+3848ALI 729                                                               
00470-1152   CUD   1     AB: Component A is the central star of the planetary nebula NGC 246.    Skf2013 
                         Adam & Mugrauer (2014) estimate spectral type of B component as K2-K5,          
                         mass 0.85 Msun.                                                         Ada2014 
             ADA   1     AC: Adam & Mugrauer (2014) detect an additional companion to the white          
                         dwarf primary. Estimated spectral type is M5-M6, mass 0.1 Msun. All             
                         components share common proper motion.                                  Ada2014 
00471+3800   J  2713     ALI 485.                                                                        
00471-7304   OGL  83     SMC100.6.7164  + SMC100.6.7261                                          Pli2012 
00473+2416   BUP   9     AB: zet And. A is an eclipsing and spectroscopic binary, P = 17.8d.             
                         AC is probably optical.                                                         
                         Proper motion +758 -1146.                                                       
00474+5106   H 5  82     H V 82. STTA  7. B is BD+50@142.                                                
00474+3314   BOW   1     Not found by Heintz at IDS position.                                    Hei1990b
00474+1730   BPM  20     [PM2000]   30911 + [PM2000]   30961.                                    Gvr2010 
00474+1726   BPM  19     [PM2000]   30878 + [PM2000]   30861.                                    Gvr2010 
00474-7345   OGL  84     SMC103.7.16909 + SMC128.5.14891                                         Pli2012 
00476+5533   TDS1614     WDS designation changed slightly when merged with STI1428 into triple           
00476-1812   LDS9101     Old LDS6101.                                                                    
00477+1253   STTA  8     LDS2796. B is BD+12@90.                                                         
                         AB: HJL   9.                                                            HJL1986 
00479-2921   I   261     Rapid, but as yet undefined, motion.                                            
                         1989.9437: Having had only one other measure in the last 35 years,              
                         this pair needs further observation, especially since we appear to be           
                         near periastron at this epoch.                                                  
00480+5127   STF  59     AB: H 1  40.                                                            MEv2010 
00481-7234   OGL  85     SMC101.7.31055 + SMC101.5.77                                            Pli2012 
00481-7348   OGL  86     SMC103.7.20241 + SMC103.7.6961  + SMC103.7.7536                         Pli2012 
00482+1737   GWP  87     XMI 149.                                                                Tob2012b
00482+1055   DAM 864     CD: GII 108.                                                                    
00484+0517   HEI 202     The AB pair was seen on two photographic plates by Heintz, but the              
                         companion was not visible on 164 other plates, nor was it seen on               
                         repeated checks with a micrometer. The parallax plates also yield               
                         large residuals, leading Heintz to suspect variability.                 Hei1984i
00486-2357   LDS  27     NLTT 2704/2705                                                          Chm2004 
00487+4619   SMA  10     A 1-deg error in WDS designation, apparently a typo in transcribing             
                         coordinates from the original source.                                           
00487+1841   BU  495     Hipparcos parallax of 0".01628 yields a mass sum of 2.14 Msun                   
                         with an uncertainty of 28%, agreeing well for a double star of                  
                         spectral type G0. The dynamical parallax is 0".0149, in reasonable              
                         agreement with the measured one. Semi-major axis erroneously given              
                         as 0.317; a = 0.617 matches Scardia's figure, so is assumed to be               
                         the intended value.                                                     Sca2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.00 +/- 0.67, 2.30, and 1.05 Msun, respectively.             Mlk2012 
                         Quadruple system. The inner AB pair, BU 495, has an orbit with a 143.6          
                         +/- 4.0 yr period (Scardia et al. 2000). The CPM component C at 152"    Sca2000b
                         from AB was found by Tokovinin & Lepine (2012), who estimate the        Tok2012c
                         probability of it being physical as 0.99. The component C was resolved          
                         by Riddle et al. (2015) into a 0".67 pair Ca,Cb. The PM is too small    RAO2015 
                         to determine if the Ca and Cb share common PM, but the low density of           
                         background stars and the small separation imply that the pair Ca,Cb is          
                         physical.                                                               Rbr2015d
00487+0735   BUP  11     del Psc = 63 Psc                                                                
00489-7434   OGL  87     SMC104.8.5148  + SMC129.2.824                                           Pli2012 
00490+4435   MCT   2     Initially entered into WDS incorrectly as 00490+5535.                           
                         GJ 3058. Estimated age 50-150 Myr; masses 0.22 +/- 0.10 and 0.18 +/-            
                         0.08 Msun; a ~19.0 AU.                                                  Jnn2014 
00490+1656   BUP  12     64 Psc. A is a spectroscopic binary.                                            
             64 Psc      Combined spectroscopic/interferometric solution by Boden et al. (1999)  Bod1999b
                         yields P=13.824621 days, T=JD 2450905.984.                                      
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.51 +/- 5.01, 2.80, and 1.10 Msun, respectively.  Mlk2012 
00491+5749   STF  60     eta Cas = 24 Cas. Proper motion of A +1141 -572. PM of B = +1105 -493.          
                         A has been reported to be a                                             Dob1927 
                         spectroscopic binary, but this is not confirmed. Doberck, Pavel, and    Pav1914 
                         Harshaw measure attributed to BC, then later to BE, was actually to     Hsw2004 
                         another faint star; confusion was due to the high proper motion of the          
                         B component and the long time span since the previous measurement.              
                         Proper Motion of E -003-001, F -010+000, G +009-005, H -006-001                 
                         System has been discussed by van de Kamp & Flather.                     Kam1955 
                         AB: H 3   3.                                                            MEv2010 
                         AB: Additional notes may be found in Simonov (1937).                    Smw1937 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.58 +/- 0.85, 1.71, and 1.60 Msun, respectively.  Mlk2012 
                         AB: Raghavan et al. (2010) do not accept the astrometric sub-system as  Rag2010 
                         real.                                                                   Tok2014d
00492+5720   A   921     Star C (mag. 14, 4.5") is probably physical.                                    
00494-7401   OGL  88     SMC103.8.8139  + SMC103.8.8451                                          Pli2012 
00496-5410   HJ 3402     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00497-1841   B  2067     Primary is Hipparcos acceleration solution (G-code) binary. Is the              
                         acceleration caused by the companion, or is it a triple?  Companion             
                         not measured by HIP, could cause false acceleration? 2MASS: another             
                         companion at 6.6", 276.2deg is listed, likely bogus.                    Tok2014d
00497-7336   OGL  89     SMC103.6.31460 + SMC103.6.31513                                         Pli2012 
00498+7027   ENG   2     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00499+3027   STTA  9     B is BD+29@139.                                                                 
00499+2743   STF  61     65 Psc = i Psc                                                                  
                         H 2  84.                                                                MEv2010 
00500-0401   RST4158     J 1440.                                                                 J__1941a
00501+1606   GWP  88     XMI 150.                                                                Tob2012b
00502+1604   GWP  89     XMI 151.                                                                Tob2012b
00502-7147   OGL  90     SMC102.4.11    + SMC102.4.92                                            Pli2012 
00503+6235   MRI  32     FMR  35.                                                                        
00503-7217   OGL  91     SMC101.4.18707 + SMC101.4.18866                                         Pli2012 
00504+5038   BU  232     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.83 +/- 2.67, 2.70, and 1.20 Msun, respectively.  Mlk2012 
00505+7538   HJ 1997     B is BD+74@31.                                                                  
00505+5930   LDS9102     Old LDS6102.                                                                    
00505+2450   LDS3203     NLTT 2805/2804                                                          Chm2004 
00506-7328   RSS   2     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
00507+6415   MCA   2     A spectroscopic binary and resolved interferometric pair. Composite             
                         spectrum: B9.5V+G0III-IV.                                                       
                         Combined spectroscopic/visual solution by Mason et al. (1997).          Msn1997b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.12 +/- 1.74, 8.22, and 2.40 Msun, respectively.             Mlk2012 
00508+5123   OSO  11     G172-024. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates.                                                       Oso2004 
00508+3203   A   922     No observations 1932-69. Apparently has completed nearly a revolution.          
00509+1215   GWP  91     XMI 152.                                                                Tob2012b
00511+2231   AZC   7     BC measure of 00511+2236LDS3204 now with this pair and decoupled with           
                         the former LDS3204AB.                                                           
00511-7204   OGL  92     SMC102.2.129   + SMC102.2.1604                                          Pli2012 
00512+2211   KU   70     motion direct.                                                                  
00513+5840   GIC  14     G218-015/G218-016.                                                              
00513-7413   OGL  93     SMC104.3.46    + SMC104.3.1506                                          Pli2012 
00515+5630   DAL  11     RoboAO: 2 faint companions near B at 16.7" and 15.0", likely optical.   RAO2015 
                         Star in cluster IC 1590 (NGC 281 nebula)                                Tok2014d
00515-7225   OGL  94     SMC101.3.29657 + SMC101.4.5258  + SMC101.3.30856                        Pli2012 
00516+4412   YR   19     Aa,B: These observations were previously presented in Horch et al       Hor2009 
                         (2009, 2010). The data presented here are the result of a reanalysis    Hor2010 
                         using a trinary fit to include the close component YR 123Aa,Ab,                 
                         although the Aa,Ab component was not always of high enough quality to           
                         include. In the course of reanalyzing these observations, it was also           
                         noticed that the magnitude differences appearing in Horch et al (2011)          
                         for the two filters shown were reversed. The values here correct that           
                         error.                                                                  Hor2011b
00516+2237   A  1808     Orbits with periods around 110y and a ~0.13" have been computed.                
                         Motion direct.                                                                  
                         Omega for Docobo (1988) solution corrected from 322.8 to 332.8          Doc1988b
                         degrees.                                                                Ruy1995 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.31 +/- 1.64, 5.27, and 2.88 Msun, respectively.             Mlk2012 
00516+0735   GWP  93     XMI 153.                                                                Tob2012b
00516-7354   OGL  95     SMC103.1.11891 + SMC103.1.11996                                         Pli2012 
00517-1600   GWP  94     ABL  82.                                                                Tob2012b
00519+3750   GIC  15     G132-035/G132-036.                                                              
00519-1553   GWP  95     ABL  83.                                                                Tob2012b
00519-5921   HJ 3404     LDS  28.                                                                        
00520+3353   HJ  628     Possibly the same a STF  66 with an error of 2 deg in dec.                      
00520+2035   GIC  16     G069-027/G069-029.                                                              
00521-1925   RSS  44     CPD-20@105                                                                      
00522-2237   STN   3     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00523-7252   OGL  96     SMC100.4.53934 + SMC100.4.11604                                         Pli2012 
00523-7350   OGL  97     SMC103.2.6804  + SMC103.2.6864                                          Pli2012 
00524-6930   DUN   2     lam 1 Tuc. B is CPD-70@38.                                                      
                         SHY 390. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Both A and B are above MS by 2 mag! The parallax can't be wrong.        Tok2014d
00527-2400   BU  734     A is a spectroscopic binary.                                                    
00528+5638   BU    1     This is a trapezium system (Abt 1986) which lies at the center of the   AbH1986 
             ABH   5     cluster IC 1590 at a distance of 2.94 +/- 0.15 kpc (Guetter & Turner            
                         1997 AJ 113, 2116).  All four components were observed and appeared to          
                         be single.                                                              Msn1998a
             BU    1     AD: HJL  10.                                                            HJL1986 
00528+0111   LDS9104     Old LDS6104.                                                                    
00528-7308   OGL  98     SMC100.3.19805 + SMC100.3.19803                                         Pli2012 
00529-0038   LDS  29     NLTT 2925/2926                                                          Chm2004 
00529-0856   LDS3208     NLTT 2931/2928                                                          Chm2004 
00531+6107   BU  497     A is a spectroscopic binary.                                                    
00533+0405   A  2307     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.12 +/- 2.18, 3.24, and 1.40 Msun, respectively.             Mlk2012 
00534-4114   CPO  24     LDS  30.                                                                        
00535+2536   BRT 119     00535+2537POU  73                                                               
                         Primary an eclipsing binary of W UMa-type, period 0.345575 day.         Zas2013 
00535-0041   TOB 359     Pair found when 00536-0039HDO  38 misidentified.                        Dam2015c
00536-0039   HDO  38     Primary is galaxy LEDA 1137438.                                                 
00537+1758   GWP  97     XMI 154.                                                                Tob2012b
00537-7236   OGL  99     SMC101.2.48111 + SMC105.6.27571                                         Pli2012 
00540-2503   HJ 3407     B is CD-25@344, spectrum F2V.                                                   
00541+2615   LDS3210     NLTT 2989/2990                                                          Chm2004 
00543-7358   OGL 100     SMC107.7.2     + SMC107.7.62                                            Pli2012 
00545+5619   CTT   2     B component is BD+55@196.                                                       
00545-7230   OGL 101     SMC105.5.24224 + SMC105.5.24308 + SMC105.5.25393                        Pli2012 
00546+3910   STF  72     B is BD+38@139.                                                                 
00546+1911   STT  20     66 Psc.                                                                 Wor1956b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.70 +/- 1.01, 4.39, and 2.57 Msun, respectively.  Mlk2012 
00547-6558   LDS9105     Old LDS6105.                                                                    
00547-7129   OGL 102     SMC109.6.11    + SMC109.6.145                                           Pli2012 
00547-7229   OGL 103     SMC105.5.24345 + SMC105.5.160                                           Pli2012 
00548+0857   GWP 100     XMI 155.                                                                Tob2012b
00548-6727   GLI   7     B is CPD-68@33.                                                                 
00548-7303   OGL 104     SMC106.5.28410 + SMC106.5.28476                                         Pli2012 
00548-7358   OGL 105     SMC107.7.205   + SMC107.7.460                                           Pli2012 
00550+5858   BU 1098     ups 1 Cas = 26 Cas                                                              
00550+2406   ENG   3     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
00550+2338   STF  73     36 And.                                     One component is                    
                         variable. A combined photometric/polarimetric/speckle spectroscopic             
                         analysis of this system was made by Tamazian et al.                     Tam2000 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Subgiant stars, spectral types G6 and K6. Calculated mass sum is 1.86           
                         +/- 0.15 Msun, in reasonably agreement with these classifications.      Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.86 +/- 0.14, 2.29, and 1.35 Msun, respectively.  Mlk2012 
             FOX 115     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
00552-4724   CD-48  216  HD 5388 was known to have a companion thought to be a planet candidate          
                         of minimium mass M sin i = 1.96 Mjup. Sahlmann et al. (2011) derive a           
                         combined astrometric/spectroscopic orbit, using values of P,e,T, and            
                         omega from the spectroscopic orbit of Santos et al. (2010 A&A 512,              
                         A47). They determine the orbit is nearly face-on, yielding an                   
                         estimated mass for the companion of  69 +/- 20 Mjup. Thus it can no             
                         longer be considered a planet.                                          SaJ2011b
00552-7401   OGL 106     SMC107.7.14    + SMC107.7.241                                           Pli2012 
00553-7318   OGL 107     SMC106.6.7246  + SMC106.6.7641                                          Pli2012 
00554+4611   ES 1298     The angle for 1914 has been increased 100 degrees.                              
                         The 1914 Espin measure is probably in error by 100deg.                  Cou1955c
00554+1545   LDS2801     LDS3212.                                                                        
00554+1253   GWP 103     XMI 156.                                                                Tob2012b
00556-4316   CBL 115     May be the omitted CPO  25.                                                     
00557+5748   ES  405     Motion for component B relative to A reflects the proper motion of A            
                         to within the errors. Therefore, in spite of the fact the small proper          
                         motions of these two components are similar, we consider their                  
                         physical relationship to be in doubt.                                   Kiy2012 
00557-7145   OGL 108     SMC109.8.11703 + SMC109.8.11918                                         Pli2012 
00558-1832   B   645     Probable rapid motion, but little observed.                                     
00560-7155   OGL 109     SMC108.5.26777 + SMC108.5.26787                                         Pli2012 
00561-8237   WHI   3     Possibly resolved                                                       Whi1991 
00564+0548   GWP 105     XMI 157.                                                                Tob2012b
00565+5928   ES 1709     STI 95 is identical                                                     Hei1983a
00566+1040   STF  76     ET Psc, W Uma (EW) type eclipsing binary, P = 0.439298 d.               Zas2011 
00566-1614   HJ 2002     Evidently a mistake in position angle by Herschel (HJ).                         
00566-5633   LPO   1     Spectral type G5?                                                               
00567+6043   BU 1028     gam Cas = 27 Cas                                                                
                         A is nova-like variable. Photocentric motion of (probably) the Aa pair          
                         detected by Gontcharov et al.                                           Gon2001 
                         1975.636: Disk unresolved in H alpha emission and H beta.               Bla1977a
                         Very small relative motion of B despite the high proper motion of A             
                         reveals this as a common proper motion companion.                               
00568+6022   BU 1099     Theta for 1979.7703 incorrectly given as 308.6 in McAlister & Hendry    McA1982d
                         (1982). Also, the measure for 1979.7730 was a spurious preliminary              
                         measure of the observation on 1979.7703, and has been deleted.                  
             BAG  10     Aa,Ab: The primary is 4.24d SB2 (Young, Pub DAO Victoria 1, 287, 1921;          
                         F.C. Fekel, personal comm.). HR  266.                                           
                         Astrometric binary (P=4.85yr) discovered in residuals to speckle                
                         data for 83-year AB pair (Cole et al. 1992), as well as in residuals    CWA1992 
                         to SB orbit.                                                                    
00568+3830   HJ 1057     mu And = 37 And                                                                 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
00568+1525   GWP 106     XMI 158.                                                                Tob2012b
00568-7210   OGL 110     SMC108.7.49889 + SMC108.7.49890                                         Pli2012 
00569+6152   HJ 1056     Aka STI 149.                                                                    
00570+5729   ES   44     Not the same as 00591+5729STI1500                                               
00570-7315   OGL 111     SMC106.6.41340 + SMC106.6.16701 + SMC106.6.15030                        Pli2012 
00572+2325   FOX 116     eta And = 38 And. A is a spectroscopic binary, P = 115.7d.                      
             MKT   2     Hummel et al. (1993) orbital elements were derived from Mark III        MkT1993b
                         interferometer astrometry. Combined with spectroscopy by Gordon (1946           
                         ApJ, 103, 13) to yield masses and distance.                                     
                         Errors are given as "error ellipses"; these values are tabulated                
                         below. Columns include date (BY), major and minor axes of the ellipse           
                         (mas), and ellipse orientation (deg):                                           
                              1990.5359     0.57     0.04     107.1                                      
                              1990.5687     0.12     0.02     105.8                                      
                              1990.5742     0.17     0.02     105.2                                      
                              1990.6125     0.43     0.05     102.7                                      
                              1990.6262     0.12     0.03      98.5                                      
                              1990.6426     0.09     0.02      96.9                                      
                              1990.6563     0.08     0.02      93.3                                      
                              1990.6591     0.06     0.01      85.7                                      
                              1990.6646     0.24     0.02      81.0                                      
                              1990.6673     0.06     0.02      82.2                                      
                              1990.6728     0.09     0.03     100.6                                      
                              1990.6837     0.61     0.09      78.9                                      
                              1990.7056     0.08     0.02      92.4                                      
                              1990.8233     0.08     0.02      98.0                                      
                              1991.6037     0.22     0.04     105.1                                      
                              1991.6557     0.10     0.02      88.5                                      
                              1991.6584     0.12     0.03      98.1                                      
                              1991.7077     0.10     0.03      96.5                                      
                              1991.7104     0.08     0.02      99.7                                      
                              1991.7132     0.05     0.01      84.4                                      
                              1991.7460     0.08     0.02      84.3                                      
                              1992.6413     0.19     0.03      85.5                                      
                              1992.6441     0.56     0.05      96.3                                      
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.88 +/- 0.22, 5.02, and 2.63 Msun, respectively.  Mlk2012 
00573+6020   ARG   3     B is BD+59@149.                                                                 
00573+2518   POU  79     LDS 871.                                                                        
00573+1100   ITF  49     Aka ITF  94.                                                                    
00574+2053   J  2587     BRT2300.                                                                        
00576-7131   OGL 112     SMC109.3.163   + SMC109.3.288                                           Pli2012 
00577+0441   GWP 107     AB: XMI 159AB.                                                          Tob2012b
             GWP 108     AC: XMI 159AC.                                                          Tob2012b
00577-7326   OGL 113     SMC106.7.19223 + SMC106.7.12940                                         Pli2012 
00578-7346   OGL 114     SMC107.5.14324 + SMC107.5.14471                                         Pli2012 
00580-7306   OGL 115     SMC106.5.52673 + SMC106.5.51760                                         Pli2012 
00586+4709   BRT  73     The 1893 observation differs substantially from modern observations.            
                         Either the 1893 observation is erroneous (which we consider the most            
                         probable), or there exist perturbations in the system. The question of          
                         the physical relationship of this system remains open.                  Kiy2012 
00587-7144   OGL 116     SMC109.1.23    + SMC109.1.460                                           Pli2012 
00587-7207   OGL 117     SMC108.3.6583  + SMC108.3.6695                                          Pli2012 
00588+1044   GWP 109     XMI 160.                                                                Tob2012b
00588-7149   OGL 118     SMC109.1.85    + SMC109.1.231                                           Pli2012 
00589+3230   SEI  10     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00589+0339   GWP 110     XMI 161.                                                                Tob2012b
00591+5729   STI1500     Not the same as 00570+5729ES   44.                                              
00592-1211   LDS3217     NLTT 3252/3253                                                          Chm2004 
00593+0706   GWP 111     XMI 162.                                                                Tob2012b
00593-0040   A  1902     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.23 +/- 0.70, 2.54, and 1.20 Msun, respectively.             Mlk2012 
00593-7142   OGL 119     SMC109.2.9765  + SMC109.1.13352                                         Pli2012 
00594+0047   STF  80     B is BD+00@158.                                                                 
                         AB: Additional notes may be found in Holden (1972).                     Hln1972 
                         A: In addition to the linear solution for the resolved pair,                    
                         astrometric orbits have been computed for an unseen close companion to          
                         A. Dommanget give two orbits calculated from perturbations seen to the          
                         rectilinear motion.                                                     Dom1969 
00595+3202   SEI  11     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
00596-0111   A  1903     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.31 +/- 0.60, 2.11, and 0.95 Msun, respectively.  Mlk2012 
00596-7549   GLI   8     B is CPD-76@82, spectrum G0/2V.                                                 
00598+0629   KUI   4     The primary is variable, WW Psc.                                                
00599-7146   OGL 120     SMC109.1.13337 + SMC113.6.34323                                         Pli2012 
00599-7208   OGL 121     SMC108.3.14363 + SMC108.3.15476                                         Pli2012 
00599-7410   OGL 122     SMC107.1.178   + SMC107.1.218                                           Pli2012 
01000+5702   MLR 626     Also known as TDS1710.                                                          
01000-7234   OGL 123     SMC105.4.9983  + SMC105.4.11297                                         Pli2012 
01001+4443   STF  79     164 And. Both A and B are spectroscopic binaries.                               
                         H N  45.                                                                MEv2010 
01001+1246   GWP 113     XMI 164.                                                                Tob2012b
01001-7135   OGL 124     SMC109.2.10029 + SMC109.2.10470                                         Pli2012 
01002+5809   SKF  56BC   Aka MRI  25.                                                                    
01005-1923   SHY 392     HIP   4702 + HIP   4833.                                                        
01006+6027   BAG  36     Primary is the alpha2 CVn type variable V551 Cas.                               
01006-7343   OGL 125     SMC107.4.12713 + SMC107.3.646                                           Pli2012 
01007-7250   OGL 126     SMC105.2.10999 + SMC105.2.12098                                         Pli2012 
01007-7328   OGL 127     SMC106.2.10337 + SMC106.2.11173                                         Pli2012 
01008-7400   OGL 128     SMC107.2.7090  + SMC107.2.7244                                          Pli2012 
01010-7154   OGL 129     SMC108.4.34907 + SMC108.4.34906                                         Pli2012 
01011-7119   OGL 130     SMC114.5.140   + SMC114.5.363                                           Pli2012 
01012+3704   BRT2585     ALI 254.  Also known as TDS1720.                                                
01012-5610   HJ 3412     B is CPD-56@199.                                                                
01013+1745   GWP 116     XMI 165.                                                                Tob2012b
01014+3535   COU 854     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.42 +/- 1.13, 2.60, and 1.10 Msun, respectively.             Mlk2012 
01014+1155   BU  867     Misidentified in BDS and ADS. Corrections by Baize and Couteau.                 
                         A premature orbit has been calculated.                                          
01014-7120   OGL 131     SMC114.5.22    + SMC114.5.226                                           Pli2012 
01014-7210   OGL 132     SMC113.7.22785 + SMC113.7.22807                                         Pli2012 
01015+6922   A  2901     1984.9965: This autocorrelogram was remeasured; the new results are             
                         listed in catalog.                                                              
01015+1024   GWP 117     XMI 166.                                                                Tob2012b
01016+5339   HJ 2008     01015+5339SMA  11                                                               
01016-1630   LDS9107     Old LDS6107.                                                                    
01017+4635   A   927     BRT  75                                                                         
01017+2518   HDS 134     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.80 +/- 0.47, 2.33, and 2.40 Msun, respectively.             Mlk2012 
01018-0652   LDS  33     NLTT 3377/3378                                                          Chm2004 
01019+1405   GRV 984     Typo in original WDS designation - entered as 01010+1405.                       
01020+0214   LDS3221     LDS5310.                                                                        
01020-7201   OGL 133     SMC113.6.22750 + SMC108.3.39755                                         Pli2012 
01020-7304   OGL 134     SMC106.4.40341 + SMC111.5.15843                                         Pli2012 
01021-1516   LDS9108     Old LDS6108.                                                                    
01023+8153   KNT   1     A is an Algol type eclipsing binary, U Cep, P =19.3d.  There is                 
                         circumstellar matter.                                                           
01023+1131   PLQ  11     LDS1085.                                                                        
01023+0552   A  2003     Close, 0.2" or under. Position angles show large changes. A premature           
                         orbit has been computed.                                                        
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.79 +/- 1.16, 2.45, and 1.05 Msun, respectively.             Mlk2012 
01024+0504   HDS 135     Mean motion indicates P ~ 80 yr, rho decreasing.                        Msn1999b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.13 +/- 0.11, 1.39, and 1.35 Msun, respectively.  Mlk2012 
             WNO  50     AC: GJ 3071 + GJ 1027. CPM pair.                                        Mkr2008 
01025+0933   GWP 119     XMI 167.                                                                Tob2012b
01025-7353   OGL 135     SMC107.3.8839  + SMC112.6.180                                           Pli2012 
01026+6221   WNO  51     GJ 49 + GJ 51. CPM pair.                                                Mkr2008 
01027+0908   RAO  39     RoboAO finds 2 companions - Optical?  2MASS: B at 32.4" 145.3d, below   RAO2015 
                         the MS, optical? Tokovinin & Lepine (2012) miss AB but list an optical  Tok2012c
                         companion at 1733".                                                     Tok2014d
                         AB: A is SB2 with P = 26.2 days (Griffin & Suchkov 2003). The tertiary  Grf2003 
                         companion B at 2".8 did not move substantially in a year since its              
                         discovery by Riddle et al. (2015), but the PM of the main component A   RAO2015 
                         is small and the astrometry is not conclusive. B is located below the           
                         MS on the CMD, although still within the errors of its photometry.              
                         Considering the small field crowding, we count B as likely physical.    Rbr2015d
01028+3148   sig Psc     Combined spectroscopic/interferometric solution (Palomar Testbed        Knc2004 
                         Interferometer) by Konacki & Lane (2004), yielding distance = 112.9             
                         +/- 0.9 pc, masses 2.65 +/- 0.27 and 2.36 +/- 0.24 Msun, spectral               
                         types B9.5V, diameters 0.16 and 0.15 mas.                                       
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.19 +/- 0.87, 5.71, and 2.40 Msun, respectively.             Mlk2012 
01028+0049   LDS5311     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01029+4702   GIC  17     G172-034/G172-035. The A component is the variable star V359 And.               
                         NLTT 3437/3438                                                          Chm2004 
01029+4121   HJ 1064     39 And.                                                                         
01029+0753   OCC 480     eps Psc                                                                         
01030+4723   STT  21     A may be a spectroscopic binary.                                                
01030-0450   BUP  13     25 Cet.                                                                         
01031-7358   OGL 136     SMC112.7.5     + SMC112.7.92                                            Pli2012 
01032+7113   JNN 250     LHS 1182. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13           
                         +/- 0.02 Msun; a ~2.7 AU.                                               Jnn2014 
01032+6032   MLB  43     This is a physical pair, with relative motion much smaller than the             
                         proper motions. Relative motion may be affected by a perturbation in            
                         the radial direction with a period of 25y.                              Kiy2012 
01032+2006   LDS 873     NLTT 3462/3463                                                          Chm2004 
01033-6006   HJ 3416     Spectrum F6/8III/IV.                                                            
01033-7123   OGL 137     SMC114.5.6465  + SMC114.6.10201                                         Pli2012 
01035+5019   STF  83     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01035-0535   RST4162     J 1442.                                                                         
01036-5516   DLR   1     AB is a low-mass binary with masses 0.19 +/- 0.02 and 0.17 +/- 0.02             
                         Msun. At a distance of 47.2 +/- 3.1 pc the projected distance between           
                         the stars is 12AU.  They are orbited by an L-type companion at 84AU,            
                         which shares common proper motion.  The companion is either a 12-13             
                         Mjup planet (assuming an age of 20 Myr) or a 14-15 Mjup brown dwarf             
                         (for an age of 50 Myr).                                                 Dlr2013 
01036-7138   OGL 138     SMC114.7.13732 + SMC114.8.18665                                         Pli2012 
01037+4051   LDS3225     AB: Also known as GIC  18.                                                      
                         BC: NLTT 3481/3482                                                      Chm2004 
                         BC: Aside from the companion seen in the AstraLux images, there is an           
                         additional possible wide companion at 26" separation, as noted in the           
                         WDS. The wide components have very similar proper motions (e.g. Roser   Rsr2010 
                         et al. 2010), so actual companionship seems probable.                   Jnn2012 
             BWL   5     AD:  Colors and/or astrometry are inconsistent with a late-type common          
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 132-50.                    Bwl2015 
01037-3024   B   649     CI Scl, Algol (EA) type eclipsing binary, P = 14.7104 d.                Zas2011 
01037-7138   OGL 139     SMC114.7.13496 + SMC114.7.13580                                         Pli2012 
01037-7158   OGL 140     SMC113.5.9293  + SMC113.5.9288                                          Pli2012 
01038+2232   J   874     J measures a pair 1912 - 1917: 345@, 3".                                        
                         Measures and magnitude differences discordant.                          J__1949a
                         Companion has variable magnitude.                                       Cou1952a
01038+0122   STF  84     26 Cet.                                                                         
             STF  84     AB: H 4  83.                                                            MEv2010 
             BU 1355     AC: 1909 and 1921 measures disagree. BDS 494 same star.                         
01039-7255   SKF1068     OGL 141. SMC110.8.23710 + SMC110.8.23860                                Pli2012 
01040+3528   HO  213     A premature orbit has been calculated.                                          
01040-6409   B  1913     Spectrum composite: K0III/IV+A/F.                                               
01040-7134   OGL 142     SMC114.7.14379 + SMC114.6.11666                                         Pli2012 
01040-7401   OGL 143     SMC112.7.11    + SMC112.7.755                                           Pli2012 
01041+4408   UC  493     Not a CPM pair. The A component is a close double, leading to a                 
                         spurious proper motion (Skiff, private comm.).                                  
01042+2256   GIC  19     G069-044/G069-043.                                                              
                         NLTT 3529/3528                                                          Chm2004 
01044-0518   STF  85     Probably the same as STF 211 with a 1 hr error in RA.                           
01044-4703   UC  495     AB and BC are probably not CPM pairs. The proper motion of the B                
                         component was effected by a nearby bright star (Skiff, private comm.).          
01047+0401   GWP 126     XMI 168.                                                                Tob2012b
01047-3929   GJ 9037     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
01048+0135   A  2310     Position angles vary widely. A premature orbit has been calculated.             
01048-0528   STF  86     AB: H 3  73.                                                            MEv2010 
01049+3649   A  1515     Periods from 86 to 419yr have been calculated. Possibly ambiguous case          
01050+2119   LDS3228     NLTT 3570.  White dwarf pair = WD 0102+21 = EGGR 462/463                Grn1986 
01050-7132   OGL 144     SMC114.3.186   + SMC114.3.569                                           Pli2012 
01051+3814   J  1804     ALI 488.                                                                        
01051+1457   HJ 1068     72 Psc. A is a spectroscopic binary.                                            
01052+1250   HJ   10     Primary is eclipsing binary of Algol-type, period 1.62785 d.            Zas2012 
01053-7331   OGL 145     SMC111.8.20419 + SMC111.8.20441                                         Pli2012 
01055+8315   MLR 482     Also known as TDS  39.                                                          
01055+4928   ES 1206     1deg error in IDS led to similar error in WDS designation.                      
01055+1523   STF  87     NLTT 3597/3598                                                          Chm2004 
01055-7215   OGL 146     SMC113.2.30    + SMC113.2.126                                           Pli2012 
01056+4927   OSO  12     G172-038. Neither is a common proper motion pair, based on color and            
                         comparison with POSS2 red plates                                        Oso2004 
01056-7342   OGL 147     SMC112.5.12714 + SMC112.5.12879                                         Pli2012 
01057+2128   STF  88     psi 1 Psc                                                                       
                         AB: HJL  12.                                                            HJL1986 
                         AB: SHY 395. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 4   9.                                                            MEv2010 
             YR    6     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.29 +/- 0.78, 4.29, and 2.19 Msun, respectively.  Mlk2012 
01058+0455   STF  90     77 Psc. STTA 10. B is BD+04@176.                                                
                         AB: HJL  13.                                                            HJL1986 
                         AB: H 4  68.                                                            MEv2010 
01058-2618   HJ 2014     LDS  34. HIP 5140. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
01058-5959   R     5     B is CPD-60@75.                                                                 
01058-7150   OGL 148     SMC114.1.170   + SMC114.1.1973                                          Pli2012 
01060+6120   LDS3230     Old LDS6109. Due probably to a typo in the epoch-1900 IDS coordinates,          
                         LDS3230 was originally listed in the WDS as 00055+6119.                         
01060+2456   BRT 122     J 2708.                                                                 J__1955 
01060+1111   BPM  21     [PM2000]   41785 + [PM2000]   41845.                                    Gvr2010 
01061-4643   SLR   1     bet Phe. Variable?                                                              
                         Quoted errors in P and a are +119/-35y, +0".51/-0".14, respectively.    Ary2002b
01062+3211   S   393     sig 2 Psc                                                                       
                         AB: H 5  16.                                                            MEv2010 
01065+5325   ES  616     One degree error in WDS designation - should be +5425.                          
01065+0154   HDO  42     Doolittle may have measured a different pair (see ADS).                 A__1932a
01065-3055   LDS2167     NLTT 3662/3663                                                          Chm2004 
01065-3441   LDS9110     Old LDS6110.                                                                    
01066+1353   SHY 396     HIP   5207 + HIP   4387.                                                        
01069-1408   GAL 306     Object #34 in Gallo's original list.                                    Gal1912a
01071+1740   BPM  22     [PM2000]   42380 + [PM2000]   42414.                                    Gvr2010 
01072+5330   H 4  66     H IV 66.                                                                        
01072+3839   A  1516     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.62 +/- 0.59, 2.89, and 1.10 Msun, respectively.  Mlk2012 
01072-0144   STF  91     B is 2mag above the MS in (K,V-K), on MS in (J,J-K). Wrong 2MASS ptm.           
                         The B component is possibly a SB.                                       Tok2014d
01072-7121   OGL 149     SMC114.4.6097  + SMC114.4.6144                                          Pli2012 
01073+0537   GWP 130     XMI 169.                                                                Tob2012b
01073-7201   OGL 150     SMC113.3.21615 + SMC113.3.21614                                         Pli2012 
01074+0101   LDS5315     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01075+4116   RAO  40     Primary is SB, P=49.480d. Estim. mass of B 0.26 Msun.                   Tok2014d
                         Triple system with inner 74.1 day spectroscopic pair (Gorynya &                 
                         Tokovinin 2014 MNRAS 441, 2316) and tertiary from Riddle et al. (2015)  RAO2015 
                         confirmed as physical by our photometry and astrometry. Observations            
                         demonstrate that photometry of B given in 2MASS is biased by proximity          
                         of bright primary, as in many other similar pairs. Their "unusual"              
                         colors derived from the 2MASS photometry are thus wrong.                Rbr2015d
01075+0244   GWP 131     XMI 170.                                                                Tob2012b
01075-4145   LDS9111     Old LDS6111.                                                                    
01076+2257   LDS9112     AB: Old LDS6112.                                                                
                         NLTT 3723/3725                                                          Chm2004 
01078-4129   RST3352     ups Phe. Variable RV suspected. The lines are poor and show a scatter           
                         of 40km/s without apparent relation to the visual motion.                       
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.16 +/- 0.34, 2.78, and 2.09 Msun, respectively.             Mlk2012 
01079-7311   OGL 151     SMC111.3.12611 + SMC111.3.12798                                         Pli2012 
01080+3915   RAO  41     Primary is SB, P=1713d.                                                 Tok2014d
01083+5455   WCK   1     Aa,Ab: mu Cas = 30 Cas. Proper motion of A +3424 -1596 (FK5).                   
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 0.01 +/- 0.01, 1.22, and 0.95 Msun, respectively.  Mlk2012 
             mu Cas      Aa,Ab: Astrometric orbit. Spectroscopic elements are somewhat                   
                         different from those of Lippincott: P = 23.0, T = 1954.0, e = 0.30,     Lip1981 
                         omega = 178.0 (Worek & Beardsley 1977).                                 Bey1977 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The pair has now been resolved by infrared speckle interferometry.      Mcy1983 
                         Pierce & Lavery (1985), Karovska et al. (1986), Haywood et al. (1992),  Pie1985 
                         and McCarthy et al. (1993) all compare their observations with          Kar1986b
                         published orbits and discuss  luminosities and masses of components,    Hay1992 
                         helium abundances, etc.                                                         
                         Hipparcos astrometric solution adopts some elements from the orbit      HIP1997d
                         of Heintz & Cantor (1994).                                              Hei1994b
             STT 551     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
01083-3535   FAR   2     SKF 328. Primary is white dwarf WD 0106-358 = GD 683.                   Far2005b
01084+0539   BUP  15     80 Psc. B is BD+04@192.                                                         
             STT 552     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01084-5515   RST1205     zet Phe. A is an Algol-type system, spectrum composite, P = 1.67d.              
                         Both B and C are probably physical.                                             
                         Ling (2004) gives a derived orbital parallax 0".01176 and a mass sum    Lin2004a
                         of 7.41 +/- 5.85 Msun                                                           
01085+6331   OSO  13     G243-062. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates. PM of A = +1047 -91.                                  Oso2004 
01086+1652   GWP 135     XMI 171.                                                                Tob2012b
01086+1917   GWP 136     XMI 172.                                                                Tob2012b
01086-1011   BUP  16     eta Cet = 31 Cet. B is BD-10@239.                                               
01088+6145   ES 1945     Aka OL  113.                                                                    
01088-7119   OGL 152     SMC119.5.5     + SMC119.6.162                                           Pli2012 
01089+4512   HJ 2018     AB,C : Same as STF  92.                                                         
01091-7225   OGL 153     SMC118.8.502   + SMC113.1.14118                                         Pli2012 
01092-7127   OGL 154     SMC119.6.1012  + SMC119.6.1006                                          Pli2012 
01093+6234   LDS5179     old LDS6113.                                                                    
01094+3543   BUP9005     A component is NGC 404.                                                 Skf2013 
01094+2949   ALP   4     2MASSW J0109216+294925                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
01094+0457   GWP 138     XMI 173.                                                                Tob2012b
01094-5636   HU 1342     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.71 +/- 0.86, 2.48, and 1.27 Msun, respectively.             Mlk2012 
01095+4715   STT 515     phi And = 42 And. Measure of 1985.830 made by MAPPIT.                   Han1987 
                         Scardia et al. (2001) orbit considered preliminary.  The real period    Sca2001d
                         is probably long (>400 yr).  The Hipparcos parallax is 0".00443 +/-             
                         0.00080, giving a mass sum of 6.9 Msun, slightly in excess for a                
                         binary of spectral type B7Ve. The dynamical parallax is 0".0033, in             
                         reasonable agreement with the measured one but not acceptable as it             
                         leads to an exaggerated mass sum (16.8 Msun).                                   
                         Calculated mass sum is 6.5  +/- 2.8 Msun, in reasonable agreement with          
                         spectral types B6IV and B9V, although mass is not well-constrained.     Mut2010b
01096+4635   ES 1300     Due to a typographical error in the ADS, the AE, AF, AG, AH, and AI     A__1932a
                         components of 01097+3537 were added as additional components to this            
                         pair (the AE and AI pairs as BAR  66, the others as ES 1300).                   
01096+2802   BRT 123     OL  149.                                                                        
01096-0507   LDS9114     Old LDS6114. LIT   3.                                                           
                         NLTT 3847/3849                                                          Chm2004 
01096-0711   HDS 151     This binary displays clear common proper motion, but the residual               
                         astrometry does not seem to follow a simple trajectory consistent with          
                         only orbital motion of the two visible components. In addition, the             
                         brightness difference is larger than the spectral type difference               
                         would imply at a common distance. This could indicate that the A                
                         component is itself an unresolved binary.                               Jnn2012 
01097+3537   BAR   1     bet And = 43 And = Mirach                                                       
                         Also, see note to 01096+4635.                                                   
01097+0856   GWP 139     XMI 174.                                                                Tob2012b
01098-2013   HJ 2023     Primary is CT Cet, a W UMa type eclipsing binary, P = 0.25649d.         Zas2012 
01099+1352   BPM  23     [PM2000]   44058 + [PM2000]   44035.                                    Gvr2010 
01100-7327   OGL 155     SMC111.2.5925  + SMC111.2.6033                                          Pli2012 
01101+5145   STT  23     AB: HJL  14.                                                            HJL1986 
01102+2447   POU 107     J 1805.                                                                         
01104-7352   OGL 156     SMC112.3.6394  + SMC117.6.1318                                          Pli2012 
01105+1326   BPM  24     [PM2000]   44379 + [PM2000]   44460.                                    Gvr2010 
01105+1019   GWP 143     XMI 175.                                                                Tob2012b
01107+8021   STF  89     B is BD+79@32.                                                                  
01107-2800   SWR   1     CPM pair                                                                Skf2004 
01108+6747   HDS 155     A spectroscopic double lined orbit has been determined as well.         Grf2012d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.02 +/- 0.23, 2.18, and 2.52 Msun, respectively.             Mlk2012 
01108+5141   DOO   3     BDS 631.                                                                        
01109+0934   HJ  634     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01111+5509   STT 553     the Cas = 33 Cas. A is a spectroscopic binary,                                  
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01111+3125   STT  25     82 Psc = g Psc                                                                  
01111-7228   SKF1069     OGL 157. SMC115.5.12    + SMC115.5.319                                  Pli2012 
01112+4113   A   655     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 0.83, 2.76, and 0.95 Msun, respectively.             Mlk2012 
01112+3743   HO  215     45 And. Also single 1903, 1906 (Doolittle), 1907 (Aitken).                      
                         A measure by Schembor (1925.60, 117.8@, 155.5", 6 - 6) belonged to      Sch1927a
                         01107+4256 ENG   4AB instead.                                                   
                         Duplicity of A is questionable.                                                 
01112+1634   GWP 144     XMI 176.                                                                Tob2012b
01114+1526   BEU   2     GJ 3076. WDS designation incorrected entered as 01224+1526.                     
                         Estimated age 10-20 Myr; masses 0.10 +/- 0.03 and 0.04 +/- 0.01 Msun;           
                         a ~5.6 AU.                                                              Jnn2014 
01114-7225   OGL 158     SMC118.8.10104 + SMC118.8.10016                                         Pli2012 
01114-7323   OGL 159     SMC116.7.144   + SMC116.7.143                                           Pli2012 
01116+0446   GWP 146     XMI 178.                                                                Tob2012b
01116+1404   GWP 145     XMI 177.                                                                Tob2012b
01117+1205   LDS3242     NLTT 3967/3952                                                          Chm2004 
01119+0455   GIC  20     G002-027/G070-044 = GJ 3077A+3078B.                                             
01120+0642   GWP 149     XMI 180.                                                                Tob2012b
01120+0955   GWP 148     XMI 179.                                                                Tob2012b
01120-7231   OGL 160     SMC115.5.9132  + SMC115.5.9369                                          Pli2012 
01121+6111   KR   10     AC: Doolittle's published position angle was 91.9deg, which does not    Doo1901 
                         match anything in the field. However, an obvious star is visible at             
                         the same separation but 90deg off his theta measure. It is assumed he           
                         made an error when rotating his micrometer.                                     
             SMA9001     AD: Doolittle noted "a 13.5 mag. companion about 7" from A was          Doo1901 
                         suspected on two nights". It is assumed he saw the Smart companion.     Sma1932 
01121+4700   BU  236     Aka HJ 2024.                                                                    
01121-7400   OGL 161     SMC117.7.58    + SMC117.3.98                                            Pli2012 
01125+0228   STT  27     35 Cet                                                                          
01126+1704   NAU   1     The primary is GU Psc, a likely member of the young AB Doradus Moving           
                         Group. Spectral types are M3 +/- 0.5 and T3.5 +/- 1. Age of the system          
                         is 100 +/- 30 Myr, distance 48 +/- 5 pc.                                Nau2014 
01129+3205   STF  98     B is BD+31@196a. The primary is a double-lined spectroscopic binary,            
                         P = 2.21d. B may also be an SB (Hube, PASP 93, 490; 1981).                      
                         AB: H 4 120.                                                            MEv2010 
01130+3004   STT  26     A is a spectroscopic binary.                                                    
01131+2942   A  1260     Angle increasing, with a probable close approach about 1950.                    
01131+1141   HD  7275    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01131-7215   OGL 162     SMC118.2.51    + SMC118.2.127                                           Pli2012 
01132-7400   OGL 163     SMC117.7.3315  + SMC117.7.3338                                          Pli2012 
01133-0152   HIP   5697  The SB1 orbit suggests mass ratio q > 0.2 and axis 0".21. The companion         
                         is probably just a bit too faint or too close to be resolved with NICI. Tok2012a
01134-3932   SHY 397     HIP   5709 + HIP   5490.                                                        
01134-7251   OGL 164     SMC115.2.45    + SMC115.2.260                                           Pli2012 
01135-3821   BRG   4     The primary star in the system is a known eclipsing binary with a               
                         period of 0.4455 days (Parihar et al. 2009 MNRAS 395, 593). Since the           
                         angular separation is inside of our inner cut-off, we count the system          
                         as a binary here for the purpose of multiplicity statistics, although           
                         it is really a triple system. To estimate the mass of the primary for           
                         the purpose of deriving the mass ratio to the tertiary component                
                         detected in our images, we use the sum of the masses corresponding to           
                         individual spectral types M1 and M3 derived for the eclipsing binary.   Jnn2012 
                         ASAS J011328-3821.1, eclipsing binary of Algol type, period 0.44559d.   Zas2016 
01136+2825   HJ  635     Previously erroneously listed as 01126+2825.  Also known as GRV  73.            
01137+2435   STF  99     phi Psc = 85 Psc. A is a spectroscopic binary.                                  
01137+0735   STF 100     zet Psc. Both A and B are spectroscopic and occultation binaries, B             
                         has P = 9.08d.                                                                  
                         AB: HJL  15.                                                            HJL1986 
                         AB: H 4   8.                                                            MEv2010 
             BU 1029     BC: Delta m given in ADS is greatly overestimated.                      Wor1967b
01137-5040   HJ 3421     B is CD-51@312.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01139+1004   GWP 154     XMI 181.                                                                Tob2012b
01141+1698   87 Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Stickland & Weatherby (1984).                                           Stc1984 
01141+0634   LDS3248     LDS5323.                                                                        
01142-4041   B  2554     Hipparcos suspected non-single.                                                 
01144-0755   STFA  3     37 Cet = LDS3250. B is BD-08@215.                                               
                         NLTT 4123/4121                                                          Chm2004 
                         AB: GJ 9045 A+B. CPM pair.                                              Mkr2008 
                         AB: H 5  24.                                                            MEv2010 
01144-7319   OGL 165     SMC116.3.3     + SMC116.3.954   + SMC116.6.11112                        Pli2012 
01145-0503   ROL   1     Primary is exoplanet host, periods 1275d, 4046d.                        Tok2014d
             RGS   1     Aa,Ab: HD 7449 has a close massive planet (P = 1270.5 +5.92/-12.1d,             
                         a =  2.33 +0.01/-0.02 AU, mass >1.09 +0.52/-0.19 Mjup) as well as a             
                         more distant stellar companion. The Ab component is likely an M4-M5             
                         dwarf. Rodigas et al. (2016) estimate P = 65.7 +227/-56y, a =  17.9             
                         +32/-12.9 AU, i = 59.7 +20.1/-25.8 deg, mass = 0.23 +0.22/-0.05 Msun.   Rgs2016 
01146-7402   OGL 166     SMC117.7.3320  + SMC117.7.3907                                          Pli2012 
01148+6056   BU 1100     The quadrant interpretation by Zulevic is less likely.                  Zul1972a
                         Muller corrected an error in his elements (Ephem. Cat. 1964).           Mlr1955b
                         One component is a SB, P = 5.33d.                                               
                         Only elements P, T, and a have been amended by Starikova (1977) from    Sta1977a
                         the orbit of Zulevic (1972).                                            Zul1972a
01148+4309   LDS3251     NLTT 4129/4124                                                          Chm2004 
01148-0058   BUP  18     38 Cet.                                                                         
                         A is a blue supergiant with multiple pulsation periods.                 IAU2014e
                         AC: C component is galaxy NGC 442.                                              
01149+3236   SEI  14     None of the components seen on POSS plate; may be flaws on AC Potsdam           
                         plate.                                                                          
01152-3419   LDS 837     LDS5325.                                                                        
01153+6040   LDS5180     old LDS6115.                                                                    
01153+2234   J  3226     BRT2304. Barton lists theta as 226.9; probably typo for 266.9.          Brt1939b
01155+3745   SHY 121     HIP   5881 + HIP   6278.                                                        
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Nidever et al. (2002). They derived component masses 0.95 and 0.28      Nid2002 
                         Msun and an estimated semimajor axis of 30.68 mas.                      Ren2013 
01155+0216   CHR 195     First detected as an occultation binary by Evn1983a.                            
01157+0241   GWP 157     XMI 182.                                                                Tob2012b
01157+0032   LDS5326     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
01158+4702   LAW   9     LSPM J0115+4702S. Law et al (2008) derive a distance of 18.7 +9.3/-3.6  Law2008 
                         pc and a projected separation of 5.2 +2.9/-0.9 AU. Estimated spectral           
                         types are M4.5 and M5.                                                          
                         In addition to the companion detected with AstraLux, it can be noted            
                         that 2MASS J01154885+4702259 has a very similar proper motion to the            
                         star J01155017+4702023 at just 27" separation (Roser et al. 2010),      Rsr2010 
                         which is itself a close binary (Law et al. 2008). Thus, this is a very  Law2008 
                         likely quadruple system.                                                Jnn2012 
01158+0947   A  2102     Quadrant change. Not seen 1948 - 1954.                                          
01158-6853   HJ 3423     kap Tuc = LDS  42.                                                              
             I    27     HJ 3423 and I 27, separated by 320", form the quadruple system                  
                         kap Tuc. The position of I 27 is 011501.0-684908 (2000).                Sca1981a
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
01158-7224   OGL 167     SMC118.1.5565  + SMC118.1.6020                                          Pli2012 
01160+5849   STI1550BC   Aka MRI  29.                                                                    
01160+1534   GRV 986     SLW  58.                                                                        
01162-7246   OGL 168     SMC115.2.6083  + SMC115.2.6082                                          Pli2012 
01163+1243   BPM  25     [PM2000]   47807 + [PM2000]   47744.                                    Gvr2010 
01163-2056   LDS  41     NLTT 4238/4239                                                          Chm2004 
01163-3217   LDS1091     LDS5327.                                                                        
01166+7402   HJ 2028     STTA 13.                                                                        
01166+1831   HDS 169     A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Latham et al. (2002). They derived component masses 1.06 and 0.28 Msun  Lat2002 
                         and an estimated semimajor axis of 14.81 mas.                           Ren2013 
01166+1507   GWP 161     XMI 183.                                                                Tob2012b
01166-0230   BU 1358     39 Cet. A semiregular variable, AY Cet, and spectroscopic binary, P =           
                         56.8d. Radio flares and soft X-rays are observed, and a white-dwarf             
                         companion is revealed by IUE observations.                                      
01167-7142   OGL 169     SMC124.7.387   + SMC124.7.163                                           Pli2012 
01168+2643   BRT3257     Originally published as BRT 124.                                        Brt1928 
01170-7311   OGL 170     SMC116.3.7036  + SMC116.3.7122                                          Pli2012 
01171+1739   BPM  26     [PM2000]   48328 + [PM2000]   48320.                                    Gvr2010 
01171-7355   OGL 171     SMC117.3.682   + SMC117.3.1102                                          Pli2012 
01172+0930   GWP 164     XMI 184.                                                                Tob2012b
01175+0131   GWP 165     XMI 185.                                                                Tob2012b
01176+4018   A  1521     Rapid change, but the measures are inadequate to define the motion.             
01177+2647   BRT3258     Originally published as BRT 125.                                        Brt1928 
01177-7150   OGL 172     SMC124.8.4147  + SMC124.8.4560  + SMC124.8.4191                         Pli2012 
01178+4945   HU  520     Quadrant indeterminate.                                                         
01178+4901   HJ 2033     Ea : Also known as STF 102 ET.                                                  
01179-7314   OGL 173     SMC116.3.7181  + SMC116.3.7479                                          Pli2012 
01180+0037   GWP 167     XMI 186.                                                                Tob2012b
01181+4707   A   937     North preceding and slightly brighter of a finder pair. Narrow                  
                         apparent orbit.                                                         B__1963b
01182+1409   BPM  27     [PM2000]   48977 + [PM2000]   49004.                                    Gvr2010 
01182-7136   OGL 174     SMC124.7.4469  + SMC124.7.4898                                          Pli2012 
01184-2332   LDS2182     Appears to be same as SKF1373. Primary is B component of 01183-2330             
                         SKF1372; pair moved to become AC pair (with quadrant flip).                     
01185+7323   A   814     Not separated about 1951 (Van Biesbroeck). Possible quadrant change.    VBs9999 
01186+3855   GIC  21     G132-069/G132-068.                                                              
                         NLTT 4342/4337                                                          Chm2004 
01186-2255   FAR  24     Primary is white dwarf WD 0116-231.                                     Far2006 
01187-0052   HJ 5453     LDS  43. HIP 6130. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         AB: NLTT 4362/4361                                                      Chm2004 
             EGN   1     Aa,Ab pair bound. Colors of Ab component consistent with M2-M5 dwarf,           
                         with mass 0.24 +/- 0.01 Msun.  B component is K7 dwarf and shares               
                         CPM with A. C component is likely a background star.                    Egn2007 
01187-2249   HDO  47     Probably = HDO 48.                                                              
01188+3724   STF 108     The A component is a spectroscopic binary.                                      
01188-5637   RST  29     Spectral type G5?                                                               
01191-7215   OGL 175     SMC123.7.2850  + SMC123.7.2849                                          Pli2012 
01192+5821   STI1560     B is BD+57@248.                                                         FMR9999 
01192-4338   B  1423     Zurlo et al. (2013) estimate the period of this system at ~300y, in an          
                         eccentric orbit with a semi-major axis of ~50AU. The companion is               
                         likely a white dwarf.                                                   Zur2013 
01194+6418   MLB 186     TDS1841.                                                                        
01194+1158   BPM  28     [PM2000]   49715 + [PM2000]   49656.                                    Gvr2010 
01194-7129   OGL 176     SMC124.3.274   + SMC124.3.22                                            Pli2012 
01194-7246   OGL 177     SMC120.7.5025  + SMC120.8.5604                                          Pli2012 
01194-7359   OGL 178     SMC122.7.221   + SMC122.7.232                                           Pli2012 
01195+5816   ES  408     CD component also known as STI1562                                              
01195+1850   GWP 169     XMI 187.                                                                Tob2012b
01195-7205   OGL 179     SMC123.6.2701  + SMC123.6.3359                                          Pli2012 
01196-0520   A   313     Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Heintz (1968).                                                 Hei1968a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.39 +/- 1.07, 2.59, and 1.10 Msun, respectively.             Mlk2012 
01197+1209   CHR 196     First detected as an occultation binary by Africano.                    Afr1975 
01197-7203   OGL 180     SMC123.6.2671  + SMC123.6.3140                                          Pli2012 
01198-0031   STF 113     42 Cet.                                                                         
                         AB: Absolute quadrant for 1998.657 determined by triple-correlation             
                         techniques.                                                             Pru2002b
                         A,BC. 1985.8430: This autocorrelogram was remeasured; the new results           
                         are listed in catalog.                                                          
                         Star A (mag. 6.3, G8III) is in slow direct motion at 1.6" separation.           
                         T incorrectly given as 1992.52 by Baize (1990); should be 1993.02       Baz1990a
                         (erratum noted in Inf. Circ. 111, 1990)                                         
             FIN 337     BC: 1982.7629, 1982.7657, 1983.7106: A mistake in reduction resulted in         
                         90 degree errors for these three measures.                              McA1987b
                         BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.79 +/- 0.56, 3.32, and 1.20 Msun, respectively.  Mlk2012 
01198-7157   OGL 181     SMC123.5.2462  + SMC123.5.2499                                          Pli2012 
01199+0350   CHE  29     BAL2084.                                                                Hln1972 
01200+5747   STI1571     Aka LYS   5. Identity not recognized due to large pm affecting pa.              
01200-1549   HJ 2036     A is an SB. Binary or triple?                                           Tok2014d
01201+5814   H 3  23     H III 23. phi Cas = 34 Cas. A is a spectroscopic binary.                        
                         A quintuple system. C has spectral type B5/6Ia/be.                              
01201+3900   GIC  22     G132-071/G132-072.                                                              
                         NLTT 4410/4412                                                          Chm2004 
01203-0933   LDS9116     Old LDS6116.                                                                    
01203-4841   HJ 3428     B is CD-49@378.                                                                 
01204+0937   GWP 171     XMI 188. BVD  15.                                                       Tob2012b
01205+0418   J  1807     BAL 2085.                                                                       
01205-1957   TOK 203     Two astrometric orbits are derived by Goldin & Makarov (2006), the      Gln2006 
                         longest one has P = 8.93 yr, axis 55 mas, and e = 0.84.                 Tok2012a
                         Retrograde motion by 4deg since first resolution in 2011. Goldin &              
                         Makarov (2006) propose two orbits with periods ~9yr; semi-major axis    Gln2006 
                         should then be 0".15, so the system is near apastron.                   Tok2013b
01207+0333   GWP 172     XMI 189.                                                                Tob2012b
01207-7145   OGL 182     SMC124.1.101   + SMC124.1.545                                           Pli2012 
01208+1127   AG   17     LDS 878. B is BD+10@167.                                                        
                         HJL  17.                                                                HJL1986 
01208+1035   PLQ  13     B is BD+09@153.                                                                 
                         HJL  16.                                                                HJL1986 
01211+6439   S   397     35 Cas. STTA 15 = H 5  81.  B is BD+63@175.                                     
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01211+1540   J   227     B is variable                                                           Cou1952a
01211+0736   SLE 257     The primary is a W UMa system, AQ Psc.                                          
01211-0403   LDS3267     G 271-42.                                                                       
01211-3508   LDS5330     Aka LDS9117 the old LDS6117.                                                    
01211-7251   OGL 183     SMC120.2.15    + SMC120.2.163                                           Pli2012 
01211-7305   OGL 184     SMC121.5.2620  + SMC121.5.3200                                          Pli2012 
01212+5159   NLTT 4450   Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Latham et          
                         al. (2002). They derived component masses 1.21 and 0.26 Msun and an     Lat2002 
                         estimated semimajor axis of 35.17 mas.                                  Ren2013 
01212+4108   LDS3266     NLTT 4468/4469                                                          Chm2004 
01213+1132   BU    4     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         The Hipparcos parallax (0".00616 +/- 0.00141) yields a mass sum of      Sca2001d
                         4.7 Msun, in excess for a binary of type F1III.                                 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 9.73 +/- 6.50, 3.62, and 1.64 Msun, respectively.  Mlk2012 
01215-2908   RUC   1     BE Scl. Spectral type of resolved companion estimated at G5-8V.         Ruc2007 
01218-2408   SEE  13     Motion direct. A premature orbit has been computed.                             
01219-4003   WG    8     BRT 643.                                                                Brt1933 
01220+1848   GWP 175     XMI 190.                                                                Tob2012b
01220-6943   I   263     A premature orbit has been computed. Motion direct.                             
01221-2654   LDS2189     NLTT 4564/4566                                                          Chm2004 
01223+0331   DEA  38     NLTT 4558 + 2MASS J01221697+0331235. Baron et al. (2015) estimate               
                         spectral types G5 and L2 +/- 1, distances 58 +/-3 and 43 +13/-40 pc,            
                         masses 1.05 -1.12 and 0.071-0.076 Msun.                                 BFr2015 
01223-7332   OGL 185     SMC121.1.5     + SMC121.1.187                                           Pli2012 
01226+1200   GWP 178     XMI 191.                                                                Tob2012b
01227+1410   GWP 179     XMI 192.                                                                Tob2012b
01227+0032   LDS3270     Aka WNO  42.  G 70-55.                                                          
01227-7258   OGL 186     SMC120.1.13    + SMC120.1.32                                            Pli2012 
01228-2440   BWL  63     Bowler et al (2013) derive the following properties: age 120+/-10 Myr,          
                         distance 36+/-4 pc, masses 0.40+/-0.05 Msun and 12-14 or 23-27 Mjup.    Bwl2013 
01230-1258   GAL 307     LDS  46. Object #40 in Gallo's original list.                           Gal1912a
             KUI   6     BC: BC shares CPM with A.                                               B__1963b
01230-3035   LDS2190     According to Richard Jaworski the precise position he determine may be  Jaw2006 
                         correct if Luyten's original separation is off by an order of                   
                         magnitude (i.e., 11.8" rather than 118").                                       
01232+4905   KU    8     HU 524.                                                                         
01233+0152   LDS5332     CVR  26.                                                                        
01233-0209   LDS3271     NLTT 4616/4615                                                          Chm2004 
01233-2105   LDS2191     NLTT 4626/4625                                                          Chm2004 
01233-7256   OGL 187     SMC120.1.3850  + SMC120.1.4139                                          Pli2012 
01234+5809   STF 115     First measured by F.W. Struve in 1836 at an angular separation of       Hrt1989 
                         0".68, this system had opened to 1".2 by 1910, then steadily closed             
                         to 0".35 at the time of the first speckle measurement in 1978.                  
                         The pair reached an apparent minimum separation of 0".01 in the                 
                         spring of 1984.                                                                 
                         1983.7107  This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.36 +/- 0.67, 2.80, and 1.20 Msun, respectively.  Mlk2012 
01235-7356   OGL 188     SMC122.3.2     + SMC122.3.173   + SMC122.5.71                           Pli2012 
01236+3415   CRJ   4     NLTT 4619. The A component is SB, P=83.9d. Primary is G8IV. The 0.3"            
                         companion is physically associated with primary, based on multi-epoch           
                         astrometry. The estimated spectral type of the companion ~M1V, its              
                         mass > 0.297 Msun.                                                      CrJ2013 
01236+0753   GWP 180     XMI 193.                                                                Tob2012b
01237-6217   RST  31     Spectral type G0?                                                               
01239+0050   GWP 182     XMI 194.                                                                Tob2012b
01239-7228   OGL 189     SMC120.4.3345  + SMC120.4.3627                                          Pli2012 
01240-0800   HJ 1079     44 Cet. A is a Delta Scuti-type variable, AV Cet.                               
01240-0811   BU  505     the Cet = 45 Cet.                                                               
01240-2933   LDS2192     NLTT 4676/4656                                                          Chm2004 
01241-1244   GAL 308     Object #42 in Gallo's original list.                                    Gal1912a
01242+1254   HJ   13     C component is galaxy NGC 514.                                                  
01243+0426   GWP 183     XMI 195.                                                                Tob2012b
01243-0655   BU 1163     The system is also detected as a spectroscopic binary.                  B__1951a
                         Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of van den Bos (1961).                                        B__1961e
                         This system underwent periastron in late 1988, an event now covered by          
                         speckle observations.                                                   Hrt1992b
                         A combined visual-spectroscopic orbit by Morbey (1975) gives almost     Mrb1975 
                         the same elements, but in the representation of position angles         Sod1999 
                         Soderhjelm's elements are preferable.                                           
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 0.41, 2.74, and 1.30 Msun, respectively.             Mlk2012 
01245+3902   STTA 17     B is BD+38@256.                                                                 
                         D is BD+38@253.                                                                 
01245+1740   BPM  29     [PM2000]   52622 + [PM2000]   52637.                                    Gvr2010 
01245-2839   LDS2194     NLTT 4694/4695                                                          Chm2004 
01245-3356   JAO   1     Aa,Ab: GJ 2022 = G274-024                                                       
                         Daemgen et al. derive a distance of 12.6 +/- 2.3 pc, a separation for           
                         the AC pair of 26.0 +/- 4.8 AU, and a predicted orbital period of 330           
                         +95/-93 yr. Spectral types for both components are M5.0 +/- 0.5;                
                         masses are 0.14 +0.03/-0.02 and 0.13 +0.03/-0.02 Msun.                  Dae2007 
01246+5311   ES 2583     B is BD+52@332.                                                                 
01247-7402   OGL 190     SMC122.2.45    + SMC122.2.104                                           Pli2012 
01248-2614   RST1218     LDS 3277.                                                                       
                         NLTT 4714/4713                                                          Chm2004 
01250+1424   GWP 185     XMI 196.                                                                Tob2012b
01251+4537   A   939     Recent observations seem to rule out Muller's short-period              Mlr1955a
                         alternative.                                                                    
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.54 +/- 1.99, 3.23, and 1.45 Msun, respectively.             Mlk2012 
01252-0412   HJ  638     01252-0409BU 1361                                                               
                         J  1445.                                                                Nsn2016 
01252-7954   HJ 3443     B is CPD-80@23.                                                                 
01253-5930   HJ 3435     B is CPD-60@111.                                                                
01254+0227   GWP 186     XMI 197.                                                                Tob2012b
01256+3133   STT  30     AC: HJL  18. Aka MAD   9.                                               HJL1986 
                         AC: SHY 402. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         STTA 18.                                                                        
                         B is above MS (wrong ptm), while A and C are on it. C is SB2,           HJL2012b
                         P=14.908d (Halbwachs et al. 2012)                                       Tok2014d
01256+2331   TOK  11     Primary is 5.4d SB1. Estimated period of visual pair 880y.              Tok2006 
01257+0258   J  1899     BC: Error in coordinates listed in Jonckheere (1941), star is at        J__1941a
                         1h 23.2m, not 0h 23.2m.  Star of mag 7.3 at 131" is BD+02  207.         J__1952 
01257+0107   GWP 188     XMI 199.                                                                Tob2012b
01257+0611   GWP 187     XMI 198.                                                                Tob2012b
01258+6014   BUP  19     del Cas = 37 Cas. A spectroscopic and (perhaps) eclipsing binary.               
01259+6808   BU 1101     psi Cas = 36 Cas.                                                               
             H 5  83     H V 83, SHJ 18, STF 117. C is BD+67@124.                                        
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01260+1450   BPM  30     [PM2000]   53515 + [PM2000]   53480.                                    Gvr2010 
01261+0925   GWP 189     XMI 200.                                                                Tob2012b
01261-2618   SWR   2     CPM pair                                                                Skf2004 
01262+3435   WSI  96     Provisionally designated WSI9101.                                       Tok2010 
                         The initial observations of WSI 96 by Mason et al. (2011) are           Msn2011d
                         considered spurous. The pair resolved by Roberts et al. (2015) using            
                         AO is believed to be a different pair, whose magnitude difference               
                         would have been beyond the dm limit of speckle. The original WSI 96             
                         designation was retained, however. Spectral types of the components             
                         are estimated as F7V and M2V, masses as 1.4 and 0.4 Msun.               Rbr2015b
01263+0711   LDS9118     Old LDS6118.                                                                    
01263-0440   TOK 204     Possible physical companion at 24".4, 227deg in 2MASS.                  Tok2012a
                         Direct motion by 20deg since first resolution in 2011, at constant              
                         separation. Estimated period ~10yr. The small RV amplitude suggests an          
                         orbit in the plane of the sky.                                          Tok2013b
01264+5929   STI 213     STI1607.                                                                        
01265+1812   HDS 187     Also a spectroscopic binary with P = 3087d which cannot be the visual   Grf2015b
                         pair.                                                                           
01267-7408   OGL 191     SMC122.1.1145  + SMC122.1.1144                                          Pli2012 
01269-5023   ART   1     Low-mass wide double, discovered on 2MASS and Digital Sky Survey                
                         frames. Artigau et al. determine sectral types M6.5V +/- 0.5 and M8V    Art2007 
                         +/- 0.5, distances 63 +/- 5 and 61 +/- 6 pc. Based on evolutionary              
                         models, the masses are 0.095 +/- 0.005 and 0.092 +/- 0.005 Msun for an          
                         age > 1Gyr, or 0.020 +/- 0.003 and 0.019 +/- 0.003 Msun for and age             
                         ~30Myr. The projected separation is ~5100 AU.                                   
01270+1500   GWP 190     XMI 201.                                                                Tob2012b
01270+1200   LDS3282     G002-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc. Also known as LIT   5.                   
                         NLTT 4817/4814                                                          Chm2004 
01270-0009   STF 125     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01270-3058   RSS   3     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
                         SHY 403. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
01270-3233   LDS2199     Some unconfirmed early observations. A is the semiregular variable              
                         R Scl.                                                                          
01270-7405   OGL 192     SMC122.2.1199  + SMC122.2.1250                                          Pli2012 
01271-5158   SHY 404     HIP   6772 + HIP   6804.                                                        
01274-0204   J  1446     BAL 6.                                                                          
01274-2220   RST2261     CD-22@503.                                                                      
01275+1546   BPM  31     [PM2000]   54366 + [PM2000]   54359.                                    Gvr2010 
01276+6429   TDS1882     CD: Originally 01276+6430 TDS1882; primary found to be C component of           
                         01276+6429.                                                                     
01276+0402   GWP 192     XMI 202.                                                                Tob2012b
01277+6321   STI 215     MLB 382.                                                                        
01277+4524   BU  999     ome And = 48 And                                                                
                         This cannot be the close 254.9-d spectroscopic binary.                  Grf2011b
                         Although the pair has been repeatedly resolved with the CHARA Array             
                         with the Separated Fringe Packet technique, a full solution is not      CIA2010 
                         yet complete.                                                                   
             CIA   4     Aa,Ab: Combined solution by Farrington et al. (2014) yields masses              
                         0.993 +/- 0.056 and 0.888 +/- 0.058 Msun, as well as an orbital                 
                         parallax 39.12 +/- 1.97 mas (compared with the Hipparcos parallax of            
                         34.94 +/- 3.1 mas).                                                     CIA2014a
             BU   82     CD: There is a faint star between the AB and CD pairs. The change in            
                         AC is due to the proper motion of A. This is common to AB.              Bu_1894 
01277+1620   BPM  32     [PM2000]   54497 + [PM2000]   54549.                                    Gvr2010 
01277+0521   BU 1164     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.51 +/- 0.76, 2.67, and 1.05 Msun, respectively.  Mlk2012 
01278+5928   STI1618     STI 217.                                                                        
01281-5238   CVN   2     Both the B and C companions are probably background objects.            Cvn2005a
01282+1244   GWP 193     XMI 203.                                                                Tob2012b
01283+5329   STF 123     AB: Also known as HU 1651, but the 1911 Hussey measure has a quadrant           
                         flip and a large sep error.                                             Hu_1911 
01283+1731   GWP 194     XMI 204.                                                                Tob2012b
01283+1429   AG   18     B is BD+13@217.                                                                 
01283-1615   LDS3284     NLTT 4889/4888                                                          Chm2004 
01284+0758   S   398     STTA 19. B is BD+07@214.                                                        
                         HJL  19.                                                                HJL1986 
01284-4319   gam Phe     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Luyten (1936).                                                          Luy1936 
01287-4710   LDS  48     Aka UC  562.                                                                    
01289+0633   PLQ  16     LDS3285.                                                                        
01290+7412   HJ 2045     LDS1529.                                                                        
                         A is above MS, B on the MS. A component possibly a close double         Mkr2005 
                         (Makarov & Kaplan 2005) but nothing on the close sub-system in SIMBAD.  Tok2014d
01291+2143   HO    9     BC: According to Griffin, the radial velocities of B and C differ by    Grf1987c
                         30km/sec. Either the pair is optical, or one component is a                     
                         spectroscopic binary.                                                           
                         AB and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
01291+1040   GWP 195     XMI 205.                                                                Tob2012b
01292+4820   BWL   6     AC: Source appears spatially extended; probably a background galaxy.            
                         Primary is G 172-56.                                                    Bwl2015 
01295+6319   MLB 330     This pair was purged from an earlier edition of the WDS as it was not           
                         found by Heintz. It has apparently been located. It and the nearby              
                         MLB 329 are in NGC 559.                                                 Hei1985a
01295+3054   BUP  20     B is BD+30@229.                                                                 
01296-2138   SEE  14     48 Cet.                                                                         
01297+4228   ZUC   6     SKF 314.                                                                        
                         Primary is white dwarf WD 0126+422 = GD 13.                             Zuc1992 
01297+2250   A  1910     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 6.11 +/- 1.86, 4.31, and 2.09 Msun, respectively.  Mlk2012 
01298+1014   CHR 197     First detected as an occultation binary by Africano.                    Afr1977b
01299+3100   ENG   6     B is BD+30@232.                                                                 
01300-2231   I   445     A,BC = LDS  51.                                                                 
01302+0609   STH   6     A: mu Psc = 98 Psc                                                              
01305-4242   I  1609     SY Phe, an Algol type eclipsing binary, P = 5.27095d.                   Zas2012 
01306-4446   DHI   1     At a distance of 40 +/- 14pc, the projected physical separation is 130          
                         +/- 50AU. Spectral types are M9.0 +/- 0.5 and L6 +/- 1. Dhital et al.           
                         conclude the pair is physical.                                          Dhi2011 
01307-1227   GAL 309     Object #45 in Gallo's original list.                                    Gal1912a
01309+5244   GIC  23     G173-002/G173-003.                                                              
                         NLTT 4991/4993                                                          Chm2004 
01312+7016   38 Cas      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright & Pugh (1954).                                                   Wri1954 
01315+1521   BU  506     eta Psc = 99 Psc. A is a Beta CMi-type variable.                        Baz1964 
01316-1901   HJ 2052     B is BD-19@263. BDS 796, HJ 3373 same star.                                     
01317+6103   STF 128     STI 227.                                                                        
01317+1506   CHR 198     First detected as an occultation binary by Beavers.                     Bvr1977 
01319+1603   BF Psc      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin (1975).                                                         Grf1975a
01319+1026   GWP 196     XMI 206.                                                                Tob2012b
01320-1604   GAL 310     Object #46 in Gallo's original list.                                    Gal1912a
01321+1657   STF 132     A is a spectroscopic binary, P = 36.6d.                                         
                         A: SB2. Combined orbit including RV data and Hipparcos Intermediate             
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.14 + 1.02, L/Lsun = 5.40 + 1.41, dm = 1.46 mag,                      
                         log age = 9.86.                                                         WaX2015b
                         AB: H 4 130.                                                            MEv2010 
                         AB, AC, and AD: Optical pairs, based on study of relative motion of             
                         the components using the method of apparent motion parameters.          Kiy2008 
01321+1434   BPM  33     [PM2000]   57016 + [PM2000]   57059.                                    Gvr2010 
01323-2633   ARG   4     B is CD-27@523.                                                                 
01325+1645   BPMA  1     [PM2000]   57224 + [PM2000]   57397.                                    Gvr2010 
01325+1417   LDS1102     NLTT 5103/5102                                                          Chm2004 
01326-2745   LDS2206     NLTT 5136/5135                                                          Chm2004 
01326-4944   SHY 405     HIP   7189 + HIP   7086.                                                        
01327+6336   EVS   9     Primary is the Cepheid V636 Cas.                                        Evs2016a
01327-0139   FIL   2     B is BD-02@235.                                                                 
01328+3551   STF 133     Confusion between C and D in ADS. With quadrant for CD north preceding,         
                         AC obviously has greater separation than AD.                            B__1962d
                         Identifications of several later AC and AD measures were switched to            
                         give motion consistent with earliest measures. Quadrants were flipped           
                         for CD measures, which now agree with AC and AD measures. AC has                
                         smaller separation than AD, and C is slightly brighter than D.                  
             A  1911     Ea,Eb: Originally 01238+3553; found to be E component of 01328+3551.            
01329+1954   LDS3289     NLTT 5133/5127                                                          Chm2004 
01329+1200   GWP 197     XMI 207.                                                                Tob2012b
01329-3652   GC 1881     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01330+1027   GWP 198     XMI 208.                                                                Tob2012b
01331-0602   LDS3290     NLTT 5155/5154                                                          Chm2004 
01331-1951   LDS1103     NLTT 5163/5169                                                          Chm2004 
01332+6041   STF 131     Spectrum of B: B3IV.                                                            
01332+3231   SEI  17     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
01333-0014   UC  582     aka ITF  47.                                                                    
01333-2411   LDS2209     NLTT 5178/5160                                                          Chm2004 
01335+6039   BUP  22     B is BD+59@273.                                                                 
01337-1213   HWE   4     The linear formula by Job & Tamburini seems ruled out, as it makes      Job1969b
                         the current quadrant opposite to what is observed.                              
01343-0827   A   314     Derived orbital parallax 0".00978, mass sum 4.14 +/- 2.34 Msun          Lin2004a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.85 +/- 0.99, 2.60, and 1.20 Msun, respectively.             Mlk2012 
01344+4844   ES 2587     G172-061. Not a common proper motion companion after comparison with            
                         POSS2 red plates                                                        Oso2004 
01344-1607   FAR  25     Primary is white dwarf WD 0131-163.                                     Far2006 
01345+1448   LDS9119     Old LDS6119.                                                                    
01347+0720   GWP 199     XMI 209.                                                                Tob2012b
01348+2935   BRT   5     An Algol-type system, RS Tri.                                                   
01349+1234   STF 136     AB: H 4 131.                                                            MEv2010 
01349-6909   GLI  12     B is CPD-69@74.                                                                 
01350-2955   BU 1000     AB,C triple+var solution (AB in HIP).                                   Sod1999 
                         B is 0.47d eclipsing binary (= BB Scl).                                         
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
01352-1829   RSS  49     CPD-19@169                                                                      
01354+6305   MLB 280     Also classified K1V.                                                            
01354+4123   ES 1494     Probably identical with ADS 1241 ( = ALD).                                      
01356+6117   STI 237     This and STI 239 are members of the multiple system HJ 1083.                    
01360+2646   BU  507     Morlet et al. note that this has similar position angle, separation,            
                         and delta-m as HDS 212. HDS 212 removed.                                Mor2000 
01360+0739   STF 138     D is BD+06@245.                                                                 
                         AB: H N  92.                                                            MEv2010 
01361-2954   HJ 3447     tau Scl. Arend orbit rejected from Fourth Orbit Catalog                 Ard1968 
                         ("orbit completely faulty and irreparable")                             Wor1983 
01361-3718   HJ 3448     Spectral type of A may be K. B is CD-37@605.                                    
01364+7909   STF 127     B is BD+78@50.                                                                  
01364+3209   SEI  18     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
01368+4124   BUP  23     ups And = 50 And. A is a spectroscopic binary.                                  
                         AB: exoplanets with P=4.61d, 237.7d, 1302d, 3848d                       Tok2014d
             LWR   1     AD. Determined to be CPM pair from examination of POSS I and II plates          
                         (epochs 1953 and 1995), plus 2MASS. Conclude spectral type of                   
                         companion M4.5V.                                                        Lwr2002 
                         AD: Raghavan et al. (2010) consider D physical, high PM (no PM given).  Rag2010 
             ups And     A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Butler       CPS1999b
                         et al. (1999).                                                          HaI2001 
01372+1147   TOB9002     Measured as HJ   16 but actually an anonymous pair added here.          Tob2010 
                                                                                                 Dam2012 
01373+1828   GWP 204     XMI 210.                                                                Tob2012b
01374+2510   G034-039    Boden et al. (2006) give combined spectroscopic/interferometric         Bod2006 
                         solution, including PTI observations. Derive distance of 42.23 +/-              
                         0.21 pc (pi = 23.68 +/- 0.12 mas), age 9.12 +/- 0.25 Gyr, with                  
                         abundances near solar. The K0IV primary appears to have evolved off             
                         the MS and is traversing the Hertzsprung gap toward red giant phase.            
                         Masses are 1.072 +/- 0.014 and 0.8383 +/- 0.0081 Msun, luminosities             
                         2.451 +/- 0.041 and 0.424 +/- 0.023 Lsun, radii 2.048 +/- 0.081 and             
                         0.887 +/- 0.071 Rsun.                                                           
01374-8217   GLI  14     Spectrum G5III:+K1/2.                                                           
01375-1135   LDS9120     Old LDS6120.                                                                    
01376+2233   STTA 20     B is BD+21@218.                                                                 
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence.                                                             
01376+1727   GWP 205     XMI 211.                                                                Tob2012b
01376+0709   PLQ  19     HJL  21.                                                                HJL1986 
01376-0645   BRG   5     BC: Initially entered as WDS 01369-0648, the primary of BRG 5 was               
                         later found to be the B component of 01376-0645 CAB 3.                          
01376-0924   KUI   7     1982.7657: This autocorrelogram was remeasured; the new results are             
                         listed here.                                                            McA1987b
                         Combined spectroscopic/visual orbit, also yielding orbital parallax             
                         and component masses and absolute magnitudes.                           Tok1993 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Martin et al. (1998) derive component masses 1.712 +/- 0.296 and                
                         1.140 +/- 0.226 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 0.43, 2.49, and 1.13 Msun, respectively.             Mlk2012 
01379-8259   TOK 426     HIP 7601 is a nearby (27pc) dwarf also known as GJ 67.1 or HR 512.              
                         According to Wichman et al. (2003 A&A, 400, 293), it is a young                 
                         spectroscopic triple detected in X-rays (1RXS J013755.4-825838). GCS            
                         also recognized the star as SB2. Spectroscopic monitoring (Tokovinin,           
                         in preparation) shows that all three components are similar stars of            
                         approximately one solar mass. Here we resolved the outer subsystem AB           
                         and observed its fast motion. In fact it was already resolved at SOAR           
                         on 2011.036 at 221.0deg and 0".044, but this low-quality observation            
                         has not been published. The available data indicate that the period             
                         of AB is 1.35years; the pair completed nearly two revolutions since             
                         its first resolution in 2011.                                           Tok2015c
01380+4600   HJ 2063     Aka A   944AB,C.                                                                
01385+7302   HJ 2054     40 Cas.                                                                         
01386-4113   CPO 110     B is CD-41@445.                                                                 
01387+0359   GWP 208     XMI 212.                                                                Tob2012b
01387-4515   HJ 3451     LDS  55.                                                                        
01388-1758   LDS 838     LUY 726-8. L 726-8 = UV Cet. Both components are active flare stars             
                         According to Harrington & Behall the mass ratio is 0.487 +/- 0.011 and          
                         the individual masses are 0.115 (0.008) 0.109 (0.008) Msun for A & B,           
                         respectively.                                                           Hrr1973 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         This pm star with flare characteristics is a difficult object.          VBs1954 
                         Magnitude uncertain due to flares.                                      USN1988b
                         AB: Kervella et al. (2016) derive a new orbit for GJ 65 and determine           
                         the following physical parameters:                                              
                            masses (Msun): A = 0.1225 +- 0.0043   B = 0.1195 +- 0.0043                   
                            radii (Rsun):      0.165  +- 0.006        0.159  +- 0.006                    
                            [Fe/H] (dex):     -0.03   +- 0.20        -0.12   +- 0.20                     
                            log (cgs):         5.092  +- 0.015        5.113  +- 0.015            Krv2016 
01393+1638   BU    5     103 Psc.                                                                        
01394-1748   HJ 2067     HJ 3380.                                                                        
01397+4602   EGB   1     ES 553.                                                                         
01397-3728   HJ 3452     B is CD-38@572.                                                                 
01398+1704   BPM  34     [PM2000]   61379 + [PM2000]   61385.                                    Gvr2010 
01398-5612   DUN   5     Some measures have been corrected by Andrew James (personal                     
                         correspondance). Note that this is p Eri, not rho Eri                           
                         (03027-0741BU   11).                                                            
                         Measures of 1947.60 and 1947.84 made by triangulation of multiple       Der9999 
                         measures.                                                                       
01399+1515   STF 142     B is BD+14@@251.                                                                
01400+2702   ALP   5     2MASSW J0140026+270150                                                          
                         Companion seen as elongated in I-band image taken at WIYN in August             
                         2002. Physical companionship to this ultracool dwarf ruled out.         AlP2007 
01400-1348   GAL 311     Object #48 in Gallo's original list.                                    Gal1912a
01404+3420   STF 143     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01405-0917   LDS9121     Old LDS6121.                                                                    
01406+4035   BU 1362     tau And = 53 And. A is a spectroscopic binary. Variable?                        
01409+6410   RAO  32     AC: C component = A component of WDS 01409+6409 TDS1951.                        
01409+6409   TDS1951     Primary = C component of WDS 01409+6410.                                        
01409+1117   A  2320     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.33 +/- 0.76, 2.02, and 0.95 Msun, respectively.             Mlk2012 
01409+4952   HU  531     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.66 +/- 0.98, 2.11, and 0.79 Msun, respectively.  Mlk2012 
01409+0138   A  2404     Quadrant uncertain.                                                             
01410-0524   TOK 228     Primary is EY Cet, variable of BY Dra type, X-ray source                Tok2014d
01412-6741   LDS  56     HIP 7869. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         Primary is V773 Cas and SB2, P=1.294d. B at 33.5" 219deg, optical?              
                         CPM according to SIMBAD.                                                Tok2014d
01413+2545   STF 145     Period of AB estimated at 7300y.                                        Tok2006 
                         Primary is SB2, P=4.435d. Aa,Ab has suspected close tertiary because            
                         K1,K2 are var, e>0. B is SB1, P=1.435d.  RoboAO find a companion to B           
                         (98deg, 4.80", dI=7.2mag), but it is considered optical.                Tok2014d
01413+1246   GWP 214     XMI 213.                                                                Tob2012b
01413+1007   STF 146     B is BD+09@203.                                                                 
                         HJL  22.                                                                HJL1986 
01414+3704   LDS3300     NLTT 5619/5621                                                          Chm2004 
01414-7909   HJ 3467     tau 1 Hyi                                                                       
01417+0712   GWP 215     XMI 214.                                                                Tob2012b
01418+4237   MCY   2     An astrometric binary now resolved by infrared speckle interferometry.          
                         Discovery designation per Todd Henry 03/02/98.                                  
                         Improved pc (Delta m > 6) orbit combining pg (Lippincott 1983) and      Lip1983 
                         Hipparcos obs. Scaling by the speckle IR (Henry 1993) gives orbit size  Hen1993 
                         and mass ratio.                                                                 
                         Martin et al. (1998) derive component masses 0.795 +/- 0.159 and                
                         0.136 +/- 0.053 Msun.                                                   Mig1998 
                         The estimated magnitude difference in V (~6 mag) is too large for the           
                         companion to have been detected.                                        Hrt2009 
01419-0907   GRV1170     Aka SLW  81.                                                                    
01420+4252   ROE  64     HJL  23.                                                                HJL1986 
01423+5134   CUD   2     Component A is the central star of the planetary nebula NGC 650/1       Skf2013 
                         = Messier 76.                                                                   
01424+2609   BRT3259     Originally published as BRT 126.                                        Brt1928 
01424-0645   A     1     A premature orbit has been computed.                                            
                         Omega corrected from 24.0 to 58.9, omega from 58.9 to 24.0              Ruy1995 
01425+5000   B  2550     BD+49 440 (8.5) and 441 (9.0) are together in a high power field. Both          
                         are close pairs; brighter star is deep orange, the fainter (ADS 1341,           
                         HU 1210) is white. At present the brighter star is the easier pair,             
                         but as its duplicity was missed by Hussey, Aitken, and van Biesbroeck,          
                         then they measured CD, it must have opened out more recently.           B__1963b
01425+2016   HJ 2071     A: 107 Psc.                                                                     
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             107 Psc     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01426+6033   BU 1363     A 3588-d spectroscopic orbit has been found for the A component.        Grf2012d
                         The primary is the E component of 01426+6033.                                   
01427+0637   J  1808     HJL  24.                                                                HJL1986 
01430+6402   STI 264     Component A is a pulsating star in the open cluster NGC 637. Since              
                         relative motions of all three components are small and in agreement             
                         with each other, we believe all three stars are members of the same             
                         cluster. It is not currently possible to determine whether of not they          
                         form a closed triple system.                                            Kiy2012 
01431+3426   COU 668     Aa,Ab: TDS1964.                                                                 
01431+2101   JNN 251     Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.15 +/- 0.03              
                         Msun; a ~4.8 AU.                                                        Jnn2014 
01432+6056   MLR 106     AC: STI 271.                                                                    
01433+6033   BU 1103     44 Cas. A is a spectroscopic binary.                                            
             FYM 160     AH: Fay (2013) notes an H component in their Figure 1, but does not     FyM2013d
                         include a measurement.                                                          
             ARN  32     AE: E component is primary of 01426+6033 BU 1363                                
01433-1736   HJ 3455     B is BD-18@292.                                                                 
01434-0705   STF 150     B is BD-07@283.                                                                 
01434-1127   GAL 312     Object #50 in Gallo's original list.                                    Gal1912a
01435+5318   HJ 2069     B is BD+52@417.                                                                 
01435-1038   GAL 313     Object #51 in Gallo's original list.                                    Gal1912a
01436+2802   GIC  24     G072-028/G072-029.                                                              
                         NLTT 5738/5740                                                          Chm2004 
01437+5014   CIA   6     Phi Per. Be+sdO binary, resolved by the CHARA Array. The hot subdwarf           
                         companion is detected in near-IR; flux contribution 1.5% in H (dH=4.6)          
                         and restricted fits indicate flux contribution rises to 3.3% (dV~3.7)           
                         in visible.  Combined interferometric/spectroscopic orbital solution            
                         yields masses 9.6+/-0.3 and 1.2+/-0.2 Msun for the Be primary and               
                         subdwarf secondary, respectvely. The inferred distance (186+/-3pc),             
                         kinematical properties, and evolutionary state are consistent with              
                         membership of phi Per in the alpha Per cluster.                         CIA2015a
01437+0934   BU  509     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.69 +/- 0.64, 1.83, and 0.85 Msun, respectively.             Mlk2012 
01438+1954   GWP 216     XMI 215.                                                                Tob2012b
01438+1206   HJ   18     Possibly BD+11@225. BDS 899, HJ 18. HJ position angle in 1820: 220@.            
                         Disagrees with 1912 - 1922: 143@.                                               
01441-1556   BUP  25     tau Cet = 52 Cet. Optical. Proper motion of A -1718 +856.                       
01442-0813   LDS9122     Old LDS6122. Primary is QSO, Z=0.239.                                           
01443+6652   HAU  10     HJL  25.                                                                HJL1986 
01443+5732   BU  870     A premature orbit has been computed.                                            
                         Primary is eclipsing binary V773 Cas (period 2.58734 day).              Zas2010 
             ARN  55     AD: HJL1011.                                                            HJL1986 
01443+0929   KPR   1     AC: Separation may be a factor of 10 too small.                                 
             STF 155     AB: H 2  49.                                                            MEv2010 
01448+5708   B  2548     Rapid motion.                                                                   
                         This close pair precedes BD+56 338 (ADS 1371, BU 453) by 12 sec of              
                         time and is 0.6' north of it. All measures given in Pub Yerkes O. IX,           
                         pt 1 and 2, by van Biesbroeck and myself, assigned to BU 453, are               
                         obviously of the new pair. My estimates of the difference in magnitude          
                         vary between 0.4 sf and 0.7 np, which seems rather large to be error            
                         of estimation, even in so close a pair.                                 B__1963b
01449+2005   109 Psc     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                         (2000).                                                                 HaI2001 
01449+1951   A  2322     EU Psc, Algol (EA) type eclipsing binary,  per 1.69261 d.               Zas2011 
                         Observed wrong star? van den Bos has 4 measures in 1962, and I have     B__1963b
                         positive measure in 1964.                                               Wor1967b
01450+6032   STI 281     AB: BKO1073AC.                                                                  
             MRI  27     AC: BKO1073AB.                                                                  
01450+5707   BU  453     Premature orbits have been calculated. Motion direct.                   Baz1972 
01450+2703   COU 750     Rapid motion.                                                                   
01450-0104   LDS9123     Old LDS6123.                                                                    
                         NLTT 5822/5818                                                          Chm2004 
01452+2317   GIC  25     G034-048/G034-049.                                                              
01454+0909   OCC9041     110 omi Psc.                                                                    
01454-3957   BRG   6     2MASS J01452133-3957204 has only been observed in one epoch, but the            
                         color and brightness of the detected companion are consistent with              
                         expectation, hence we count it as an unconfirmed binary.                Jnn2012 
01455-6035   JSP9001     Previously known as JSP  13a.                                                   
01456+1148   GWP 217     XMI 216.                                                                Tob2012b
01456-0224   J  1448     BC. Gauchet (1926) measure originally listed as CD pair, with theta     Gau1926a
                         flipped by 180deg.                                                              
01456-2503   HJ 3461     eps Scl. A premature orbit has been computed.                                   
01457+0834   BAG  38     Primary is the alpha2 CVn type variable UZ Psc.                                 
01458+1200   BPM  35     [PM2000]   64864 + [PM2000]   64876.                                    Gvr2010 
01458+0043   GWP 219     XMI 217.                                                                Tob2012b
01459+7142   HJ 1090     01459+7142FOX 119CD. WDS designation for HJ 1090 changed from                   
                         01461+7143 due to inclusion in multiple.                                        
01459-4357   HJ 3463     B is CD-44@509.                                                                 
01460+8005   GW Cep      Multiple system including contact binary.                               Pbl2006 
01460+6113   STF 151     STF 151rej and Duner 1 are identical.                                           
01462+5326   HJ 2079     Confused with nearby 01463+5328 HJ 2080, as pairs are also of similar           
                         separation and position angle.                                                  
01462+3343   HU  804     A premature orbit has been computed.                                            
01463+5328   HJ 2080     Confused with nearby 01462+5326 HJ 2079, as pairs are also of similar           
                         separation and position angle.                                                  
01466+1639   GWP 221     XMI 218.                                                                Tob2012b
01467+0214   GWP 222     XMI 219.                                                                Tob2012b
01469+4234   DUP   1     Dupuy et al. (2015) resolved a low-luminosity T9/Y0 binary, using Keck          
                         laser guide star imaging. Masses are estimated as 4.6 +1.0/-1.1 and             
                         4.3 +1/0/-1.2 Mjup (for age of 1Gyr) or 16.9 +3.8/-4.0 and                      
                         15.9 +3.5/-4.4 Mjup  (for age of 10Gyr).                                Dup2015 
01474+0355   HJ 2084     Aka STT  36.                                                                    
01474-2157   GD 1400     Song et al. (2006) confirm common proper motion of this brown dwarf     Son2006 
                         and its planetary mass companion.                                               
01475-4955   RED  15     2MASS J01473282-4954478. Spectral types M8: and L2:                     Red2006b
01476+3453   CSW   1     AB: This star has a possible wide brown dwarf companion at 43"          Csw2008 
                         separation, according to Casewell et al. (2008).                        Jnn2012 
             KIR   6     BC: B component is an L0.5V brown dwarf. The spectrum of the secondary          
                         shows it to be a background M star.                                     Kir1999 
01477+6351   ENG   7     A is GJ 75 = V987 Cas. B is BD+63@241.                                          
01477+1643   BPMA  2     [PM2000]   65958 + [PM2000]   65844.                                    Gvr2010 
01478-8011   HJ 3474     tau 2 Hyi                                                                       
01479+4440   A   949     BJN  26.                                                                        
                         This measure was published as BRT 346. Note to BRT 346: This seems to           
                         be ADS 1412, although the magnitude difference is discordant.                   
                         BD+44  369, with which ADS 1412 is identified, was not seen as double.  Brt1939a
01480+4353   ES 1498     BRT 325.                                                                Brt1930 
01481-2533   FAR  26     Primary is white dwarf WD 0145-257.                                     Far2006 
01483+1203   LDS1116     LDS3311.                                                                        
                         NLTT 6012/6013                                                          Chm2004 
01483-4130   RGS   2     GJ 77. Rodigas et al. (2016) detect a companion to the old solar-type           
                         star HD 11112, and determine it is likely a gravitationally bound cool          
                         white dwarf. SED fits (pure-H and pure-He models) suggest a mass for            
                         the companion in the range 0.90-1.08 Msun, Teff 7300-9800K,                     
                         log (L/Lsun) -3.69 - -3.36, and age 2.43-3.92 Gyr.                      Rgs2016b
01486+1618   BU  510     AC: H 5  92.                                                            MEv2010 
01486-0955   JNN  17     LP 708-465.                                                                     
01487+7528   HJ 2075     LDS1540.                                                                        
01487+3306   GIC  26     G072-038/G072-037.                                                              
                         NLTT 6030/6027                                                          Chm2004 
01487-2916   HJ 3466     B is CD-29@590.                                                                 
01488-0125   STF 171     B is BD-02@300.                                                                 
01489+1411   GWP 223     XMI 220.                                                                Tob2012b
01489-2053   ARA1256     Primary is TW Cet, a W UMa type eclipsing binary, P = 0.31685d.         Zas2012 
01489-3153   LDS3316     NLTT 6087/6088                                                          Chm2004 
01491+0236   GWP 224     XMI 221.                                                                Tob2012b
01493+4754   CHR   4     Aa,Ab: Although this new component is indicated as Aa,Ab we have not            
                         firmly established whether it is associated with the A or B component           
                         of the wide pair.                                                       McA1987b
                         B is a spectroscopic binary. The system appears to be quintuple.                
01493+1808   GWP 225     XMI 222.                                                                Tob2012b
01496+1741   GWP 226     XMI 223.                                                                Tob2012b
01496-1041   ENG   8     53 Cet = chi Cet. LDS2222.                                                      
                         SHY   8. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
01497-1414   HU  422     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.42 +/- 0.46, 2.45, and 1.20 Msun, respectively.             Mlk2012 
01498-3824   GC 2219     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
             HDO 186     Additional notes may be found in Herschel (1847).                       HJ_1847b
01499+8053   STT  34     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.28 +/- 6.95, 4.72, and 2.24 Msun, respectively.            Mlk2012 
01499+1324   LDS1118     Also known as LDS6124 and LDS9124. Richard Jaworski first               Jaw2006 
                         recognized that these systems were the same.                                    
01501+3538   ALI  28     No stars seen at AC catalog locations - probably plate flaws.                   
01501+2217   STF 174     1 Ari. Spectrum composite; K1III+A6V. Spectroscopic binary?                     
                         H 1  73.                                                                MEv2010 
01502+1600   BPM  36     [PM2000]   67462 + [PM2000]   67449.                                    Gvr2010 
01503+1146   GWP 227     XMI 224.                                                                Tob2012b
01504+2942   MLB1059     Aka MLB 448.                                                                    
01509+1626   BPM  37     [PM2000]   67854 + [PM2000]   67921.                                    Gvr2010 
01509+1031   GWP 228     XMI 225.                                                                Tob2012b
01510+2107   STF 175     AB: H 2  56.                                                            MEv2010 
01511+1135   BPM  38     [PM2000]   68017 + [PM2000]   67969.                                    Gvr2010 
01512+2439   HO  311     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.19 +/- 1.30, 3.38, and 1.40 Msun, respectively.             Mlk2012 
01513+6451   STF 163     B is BD+64@244.                                                                 
01513-3800   LDS9125     Old LDS6125.                                                                    
01514+4329   HJ 2089     B is BD+42@388.                                                                 
01515+0457   STF 177     Formerly, BD+04@320. Corrected by Weis.                                         
01515-0744   HIP   8653  Small acceleration of 2 mas yr-2, possibly single.                      Tok2012a
01515-1020   BNU   1     Aa,Ab: zet Cet = 55 Cet. A is a long-period spectroscopic binary,               
                         P = 1652d, and has been resolved by speckle interferometry.                     
                         B is BD-11@360.                                                                 
01515-1858   LDS9126     Old LDS6126.                                                                    
01516+1618   BPM  39     [PM2000]   68302 + [PM2000]   68249.                                    Gvr2010 
01518-5458   SHY 128     AC: HIP   8687 + HIP   7387.                                                    
01519+6426   GIC  27     G244-037/G244-036 = GJ 3117A/3118B.                                             
01520+1049   STF 178     H 1  56.                                                                MEv2010 
                         Additional notes may be found in Couteau (1952).                        Cou1952a
01521+5430   SMA  24     Also known as STI1703.                                                          
01522+6627   STF 167     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
01522-5220   CVN   3     CPM pair. The spectral type of the B component is M9.5 +/- 1,                   
                         Teff = 2100 +/- 200K; age ~30 Myr, mass 25 +/- 10 Mjup.                 Cvn2005a
01523-0620   LDS9127     Old LDS6127.                                                                    
01525+1710   GWP 232     XMI 226.                                                                Tob2012b
01528+4016   MLB 999     BRT 2198.                                                                       
01528+1544   BPM  40     [PM2000]   69032 + [PM2000]   69018.                                    Gvr2010 
01528+0117   GWP 233     XMI 227.                                                                Tob2012b
01530-2805   HJ 3472     SWR   3. CPM pair                                                       Skf2004 
01531+2935   BUP  27     alp Tri = 2 Tri. A is a spectroscopic binary, P = 1.77d.                        
01532+3719   STF 179     H 1  89.                                                                MEv2010 
01533+4044   HJ 1094     55 And.                                                                         
01534+7003   STF 169     Primary is V776 Cas, a W UMa type eclipsing binary, P = 0.44042d.       Zas2012 
01535+1918   STF 180     gam Ari = 5 Ari. According to R.G. Aitken, Robert Hooke noted this as   A__1935f
                         a double in 1664. Hooke wrote: "I took notice that it consisted of      Hoo1665 
                         two small stars very near together; a like instance to which I have             
                         not else met in all the heavens."                                       HFC1928 
                         A is a variable of the Alpha CVn type.                                          
                         AB: H 3   9.                                                            MEv2010 
             BU  512     Primary is C component of STF 180. WDS designation changed from                 
                         01538+1918 and components labelled CD.                                          
01536+6324   PTT   3     OL 114, STI 317 are identical.                                                  
01536+0311   xi Psc      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Herbig (1981).                                                Grf1981b
01541-7729   JSP  31     Apparent rapid retrograde motion, but measures sparse.                          
01543+6542   GIC  28     G244-042/G244-041.                                                              
01543-1543   GAL 314     Also known as LDS1120.                                                          
                         Object #55 in Gallo's original list.                                    Gal1912a
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             CHM   3     AC. NLTT 6398 + 6395.                                                           
01544-2250   LDS3322     NLTT 6400/6399                                                          Chm2004 
01544-4230   phi Phe     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Chemically peculiar late-B star, initially thought to be a triple,              
                         with spectroscopic period 41.4d and astrometric period 878d. Using              
                         Coralie spectra from 2000-2010, Korhonen et al. (2013 A&A 553, A27)             
                         find a spectroscopic period of 1126d. Spectroscopic data by Pourbaix            
                         et al. (2013) exclude the 40d period, but are insufficient to refine            
                         the Korhonen solution. Their spectroscopic elements are combined                
                         with the Hipparcos astrometry to refine the initial astrometic orbit.   Pbx2013 
01546+2049   MKT   3     bet Ari. Astrometry from Mark III interferometer is combined with               
                         spectroscopy (Tomkin & Tran 1987) by Pan et al. (1990) to determine     Tom1987b
                         orbital elements, masses, and distance. Masses agree well with          MkT1990 
                         empirical mass-luminosity relation.                                             
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Pan et al. (1990).                                                      MkT1990 
                         Martin et al. (1998) derive component masses 2.067 +/- 0.203 and                
                         1.281 +/- 0.178 Msun.                                                   Mig1998 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.19 +/- 0.13, 3.51, and 1.82 Msun, respectively.             Mlk2012 
01549+1124   BPM  41     [PM2000]   70299 + [PM2000]   70233.                                    Gvr2010 
01551+2847   STF 183     According to Scardia et al. (2001), orbital elements are well defined;  Sca2001d
                         only the period is still rather uncertain. The Hipparcos parallax               
                         (0".00727 +/- 0.00189) gives a mass sum of 3.8 Msun +/- 82%, in excess          
                         for a binary of type F2. The dynamical parallax (0".0074) agrees well           
                         with the observed one.                                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.82 +/- 2.85, 3.45, and 1.35 Msun, respectively.  Mlk2012 
01551-1204   LDS9128     Old LDS6128.                                                                    
01553-2134   DON  26     CD-22@641.                                                                      
01554+0257   A  2407     A premature orbit has been computed.                                            
01556+0146   BU 1367     A 2408.                                                                         
01559+0151   STF 186     Spectroscopic binary?  Spectrum composite; F7V+G0V.                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.22 +/- 1.22, 2.56, and 1.07 Msun, respectively.             Mlk2012 
01560+0529   GWP 236     XMI 228.                                                                Tob2012b
01560+0046   RST5186     BD+00@311a.                                                                     
01560-5137   HJ 3473     chi Eri                                                                         
01561+6035   AG  301     HJL  26.                                                                HJL1986 
01561+3745   HJ 1097     ALI 494.                                                                        
01562+3715   BU 1368     Bb: b is BD+36@349.                                                             
             STFA  4     56 And. B is BD+36@354.                                                         
01563+0829   GWP 237     AB: XMI 229AB.                                                          Tob2012b
             GWP 238     AC: XMI 229AC.                                                          Tob2012b
01564+3650   J  2719     ALI 259.                                                                        
01568+3931   ALI1022     Not found by Heintz at IDS position.                                    Hei1990b
01568+3802   TOB9001     BC: A measure by Espin incorrectly attributed to this pair led to its           
                         earlier designation as 01569+3759ES  228CD.                                     
01568+2303   BVD  21     RoboAO resolved the B component (201.1deg, 0.199", dI=1.61 mag) but             
                         the pair was not accepted as real.                                      Tok2014d
01570+3101   A   819     A premature orbit has been computed.                                            
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.97 +/- 1.00, 2.49, and 1.20 Msun, respectively.  Mlk2012 
                         AB,C: HJL  27.                                                          HJL1986 
01571+1517   BPM  43     [PM2000]   71640 + [PM2000]   71653.                                    Gvr2010 
01571+1414   BPM  42     [PM2000]   71596 + [PM2000]   71608.                                    Gvr2010 
01572+1644   GWP 241     XMI 230.                                                                Tob2012b
01572-1015   GAL 315     LDS  60. Object #56 in Gallo's original list.                           Gal1912a
                         HIP 9094. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 6529/6530                                                          Chm2004 
01575+5558   ES 1811     STI1732.                                                                        
                         Vatican zone coordinates yield 1911.9, 295.2, 5.61, showing Espin's             
                         distance is too small and that there is no change so far.               VBs1954 
01576+4205   YSC 125     There is some evidence of a very faint third component in this system           
                         with separation of 0.45 arcsec.                                         Hor2011b
             NLTT 6522   Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 0.99 +/- 0.11 and 0.75 +/- 0.05 Msun.    Ren2010 
01577-3625   LDS  62     LDS5359. TSN  72.                                                               
01579+2336   H 5  12     H V 12. STTA 21. 9 Ari = lam Ari. A is a Beta Lyrae-type and                    
                         spectroscopic binary.  B is BD+22@289.                                          
                         AB: HJL  28.                                                            HJL1986 
01579+0924   GWP 243     XMI 231.                                                                Tob2012b
01579-2851   LDS  61     NLTT 6581/6583                                                          Chm2004 
01581+4123   S   404     Same as STF 190 rej, SHJ 404, H IV 104, H 4 104, H IV 128, H 4 128.             
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01583+0250   GWP 245     XMI 232.                                                                Tob2012b
01583-8218   I   311     Composite spectrum: G8/K0(V)+(G).                                               
01584+2547   A  2011     B is strongly above MS, very red in V-K (wrong 2MASS ptm?). Hipparcos           
                         does not resolve AB, but has X-solution and suspected non-single.       Tok2014d
01584-2304   LDS3330     NLTT 6605/6606                                                          Chm2004 
01585+3643   J  1809     ALI 262.                                                                        
01586+3834   LPL   1     La Palombara et al. (2012) detect a companion to the hot subdwarf               
                         BD+37 442, using the XMM Newton satellite. The companion is thought to          
                         be a white dwarf or neutron star, likely powered by accretion from the          
                         wind of the primary.                                                    LPl2012 
01586-5332   HU 1557     Primary is CI Eri, an Algol type eclipsing binary, P = 1.23819d.        Zas2012 
01588+1702   GWP 247     XMI 233.                                                                Tob2012b
01588-0949   J  1449     BD-10  410. Previously published declination corrected by +4'.          J__1949a
                         GAL 316. Object #57 in Gallo's original list.                           Gal1912a
01588-2212   HJ 2103     B is BD-22@329.                                                                 
01588-6134   alf Hyi     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
01589-5652   LDS  63     LDS6106 = LDS9106 (incorrectly listed in the WDS as 00593-5652).                
                         B is CPD-57@385 = CD-57@396.                                                    
01590-1640   LDS9129     Old LDS6129.                                                                    
01590-2255   H 2  58     H II 58. A is a W UMa-type system, AA Cet.                                      
01591+3313   ENG   9     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
01591+1523   GWP 248     XMI 234.                                                                Tob2012b
01598+1543   BPM  44     [PM2000]   73241 + [PM2000]   73209.                                    Gvr2010 
02000+1334   LDS5181     old LDS6130.                                                                    
02003-0138   BAL   9     J  3333.                                                                Nsn2016 
02004-0831   HJ 3476     AB: A is AR Cet, probably a semi-regular variable.                              
02005-0240   BRG   8     The companion to 2MASS J02002975-0239579 has yet to be tested for               
                         common proper motion, but since its color and brightness are                    
                         consistent with expectation and its separation is small (~0.32"), it            
                         is counted as a physical companion here.                                Jnn2012 
02005-6246   HJ 3479     B is CPD-63@142.                                                                
02006+2753   J  3257     A is an Algol-type binary, X Tri, P = 0.97d.                                    
02011+3518   STF 197     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02011-1741   LDS5362     NLTT 6759/6757                                                          Chm2004 
02012-0729   GWP 250     ABL   1.                                                                Tob2012b
02012-3000   CUS   1     Assuming a primary mass of 1.02 +/- 0.19 Msun, the derived flux ratio           
                         (~0.028 in H and K) gives a mass of ~0.5 Msun for the secondary.        Cus2012 
02013+1227   BPM  45     [PM2000]   74159 + [PM2000]   74128.                                    Gvr2010 
02013-0752   GWP 251     ABL   2.                                                                Tob2012b
02015+1830   BPM  46     [PM2000]   74328 + [PM2000]   74271.                                    Gvr2010 
02019+7332   JNN 252     GJ 3125. Estimated age 30-300 Myr; masses 0.12 +/- 0.07 and 0.06 +/-            
                         0.04 Msun; a ~5.0 AU.                                                   Jnn2014 
02019+2415   POU 157     ID uncertain. Nothing at Pourteau's coordinates.                        Pou1933 
02020+7054   BU  513     48 Cas. A is a spectroscopic binary, same period as the visual pair.            
                         Suspected sub-periods of 39 yr (Baize) and 26 yr (Muller) are not       Baz1941b
                         confirmed by later measures.  The radial velocities of the primary may  Mlr1949c
                         show a trace of a period of about 4 yr (Heintz).                        Hei1981e
                         See Baize & Petit catalog of doubles with variable component.           Baz1989d
                         Masses and bolometric magnitudes are derived for the two components             
                         based on assumed spectral types and available parallaxes.                       
                         1980.7205: This measure was incorrectly attributed to ADS 1958 in               
                         McAlister et al. (1983).                                                McA1983 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.96 +/- 0.42, 3.07, and 2.00 Msun, respectively.  Mlk2012 
02020+0246   STF 202     alp Psc. Both components are listed as Alpha CVn variables of small             
                         amplitude, and both may have variable RV.                               Sca1983f
                         See Baize & Petit catalog of doubles with variable component.           Baz1989d
                         Absolute quadrant for 1998.657 determined by triple-correlation                 
                         techniques                                                              Pru2002b
                         Chevalier identified this star as alp Psc, but gave an incorrect        Che1911 
                         declination, leading to its initial designation as 02020+0320 CHE 32.   Hrt2012b
             PWL   1     AC: SHY 132. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             STF 202     AB: H 2  12.                                                            MEv2010 
02021+0355   OSV   1     LDS5363.                                                                        
02021-1321   GAL 317     Object #59 in Gallo's original list.                                    Gal1912b
02022+7530   STF 185     Primary is V779 Cas, an Algol type eclipsing binary, P = 6.35340d.      Zas2012 
02022-1441   GWP 253     ABL   4.                                                                Tob2012b
02022-1808   GWP 252     ABL   3.                                                                Tob2012b
02022-4550   SHY 410     HIP   9495 + HIP   9672.                                                        
02022-6236   TOK  70     HIP 9499. A is SB, no orbit, dRV=70.7 (Nordstrom et al. 2004).          Nrd2004 
02023-2634   LDS  65     NLTT 6825/6826                                                          Chm2004 
02025-1410   GWP 254     ABL   5.                                                                Tob2012b
02026-1719   GWP 255     ABL   6.                                                                Tob2012b
02027-3019   HJ 3478     B is CD-30@717.                                                                 
02030+3317   STF 201     eps Tri = 3 Tri                                                                 
02031-0725   STF 209     B is BD-08@371.                                                                 
02031-1229   GWP 256     ABL   7.                                                                Tob2012b
02032+5514   BLL   4     A is a semi-regular variable, XX Per. B is BD+54@445.                           
02034+3919   MLB  10     AB: Also known as SMA  27.                                                      
02035+6408   HJ 1101     STI 337 (three Vat1926 measures from STI 337 merged 2008/06/25)                 
02035+1744   BPM  47     [PM2000]   75525 + [PM2000]   75508.                                    Gvr2010 
02037+2556   STF 208     10 Ari. Malkov et al. (2012) derive dynamical, photometric, and                 
                         spectroscopic masses 2.94 +/- 0.84, 2.35, and 1.29 Msun, respectively.  Mlk2012 
02038+7013   MLR 375     1983.0663: This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                  McA1987b
02038-0020   H 5 102     H V 102. 61 Cet. Spectrum composite; G5II-III+G5V.                              
02039+8221   HJ 2090     The measure in BDS by Cogshall belongs to some other pair.              Bu_1906 
                         1904.69, 243.9@, 3.52" (Van Biesbroeck).                                VBs1914 
02039+4220   STF 205     H III 5, SHJ 26. gam And. A quadruple system.                                   
                         Star A (mag 2.3, K3II) forms with BC the pair STF 205, separation 10".          
                         Star B is SB, P = 2.67 d (Maestre & Wright, ApJ 131, 119, 1960).                
                         See discussion by Morgan et al. (1978).                                 BLM1978 
                         A,BC: H 3   5.                                                          MEv2010 
             STT  38     BC: See discussion by Morgan et al.                                     BLM1978 
                         BC: Poor agreement between two theta measures.                          Mlr1956d
                         BC: Additional notes may be found in Muller (1954).                     Mlr1954a
02039+1231   BPM  48     [PM2000]   75778 + [PM2000]   75779.                                    Gvr2010 
02039-4525   RST2272     Primary is SB2, P=0.851 y. Aa,Ab UR in speckle. Koen et al. (2002               
                         MNRAS 331, 45) find 311d photometric period.                            Tok2014d
02042+5257   HJ 2104     B is BD+52@501.                                                                 
02042+4641   ADM   1     HTP  32. HAT-P-32. Primary is exoplanet host star.                      Adm2013 
02042-1039   GAL 318     Object #62 in Gallo's original list.                                    Gal1912b
02044+1230   CHE  36     CHE  37.                                                                        
02046+2525   LTT 17328   Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from the Geneva           
                         Extrasolar Planet Search Programs home page.                            HaI2001 
02046+1757   GWP 257     XMI 235.                                                                Tob2012b
02051+7717   SHJ  22     47 Cas.                                                                         
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             47 Cas      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02051-1737   BEU   3     PM = +1318-174.                                                                 
02053+2906   CHE  38     CD: Originally 02053+2907 CHE  38AB, until C component of 02053+2906            
                         found to be prmary of 02053+2907.                                               
             WAK  14     CE: Originally 02053+2907 WAK  14AC.                                            
02053-2803   LDS  67     NLTT 6979/6980                                                          Chm2004 
02054-5910   HJ 3481     B is CPD-59@185.                                                                
02055+7607   BU  785     49 Cas.                                                                         
02055+0056   LDS5365     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02056+1444   BPM  49     [PM2000]   76857 + [PM2000]   76899.                                    Gvr2010 
02057-2423   I   454     CPD-24@891. C is CPD-24@889.  AB,C = LDS  68.                                   
                         AB,C: SHY 135. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
             WSI   7     Aa,Ab: Tokovinin et al. (2014) derive a combined spectroscopic/                 
                         interferometric orbit of the Aa,Ab pair, as well as a new orbit of the          
                         AB pair. Resulting component masses for Aa, Ab, B, and C are 0.74,              
                         0.72, 0.57, and 0.78 Msun, respectively.                                Tok2014b
02058+1241   CHE  42     There are no obvious errors in applying the offset from Chevalier's     Che1910 
                         plate center, but there are no appropriate pairs near his coordinates,          
                         nor at coordinates found by reversing the sign of either or both                
                         offsets. The pair is likely lost.                                       Hrt2012b
02062-1808   GWP 258     ABL   8.                                                                Tob2012b
02065+5703   BAR  23     J 880.                                                                          
02068+2542   HO  312     11 Ari.                                                                         
02069-1126   SLW  99     Aka ABL   9.                                                                    
02070-1017   GAL 319     Object #63 in Gallo's original list.                                    Gal1912b
02070-4406   JNN 149     2MASS J02070176-4406380 and J02070198-4406444 are separated by only 7"          
                         and have similar estimated spectroscopic distances (13 and 21 pc,               
                         respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                         a physical pair.                                                        Jnn2012 
02074-5941   HJ 3484     B is CPD-60@183.                                                                
02076+1355   ZHN   2     BDK   4. G 73-26 + SDSS J020735.60+135556.3.   Distance 26 +/- 10 pc            
                         for primary, 35 +/- 5 pc for secondary. Estimated age of system 3-4             
                         Gyr. Mass of secondary estimated at 0.079-0.081 Msun.                   Fah2010 
02076-0037   LDS3346     NLTT 7066/7064                                                          Chm2004 
                         HJL  29.                                                                HJL1986 
02079+1343   GWP 259     XMI 236.                                                                Tob2012b
02080+2814   CHE  55     MLB 452.                                                                        
02080-0951   GAL 320     Object #64 in Gallo's original list.                                    Gal1912b
02081+1336   FAR  27     SKF  23.  Primary is white dwarf WD 0205+133.                           Far2006 
02082+1509   LDS5183     old LDS6131.                                                                    
02083+2543   ALP   6     2MASSW J0208183+254253                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this triple.                                                  AlP2007 
02084+2819   KUI 118     G072-058. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 7087/7088                                                          Chm2004 
02085-0641   HDS 285     Possible sub-diffraction-limited component, but the astrometry is not           
                         consistent between the two observations.                                Hor2011b
02087-0026   STF 218     Same as STF 220.                                                                
02089+4927   BWL   9     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3136.                     Bwl2015 
02090+5745   STI1791     AB. WDS designation changed from 02099+5744 when it was determined              
                         that TDS2135 comprised the primary of this wider pair.                          
02091+5104   STF 213     C easily seen 8" north following. Magnitude about 10.5, not 12.5.       B__1963b
02091+4341   LDS3349     NLTT 7117/7118                                                          Chm2004 
02091+4048   STF 215     A is an eclipsing binary, BX And.                                               
02091+1511   GWP 260     XMI 237.                                                                Tob2012b
02093-1958   GWP 261     ABL  10.                                                                Tob2012b
02094+2556   H 6  69     H VI 69. 14 Ari. STTA 23.                                                       
                         AC: HJL1012.                                                            HJL1986 
02094-1011   HJ 2116     Richard Jaworski, in analysis of SuperCOSMOS data, has determined that  Jaw2005 
                         component C is the galaxy NGC 833, D is the galaxy NGC 835, E is the            
                         galaxy NGC 838 and F is the galaxy NGC 839. Thus, in the pairing "CD"           
                         both components are galaxies and not stars.                                     
02095+3459   MKT   4     bet Tri.                                                                        
                         Hummel et al. (1995) visual orbit based on astrometry from Mark III     MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.11 +/- 0.18, 5.26, and 1.82 Msun, respectively.             Mlk2012 
02096+4251   ES   48     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
02097+2021   STF 221     AB: H 3  68.                                                            MEv2010 
02097+0857   GWP 262     XMI 238.                                                                Tob2012b
02098-4052   TOK 427     HIP 10096 is SB2 according to GCS. The separation corresponds to a              
                         period of ~5yr.                                                         Tok2015c
02099+3449   HU 1034     Not seen 1948, 1951. No observations since that time.                           
02104+3911   HJ 1109     C is a nebula.                                                                  
02104-5049   ESG   1     Gl 86. Magnitudes are K magnitudes of Lagrange et al. (2006).                   
                         Lagrange et al. (2006) give two possible orbital solutions, based on    Lgr2006 
                         different assumed masses (70 Mjup and 0.5 Msun) for the secondary.              
                         Semi-major axes converted from AU (47.58 and 18.42 AU, respectively)            
                         to arcseconds assuming an Hipparcos-based distance of 10.9 pc.                  
                         JHK photometry of primary from 2MASS, that of secondary transformed             
                         from NACO to 2MASS filters.                                                     
                         2001.7454: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 112.1.                                            Rbr2011d
                         Farihi et al. (2013) derive a mass of 0.59 +/- 0.01 Msun and                    
                         Teff = 8180 +/- 120K for the white dwarf companion to GJ 86. Monte              
                         Carlo simulations yield the following orbital constraints:                      
                         P = 120-481y, T0 = 1933-2067, e = 0.00-0.61, i = 114.7-122.6deg,                
                         a = 2.57-6.47" (27.8-69.8 AU) Omega = 63.7-76.1deg, omega=0-358deg.             
                         The upper ranges of P and a are considered less likely.                 Far2013 
             GJ 86       A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Queloz       Que2000 
                         et al. (2000).                                                          HaI2001 
02106+1027   GWP 263     XMI 239.                                                                Tob2012b
02107-1507   FAR  28     Primary is white dwarf WD 0208-153.                                     Far2006 
02109+3902   STF 222     59 And.                                                                         
                         H 4 129.                                                                MEv2010 
02109+1341   STF 224     H N 105; BDS 1146 is identical.                                                 
02110+0317   GWP 264     XMI 240.                                                                Tob2012b
02112+2604   BRT3260     Originally published as BRT 127.                                        Brt1928 
02114+1848   GWP 265     XMI 241.                                                                Tob2012b
02115+5739   BU  874     5 Per.                                                                          
02117-0531   GWP 266     ABL  11.                                                                Tob2012b
02117-1927   GWP 267     ABL  12.                                                                Tob2012b
02122+4440   RUC   2     Aa,Ab. GZ And. Spectral type of Ab component estimated at M3-4V.        Ruc2007 
             HJ 2117     A is a W UMa-type binary, GZ And.                                               
02123-0908   GWP 268     ABL  13.                                                                Tob2012b
02124+3018   STF 227     iot Tri = 6 Tri. A is a spectroscopic binary, P = 14.73d. B is also an          
                         SB, P = 2.24d. One component is variable: TZ Tri.                               
             TZ Tri      Koresko et al. (1998) PTI solution has period fixed at spectroscopic    Krs1998 
                         value of Kaye et al. (1995).                                            Eat1995b
             STF 227     H 2  34.                                                                MEv2010 
02124+1249   LDS1126     NLTT 7300/7301                                                          Chm2004 
02124-0223   HDO  56     Not found. There must be a large error in the Hd place. Burnham         Bu_1909 
                         could not find it anywhere in the vicinity.                                     
02124-0455   GWP 269     ABL  14.                                                                Tob2012b
02124-7023   R    15     HLN   3.  B is CPD-70@131.                                                      
02125-0804   BRT 357     Also known as LDS3357.                                                          
02127+1614   GWP 270     XMI 242. SLW 100.                                                       Tob2012b
02128+7941   S   405     STTA 22. A is a Delta Scuti-type variable and spectroscopic                     
                         binary, P = 4.12d. B is BD+78@71.                                               
                         AB: H 5  84.                                                            MEv2010 
02128+0309   GWP 271     XMI 243.                                                                Tob2012b
02128-0224   STF 231     66 Cet. B is BD-03@335.                                                         
                         Aka SHJ  29 = H 4  25.                                                          
                         AB: NLTT 7323/7321                                                      Chm2004 
                         HIP 10305. A is SB2, period 94.788d, resolved by speckle (TOK 39).              
                         A is evolved. B = HIP 10303.                                            Tok2011a
02129+5712   STTA 24     AB and AC: Optical pair, based on study of relative motion of the               
                         components using the method of apparent motion parameters.              Kiy2008 
02129-0349   GWP 272     ABL  15.                                                                Tob2012b
02130+0851   MCA   5     xi 1 Cet = 65 Cet. Also a spectroscopic binary.                                 
                         A 1985.8375 measure attributed to this pair by Mcalister actually               
                         actually belonged to 02157+2503COU  79.                                 McA1987b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Herbig (1981).                                                Grf1981b
                   5     1985.8375: A measure at this date, belonging to 02157+2503 = COU  79,           
                         was erroneously attributed to MCA 5 in McAlister et al. (1987). This    McA1987b
                         measure has been moved to COU 79 and averaged with a re-reduced                 
                         measure from these data published by Hartkopf et al. (1996).            Hrt1996a
02131+5805   SHY 145     AC: HIP  10332 + HIP  12685.                                                    
02132+4414   CHR   5     60 And. A spectroscopic binary.                                                 
                         The negative results obtained during 1976 - 1980 are apparently due to          
                         a large magnitude difference.                                           Hrt1984 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Griffin & Herbig (1981).                                                Grf1981b
02132+4030   SHY 136     AB: HIP  10339 + HIP  10321. B component is V450 And.                           
02133+3649   JNN  18     Estimated age 30-300 Myr; masses 0.26 +/- 0.06 and 0.09 +/- 0.03 Msun;          
                         a ~2.8 AU.                                                              Jnn2014 
02135+5926   STI 351     STI1807                                                                         
02135-0502   GWP 273     ABL  16.                                                                Tob2012b
02135-2546   HJ 2120     B is CD-26@800.                                                                 
02136+5104   BAG   1     Aa,Ab: 6 Per. A is a long-period spectroscopic binary, now resolved by          
                         speckle interferometry.                                                         
                         SB1, P = 4.5 yr. Halbwachs (1981) predicts maximum separation 0".047.   HJL1981 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
             STT 555     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
02136-0945   GWP 274     ABL  17.                                                                Tob2012b
02137-0302   H 6 110     H VI 110. B is BD-03@341.                                                       
02138-1933   RSS  54     CPD-20@248                                                                      
02140+4729   STF 228     Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Scardia says the quadrant unambiguous for their 2004 theta values of            
                         105.8; this does not agree with other determinations of magnitude               
                         difference, however.                                                    Sca2005a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.34 +/- 0.36, 2.52, and 2.47 Msun, respectively.             Mlk2012 
02140+1652   GWP 275     XMI 244.                                                                Tob2012b
02142+0555   GWP 276     XMI 245.                                                                Tob2012b
02142-1811   GWP 277     ABL  18.                                                                Tob2012b
02144+3454   HU  807     Motion in separation, with little angular change. Close 1950-1960.              
02144-1441   GWP 278     ABL  19.                                                                Tob2012b
02145+6631   MCA   6     55 Cas. Composite spectrum star: B9V + G0II-III, delta m = 0.2 mag      Bnu1984 
                         (Markowitz 1969)                                                        Mrz1969 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.70 +/- 1.31, 6.94, and 2.57 Msun, respectively.             Mlk2012 
02145+5912   STI1812     SMA  31.                                                                        
02145-1103   LDS5373     SLW 102.                                                                        
02146-0142   GWP 279     ABL  20.                                                                Tob2012b
02147+3024   STF 232     H 2  35.                                                                MEv2010 
02147+1657   GWP 280     XMI 246.                                                                Tob2012b
02149+5829   STF 230     B spectrum B9IV.                                                                
02149+1353   GWP 281     XMI 247.                                                                Tob2012b
02150+5903   MLR 447     Also known as TDS2174.                                                          
02152-3507   SHY 415     HIP  10483 + HIP  10385.                                                        
02154+1126   GWP 282     XMI 248.                                                                Tob2012b
02155+5231   GC 2695     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin & Radford (1977).                                               Grf1977c
02155+1220   GWP 283     XMI 249.                                                                Tob2012b
02156+4223   GIC  29     G133-079/G134-019.                                                              
                         NLTT 7438/7440                                                          Chm2004 
02157+6740   ENG  10     B is BD+66@193.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY  10     BC: HIP  10529 + HIP  11167.                                                    
02157+2503   COU  79     21 Ari. Couteau & Morel (1982) computed masses disagree with spectral   Cou1982d
                         type. Authors suggest 3rd component (mass ~1 Msun) as possible                  
                         explanation. 1985.8375: This measure was erroneously attributed to              
                         02130+0851 = MCA 5 by McAlister et al. (1987). The data were re-reduced McA1987b
                         by Hartkopf et al., giving similar results. The measure has now been    Hrt1996a
                         replaced by the mean of the two separate reduction results.                     
                         1986.567: The separation of this partially resolved pair was                    
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference. Pair passed periastron earlier than predicted; now the              
                         orbit is definitive                                                     Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.09 +/- 0.30, 3.04, and 1.17 Msun, respectively.             Mlk2012 
02157+1046   STF 237     AB: HJL  30.                                                            HJL1986 
02157-0217   GWP 285     ABL  21.                                                                Tob2012b
02157+1657   GWP 284     XMI 250.                                                                Tob2012b
02158-1814   HTG   1     Orbit poorly covered, period rather indeterminate.                      Hei1978c
                         Additional notes may be found in Burnham (1894).                        Bu_1894 
02159+1416   GWP 286     XMI 251.                                                                Tob2012b
02159+0638   A  2013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.60 +/- 0.37, 1.51, and 0.79 Msun, respectively.             Mlk2012 
02160-0929   BRG  10     This likely triple system has only been observed in one epoch, hence            
                         it remains unconfirmed. The brightnesses and colors of all components           
                         are however consistent with expectation for a physical triple.          Jnn2012 
02160-1626   GWP 287     ABL  22.                                                                Tob2012b
02161+1651   GWP 288     XMI 252.                                                                Tob2012b
02161+1630   BPM  50     [PM2000]   83035 + [PM2000]   83004.                                    Gvr2010 
02162-2302   I   457     ADS 1744a.                                                                      
02163-0949   STF 242     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02164-0731   SLW 106     = GWP 289 = ABL  23.                                                            
02164-1233   SLW 105     = ABL  24.                                                                      
02164-1632   GWP 290     ABL  25.                                                                Tob2012b
02165-2227   LDS3364     NLTT 7520/7519                                                          Chm2004 
02165-5131   DUN   6     phi Eri. B is CPD-52@284.                                                       
             SHY 137     AC: HIP  10602 + HIP   9685.                                                    
             SHY 137     AD: HIP  10602 + HIP   7699.                                                    
             SHY 133     CD: HIP   9685 + HIP   7699.                                                    
             SHY 143     CE: HIP   9685 + HIP  12225.                                                    
             SHY 130     DF: HIP   7699 + HIP   6485.                                                    
02167-0430   GWP 291     ABL  26.                                                                Tob2012b
02167-3100   LDS  71     NLTT 7535/7528                                                          Chm2004 
02167-6324   TOK  71     HIP 10621. NOMAD: PM(B)=(0,-30), PM(A)=(18,60).                                 
                         D is HIP 10754.                                                         Tok2011a
02168+4346   GNS   1     Based on 2MASS and AstraLux images, Ginski et al. (2012) conclude the           
                         companion is a background object.                                       Gns2012 
02169+5703   STTA 25     B is BD+56@470.                                                                 
02169+0448   GWP 292     XMI 253.                                                                Tob2012b
02169-2322   BRG  11     The companion to 2MASS J02165488-2322133 has not yet been confirmed to          
                         share a common proper motion, but the color and brightness of it are            
                         well consistent with a physical companion, hence it is counted as such          
                         in the statistics.                                                      Jnn2012 
02171+3413   DOR  66     del Tri = 8 Tri. A is a double-lined spectroscopic binary, P = 10.02d.          
                         Proper motion +1154 -245.                                                       
             MKT   5     Aa,Ab: PM = +1154 -245. del Tri.                                                
                         Hummel et al. 1995) visual orbit based on astrometry from Mark III      MkT1995 
                         interferometer. Additional spectroscopic data yield component masses,           
                         luminosities, radii, effective temperatures, and distance.                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1995).                                                   MkT1995 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.57 +/- 3.14, 1.92, and 1.05 Msun, respectively.  Mlk2012 
02172+5838   YSC  87     Ba,Bb: Originally 02171+5839 YSC  87, but found to correspond to B              
                         component of 02172+5838.                                                        
02172-2849   LDS3365     NLTT 7557/7558                                                          Chm2004 
02173+3351   VIG   1     Primary is gam Tri. The B and C components are background stars, the D          
                         component ambiguous.                                                    Vig2012 
02174+2845   STF 239     HJL  32.                                                                HJL1986 
                         Aka H 4  40 = SHJ  31.                                                          
02174+2708   GIC  30     AC: G035-037/G036-007.                                                          
02176+2214   STF 244     HJL  33.                                                                HJL1986 
02176-5400   RSS  55     CD-54@487                                                                       
02178+5638   A  1272     V438 Per, a W UMa type eclipsing binary, P = 3.50939d.                  Zas2012 
02179+1941   TOK  72     HIP 10710. Primary is astrometric binary (Makarov & Kaplan 2005)        Mkr2005 
02179+1614   GWP 293     XMI 254.                                                                Tob2012b
02180+1958   GWP 294     XMI 255.                                                                Tob2012b
02180+0145   GC 2770     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1935).                                                          Hrp1935 
                         Combined astrometric/spectroscopic orbit by Fekel et al. (2007). For    Fek2007 
                         primary, derive mass = 1.15 Msun, radius = 1.64 +/- 0.07 Rsun,                  
                         Luminosity = 3.0 +/- 0.1 Lsun. Spectral types are G0IV and ~M0V.                
                         SB1. Combined orbit including RV data and Hipparcos Intermediate                
                         Astrometric data. Semimajor axis derived from photocentric a0 plus              
                         stellar evolutionary model. Derived properties for A and B:                     
                         M/Msun = 1.20 + 0.53, L/Lsun = 2.76 + 0.04, dm = 4.60 mag,                      
                         log age = 9.65.                                                         WaX2015b
02180-1229   LDS  73     NLTT 7592/7593                                                          Chm2004 
02181+5731   BU 1170     7 Per = chi Per                                                                 
                         S   409 = H 6  19.                                                              
02181+5616   UC   29     Primary appears to be a close pair.                                     Cbl2010c
02182+5715   STI1836     BKO 165.                                                                        
02182+3920   A   207     Scardia et al. (2001) orbit preliminary as all the orbital elements     Sca2001d
                         are still rather uncertain. Hipparcos parallax (0".01200 +/- 0.00311)           
                         seems to be overestimated and leads to a mass sum 0f 0.46 Msun,                 
                         unacceptable for a system of type F5. Scardia (1982) classified the     Sca1982a
                         star as type F9. Dynamical parallax is 0".0065; the corresponding mass          
                         sum is 2.87 Msun.                                                               
02184+5758   STI1839     STI1844.                                                                        
02184-0636   GWP 295     ABL  27.                                                                Tob2012b
02186+4017   STF 245     ALI1193.                                                                        
             EGG   2     Aa,Ab: This system has spectral type F2 from SIMBAD and parallax of             
                         10.26 +/- 2.92 mas from van Leeuwen (2007). A previous orbit was        VlF2007 
                         calculated by Cvetkovic (2008) with period of 109 years and semimajor   Cve2008c
                         axis of 0.344 arcsec. However, our new observation shows that the               
                         system has a much shorter period and smaller semimajor axis. However,           
                         our orbit yields roughly the same total mass, with large uncertainty.           
                         The system appears to have executed nearly a full orbit since the               
                         first speckle observations taken of it in 1985 by McAlister et al.              
                         (1987). More data will be needed to confirm this orbital trajectory,            
                         but if correct, the smaller period makes the system much more                   
                         attractive for future study.                                            Hor2015b
02186-2940   B    34     AV For, Algol (EA) type eclipsing binary, P = 1.8797 d.                 Zas2011 
02187+3429   STF 246     H III 42, BDS 1165.                                                             
                         HJL  34.                                                                HJL1986 
                         H 3  42.                                                                MEv2010 
02187+0412   BU  437     Some observations erroneously ascribed to STF 247, even Struve's                
                         discovery, seems to belong to this pair, whose delta-m = 2 is less              
                         than Burnham's estimate.                                                Hei1992a
02188+0840   GWP 296     XMI 256.                                                                Tob2012b
02188+1440   GWP 297     XMI 257.                                                                Tob2012b
02190+2839   HJ 1115     10 Tri.                                                                         
02191-0651   HJ  327     AC: The C component is the galaxy NGC 883.                                      
02193-0259   JOY   1     Aa,Ab: The primary is omi Cet = VZ Cet = 68 Cet = MIRA, prototype of            
                         the Mira-type variables. "Orbits" have been computed for the visual             
                         pair, but are most likely false. B has in the past been identified as a         
                         Cepheid, VZ Cet; however, it appears that the component seen as                 
                         variable is the Joy component, recently determined to be a White Dwarf. Skl2010 
                         Recent papers (in particular 1995 PhD thesis by Harold L. Chambers II)          
                         suggest that the visible companion is not the star itself, but the              
                         accretion disc around it (material captured from Mira's stellar wind).          
                         Rapid fluctuations of brightness are described by Warner (1972 MNRAS            
                         159, 95).                                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aa,Ab: Pair seen but not measured.                                      Cou1958c
                         Aa,Ab: Additional notes may be found in Couteau (1963).                 Cou1963a
             H 6   1     H VI 1. C is BD-03@355.                                                         
02198-2352   HJ 2130     B is CD-24@1022.                                                                
02200-2213   BRT1373     CD-22@784.                                                                      
02201-1703   GWP 298     ABL  28.                                                                Tob2012b
02204+2456   POU 175     Also known as KU    9.                                                          
02204+1617   BPM  51     [PM2000]   85486 + [PM2000]   85504.                                    Gvr2010 
02204+0135   GWP 299     XMI 258.                                                                Tob2012b
02205+1733   BPM  52     [PM2000]   85552 + [PM2000]   85616.                                    Gvr2010 
02209-0954   GWP 300     ABL  29.                                                                Tob2012b
02209-5632   RST  51     CD-57@470.                                                                      
02210-1650   GWP 301     ABL  30.                                                                Tob2012b
02211+4246   STF 248     Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Combined spectroscopic/visual solution, yielding masses, etc.           Trr1995a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.39 +/- 0.49, 1.78, and 0.85 Msun, respectively.             Mlk2012 
02212+5651   BU 1171     Not seen in 1951 with 82-inch (Van Biesbroeck).                         VBs9999 
02212+3653   GIC  31     AB,C: NLTT 7710/7708                                                    Chm2004 
02213-1057   HJ 3495     B is BD-11@445.                                                                 
02215-1251   GWP 302     ABL  31.                                                                Tob2012b
02215-1354   GWP 303     ABL  32.                                                                Tob2012b
02216+2338   STF 254     POU 178.                                                                        
02219+0824   GWP 304     XMI 259.                                                                Tob2012b
02220+0445   TOK 231     Primary is SB1, P= 79.700 d. Companion at 53" is possibly a white       Tok2012c
                         dwarf (Tokovinin & Lepine 2012)                                         Tok2014d
02220-0034   GWP 305     ABL  33.                                                                Tob2012b
02222-0348   GWP 306     ABL  34.                                                                Tob2012b
02224+5551   BU  875     9 Per. Variable, V474 Per.                                                      
02225+2830   FAR  29     Primary is white dwarf WD 0219+282.                                     Far2006 
02225-0536   GWP 307     ABL  35.                                                                Tob2012b
02225-2349   LAF  27     TOK  40.                                                                        
                         Astrometric binary with 26.5 yr orbit has massive secondary with q~1.   Tok2012a
                         Tokovinin (2013) derived a combined spectroscopic/interferometric               
                         solution, including echelle spectroscopy and speckle interferometry.            
                         The B component is a close binary (tentative period 3.7d); masses of A          
                         and Ba+Bb are nearly equal.                                             Tok2013a
                         Astrometric binary with large acceleration, where the massive                   
                         companion B is in fact a close pair of M dwarfs.                        Tok2013b
             kap For     Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit based on   Gon2002a
                         combination of ground-based catalogs with Hipparcos.                            
02226+1531   LDS3375     G004-016. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 7795/7794                                                          Chm2004 
02229+5835   BLL   7     A is the semi-regular variable, S Per.                                          
02229+4129   TRN  10     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7451 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
             HD  14633   Rodgers (1974 M.S. Thesis, Univ. Toronto) made a preliminary orbital            
                         analysis (P =15.3 d) but the variations appear to be more complicated           
                         than originally claimed (Bolton & Rodgers 1978 ApJ 222, 234).           Msn1998a
02229-1718   GWP 308     ABL  36.                                                                Tob2012b
02229-5106   EHR   1     CPM pair.                                                               Ehr2010 
02230+0443   GWP 309     XMI 260.                                                                Tob2012b
02231+7021   MLR 377     A premature orbit has been published.                                           
                         Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995)            Ruy1995 
02231+0246   GWP 310     XMI 261.                                                                Tob2012b
02232-2952   BU  738     T incorrectly listed as 1953.489 by Scardia et al. (1990); should be    Sca1990a
                         1953.849 (erratum noted in Inf. Circ. 112, 1990)                        Sca1990b
                         Parabolic orbit.                                                        Fin1969b
                         sigma = areal constant in the true orbit = 0.0199 arcsec^2/yr                   
                         q = periastron distance in the true orbit = 0".4991                             
02233+2230   LDS3378     NLTT 7840/7842                                                          Chm2004 
02233+1525   AG   38     LDS 879. B is BD+14@387.                                                        
                         AB: NLTT 7845/7843                                                      Chm2004 
                         AB: SHY 417. Bayesian  analysis by Shaya & Olling (2011) indicates      Shy2011 
                         very high (near 100%) probability pair is physical.                          .  
                         HIP 11137. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: HJL  35.                                                            HJL1986 
02233+1452   GWP 311     XMI 262.                                                                Tob2012b
02236-1056   RST4203     Also known as OL  111.                                                          
02238+4920   STF 256     Also known as STF 243.                                                          
02239+5751   MLR 656     Also known as HDS 311.                                                          
02239+5522   BU 1373     The primary is the Cepheid variable V440 Per.                           Evs2016a
02239+3330   STF 258     Also known as STF 253.                                                          
02242+1016   CHR 199     First detected as an occultation binary by Evans.                       Evn1980 
02244-2253   LDS3382     NLTT 7922/7928                                                          Chm2004 
02245-0145   STF 265     HJL  36.                                                                HJL1986 
02246+5959   STF 255     STI 360.                                                                        
02246+2537   ALP   7     2MASSI J0224367+253704                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this pair.                                                    AlP2007 
02246-4050   GC 2912     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Barker et al. (1967).                                                   Evn1967 
02247+4008   LDS3381     NLTT 7887/7890                                                          Chm2004 
02249+5153   ES  764     B is BD+51@567.                                                                 
02249+3039   UC  733     AC: Candidate on Tokovinin list, now reconfirmed as CPM. The primary            
                         hosts an exoplanet.                                                     Tok2013c
02250-1501   GWP 312     ABL  37.                                                                Tob2012b
02252+1217   BRT1170     1deg error in WDS designation, apparently an error in transcribing              
                         coordinates from the original source.                                           
02253-0802   GWP 314     ABL  39.                                                                Tob2012b
02253-1242   GWP 313     ABL  38.                                                                Tob2012b
02255-1834   GWP 315     ABL  40.                                                                Tob2012b
02256+5017   BUP  31     65 And.                                                                         
02257+6133   STF 257     The primary is SB1 V559 Cas, P = 1.58 d.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
02257+0846   GWP 316     XMI 263.                                                                Tob2012b
02257-2119   HJ 3500     HIP 11324. B = HIP 11323. Both components are below the MS, the true            
                         parallax should be 12.6 mas (as for the B-component in Hipparcos).      Tok2011a
02258-1038   HJ 2140     Identical with HJ 2134, 4 minutes west.                                         
02259+1747   JNN  19     LP 410-22.                                                                      
02260-1520   H 3  80     H III 80. A is a variable of the Alpha CVn type, AB Cet, and a                  
                         spectroscopic binary.                                                           
02262+3428   HDS 318     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.48 +/- 0.19, 1.81, and 1.80 Msun, respectively.             Mlk2012 
02262-0833   GWP 318     ABL  42.                                                                Tob2012b
02262-1602   GWP 317     ABL  41.                                                                Tob2012b
02263+0618   VIG   2     The B component appears to be a faint background star.                  Vig2012 
02265+5417   STF 260     HJL  37.                                                                HJL1986 
02268+5853   HD  14947   Garmany & Stencel (1992 A&AS 94, 211) include this star in Per OB1.     Msn1998a
02268+1034   STTA 27     B is BD+09@322. A is VW Ari, a Delta Scuti-type variable.                       
02269+3733   ADM   2     WSP  33. WASP-33. Primary is del Sct-type variable and exoplanet host.  Adm2013 
02270-0326   GWP 319     ABL  43.                                                                Tob2012b
02272+0309   GWP 320     XMI 264.                                                                Tob2012b
                         HIP 11417. SB, no orbit. NOMAD: PM(B)=(-12,-68), V=14.73.               Nrd2004 
                         Primary is SB2, P=5.997d, but the mass ratio is unknown.                Tok2014d
02273+5433   LAW  10     LSPM J0227+5432. Law et al (2008) derive a distance of 18.6 +9.5/-3.4   Law2008 
                         pc and a projected separation of 13.2 +7.2/-2.2 AU. Estimated spectral          
                         types are M4.5 and M5.                                                          
02273-0304   GWP 321     ABL  44.                                                                Tob2012b
02274+3059   INN   1     Rotation periods 12.1d (AG Tri, 13.7d wrong) and 4.7d.                  Skf2013 
02274+1807   GWP 322     XMI 265.                                                                Tob2012b
02278+0426   A  2329     Using the Hipparcos parallax value of 60.22 +/- 1.75 mas, the orbital           
                         elements of Andrade (2007) yield a mass sum of 1.25 +/- 0.14 Msun.      Ana2007 
                         Masses of the two K7V components are estimated at 0.63 +/- 0.01 and             
                         0.62 +/- 0.01 Msun.                                                             
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.37 +/- 0.12, 1.25, and 0.65 Msun, respectively.             Mlk2012 
02279+4710   BWL  10     AB: Primary is a probable member of the AB Dor moving group.            Bwl2015 
02280+0248   GWP 324     XMI 266.                                                                Tob2012b
02280-0520   GWP 323     ABL  45.                                                                Tob2012b
                         WDS designation corrupted at some point to 02280-0303. Corrected.               
02280-3349   SHY 140     HIP  11477 + HIP  11448.                                                        
02281+3251   ES 2407     GCB 6.                                                                          
02282+5423   STF 267     B is BD+53@530.                                                                 
02282+2952   STF 269     STT  41. May also be H 1  21.                                                   
02284-0404   GWP 325     ABL  46.                                                                Tob2012b
02286+5521   ES  872     There is a difference of 18 degrees in the measured angles. The Espin           
                         measure appears correct.                                                Es_1910b
02286-0704   A   447     WSP  77.                                                                        
02287+1850   GWP 326     XMI 267.                                                                Tob2012b
02287-3114   TOK  73     HIP 11537. The V-photometry is affected by small separation. B is red           
                         in the V-K color, variable? Astrometric binary in HIPPARCOS (Makarov            
                         and Kaplan), possibly new triple?                                       Mkr2005 
                         PMS star (Torres et al. 2006).                                          TrC2006 
                         SIMBAD: PMS star and X-ray source 1RXS J022843.6-311332.                Tok2011a
                         Companion is partially resolved in 2MASS images, for that reason the            
                         star is not found in the 2MASS point-source catalog. Pre-main-sequence          
                         star according to SIMBAD.                                               Tok2012a
02288+3215   WOR   2     Tamazian et al. derive a dynamical mass sum of 1.40 +/- 0.25 Msun       Tam2005 
                         and classify the stars as K6-7V and M0V. Absolute magnitudes of                 
                         the two components are estimated at +8.0 and +8.6, leading to                   
                         individual masses of 0.65 and 0.61 Msun, in good agreement with                 
                         the dynamical mass sum.                                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.46 +/- 0.20, 1.25, and 0.55 Msun, respectively.             Mlk2012 
02288-0826   GWP 327     ABL  47.                                                                Tob2012b
02290-0302   GWP 328     ABL  48.                                                                Tob2012b
02291+6724   STF 262     iot Cas. The primary is an unresolved binary, also an Alpha CVn                 
             CHR   6     type variable, P = 1.74 d, and an astrometric, spectroscopic, and               
                         spectrum variable (Rakos 1962; Klock, AJ 70, 176, 1965). The RV         Rak1962 
                         variation has not been confirmed.                                               
                         Heintz (1962) also detected this pair as a submotion to the visual      Hei1962 
                         orbit of the AB pair with a period of 52 years and an amplitude of              
                         0".11. Star C (mag. 8.4, dG4) is probably physical, but Hopmann         Hop1960b
                         (1960) computed a hyperbolic orbit for it, as there is some RV                  
                         difference between C and A.   q = periastron distance in the true               
                         orbit = 6".7056. All hyperbolic orbits were rejected from the                   
                         Fourth and subsequent orbit catalogs.                                   Wor1983 
                         Soderhjelm gives Aa,Ab,B,C quadruple solution (AB in HIP). High         Sod1999 
                         mass-sum, strangely well-behaved speckle obs at  Delta m=4?                     
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Drummond et al. (2003) give solution for Aa,Ab incorporating motion of  Dru2003 
                         the AB pair. The authors conclude that the motion of B relative to              
                         the CHR pair appears to be rectilinear. Masses of the CHR components            
                         are derived.                                                                    
                         1985.8540: This autocorrelogram was remeasured; the new results are             
                         listed in the catalog.                                                  McA1987b
             STF 262     AB: H 1  34.  AC: H 3   4.                                              MEv2010 
                         AC: Hyperbolic orbit.                                                   Hop1960b
02291+2331   VBS   6     The inclination must be high.                                                   
02294+5532   STF 268     A is a spectrum variable and shell star.                                        
02296+6039   STF 263     A is a possible Beta Cep variable, V528 Cas.                                    
02297-0030   GWP 329     ABL  49.                                                                Tob2012b
02297+0134   GWP 330     XMI 268.                                                                Tob2012b
02297-0955   GAL 321     Object #69 in Gallo's original list.                                    Gal1912b
02305+2514   STF 271     AB: H N  12.                                                            MEv2010 
02307-0407   GWP 331     ABL  50.                                                                Tob2012b
02308+5533   STF 270     AB: HJL  38.                                                            HJL1986 
                         Is there a wobble in the PA of AB?                                      Tok2014d
02309+0158   GWP 332     XMI 269.                                                                Tob2012b
02310+1358   GWP 333     XMI 270.                                                                Tob2012b
02310+0823   GIC  32     G004-024/G073-059.                                                              
02313-1310   GAL 322     Object #70 in Gallo's original list.                                    Gal1912b
02315+0106   SHY 422     BC: HIP  11736 + HIP  12728.                                                    
02318+8916   STF  93     alp Umi = 1 UMi = Polaris. Cepheid variable and spectroscopic binary,           
                         P = 30y. A close companion has been suspected. The close pair,                  
                         measured three time from 1937-1939 by R.H. Wilson using an eyepiece     WRH1941b
                         interferometer, was not seen again until Evans et al. (2006) resolved   Evs2006 
                         it with HST.  Wilson's measures agree with the combined astrometric/            
                         spectroscopic solution by Gerasimovic (1936), although both orbit and   Ger1936 
                         measures are called into dispute by the more recent orbit of Wielan et  Wln2000 
                         al. (2000), whose solution includes mass estimates, etc.                        
                         An earlier orbit by Wyller (1957) was rejected from Fourth Orbit        Wye1957 
                         Catalog ("amplitude below noise level")                                 Wor1983 
                         Component B = BD+88@@@7. See discussion of this system by Roemer.       Re_1965 
                         The C component was observed by Burnham in the late 19th century, then  Bu_1894 
                         not seen again until the early 21st century by Daley and Ashcroft.      Dal2006a
                         The extremely large magnitude makes the pair too close for most large           
                         astrometric surveys.                                                            
                         The D component has also been recently recovered in 2MASS data.         TMA2003 
                         According to Jim Daley, the R-I color for C is 0.56 and for D it is             
                         0.67. The V-I color for D is 1.08.                                      Dal2006b
                         AB: H 4   1.                                                            MEv2010 
02318-0021   GWP 334     ABL  51.                                                                Tob2012b
02319+5742   BU 1314     V425 Per. Variable in light and radial velocity.                                
02319+0108   LDS9132     Old LDS6132. Primary is confirmed quasar: Z = 1.26.                             
02320+1822   STF 273     H N 106.                                                                MEv2010 
02320-1955   BRT 297     LDS3400.                                                                        
02321-1515   GWP 335     ABL  52.                                                                Tob2012b
                         SHY 141. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
02323+4630   BRT 330     Since precise position has been corrected from previous precise         WSI2002 
                         position null detection not relevant.                                           
02324-1849   GWP 336     ABL  53.                                                                Tob2012b
02327+6127   STI 368     Both visual components were observed and appeared to be single.         Msn1998a
             MZA   8     EL and EM pairs were originally 02326+6128 MZA   8AB and AC, until              
                         match of E component of 02327+6127 to primary of 02326+6128 noticed.            
02327+0704   GWP 337     XMI 271.                                                                Tob2012b
02328+0021   GRV1174     SLW 119.                                                                        
02328-3421   LDS9133     Old LDS6133.                                                                    
02329+3433   GC 3048     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02329+1502   TOK  12     Estimated period of visual pair 160y.                                   Tok2006 
                         Primary is SB2, P=19.4161d (Katoh et al. 2013 AJ 145, 41)               Tok2014d
02330+4852   HJ 2144     B is BD+48@694.                                                                 
02332-2207   DON  35     CD-22@863.                                                                      
02333+5219   STT  42     Distance small, measures often discordant.                                      
                         1982.7604: This autocorrelogram was remeasured; the new results are             
                         listed in catalog.                                                      McA1987b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.00 +/- 1.28, 4.13, and 2.19 Msun, respectively.  Mlk2012 
02333-1933   GWP 338     ABL  54.                                                                Tob2012b
02333-7554   HJ 3522     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
02335+5732   HJ 2143     B is BD+56@657.                                                                 
02338-2814   HJ 3506     ome For.                                                                        
02340-1812   BRG  13     There is insufficient motion between the two epochs of observation of           
                         2MASS J02335984-1811525 to establish common proper motion of the                
                         binary, but the components are nearly equal brightness and color, and           
                         reside at a relatively small separation of ~0.85" hence it is almost            
                         certainly a physical pair.                                              Jnn2012 
02342+0916   GWP 339     XMI 272.                                                                Tob2012b
02342+0139   LDS9134     Old LDS6134.                                                                    
02343+4017   AG   42     STF 275.                                                                        
02344+3542   J  1810     ALI 35.                                                                         
02344+2040   A  2218     Identification error in ADS. Pair is BD+20 426, not BD+19 375.          Cou1970c
02344-4259   HJ 3510     Spectrum: G3/5III/IV.                                                           
02347-0752   BUP  32     77 Cet.                                                                         
02350-1522   GWP 340     ABL  55.                                                                Tob2012b
02351-1046   GAL 323     Object #71 in Gallo's original list. Aka J  1452.                       Gal1912b
02352+0407   TOK 649     Resolved using ANDICAM2. Primary SB?                                    Tok2014d
02353+4017   A  1818     Baize suspected another close pair in the region.                               
02353-0334   MUG   2     Followup spectroscopy confirmed the B component is a dwarf; estimated   Mug2005 
                         mass is 0.286 +- 0.017 Msun. Primary is planet host star. Colors of B   Egn2007 
                         component consistent with M1-M4 dwarf with mass 0.31 +/- 0.02 Msun.     Met2009 
                         HIP 12048. The B component estimated mass 0.29Msun.                             
                         2001.7454: PA is measured in zenith mode. If data collected in                  
                         equatorial mode, PA = 183.7.                                            Rbr2011d
             79 Cet      A: Combined solution, based on reduction of Hipparcos intermediate              
                         astrometric data together with spectroscopic elements from Marcy et al. CPS2000b
02354-0228   GWP 341     ABL  56.                                                                Tob2012b
02355+5948   HIP  12062  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Latham et al. (2002). They derived component masses 0.96 and 0.45 Msun  Lat2002 
                         and an estimated semimajor axis of 35.47 mas.                           Ren2013 
02356+6106   RAO   7     Primary is close astrometric binary; also SB?                           Tok2014d
02356+3719   STF 279     AB: H N  47.                                                                    
02358+3441   AG  304     15 Tri. B is BD+34@471.                                                         
02359+6338   CTT   3     The B component is BD+62@423.                                                   
02359+1515   GWP 342     XMI 273.                                                                Tob2012b
02359+0536   STF 281     nu Cet = 78 Cet                                                                 
                         The A component is a 714d spectroscopic binary. B is not a binary, so           
                         this is a physical triple.                                              Grf2015a
02359-2830   SWR   4     CPM pair                                                                Skf2004 
02360-0750   BUP  33     80 Cet.                                                                         
02360-1312   GWP 343     ABL  57.                                                                Tob2012b
02360-2331   GIZ   1     GJ 1048.  Discovered by Gizis et al. (2001) on 2MASS images. The A      Giz2001 
                         component is K2V; conclude secondary is L1, mass ~0.077 Msun.                   
                         Seifahrt et al. (2004) combine 2MASS measure with earlier UK Schmidt    Sef2004 
                         near-IR southern survey data to show stars have similar proper motion,          
                         so are likely physical companions.                                              
02361+0653   GKI   1     AB: This object was misidentified as HD 61660 by McAlister (1978).      McA1978c
             PLQ  32     AC: GJ 105. Proper motion of A +1811 +1451 (FK5). Spectroscopic binary          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         HIP 12114. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
02362-1656   GWP 344     ABL  58.                                                                Tob2012b
02363-0500   GWP 345     ABL  59.                                                                Tob2012b
02363-6329   B  1435     Spectral type F6?                                                               
02366+1231   GWP 346     XMI 274.                                                                Tob2012b
02366+1227   MCA   7     31 Ari. This system has a small Delta m (~0.1 in the blue, 0.3 in the           
                         red) as determined from lunar occultation measures by Africano et al.   Afr1978 
                         Measures in 1982.7659, 1984.7046, and 1988.6544 were based on           Hrt1994 
                         reprocessing of archival video data.                                    Hrt2000a
                         Martin et al. (1998) derive component masses 11.001 +/- 1.969 and               
                         9.407 +/- 1.707 Msun.                                                   Mig1998 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 19.08 +/- 2.57, 2.95, and 1.13 Msun, respectively.            Mlk2012 
02368+1723   BPM  53     [PM2000]   95004 + [PM2000]   94927.                                    Gvr2010 
02368-1929   ARA 523     BRT1374.                                                                Brt1935b
02369+5953   STF 277     V791 Cas, a Beta Lyr type eclipsing binary, P = 2.88680d.               Zas2012 
02370+2439   STFA  5     30 Ari. STTA 29. A is 1.1d SB1; AB has estimated period of 34,000y.     Tok2006 
                         B is BD+24@375.                                                                 
                         HJL  39.                                                                HJL1986 
                         SHY 142. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         H 5  49.                                                                MEv2010 
                         Primary is SB2, P=1.109d. B is exoplanet host, P=335d. A is F6III, but          
                         on the MS.                                                              Tok2014d
             RAO   8     BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral            
                         types of B and C as F8V and M1V.                                        Rbr2015a
02370-3435   MUG  12     Primary is GJ 9088 = lam 2 For. Spectral type of comoving secondary             
                         estimated as M5-6, confirmed by follow-up spectroscopy. Mass of                 
                         secondary ~0.11 Msun.                                                   Mug2014 
02371+6232   MLR  31     No significant movement since first resolution.                         Drd2009 
02371+1740   GWP 347     XMI 275.                                                                Tob2012b
02371-0926   ITF  62     BD: Originally 02368-0926ITF  62.                                               
02371+0055   LDS5388     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02371-2951   LDS3405     NLTT 8520/8519                                                          Chm2004 
02374-5233   EHR   2     Primary is eta Hor. Physical/optical nature ambiguous.                  Ehr2010 
             TOK 186     Aa,Ab: The Marion et al. (2014) measure is in good agreement with the   Mrn2014 
                         Hartkopf et al. (2012) discovery observation, but hints at a            Tok2014a
                         significantly eccentric and/or inclined orbit. A face-on, circular              
                         orbit with a semimajor axis of 3.6AU would have a period of ~3.7y,              
                         which is in line with the 3.0y astrometric period found by Goldin &             
                         Makarov (2007).                                                         Gln2007 
02376+2250   LDS1132     NLTT 8503/8502                                                          Chm2004 
02378+1737   BPM  54     [PM2000]   95638 + [PM2000]   95705.                                    Gvr2010 
02380+1418   GWP 348     XMI 276.                                                                Tob2012b
02381-0541   SLW 126     Aka ABL  60.                                                                    
02382+4604   A  1278     A premature orbit has been computed.                                            
02382-1123   STF 288     H 3  79.                                                                MEv2010 
02383-3012   UC  766     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02386+0327   KUI   9     HR 775 in Cetus. Some scatter in measured position angles.                      
02387-5257   COO  14     Spectrum: F8IV/V + G/K.                                                         
             SHY 424     AC: HIP  12326 + HIP  12361.                                                    
02388+3325   STF 285     H 1  21.                                                                MEv2010 
02389+1526   AG   43     HU 1043.                                                                        
02389-5450   HJ 3520     B is CPD-55@444.                                                                
02390+6235   STTA 28     B is BD+61@445.                                                                 
02390+1452   STF 287     H N 107.                                                                MEv2010 
02392-0016   GWP 350     ABL  62.                                                                Tob2012b
02392-0933   GWP 349     ABL  61.                                                                Tob2012b
02394-0318   GWP 351     ABL  63.                                                                Tob2012b
02396-1152   FIN 312     eps Cet = 83 Cet. Pourbaix gives combined solution for this resolved            
                         SB2, yielding orbital parallaxes and component masses.                  Pbx2000b
                         Arenou give combined solution of astrometric orbits and DSBs. Paper             
                         includes masses and distances.                                          Are2000 
                         Systematic errors are clearly present and the period remains in doubt.  Fin1954c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.68 +/- 0.35, 2.39, and 2.40 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 41.43 +/- 0.68           
                         mas and component masses 1.37 +/- 0.09 and 1.03 +/- 0.08 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
02398-1522   GWP 352     ABL  64.                                                                Tob2012b
02398-3354   LDS3413     HIP 12411. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
02399+0009   A  1928     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.83 +/- 0.56, 2.33, and 1.05 Msun, respectively.             Mlk2012 
02399-2429   TOK 205     A faint companion near the detection limit is found, our measures are           
                         uncertain. The estimated long period P ~ 100 yr suggests that the               
                         Hipparcosacceleration of 17 mas yr-2 is spurious.                       Tok2012a
                         The tentative resolution on 2011.84 at 78deg, 0".34, dK=3.8 is not              
                         confirmed here, with new good-quality images. The star has constant RV          
                         so could be single.                                                     Tok2013b
02401+1148   FAR  30     Primary is white dwarf WD 0237+115.                                     Far2006 
02401+0255   UC  771     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02402+0436   HDS 347     Mean motion indicates P ~ 90 yr, rho increasing.                        Msn1999b
02405-1341   GAL 324     Object #74 in Gallo's original list.                                    Gal1912b
02406+3420   WNO  43     Aa,Ab: Identified as WNO  13 by Routley.                                USN1972 
             GIC  33     AB = G074-039/G074-040. AC = G074-039/G074-041.                                 
                         AB: NLTT 8633/8634                                                      Chm2004 
02407+6117   STF 284     A is a Beta CMa-type variable, V482 Cas.                                        
             CHR 208     Both visual components were observed: A was resolved (CHR 208Aa,Ab),            
                         B appeared to be single.  Gies & Bolton (1986) found a large scatter    Gie1986 
                         in radial velocities (but could not find a suitable period), and this           
                         suggests that at least one component may be a spectroscopic binary.     Msn1998a
02407+2704   STF 289     33 Ari. A spectroscopic binary.                                                 
                         HJL  41.                                                                HJL1986 
                         H 4   5.                                                                MEv2010 
02407+2637   STT  43     Scardia et al. (2001) orbit considered preliminary because the arc of   Sca2001d
                         the observed orbit is only 90 degrees and is placed completely around           
                         aphelion. The Hipparcos parallax of 0".01385 +/-  0.00125 gives a mass          
                         sum of 3.1 Msun, an overestimate for a star of type F7V. The dynamical          
                         parallax of 0".0149 agrees well with the measured one.                          
02410+6539   STF 282     AB: HJL  40.                                                            HJL1986 
02410+3905   A  1820     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
02410-2506   LDS3414     NLTT 8688/8689                                                          Chm2004 
02412-0042   STF 295     84 Cet. A is a Delta Scuti-type variable.                                       
02413+2659   L    55     Since precise position has been corrected from previous precise         WSI2013 
                         position null detection not relevant.                                           
02413-0432   BWL  12     Colors and/or astrometry are inconsistent with a late-type common               
                         proper motion companion based on visual inspection of the field from            
                         2MASS, SDSS, DSS1, and/or DSS2. Primary is G 75-35.                     Bwl2015 
02413-5725   BRG  14     2MASS J02411909-5725185 is yet to be confirmed as a common proper               
                         motion binary, but the color and brightness of the companion are well           
                         consistent with it being bound.                                         Jnn2012 
02414+3629   HJ  328     Aka ALI 269.                                                                    
02415+4053   COU1511     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.86 +/- 1.13, 2.54, and 1.05 Msun, respectively.             Mlk2012 
02415+1115   GWP 353     XMI 277.                                                                Tob2012b
02418-5300   JFF   1     Aka CAB   6.                                                                    
02420+4248   HJ 1123     B is BD+42@588, spectrum B9IVp(Hg,Mn,Eu).                                       
02420-1824   GWP 354     ABL  65.                                                                Tob2012b
02421+1351   LDS3416     NLTT 8720/8721                                                          Chm2004 
02421-0134   OL    9     Since precise position has been corrected from previous precise         WSI2004b
                         position null detection not relevant.                                           
                         Aka RST4211.                                                                    
02422+4242   HJ 1124     Aka BKO 172.                                                                    
02422+4012   MCA   8     12 Per. SB2 resolved by speckle interferometry by McAlister (1977).     McA1977 
                         Elements P = 331.0d, T, e, and longitude of periastron for McAlister    McA1978a
                         solution are from the spectroscopic orbit by Colacevich (1941).         Cla1941 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Colacevich (1941).                                                              
                         Martin et al. (1998) derive component masses 1.125 +/- 0.169 and                
                         1.389 +/- 0.193 Msun.                                                   Mig1998 
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Bagnuolo et al. (2006) solution combines speckle data with data from    Bgn2006 
                         the CHARA Array. Authors derive orbital parallax 41.19 +/- 0.21 mas,            
                         masses 1.382 +- 0.019 and 1.240 +- 0.017 Msun, and a magnitude                  
                         difference 0.409 +/- 0.013 mags in K' (2136 nm). Values for omega and           
                         Omega are switched in their Table 3.                                            
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.59 +/- 3.80, 2.58, and 1.07 Msun, respectively.             Mlk2012 
02422-2445   LDS3418     NLTT 8753/8759                                                          Chm2004 
02423+1639   BPM  55     [PM2000]   98625 + [PM2000]   98718.                                    Gvr2010 
02423+1415   GWP 355     XMI 278.                                                                Tob2012b
02424+3837   EVT   1     Aa,Ab: Exo-planet host                                                  Tok2014d
02424+2001   BLA   1     Aa,Ab: mu Ari = 34 Ari. Occultation binary, known to have variable              
                         radial velocity.                                                        Bag1984b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 3.64 +/- 0.47, 5.77, and 2.24 Msun, respectively.  Mlk2012 
02424+0247   GWP 356     XMI 279.                                                                Tob2012b
02424-0214   LDS9135     Old LDS6135.                                                                    
02424-1358   LDS3419     NLTT 8758/8757                                                          Chm2004 
02425+4016   STF 292     B is BD+39@611.                                                                 
                         H 4  64.                                                                MEv2010 
02425+1045   CHR 200     First detected as an occultation binary by Blow et al.                  Blw1982a
02426-5048   iot Hor     Combined solution, based on reduction of Hipparcos intermediate                 
                         astrometric data together with spectroscopic elements from Kurster      CPS2000e
                         et al. (2000).                                                          HaI2001 
             HD  17051   No comoving objects found within separation/magnitude range listed.             
                         However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                         background object.                                                              
02426-7947   TOK 362     This 0.6" pair with dK=1.1 is obvious and should have been resolved             
                         both by visual observers and by Hipparcos, yet there are no                     
                         indications of previous resolution in the literature. The declination           
                         of -79deg may have something to do with the missed companion, as the            
                         southern sky is less well surveyed for binaries.                        Tok2013b
02427+3932   J  2401     Jonckheere says is two faint condensations of a nebula. Galaxy           .      
                         UGC 2180.                                                               J__1962a
02427+1434   GWP 357     XMI 280.                                                                Tob2012b
02427-1513   GWP 358     ABL  67.                                                                Tob2012b
02428+4249   HJ 2155     B is BD+42@605.                                                                 
02431+0330   GWP 359     AB: XMI 281AB.                                                          Tob2012b
             GWP 360     AC: XMI 281AC.                                                          Tob2012b
02433+1926   BAG  20     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin et al. (1985).                                                  Grf1985b
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, this is a Hyades non-member                                    Grf1988 
                                                                                                 Grf2013c
02433+1718   BPM  56     [PM2000]   99282 + [PM2000]   99285.                                    Gvr2010 
02433+0314   STF 299     gam Cet = 86 Cet. AC is a CPM pair, according to Alden.                 Ald1924 
                         AB: Additional notes may be found in Muller (1946).                     Mlr1946a
02434-3756   TOK 187     Triple. The A-component is 0.955d SB2; the tertiary is resolved with            
                         speckle. As A is located some 1.7m above the main sequence, the object          
                         can be closer than indicated by the Hipparcos parallax of 24.6 mas.     Tok2012a
02434-6643   FIN 333     Probably an ambiguous case, although only one solution has been                 
                         tested.                                                                         
                         More speckle obs needed to define orbit.                                        
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.55 +/- 4.04, 2.67, and 1.20 Msun, respectively.            Mlk2012 
02435+2742   35 Ari      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Abt & Levy (1978).                                                      AbH1978 
02435+1611   BPM  57     [PM2000]   99396 + [PM2000]   99434.                                    Gvr2010 
02438-2754   BU  261     Aka HDO  59.                                                                    
02440-0601   TOK  75     HIP 12764. A is SB, no orbit, dRV= 2.5). Contradictory photometry of    Nrd2004 
                         B, it is too close in 2MASS (5"). NOMAD: PM(B)=(-99,-71) V=7.79 (??)            
                         Considering the brightness of B and  N*=15, it is almost certainly      Tok2011a
                         physical. A new triple system. See Bonavita & Desidera (2007).          Bnv2007 
02442+4914   STF 296     the Per = 13 Per. A premature orbit has been computed.                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Data appear equally well fit by rectilinear solution - see catalog.             
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: H 3  58.                                                            MEv2010 
02442-2530   FIN 379     Aa,Ab: More than one revolution apparently has occurred.                        
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.55 +/- 0.22, 2.20, and 1.02 Msun, respectively.  Mlk2012 
             BSO   1     HIP 12780. A is visual binary FIN 379, 0.1". B = HIP 12779.             Tok2011a
02443+5704   STF 293     AB: Additional notes may be found in van den Bos.                       B__1963b
02443+1600   GWP 361     XMI 282.                                                                Tob2012b
02445-1859   GWP 362     ABL  68.                                                                Tob2012b
02446+7912   BVD  26     Primary is V405 Cep.                                                            
02446+2928   STF 300     H 1  74.                                                                MEv2010 
02448+4231   LDS3424     NLTT 8830/8829                                                          Chm2004 
02448+1536   KIR   7     A close double dwarf pair,spectral types M5V and M5.5V.                 Kir1999 
02449+5456   ES   50     Initially assigned as TDS  94. Corrected 11/27/01.                              
02449+1007   TOK   1     Aa,Ab: mu Cet = 87 Cet. Considered somewhat uncertain by Tokovinin.             
                         Not resolved by McAlister on several occasions.                                 
                         A preliminary spectroscopic orbit with a period of 1202 days has been           
                         published by Abt (1965).                                                AbH1965 
02449-1336   GWP 363     ABL  69.                                                                Tob2012b
02451-1834   tau 1 Eri   Despite a large acceleration of 26 mas yr-2, no RV variability was              
                         found in the GCS from two measures.                                     Tok2012a
02452-4344   CPO  29     LDS  78.                                                                        
             BRG  15     Aa,Ab: 2MASS J02451431-4344102 is a member of an approximately equal-           
                         brightness binary with ~50" separation, in addition to being a close            
                         binary discovered with AstraLux.                                        Jnn2012 
02452-6700   GLI  18     Spectrum: F5/6III/IV.                                                           
02455-6342   HDO 306     gam Hor. A spectroscopic binary.                                                
02456-7114   HDS 357     Primary is CN Hyi, a W Uma type eclipsing binary, period 0.45611d.      Zas2012 
02457+4456   LDS5393     old LDS6136.                                                                    
                         AB: NLTT 8869/8870                                                      Chm2004 
             GIC  34     AC = G078-004/G078-003 = GJ 3178A+3179B.                                        
02457-3943   B  2077     Astrometric orbit for primary, P=2.303y (Golden & Makarov 2007). PM(A)  Gln2007 
                         moves almost towards B, so the increased separation is not reflex PM.   Tok2014d
02460-0457   BU   83     A premature orbit has been calculated.                                          
                         A: Dommanget (1972) astrometric orbit calculated from perturbations     Dom1972a
                         seen to rectilinear motion.                                                     
02461+1250   GWP 364     XMI 283.                                                                Tob2012b
02462+0536   RAO   9     AB: Primary is HIP 12925. A 13.8m star at 221.7deg, 494.3" appears to           
                         share common proper motion, but the probability of physicality is only          
                         36%. It is likely this star is another member of the Tuc-Hor moving             
                         group.  HIP 12925 and 12862 also appear to be a co-moving pair.         Tok2013c
                         AB: The primary is a spectroscopic binary.                              Tok2014d
                         Quadruple system with 3-tier hierarchy: a close spectroscopic pair              
                         with yet unknown period, Robo-AO companion D at 1".89, and CPM                  
                         companion C at 494" (Tokovinin & Lepine 2012). Yet another star,        Tok2012c
                         HIP 12862, at 0.9deg, also shares common PM and parallax. The stars             
                         are young and belong to the Tucana–Horlogium moving group (Zuckerman    .     
                         et al. 2011 ApJ 732, 61). Our photometry places D slightly above the            
                         MS. D was  independently discovered by Brandt et al. (2014) by high-    Bdt2014 
                         contrast imaging at Subaru. They measured it on 2012.0 at 252.9 deg     RAO2015 
                         and 1".893, in excellent agreement with Riddle et al. (2015).           Rbr2015d
             TOK 651     AC: Tuc-Hor moving group? Additional CPM companions at 725" and 1536".  Tok2014d
                         AD: Too wide to be a companion at 3271", but CPM, common parallax. F            
                         is a rapid rotator (Vsini=109km/s), on main sequence.                           
02462-0619   GWP 365     ABL  70.                                                                Tob2012b
02463+1427   GWP 366     XMI 284.                                                                Tob2012b
02464+0301   GWP 367     XMI 285.                                                                Tob2012b
02470-0952   A  2608     The northern pair, CD, is slightly fainter                              Hei1985a
02470-1320   RST3371     Variable: CU Eri.                                                               
02472+3611   ALI  38     No star seen at AC catalog location of the purported secondary                  
                         - probably a plate flaw.                                                        
02473+1812   BPM  58     [PM2000]  102021 + [PM2000]  102010.                                    Gvr2010 
02473+1803   GWP 368     XMI 286.                                                                Tob2012b
02473+1717   A  2222     CD: Aitken gives the magnitude of B as 13.8. I could not see it at all          
                         on the first two nights, glimpsed it on the fourth, and made a very             
                         uncertain measure on the third. Variable?                               B__1962d
02474-1733   GWP 369     ABL  71.                                                                Tob2012b
02475+1922   STF 305     A premature orbit has been computed.                                            
02476+5357   STF 301     A is a long-period spectroscopic binary, P = 675d.                              
02476+1014   HJ  655     Hipparcos identified the B component as a candidate for Hyades          HIP1998 
                         membership. However, re-reduction of the Hipparcos parallax places      VlF2007 
                         the B component elsewhere, so this is an optical pair.                  Grf2013c
02478-0411   GWP 370     ABL  72.                                                                Tob2012b
02479-0529   GWP 371     ABL  73.                                                                Tob2012b
02480-0108   GRV 993     SLW 134.                                                                        
02480-0940   GAL 325     Object #76 in Gallo's original list.                                    Gal1912b
02480-2836   RED  20     One companion is ~10" from CD-29 1020 = 2MASS J02481094-2835382.  To            
                         the SW at a milar distance is 2MASS J02480263-2835465. There are no             
                         USNO-B1 proper motions for the fainter stars, but comparison of                 
                         Digitized Sky Survey UKST and 2MASS images show little evidence of              
                         significant relative motion. IR colors are consistent with a K0/M3/M6           
                         triple at 60pc. System appears non-hierarchical, with projected                 
                         separations of ~600AU between each component.                           Red2007a
02481-1244   GAL 326     Object #77 in Gallo's original list.                                    Gal1912b
02482+2704   LDS1138     HIP 13081. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
             LDS1138     NLTT 8997/8996                                                          Chm2004 
02483+1532   BPM  59     [PM2000]  102707 + [PM2000]  102652.                                    Gvr2010 
02486+1344   GRV 146     NI    4.                                                                        
                         Primary is BQ Ari, a W UMa type eclipsing binary, period 0.282335d.     Zas2011 
02487+3107   GJ 9102     1981.6875: HD 17433 was misidentified as Gliese 113 by Balega et al.    Bag1984b
                         (1984). It is uncertain whether this observation is of HD 17433 or of           
                         GJ 113 = HD 17382.                                                              
02488-0301   GWP 372     ABL  74.                                                                Tob2012b
02489+3823   ALD  10     First measure probably 90@ in error.                                    Ali1955 
02490-1029   BRG  16     The system is precisely at the 3 sigma threshold for statistically              
                         significant exclusion of the background star hypothesis. By chance,             
                         the AB astrometry is just below the criterion (2.7 sigma) and BC is             
                         just above (3.1 sigma), so in principle the BC pair is inconsistent             
                         with chance alignment, if the pair does share a common proper motion            
                         with  A. However, the proper motion of the system has of course been            
                         determined based on A, so until the AB physical connection has been             
                         demonstrated to the required accuracy, the 3.1 sigma confidence of the          
                         BC pair is irrelevant. Hence, we label the entire system as                     
                         undetermined for now, although it is obviously very likely that the             
                         whole system is indeed bound.                                           Jnn2012 
02491-1712   GWP 373     ABL  75.                                                                Tob2012b
02491-3224   B  1031     bet For                                                                         
02493+1728   STF 311     pi Ari = 42 Ari. A is a spectroscopic and occultation binary.                   
                         AB: H 1  64.                                                            MEv2010 
02494+4336   LDS3429     LDS9137. LDS6137.                                                               
                         NLTT 9035/9037                                                          Chm2004 
02495+5705   MCA   9     V480 Per.                                                                       
02496-0932   GWP 374     ABL  76.                                                                Tob2012b
02497+1209   CHR 201     First detected as an occultation binary by Evn1983a.                            
02498-0220   GWP 376     ABL  78.                                                                Tob2012b
02498-0346   GWP 375     ABL  77.                                                                Tob2012b
02498-2015   HJ 3533     B is BD-20@523.                                                                 
02498-2434   BU  877     gam 1 For. AB =? LDS  80. Separation and position angle (sf)                    
                         agree, as does the DM number from LDS catalog. The quoted primary               
                         magnitude of the LDS pair is much fainter, however - possibly a poor            
                         measure of CB instead?                                                          
02499+0856   STF 313     B component is EE Cet, a W UMa type eclipsing binary, P = 0.37992d.     Zas2012 
02499-0206   GWP 377     ABL  79.                                                                Tob2012b
02500+2716   MCA  10     Aa,Ab: 41 Ari. Aa is a spectroscopic binary and resolved                        
                         interferometer pair.                                                            
             STT  47     AB: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             H 5 116     AC: H V 116.                                                                    
                         AC: Optical pair, based on study of relative motion of the                      
                         components using the method of apparent motion parameters.              Kiy2008 
             H 6   5     AD: H VI 5. D is BD+26@470.                                                     
02501+1646   GWP 378     XMI 287.                                                                Tob2012b
02502+7255   HJ 2157     Also known as STF 298.                                                          
                         Primary is V793 Cas, an Algol-type eclipsing binary, period 1.652303d.  Zas2011 
02502+1343   SHY 426     HIP  13223 + HIP  13122.                                                        
02502+0641   AG   55     AB,C: HJL  42.                                                          HJL1986 
02502-3551   HJ 3536     eta 2 For                                                                       
02504+3551   LDS3430     Old LDS6138. LDS9138.                                                           
                         NLTT 9076/9097                                                          Chm2004 
02505+1113   BPM  60     [PM2000]  104291 + [PM2000]  104261.                                    Gvr2010 
02505-0414   GWP 379     ABL  80.                                                                Tob2012b
02506+3819   BUP  34     16 Per.                                                                         
02507+5554   STF 307     eta Per = 15 Per. A is a spectroscopic binary. B is BD+55@712.                  
02507+1910   TOK  76     HIP 13269. The 2MASS PSC companion at 17.2" is likely an artifact (not          
                         detected in J and H bands). A is an astrometric binary.                 Tok2011a
02507+1601   BPM  61     [PM2000]  104457 + [PM2000]  104476.                                    Gvr2010 
02508-3956   SHY 427     AB: HIP  13271 + HIP  13499.                                                    
02509+0331   PLQ  36     LDS3432.                                                                        
02510+1317   GWP 381     XMI 289.                                                                Tob2012b
02510+1329   GWP 380     XMI 288.                                                                Tob2012b
02510-2100   SEE  20     tau 2 Eri = 2 Eri                                                               
02511+6025   STF 306     Spectroscopic binary, also classified Oe5V and O7.5.                            
                         AC: See BDS 1430.                                                               
                         AG: G component = A component of 02512+6023.                                    
             STI 398     EF: previously 02512+6025STI 298AB, merged with STF 206 system.                 
                         fh: previously 02512+6025STI 298bc, merged with STF 206 system.                 
02512+6023   D  9001     See BDS 1431.                                                                   
02513+0303   HO  218     Position angle and distance changing rapidly but                                
                         period not established. Needs speckle.                                          
02514-1526   GWP 382     ABL  81.                                                                Tob2012b
02516+6033   BU 1374     B component spectral type B0III                                         AbH2000 
                         CD: Also known as STI 400.                                                      
02517+5921   GIC  35     G246-014/G246-013.                                                              
02518+5819   BLL   8     A is a spectroscopic binary. B is BD+57@652.                                    
02518-2117   SEE  21     This very close visual system was discovered at a separation of 0".36   See1898b
                         and has closed steadily for over 90 years. It is unknown at this                
                         point whether the system is still approaching periastron or has                 
                         begun to widen.                                                         Hrt1993 
02520-5347   BRT2020     CD-54@578.                                                                      
02521+1536   GWP 383     XMI 290.                                                                Tob2012b
02521-6054   HJ 3540     CD-61@515.                                                                      
02522+1520   BPM  62     [PM2000]  105424 + [PM2000]  105482.                                    Gvr2010 
02525+2505   LDS1140     NLTT 9175/9176                                                          Chm2004 
02525-1246   LWR   4     EP Eri                                                                          
02527-1105   GWP 384     ABL  84.                                                                Tob2012b
02529+5300   STF 314     AB,C: H 1  38.                                                          MEv2010 
02531-1212   GAL 327     Object #78 in Gallo's original list.                                    Gal1912b
02532+4155   LDS9139     Old LDS6139.                                                                    
02532-1007   GWP 385     ABL  85.                                                                Tob2012b
02533+2714   ALP   8     2MASSI J0253202+271333                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
02536-0745   GWP 386     ABL  86.                                                                Tob2012b
02536-3826   TOK 652     Primary is psi For                                                      Tok2014d
02537+3820   BU  524     AB: 20 Per. Barnard gives this as 20 Per = BU 520.                      Bar1898b
                         Star A is a suspected variable of Delta Scuti type. A suspected                 
                         spectroscopic 3.5 yr period is not confirmed (Scarfe & Fekel 1978).     Scf1978 
                         A measure on 1979.5326 was incorrectly attributed to ADS 2200 by                
                         McAlister & Hendry (1982); it actually belongs to ADS 490.              McA1982d
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Aristidi et al. (1999) orbit includes mass determination.               Ari1999 
                         Docobo et al. (2001) orbit includes mass determination.                 Doc2001c
                         Calculated mass sum is 3.88 +/- 0.58 Msun, a bit high for a pair of             
                         mid-F dwarfs.                                                           Mut2010b
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.88 +/- 0.60, 2.99, and 1.38 Msun, respectively.  Mlk2012 
             STF 318     AB,C: HJL  43.                                                          HJL1986 
                         AB,C: H 3  60.                                                          MEv2010 
02542+3644   ES 2555     ALI 274.                                                                        
02542-1225   GWP 387     ABL  87.                                                                Tob2012b
02543+5246   LAB   1     Aa,Ab: tau Per = 18 Per. Spectrum composite; G4III+A4V. A is a                  
                         long-period spectroscopic binary, resolved by speckle interferometry.   Lab1974 
                         Speckle observations have resolved the pair and invalidate an                   
                         astrometric solution by Kamper (1969).                                  Kam1969a
                         van de Kamp & Andersen orbit rejected from Fourth Orbit Catalog         Kam1969a
                         ("amplitude below noise level")                                         Wor1983 
                         The elements P, T, e, and longitude of periastron for the McAlister     McA1981c
                         (1981) orbit are from the orbit by Colacevich (1941).                   Cla1941 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Demircan & Selam (1992).                                                Dmr1992 
                         The 52" distant, visual double BC may be physical.                              
02544+0946   HJ  658     HIP 13543. B is a known close binary A 2341 of 1.3" separation,                 
                         partially resolved in the ANDICAM images in K and V bands.              Tok2011a
02544-0030   GWP 390     AB: ABL  88AB.                                                          Tob2012b
             GWP 391     AC: ABL  88AC.                                                          Tob2012b
02544+0635   GWP 388     XMI 291.                                                                Tob2012b
02544+1754   GWP 389     XMI 292.                                                                Tob2012b
02546+2819   COU 677     Previously combined with the nearby BRT 130.                                    
02546+1306   BPM  63     [PM2000]  107057 + [PM2000]  107037.                                    Gvr2010 
02548+4332   HJ 2162     Star C is A of HJ 2163, BDS 1479.                                               
02548+2916   BRT 130     1deg error in WDS designation, apparently an error in transcribing              
                         coordinates from the original source.                                           
02548-0640   GWP 393     ABL  89.                                                                Tob2012b
02548+1401   GWP 392     XMI 293.                                                                Tob2012b
02548-2754   HDO  58     Aka HDO  61.                                                                    
02549+1913   GWP 394     XMI 294.                                                                Tob2012b
02549-0709   JNN  21     The primary is an SB2 binary with an 11.8 day period (Torres et al.             
                         2002 AJ, 123, 1701). Since the angular confirmed to share a common              
                         proper motion) for the purpose of multiplicity statistics, although it          
                         is really a triple system. To estimate the mass of the primary for the          
                         purpose of deriving the mass ratio to the tertiary component detected           
                         in our images, we adopt the mass ratio of 0.58 derived from the                 
                         spectroscopic orbit and use the mass corresponding to an M3 spectral            
                         type for the primary.                                                   Jnn2012 
02550-1402   GAL 328     Object #81 in Gallo's original list.                                    Gal1912b
02552-0800   EGN   2     Pair likely unbound.                                                    Egn2007 
02552-4549   CPO 113     This is ESO 247-11, B is an interacting galaxies.                       Dam2010 
02553-0348   GWP 396     ABL  91.                                                                Tob2012b
02553-1209   GWP 395     ABL  90.                                                                Tob2012b
02555+0731   GWP 397     XMI 295.                                                                Tob2012b
02556+2652   STF 326     Parabolic orbit by Hopmann (1967).                                      Hop1967 
                         sigma = areal constant in the true orbit = 0.05215 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 2".827                              
                         Data appear equally well fit by rectilinear solution - see catalog.             
02556+1311   HU 1047     Close, position angles scattered. No positive observations since 1937.          
02557-1223   GAL 329     Object #82 in Gallo's original list.                                    Gal1912b
02558+3429   LDS9140     BC: Old LDS6140.                                                                
                         NLTT 9308/9312                                                          Chm2004 
02558+1909   A  2342     Closing in with little angular change.                                          
02558-1606   GWP 398     ABL  92.                                                                Tob2012b
02559+1455   BPMA  3     [PM2000]  107836 + [PM2000]  107938.                                    Gvr2010 
02559-1521   LDS3441     NLTT 9361/9360                                                          Chm2004 
02560+1221   GWP 399     XMI 296.                                                                Tob2012b
02561+2003   HER   6     AC: Additional notes may be found in Herbig (1962).                     Her1962 
             CVN   6     Ca,Cb: COR   1Aa,Ab previously cataloged is actually this pair.                 
02562+2359   JNN 253     Estimated age 1000-10000 Myr; masses 0.07 +/- 0.02 and 0.07 +/- 0.01            
                         Msun; a ~0.4 AU.                                                        Jnn2014 
02563+5852   STF 321     B is BD+58@531.                                                                 
02563-1816   GWP 400     ABL  93.                                                                Tob2012b
02564+1534   BPM  64     [PM2000]  108162 + [PM2000]  108210.                                    Gvr2010 
02564-1722   LDS3442     NLTT 9390/9388                                                          Chm2004 
02565+6322   MLB 390     Also known as STI 405.                                                          
02565+5526   LDS5401     Duplicity first noted by Ross: Ross 364-5.                              Ros1926 
02567+4248   LDS9141     old LDS6141. A is possibly the same as A of LDS2815.                            
                         AB: NLTT 9354/9355                                                      Chm2004 
02570+1244   BPM  65     [PM2000]  108547 + [PM2000]  108528.                                    Gvr2010 
02571-1244   GWP 401     MBL   1.                                                                Tob2012b
02572+1157   GWP 402     XMI 297.                                                                Tob2012b
02572+0153   A  2413     Component variable?                                                     Hln1963 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         According to Scardia et al. (2001), this orbit is now well defined and  Sca2001d
                         will certainly change little in the future; only the period is still            
                         slightly uncertain. The Hipparcos parallax is 0".02012 +/- 0.00150.             
                         This gives a mass sum of 2.1 Msun +/- 29%, agreeing very well with              
                         expected values for a system of type G0. Compared to the orbit                  
                         calculated by Scardia in 1980, the total mass of the system, whose      Sca1980e
                         uncertainty was then 55%, is now much better defined. The dynamical             
                         parallax is 0".0193, well in agreement with the measured parallax.              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.64 +/- 0.52, 2.04, and 1.05 Msun, respectively.             Mlk2012 
02572-2458   BU  741     Rica (2012) derived a dynamical parallax of 45.0 mas (compared with     FMR2012g
                         44.51 +/- 2.09 mas from Hipparcos) and a mass sum (using the Hipparcos          
                         parallax) of 1.5 +/- 0.3 Msun.                                                  
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.46 +/- 0.44, 1.66, and 0.79 Msun, respectively.  Mlk2012 
02578+4431   STF 328     Statistically the same parallax within the errors would indicate the            
                         components are physical.                                                        
02579+6400   STI 409     PTT 7.                                                                          
02579+0025   STF 332     HJL  44.                                                                HJL1986 
02581+6912   STF 317     BDS mentions a third star 15 sec f at 102.4@.                                   
02582+0310   GWP 403     XMI 298.                                                                Tob2012b
02583-0002   GWP 404     MBL   2.                                                                Tob2012b
02583-4018   PZ    2     the Eri. A is a spectroscopic binary.                                           
02584-0135   A   208     C is BD-02@528.                                                                 
02585-1453   GWP 405     MBL   3.                                                                Tob2012b
02586+2408   BU 1173     Star C (mag. 13, 4.6") is probably physical.                                    
02586+1741   HO  498     Last star in a row of four. STT 49 20' n, 1.9m f.                       Ho_1899a
02586+1302   GWP 406     XMI 299.                                                                Tob2012b
02586-1628   GWP 407     MBL   4.                                                                Tob2012b
02588+4322   LDS2816     B is BD+42@664.                                                                 
02590-0746   GRV 996     SLW 141.                                                                        
02592+2120   STF 333     eps Ari. Variable velocity suspected.                                           
                         Rica (2012) derived a mass sum (using the Hipparcos parallax 9.81 +/-   FMR2012g
                         0.79 mas) of 7.4 +/- 1.8 Msun.                                                  
02594+6034   TRN  14     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7451 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
                         Position angle ambiguity solved by Jesus Maiz Apellaniz.                        
02595+3916   BRT2202     ALI 763.                                                                        
02596+3849   MLB1002     ALI 764.                                                                        
02596+0508   BAL2603     J 1811.                                                                         
02596-1436   LDS3445     NLTT 9570/9569                                                          Chm2004 
02596-2516   LDS3446     zet For                                                                         
                         NLTT 9579/9563                                                          Chm2004 
02598+3856   LAW  11     LSPM J0259+3855 = NLTT 9527. Law et al (2008) derive a distance of      Law2008 
                         18.8 +9.3/-3.4 pc and a projected separation of 17.6 +9.4/-2.8 AU.              
                         Estimated spectral types are M4.5 and M5.5.                                     
03001+6244   STI 417     MLB 391.                                                                        
03001+3911   ALI 765     A is the eclipsing binary ST Per.                                               
03001+1139   BPM  66     [PM2000]  110407 + [PM2000]  110416.                                    Gvr2010 
03002-1110   BRT2627     J 1454.                                                                         
03006+4753   A  1529     Round 1951 - 1954.                                                              
03007+5700   KR   15     Heintz gives the correct identification and position.                   Hei1983a
03008+1527   BPM  67     [PM2000]  110893 + [PM2000]  110922.                                    Gvr2010 
03009+5940   STTA 31     B is BD+59@581.                                                                 
03009+5221   STF 331     Both components are spectroscopic binaries.                                     
                         H 3  36.                                                                MEv2010 
03011+4453   HJ 2167     AB: HJL  45.                                                            HJL1986 
03012-1816   GWP 408     ABL  94.                                                                Tob2012b
03013+6035   MLR 108     V1018 Cas, an Algol-type eclipsing binary, period 4.12781d.             Zas2011 
03013-0636   GWP 409     ABL  95.                                                                Tob2012b
03014+1607   BPM  68     [PM2000]  111250 + [PM2000]  111338.                                    Gvr2010 
03014+0615   HDS 385     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.32, 1.76, and 1.82 Msun, respectively.             Mlk2012 
03014-1409   GWP 410     ABL  96.                                                                Tob2012b
03015+6029   ALV   1     RAFGL 4029 IRS 1. Massive YSO, member of cluster of IR sources.         Alv2004 
03019-1633   RST2292     AB: LDS3448.                                                                    
03021+0005   GAU   2     BAL 652.                                                                        
03023+4124   STF 337     B is below MS in both (V,V-K) and (J,J-K) CMDs: wrong plx(B)=39.9mas!           
                         Wrong PM(B) in HIP?                                                     Tok2014d
03023+1820   A  2414     A premature orbit has been computed.                                            
03023+0405   alp Cet     1975.634: Disk possible marginally resolved (0".014 +/- 0".005) at 400          
                         and 425 nm.                                                                     
                         1975.639: Disk possible marginally resolved at 460 nm.                  Bla1977a
03023-7154   FIN 360     the Hyi. Not seen for certain 1962-1969, and not observed since.                
                         Needs speckle.                                                                  
03024+4204   BRT1135     LDS2824.                                                                        
03025-1516   HJL1114     IR Eri. A combined interferometric/spectroscopic solution by                    
                         Halbwachs et al. (2016) yields masses 0.982 +/- 0.010 and 0.8819 +/-            
                         0.0089 Msun.                                                            HJL2016 
03027-0741   BU   11     rho 2 Eri = 9 Eri. Note: this is not p Eridani (= 01398-5612DUN   5).           
03030-0205   STF 341     Primary is possible SB? On Keck RV program, but only small RV var.      Tok2014d
03031-0049   GWP 413     ABL  97.                                                                Tob2012b
03032-0215   J  1455     BAL 21.                                                                         
03033-1848   GWP 414     ABL  98.                                                                Tob2012b
03034-0804   LDS5409     A possible wide companion to 2MASS J03032132-0805153 at 172" with               
                         similar proper motion is noted in WDS.                                  Jnn2012 
03035+2304   HDS 389     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.50 +/- 0.27, 1.91, and 1.79 Msun, respectively.  Mlk2012 
                         Primary is SB, P(AB)=2152d=5.89y.  Metchev & Hillenbrand (2009)         Met2009 
                         resolve AB and list two faint optical(?) companions at 4", dK~5.        Tok2014d
03036+3627   BUP  37     The COU 869Aa companion was suspected by Burnham.                       Bu_1913 
03036-1001   GWP 415     ABL  99.                                                                Tob2012b
03036-2536   BRG  17     One or both of the stars in this system must be highly variable. The            
                         magnitude differences between the primary and secondary vary from 5.14          
                         mag to 1.72 mag between different observations in Bergfors et al.       Brg2010 
                         (2010) and here. In contrast to the individual note on this system in           
                         Bergfors et al., we assume here that the designation LTT 1453 refers            
                         to the primary star.                                                    Jnn2012 
                         First noted as a likely binary by Makarov & Kaplan (2005), based on     Mkr2005 
                         significant differences between Hipparcos and Tycho proper motions,             
                         then later resolved as part of the Astralux Lucky imaging survey by             
                         Bergfors et al. (2010) and Janson et al. (2012). Their 2008 and 2010    Brg2010 
                         measures, together with measures from 2011 reveal a constant            Jnn2012 
                         separation but a P.A. changing by ~3 deg/yr.                            Bwl2015 
03039+1514   BPM  69     [PM2000]  112964 + [PM2000]  112917.                                    Gvr2010 
03041+3509   POP  11     Popovic coordinate offset was apparently in error.                      Pop1969c
03042+6142   LDS9142     Old LDS6142.                                                                    
03044+2118   JNN  23     The close (~0.40") companion to 2MASS J03042184+2118154 is counted as           
                         an unconfirmed binary companion, since it has not yet been tested for           
                         common proper motion.                                                   Jnn2012 
03045+3844   SMA  33     ALI 766.                                                                        
03046-5119   DUN  10     B is CD-51@706.                                                                 
                         SHY 433. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         HIP 14307 and 14313 form a 38" pair belonging to the FG-67 sample.              
             TOK 428     AC: AC is not co-moving. C=HIP14257 has different parallax              Tok2014d
             TOK 428     Ba,Bb: The component B is resolved here at 0".19. The estimated                 
                         period of Ba,Bb is ~25yr. No motion is seen in 2 months. The subsystem          
                         Ba,Bb is also manifested by asymmetric line profiles (Tokovinin, in             
                         preparation). The A component has never been observed at high angular           
                         resolution.                                                             Tok2015c
03047+6346   STF 335     B is BD+63@388.                                                                 
03048+5330   WRH  29     Aa,Ab: gam Per = 23 Per. SB2. Spectrum composite: G8III+A2V.            WRH1955 
                         1975.781: Uncertain angle readout                                       Bla1977a
                         Analyses of the spectroscopic/interferometric orbit are given by        McA1982a
                         McAlister (1982) and Popper & McAlister (1987). Elements P, T, e for    Ppp1987 
                         the McAlister (1982) orbit are from the spectroscopic orbit by                  
                         McLaughlin (1948).                                                      MLa1948 
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         McAlister (1982).                                                       McA1982a
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
                         The physical nature of visual companion B (57", mag. 11) is uncertain.          
                         Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         5.80 +/- 88.31 and 4.72 Msun, respectively.                             Mlk2012 
03048-0603   GWP 416     ABL 101.                                                                Tob2012b
03049+3446   HU  812     Hussey position angle 1902: 199.4@. Probably wrong quadrant.            Hu_1905a
                         HIP 14342. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
03052-0156   GWP 417     ABL 102.                                                                Tob2012b
03052-3725   BRG  18     This target, like BRG  23, gives conflicting information about whether          
                         the AB pair is physically bound. The brightness and color are fully             
                         consistent with B being an M3.5 companion to the M2.0 primary.                  
                         Furthermore, the separation is only 0.2", and the whole field is                
                         otherwise empty. This indicates physical companionship. However, the            
                         deviation from the expectation of a background source is only 1.1               
                         sigma, and the companion has moved 3.6 times closer to the background           
                         expectation than its original position where the motion has a 14 sigma          
                         confidence. This, by contrast, suggests a chance alignment. Since the           
                         magnitude of motion is not inconsistent with what could be expected             
                         for orbital motion of a real physical pair, we keep it as binary in             
                         our analysis, but we note that further observations will be necessary           
                         in order to resolve this issue satisfactorily.                          Jnn2012 
03054+2515   STF 346     52 Ari. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                         spectroscopic masses 9.10 +/- 6.84, 6.89, and 3.39 Msun, respectively.  Mlk2012 
03054-1432   GWP 418     ABL 103.                                                                Tob2012b
03055+0234   BAL1630     OL  183.                                                                        
03056+1150   GIC  36     G005-013/G005-012.                                                              
03056-0238   GWP 419     ABL 104.                                                                Tob2012b
03059+1302   BPMA  4     [PM2000]  114294 + [PM2000]  114392.                                    Gvr2010 
03061+7925   STF 320     Spectroscopic binary? Spectrum composite; M1III+F7IV.                           
03063-1243   LDS3452     NLTT 9888/9881                                                          Chm2004 
03064+1545   ALP   9     2MASSW J0306268+154514                                                          
                         Physical companionship to this ultracool dwarf ruled out based on I-J           
                         color, using I-band photometry taken at WIYN in February 2003.          AlP2007 
03071+3757   BRT2203     ALI 513.                                                                        
03072-0520   GWP 423     ABL 105.                                                                Tob2012b
03073-1346   CRJ   7     Crepp et al. (2015) determine effective temperatures for the A and B            
                         components of 5680 +/- 40 and 978 +20/-43K. Spectral types are G3V and          
                         T5.5 +/- 1, masses 0.95 +/- 0.02 and >51.9 +3.6/-4.3 Mjup,                      
                         ages 4.6-10 Gyr.                                                        CrJ2015 
03074+5831   RAFGL 437   Shows subarcsecond monopolar nebula extending towards SE at PA                  
                         135 +/- 10deg.                                                          Alv2004 
03075-7859   HJ 3568     A is a spectroscopic binary.                                                    
03076-4702   TOK 206     The companion with q = 0.29 is resolved with NICI but unresolved with           
                         speckle,  being too faint in the optical.                               Tok2012a
03077+3637   ENG  11     B is BD+36@631.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
03078+2533   TOK 234     The B component was suspected of duplicity (0".253, 240.5deg,                   
                         dI=2.7mag) by RoboAO, but the pair was not accepted as real             Tok2014d
03078+1223   BPM  70     [PM2000]  115596 + [PM2000]  115589.                                    Gvr2010 
03078-2750   VIG   3     Optical/physical nature of the faint companion is undefined.            Vig2012 
03079-2813   LDS  86     AB: NLTT 9987/9985                                                      Chm2004 
03080-0135   GWP 425     ABL 107.                                                                Tob2012b
03080-0537   GWP 424     ABL 106.                                                                Tob2012b
03082+4057   LAB   2     Aa,Ab: bet Per = 26 Per = Algol, prototype of the Algol-type binaries.          
                         The eclipse phenomena, known since historical times (although the time          
                         of minimum brightness was first measured by Montanari on 8 Nov 1670)            
                         was first explained as an eclipsing binary by Goodericke as early as            
                         1782. According to R.G. Aitken, this was verified when it was noted as  A__1935f
                         the second spectroscopic binary based on photographic spectra                   
                         obtained by Prof. H.C. Vogel at Potsdam in November, 1889. Belopolsky           
                         discovered a variation in the radial velocity with a period of order            
                         1.8 years, later resolved by Labeyrie and his speckle camera in 1973;   Lab1974 
                         the magnitude difference is about 2.5.                                          
                         The binary, a radio and X-ray source, is triple (and possibly                   
                         quadruple, but the variation with the 32 yr period is more probably an          
                         apsidal rotation of the eclipsing pair).                                        
                         The spectroscopic data were discussed by Hill et al. (1970, 1971).      HlG1970 
                         ADS lists several distant, faint, and probably optical companions.      HlG1971 
                         Elements P, T, e, and omega for Labeyrie et al. (1974) orbit adopted    Lab1974 
                         from the spectroscopic orbit of Hill et al. (1971).                             
                         Analysis of the spectroscopic/interferometric orbit is given by                 
                         Bonneau (1979)                                                          Bnu1979 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Hipparcos astrometric solution adopts some elements from the orbits of  HIP1997d
                         Pan et al. (1993) and                                                   MkT1993a
                         Gatewood et al. (1995).                                                 Gat1995 
                         Peterson et al. (2011) orbits of both the outer (LAB   2Aa,Ab) and      Ptn2011 
                         inner (CSI   1Aa1,Aa2) are based on VLBI measures combined with                 
                         speckle and radial velocity data. Assuming masses of the primary and            
                         secondary of 3.70 and 0.79 Msun, respectively, they derive a mass for           
                         the tertiary of 1.51 +/- 0.02 Msun.                                             
             BU  526     AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
03084+4020   BRT2204     ALI 1031.                                                                       
03084+2620   OSO  14     G037-026. Not a common proper motion pair, based on color               Oso2004 
03084-2410   LDS  87     NLTT 10008/10007                                                        Chm2004 
03084-7033   HLN  19     DAM 782.                                                                        
03087+1736   COU2680     BD+17@499a.                                                                     
03087-1432   GWP 426     ABL 108.                                                                Tob2012b
                         Not a double star, but an edge-on galaxy: USNO-B1.0 proper motion is    Skf2012 
                         spurious.                                                                       
03088-0952   GWP 427     ABL 109.                                                                Tob2012b
03090+4415   STF 351     B is BD+43@637.                                                                 
03090+1740   COU 358     BD+17 501a. Mistaken identification with BD+17 501 led to earlier               
                         incorrect WDS designation as 03088+1801.                                        
03091+4937   BUP  38     iot Per. Proper motion of A +1263 -091.                                         
03092+0728   STFA  6     STTA 32. B is BD+06@487.                                                        
03094-3004   LDS3460     NLTT 10074/10076                                                        Chm2004 
03095+4544   HDS 404     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.90 +/- 0.09, 0.87, and 0.75 Msun, respectively.             Mlk2012 
03095+4451   ES 2596     kap Per = 27 Per. A is a spectroscopic binary.                                  
03096+0512   A  2030     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.41 +/- 0.32, 2.11, and 1.05 Msun, respectively.             Mlk2012 
03096-0054   CHE  75     Aka BAL 281.                                                                    
03098-1238   GWP 428     ABL 110.                                                                Tob2012b
03099-0654   UX Eri      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.901 Msun and the minimum             
                         mass of the wider component at 0.59 Msun.                                       
03101-6355   HJ 3559     B is CPD-64@231.                                                                
03104+0238   OL  177     Not found by Heintz at IDS position. Position corrected.                Hei1990b
03104-0004   GWP 429     ABL 111.                                                                Tob2012b
03105+5040   LDS9143     Old LDS6143.                                                                    
03107+2226   LDS3461     NLTT 10112/10110                                                        Chm2004 
03107-4023   LDS9144     Old LDS6144.  Recognized to be the same as LDS5414 by John Greaves.     Grv2006c
03108+3724   LDS9145     Old LDS6145.                                                                    
                         NLTT 10082/10091                                                        Chm2004 
03110+1648   SPF   1     L dwarf 2MASS J03105986+1648155 resolved into close components at L/T           
                         boundary. Approximate orbital period 72 +/- 4 years, distance 25 +/- 4          
                         pc, system mass ~30-60 Mjup. Spectral types of both components are              
                         estimated at L9 +/- 1.                                                  Spf2010 
03112+2225   H 5 117     Also known as STF 359.                                                          
03113+3937   BLL  10     ome Per = 28 Per                                                                
03117+8128   STF 327     A is a spectroscopic binary.                                                    
03118+3525   GIC  37     G095-014/G095-013.                                                              
03121-2859   HJ 3555     alp For = 12 Eri. The magnitude of B is uncertain and has been                  
                         suspected to vary. Another century is needed for apastron coverage.             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A is GJ 127. B is possible SB. Variability of RV(B) is based on                 
                         historic RV (Eggen, van den Bos)                                        Tok2014d
03121-6420   HJ 3562     B is CPD -64@231.                                                               
03122+3713   STF 360     A premature orbit has been calculated. Data appear equally well fit by          
                         rectilinear solution - see rectilinear elements catalog.                        
                         A is SB1, P=415d. B is possible long-period SB.                         Tok2014d
03123-2727   LDS  88     NLTT 10222/10227                                                        Chm2004 
03124-1157   GWP 432     AB: ABL 112AB.                                                          Tob2012b
             GWP 433     AC: ABL 112AC.                                                          Tob2012b
03124-4425   JC    8     Variable RV of AB, not explained by the visual motion, has been                 
                         reported (Eggen 1965), but Heintz's mass ratio does not support         Egg1965b
                         the presence of a fourth body.                                          Hei1979a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.59 +/- 0.73, 2.18, and 3.82 Msun, respectively.  Mlk2012 
             HJ 3556     AB,C: Star C (mag. 9.2, 3.5") is in slow retrograde motion.                     
                         Heintz (1979) gives AB orbit, attempts AC orbit with P=987yr.           Hei1979a
                         The motion of AC is not directed away from PM(A), hence physical.       Tok2014d
03125-3449   LDS  89     LDS5418.                                                                        
03127+7133   STT  50     A premature orbit has been calculated.                                          
                         Bespalov (1961) has a = 1".618, Finsen & Worley (1970) assume this      Bsp1961 
                         is a misprint.                                                          Fin1970b
03128+3720   WZ    6     ES 2556.                                                                        
03128-0112   HJ  663     94 Cet.                                                                         
                         AB: B is PMS star and SB1 (P=2.026y). Planet (P= 1.2y=535.7d) around            
                         A. Is this true planet or Ba,Bb effect?                                 Tok2014d
             TOK 654     AF: CPM companion HD 20619 = GJ 135: 7.03V, G1.5, HD 20169 at 133'              
                         from AB (0.7 pc)                                                        Tok2014d
03130+3254   LDS9146     AB: Old LDS6146.                                                                
                         B is deeply below MS, blue in V-K and J-K. White dwarf?  WDS: too fast          
                         motion of AB, optical? Hyades cluster. CfA: RV var?                     Tok2014d
                         Hyades cluster. The 2MASS companion B can be physical.                  Tok2014d
                         Previous AD companion, TOK 655, is the same as the known AB pair. The   Dam2015d
                         Luyten measure was poor.                                                        
03130-0343   GWP 434     ABL 113.                                                                Tob2012b
03132+1710   BPM  71     [PM2000]  119048 + [PM2000]  119061.                                    Gvr2010 
03134-0852   GWP 438     ABL 114.                                                                Tob2012b
03135+4417   ES  559     Also known as LDS9147, LDS6147, and LDS2836. These were all recognized          
                         by John Greaves (personal corres.) to be the same pair.                         
                         NLTT 10231/10232                                                        Chm2004 
03136+3909   STF 364     HJL  46.                                                                HJL1986 
03141+5934   TRN  15     CC Cas. Classification in Mason et al. (1998) is from the tomographic   Msn1998a
                         analysis of Hill et al. (1994 A&A 282, 455).                                    
                         The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7452 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
03141+0832   GIC  38     G079-015/G079-016.                                                              
03144-0227   GWP 440     ABL 115.                                                                Tob2012b
03146-0940   GWP 441     ABL 116.                                                                Tob2012b
03149-1400   HJ 3558     HJ 3551 is identical.                                                           
03150+0101   GIC  39     G077-035/G077-034. See Allen et al. (2000) for  information on          AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03151+1618   HU 1055     The companions C, D, and E, given in the ADS, do not exist. They                
                         should be under ADS 2426.                                               B__1963b
03154-6930   R    22     Also appears to be R    27.                                                     
03158+5057   HU  544     A = V572 Per: eclipsing binary of Algol type, period 1.21317 days.      Zas2015
03158-0849   SHY 154     HIP  15197 + HIP  15244. Primary is zet Eri.                                    
03160+4853   LDS9148     Old LDS6148.                                                                    
                         NLTT 10355/10353                                                        Chm2004 
03160+3441   HO  503     A spectroscopic binary and ellipsoidal variable, V423 Per.                      
03162+1302   BPMA  5     [PM2000]  120872 + [PM2000]  120882.                                    Gvr2010 
03165-0642   GWP 443     ABL 117.                                                                Tob2012b
03165-3541   SHY 439     AB: HIP  15239 + HIP  15432.                                                    
             SHY 439     AC: HIP  15239 + HIP  15152.                                                    
             SHY 439     AD: HIP  15239 + HIP  15933.                                                    
             SHY 441     BC: HIP  15432 + HIP  15152.                                                    
03166+4943   ES  463     Aka OL  150.                                                                    
03166+3238   STF 370     According to Burling, the long unconfirmed system, 03064+3153HJ 5456,           
                         may also be this pair.                                                  Bur2005 
03167+4237   LDS9149     Old LDS6149.                                                                    
03167+2639   TOR   4     Formerly known as PAN   1.                                                      
03167-0332   TOK  78     HIP 15247. A is SB without orbit, dRV= 6.6.                             Nrd2004 
03168+7830   STF 345     Also known as STF 340.                                                          
03168+0501   A  2032     HIP 15253. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
03172+4522   PRV   2     GJ 3213. Pravdo et al. (2006) derive masses 0.370 +/- 0.034 and                 
                         0.195 +/- 0.021 Msun.                                                   Prv2006 
03174+0739   BU 1039     Hyades vB 1. BU 1039AB, with rho = 2".2 and Delta m = 6.0 is outside            
                         the detection window.                                                   Msn1993a
                         AC: HJL  47.                                                            HJL1986 
                         AC: SHY 155. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03175+6540   STT  52     A premature orbit has been calculated.                                          
03175-0107   GWP 445     ABL 118.                                                                Tob2012b
03175-1222   J  1456     BRT2628.                                                                Brt1947 
03176-1412   GWP 446     ABL 119.                                                                Tob2012b
03177+6108   STI 441     03175+6108SMA  36                                                               
03177+3838   STT  53     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.51 +/- 0.99, 2.40, and 1.05 Msun, respectively.             Mlk2012 
03178-7029   R    28     Aka RSS  62.                                                                    
03180-6656   EHR   3     Physical/optical nature undefined.                                      Ehr2010 
03182-6230   BNU   2     Aa,Ab: zet 2 Ret. B has common proper motion, +1370 +660, and is                
                         CPD-63@217 = zet 1 Ret.                                                         
                         Aa,Ab: Likely a spurious pair. Last measured 1978 and unresolved by             
                         SOAR on 3 occasions 2008–2012.                                          Tok201
                         Aa,Ab is suspicious, 1 observation in WDS, not binary in Raghavan et    Rag2010 
                         al. (2010). Jones et al. (2002) do not detect SB with precise RV at     CPS2002b
                         the AAT.                                                                Tok2014d
             ALB   1     AB = LDS  92.  HIP 15371. See Allen et al. (2000) for information       AlC2000 
                         on metallicity, age, galactic orbital parameters, etc.                          
                         AB: SHY  16. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03184-0056   AC    2     95 Cet. According to Eggen this pair shares common proper motion with   Egg1960 
                         BD -01 474 at 11'.                                                              
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03184-0708   LDS3473     HIP 15396. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 10536/10548                                                        Chm2004 
03184-2231   SEE  23     15 Eri. CD-22@1146. Motion direct.                                              
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.33 +/- 0.80, 3.35, and 1.20 Msun, respectively.             Mlk2012 
03185+4721   MET   1     V522 Per.                                                               Met2004a
03185+1511   LDS9150     Old LDS6150. HIP 15394. See Allen et al. (2000) for information on      AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03186+0827   LUH   6     AC: LSPM J0318+0827S + 2MASS J03184214+0828002.                         Luh2012b
03187+1527   LDS9151     Old LDS6151. SLE  41.                                                           
03187-1834   HJ 3565     A is a spectroscopic binary.                                                    
03188-0028   ABT   3     BAL 656.                                                                        
03188-0321   GWP 447     ABL 120.                                                                Tob2012b
03190-1549   GWP 448     ABL 121.                                                                Tob2012b
03192-5306   HJ 3571     CD-53@674.                                                                      
03193-0232   GWP 449     ABL 122.                                                                Tob2012b
03194+6156   JNN 254     G 246-33. Estimated age 35-300 Myr; masses 0.29 +/- 0.11 and 0.17 +/-           
                         0.07 Msun; a ~10.8 AU.                                                  Jnn2014 
03194+0322   STT 557     AB: kap 1 Cet = 96 Cet. Variable? A is a spectroscopic binary.                  
                         B is BD+02@521.                                                                 
03195-2145   JC    1     tau 4 Eri = 16 Eri. A is an irregular variable.                                 
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03199-0321   GWP 450     ABL 123.                                                                Tob2012b
03200+6539   BUP  43     Shell star. Light and spectrum variable, BK Cam. May also be a long-            
                         period spectroscopic binary.                                                    
03200+3845   BRT2205     MLB 819. ALI 774.                                                               
03201-2851   LDS  93     van den Bergh reports a third star at 38@, 105.6".                      Bgh1958 
                         A is exoplanet host, P=592d. B = HIP 15526 hosts exoplanets with                
                         P=29.1d, 85.1d.                                                         Tok2014d
                         B is CD-29@1229.                                                                
                         NLTT 10636/10635                                                        Chm2004 
                         SHY 157. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03202-1457   LDS3479     NLTT 10629/10617                                                        Chm2004 
03202-1632   GWP 452     ABL 124.                                                                Tob2012b
03203+1944   STF 376     H 2  76.                                                                MEv2010 
03203+1625   SLE  42     Hipparcos suspected non-single.                                                 
03206+0902   GIC  40     G079-029/G079-030 = GJ 9114AB.                                                  
                         HIP 15572. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         Primary is SB1, P=321.6d                                                Tok2014d
03207+8459   STF 319     Schiller measures 1910.87,331.1@,42.32",7.7-9.2.                        Shr1913 
03207+1736   HJ 3245     See BDS for components.                                                         
03210-0054   LDS5420     LDS5420A was B component of 03211-0054ITF  55AB, LDS5420B was ITF 55C           
                         Pairs merged; ITF 55AB --> 03210-0054ITF 55AD (with quadrant flip),             
                         ITF 55AC --> 03210-0054ITF 55BD (also with quadrant flip).                      
03211-2632   SWR   5     CPM pair                                                                Skf2004 
03212+2109   COU 259     tau 1 Ari = 61 Ari. A is an irregular variable.                                 
03213+4302   A  1706     LDS2842.                                                                        
03214+4320   VIG   4     Optical/physical nature of the faint companion is undefined.            Vig2012 
03216-0841   GWP 454     ABL 126.                                                                Tob2012b
03217+0845   STF 380     A premature orbit has been calculated.                                          
03219+4904   WEB   1     B is BD+48@892.                                                                 
03220+1715   LDS3483     G006-003. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 10701/10698                                                        Chm2004 
03220-1636   LDS3485     NLTT 10725/10724                                                        Chm2004 
03226-0210   GWP 456     ABL 127.                                                                Tob2012b
03226-3011   LDS3487     LDS5422.                                                                        
                         NLTT 10762/10761                                                        Chm2004 
03227+1717   BPM  72     [PM2000]  124803 + [PM2000]  124860.                                    Gvr2010 
03227+1037   GIC  41     BC: 03328+1040 UC  997.                                                         
03228-0042   GWP 457     ABL 128.                                                                Tob2012b
03229+2949   STF 379     H III 91, BDS 1688.                                                             
                         H 3  91.                                                                MEv2010 
03230-0548   GWP 458     ABL 129.                                                                Tob2012b
03232+4554   LDS9152     Old LDS6152.  HD 20835. See Allen et al. (2000) for information on      AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
03232-1404   GWP 459     ABL 130.                                                                Tob2012b
03233-0337   GWP 460     ABL 131.                                                                Tob2012b
03233-5000   HJ 3573     LDS  94. A is CD-50@1015, B is CD-50@1014 (Roman).                              
03234-0710   GWP 461     ABL 132.                                                                Tob2012b
03234-1015   HJ 2188     STF 387.                                                                        
03236+0453   BU 1178     A is a spectroscopic binary.                                                    
                         Greenwich measure of 1921 erroneous. No certain change since 1890.      B__1963b
03236-4005   I   468     glimpsed?                                                               I__1948a
                         Soderhjelm (1999) gives possible orbit from two widely spaced visual    Sod1999 
                         observations + Hipparcos data.                                                  
03236-8116   SHY 161     AC: HIP  15803 + HIP  17184.                                                    
03237-0609   GWP 462     ABL 133.                                                                Tob2012b
03238+2432   LDS1144     NLTT 10780/10781                                                        Chm2004 
03240-0007   GRV 997     = GWP 464 = ABL 135.                                                    Tob2012b
03240-2613   HJ 3572     B is CD-26@1270.                                                                
                         SWR   6. CPM pair                                                       Skf2004 
03242+2347   LDS 884     AB,C: NLTT 10804/10808                                                  Chm2004 
03242-1048   GWP 463     ABL 134.                                                                Tob2012b
03243+4952   BUP  44     alp Per = 33 Per                                                                
03244-1539   A  2909     There are many negative observations. Needs speckle.                            
                         HIP 15868. A is the close pair A 2909, 0.1". The 2MASS PSC companion            
                         at 17" is called C in the WDS.                                          Tok2011a
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 0.62 +/- 0.11, 2.10, and 1.01 Msun, respectively.  Mlk2012 
                         CfA: SB? P=9115d? =25y?  UR at SOAR from 2008.6 to 2012.9, in           Mlr1955a
                         contradiction with orbit of Muller (1955).                              Tok2014d
03245+4626   LDS9153     Old LDS6153.                                                                    
03248-1533   GWP 466     ABL 136.                                                                Tob2012b
03249+1552   BPM  73     [PM2000]  126226 + [PM2000]  126261.                                    Gvr2010 
03249-0356   GWP 467     ABL 137.                                                                Tob2012b
03253+1158   BPM  74     [PM2000]  126464 + [PM2000]  126473.                                    Gvr2010 
03256-1855   GWP 468     ABL 138.                                                                Tob2012b
03257+0551   JNN 255     AB: GJ 3224. Estimated age 300-1000 Myr; masses 0.25 +/- 0.06 and 0.14          
                         +/- 0.01 Msun; a ~6.3 AU.                                               Jnn2014 
                         AC: Estimated age 300-1000 Myr; masses 0.48 +/- 0.25 and 0.45 +/- 0.24          
                         Msun; a ~48.1 AU.                                                       Jnn2014 
03259+4540   COU1682     TDS2544.                                                                        
03261+1229   A   829     Probably ambiguous case, but only one solution has been tested.                 
03262+2950   ALP  10     2MASSW J0326137+295015                                                          
                         Further observations are required to determine the physical/optical             
                         nature of this pair.                                                    AlP2007 
03262-1817   GWP 469     ABL 139.                                                                Tob2012b
03263+1709   JNN 256     Estimated age 1000-10000 Myr; masses 0.24 +/- 0.03 and 0.16 +/- 0.03            
                         Msun; a ~20.6 AU.                                                       Jnn2014 
03264+3520   HDS 430     Cvetkovic et al. (2016) estimate spectral types F7 and G8, masses 1.30          
                         and 0.97 Msun. Dynamical parallax is 15.60 +/- 0.44 mas.                Cve2016b
03265+5909   GIC  42     G246-036/G246-035.                                                              
03266+2843   CHR   9     Aa,Ab: This is UX Ari, an RS CVn type binary that is not eclipsing.             
                         Peterson et al. (2011) orbits of both the outer (CHR   9Aa,Ab) and      Ptn2011 
                         inner (UX Ari Aa1,Aa2) are based on VLBI measures combined with                 
                         speckle and radial velocity data. Assuming masses of the primary and            
                         secondary of 1.10 and 0.95 Msun, respectively, they derive a mass for           
                         the tertiary of 0.75 +/- 0.01 Msun.                                             
             TOK  13     AB: AB is CPM, estimated period 20,000y. Primary is 6.4d SB2.                   
                         The spectrum shows 3 components (Fekel, 1986 private communication),            
                         two of which are identified with the 6.44-day system described by               
                         Carlos & Popper (1971), while the third is possibly the component       Ppp1971 
                         listed here.                                                                    
                         Evolved or bad 2MASS photometry.                                        Tok2006 
03266+1406   BPM  75     [PM2000]  127254 + [PM2000]  127284.                                    Gvr2010 
03269+1609   BPM  76     [PM2000]  127466 + [PM2000]  127423.                                    Gvr2010 
03269-2344   RSS   4     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
03271+1845   CHR  10     Resolution of an occultation binary.                                            
03272+0944   HDS 433     1975.629: Marginally resolved at 450 nm?                                Bla1977a
03276+5847   RAFGL 490   Extended emission seen in H-band, no subarcsecond structure resolved.   Alv2004 
03278+5627   STI1984     The relative motion is small but fairly certain; it is smaller than             
                         the proper motions of both components. Therefore, although the                  
                         component proper motions are of the same order, we consider this to be          
                         a physical pair.                                                        Kiy2012 
03278-2352   LDS3496     NLTT 11000/10999                                                        Chm2004 
03279+5625   MLB 116     Triple star with weak hierarchy. Motions of all components relative to          
                         each other are small. If we trust the relatively large pm for A from            
                         the WDS, the system is physically bound; however there is an                    
                         appreciable discrepancy between this pm and the value given by                  
                         Kharhenko & Rezer (2001, Kinemat. Fiz. Nebesn. Tel 17, 409). Therefore          
                         we are not yet able to determine with confidence whether or not the             
                         components are physically bound.                                        Kiy2012 
03279-1948   GC 4128     Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                         Cluster Melotte 25 #EGG21.                                                      
03280+2631   LDS1146     NLTT 10977/10976                                                        Chm2004 
03280+2028   STF 394     AB: H 3  77.                                                            MEv2010 
03282+5628   ES 1777     Relative and proper motions are of the same order, making it                    
                         impossible to judge whether the pair is physically bound.               Kiy2012 
03282-1335   GAL 330     Object #94 in Gallo's original list.                                    Gal1912b
03282-3551   I    58     chi 3 For                                                                       
03284+2248   BAG   2     Aa,Ab: 66 Ari. A is a spectroscopic and occultation binary.                     
                         Agreement is poor between this observation and the only other                   
                         measurement, by Balega (1988, private communication).                   Hrt1992b
03284-1425   GWP 470     ABL 140.                                                                Tob2012b
03286-1537   LDS3498     NLTT 11020/11021                                                        Chm2004 
                         Also known as GJ 3228A, this star has a wide binary companion at 16"    VVO1991 
                         separation (e.g., Weis 1991).                                           Jnn2012 
03289+4039   ES 2598     LDS6169.                                                                        
03289-2723   LDS9154     Old LDS6154.                                                                    
03291+0118   MET   2     RX J0329.1+0118                                                                 
03292-0226   GWP 471     ABL 141.                                                                Tob2012b
03294+4931   BU 1179     34 Per.                                                                         
                         Magnitude 11.6 of Burnham is underestimate; mine are similar to the             
                         photometric values of Kuiper (1.93)                                     Baz1954a
03294-6256   HJ 3580     kap Ret. LDS 100.                                                               
03295-1558   GWP 472     ABL 142.                                                                Tob2012b
03296+2431   SAR   1     HBC 347 = V1224 Tau.                                                            
03297+5955   HLM   2     Aka HLM  42.                                                                    
03297-0850   GAL 331     Object #95 in Gallo's original list.                                    Gal1912b
03298+8402   STF 343     STF 347.                                                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03300+5527   STF 390     Aka H N  66.                                                                    
03301+1258   BPMA  6     [PM2000]  129571 + [PM2000]  129567.                                    Gvr2010 
03301-1019   GWP 473     ABL 143.                                                                Tob2012b
03302+7402   GIC  43     G221-010/G221-011.                                                              
                         NLTT 10954/10953                                                        Chm2004 
             FAR  31     NLTT 10954. Primary is white dwarf WD 0324+738.                         Far2006 
03304-1257   GWP 474     ABL 144.                                                                Tob2012b
03305+5418   LEP  15     NI    7.                                                                        
03305+2006   STF 399     AB: H 4  89 (aka, H IV 89)                                              MEv2010 
                         A component SB1, P=32.5y. Is AB a real physical pair, or just two               
                         members of Hyades?                                                      Tok2014d
03307-1926   HDS 441     Cvetkovic et al. (2016) estimate spectral types G2 and G5, masses 1.11          
                         and 1.05 Msun. Dynamical parallax is 24.78 +/- 1.48 mas.                Cve2016b
03309+7041   JNN 257     LHS 1553. Estimated age 1000-10000 Myr; masses 0.31 +/- 0.03 and 0.17           
                         +/- 0.02 Msun; a ~7.9 AU.                                               Jnn2014 
03309+1256   5 Tau       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Harper (1924).                                                          Hrp1924 
03309-6200   TOK 190     The double-lined SB detected in GCS is resolved by speckle. Its                 
                         estimated orbital period of 4 yr explains the acceleration.             Tok2012a
03311+2744   STFA  7     STTA 34. B is BD+27@513.                                                        
                         HJL  49.                                                                HJL1986 
03311+1544   HDS 443     1997.7181  Large change in separation seen since Hipparcos epoch.       Msn1999b
03312+1947   STF 403     AB: H 1  55.                                                            MEv2010 
03313+6644   OSO  15     G246-038. Not a common proper motion pair, based on comparison with             
                         POSS2 red plates. PM = +1193 -1066.                                     Oso2004 
03313+2734   SHY 445     BC: HIP  16410 + HIP  16742.                                                    
03313-5955   JSP  47     CD-60@724.                                                                      
03314+5842   STI1991     STI1997.                                                                        
03316+4752   STT  56     Primary also is classified B8.5VeShell.                                         
03317+1331   BPM  77     [PM2000]  130670 + [PM2000]  130734.                                    Gvr2010 
03318+3803   ES 2458     ALI 517 is the same pair.                                               Hei1980a
03319+3536   ES 2559     BRT 3235.                                                                       
03319-2537   VIG   5     The B component appears to be a faint background star.                  Vig2012 
03320+6735   STT  54     B is BD+67@@274.                                                                
03320+1820   LDS3501     NLTT 11140/11139                                                        Chm2004 
03321+4801   BAG  40     Primary is the rotationally variable star V396 Per.                             
03321+4340   COU1688     AB: A premature orbit has been calculated with very sparse data, since          
                         most of the observations are negative.                                          
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.58 +/- 1.35, 2.16, and 0.95 Msun, respectively.  Mlk2012 
             LDS9155     AC: Old LDS6155. HIP 16467. See Allen et al. (2000) for information on  AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 11124/11125                                                        Chm2004 
03322+1133   AG   68     H IV 44. Also known as STF 409.                                                 
                         H 4  44.                                                                MEv2010 
03323-0705   STF 411     B is BD-07@619 (Roman).                                                         
                         B component spectral type F9IV                                          AbH2000 
03326+2844   JNN  24     This is a close triple system discovered with AstraLux, where in                
                         particular the tertiary component is difficult to fit for. Since the            
                         relative positions of the BC pair components are therefore clearly              
                         dominated by noise scatter in both separation and position angle, we            
                         set the error of each epoch to the scatter among the data points and            
                         make no assessment of orbital motion for the BC pair (although by               
                         contrast, clear orbital motion is seen of the pair with respect to the          
                         A component).                                                           Jnn2012 
                         Estimated age 10-20 Myr; masses 0.07 +/- 0.01 and 0.04 +/- 0.01 Msun;           
                         a ~8.7 AU.                                                              Jnn2014 
03327+3540   CHR 261     This object is a new addition to older Hyades member lists added by             
                         Schwan (1991 A&A, 243, 386), although Griffin (1992 private comm.)              
                         doubts that this object is actually a cluster member. While its status          
                         is not definitive, subsequent confirmation or suspected duplicity (by           
                         another technique) makes the discovery measurement somewhat more                
                         probable.                                                               Msn1993a
03327-0553   GWP 476     ABL 145.                                                                Tob2012b
03328-0247   GWP 477     ABL 146.                                                                Tob2012b
03329-0927   BLA   2     eps Eri = 18 Eri. Macintosh et al (2003) made a K-band search for       MBA2003 
             MBA   1     extrasolar planets in the dust surrounding eps Eri, using Keck, NIRC2,          
                         and AO. The relative motions for these 10 objects between 2001 Dec and          
                         2002 Aug were all well below expected motions for true companions,              
                         leading to conclusion all these faint companions are background stars.          
03332+4615   ES  560     NLTT 11174/11176                                                        Chm2004 
03334+2322   STT  57     STTA 35 = S   429.                                                              
03335+5846   STF 396     B is BD+58@618. Spectrum of A: Am(A3/A7/F0).                                    
03336-0735   GWP 478     ABL 147.                                                                Tob2012b
03336-1904   RSS  66     CPD-19@376                                                                      
03337+5752   CHR 117     Cf orbit in McAlister et al. (1992).  High-space-velocity binary.       McA1992 
                         See Balega et al. (2001) for further discussion of Li abundance.        Bag2001 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.47 +/- 0.38, 3.40, and 1.13 Msun, respectively.             Mlk2012 
03339+3205   HJ  334     STT 540.                                                                        
03339-3105   B    52     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.62 +/- 1.43, 2.46, and 1.20 Msun, respectively.             Mlk2012 
03342+4837   BU  787     Burnham notes: "Hussey measures a third star, 175.8deg, 12.70arcsec     Hu_1903b
                         (1898.70) 1n. I could not see this on one night with the 40-inch, but           
                         measured 11m star in nearly the same direction, 175.6deg, 36.78arcsec           
                         (1899.13) 1n."                                                          Bu_1906 
                         C does not exist.                                                       B__1960b
03342+4651   HDS 452     V578 Per, eclipsing binary of bet Lyr type, period 0.97077d.            Zas2016 
03343+6348   MLB 190     Also known as WFC  16.                                                          
03343+2625   OL  152     COU 687.                                                                        
03344+2428   STF 412     7 Tau. Only P, T, and a were redetermined by Vlaicu & Vasile (1961);    Vla1965 
                         the remaining elements were from the orbit of Luyten (1934).            Luy1934c
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.04 +/- 1.54, 4.91, and 2.09 Msun, respectively.  Mlk2012 
                         AB,C: H 4  88.                                                          MEv2010 
03344-1940   GWP 480     ABL 148.                                                                Tob2012b
03345+1948   STF 414     H III 78. STT  58.                                                              
                         H 3  78.                                                                MEv2010 
03346-1613   GAL 332     Object #96 in Gallo's original list.                                    Gal1912b
03346-3104   LDS3508     NLTT 11300/11288                                                        Chm2004 
03348+2126   BRT3261     AB: Also known as TDS2588.                                                      
                         AB: Additional notes may be found in Couteau (1952).                    Cou1952a
             J   932     AB,C: Additional notes may be found in Jonckheere (1949) and            J__1949b
                         Couteau (1952).                                                         Cou1952a
03349-1604   GAL 353     Object #97 in Gallo's original list. ARA  17.                           Gal1912b
03350+6002   STF 400     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.96 +/- 1.62, 2.62, and 1.30 Msun, respectively.  Mlk2012 
03350+3201   STF 410     A is an ellipsoidal variable, IX Per.                                           
03352+0543   TOK 657     CPM, common parallax, both on MS.                                       Tok2014d
03353+1549   BPM  78     [PM2000]  133139 + [PM2000]  133157.                                    Gvr2010 
03354+3948   MLB1064     ALI 1035.                                                                       
03355-3218   LDS3510     NLTT 11346/11349                                                        Chm2004 
03356+4253   LDS9156     Old LDS6156.                                                                    
                         AD: NLTT 11280/11270                                                    Chm2004 
03357-1644   GWP 484     ABL 149.                                                                Tob2012b
03361-0320   J  1457     HD 22393.                                                               J__1941a
03362+4220   A  1535     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.99 +/- 0.69, 2.06, and 0.95 Msun, respectively.             Mlk2012 
03368+2106   LDS3511     NLTT 11370/11371                                                        Chm2004 
03368+0035   STF 422     A premature orbit has been computed. The primary is a variable of the           
                         RS CVn type, V711 Tau., and also a spectroscopic binary, P = 2.8 d.             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         H 3  45.                                                                MEv2010 
03369-4957   SEE  29     The astrometric orbit of the stars comprising the A component was               
                         generated by a fit to individual data points available in Hipparcos             
                         Intermediate Astrometry Data.                                           Mkr2007a
                         Primary is possible SB.                                                 Tok2014d
             TOK 207     Likely triple. The inner pair produces RV variability and acceleration,         
                         the outer companion at 2".7 is discovered with NICI.                    Tok2012a
03370-2808   LDS 840     NLTT 11423/11421                                                        Chm2004 
03372+3710   BRT3236     ALI 283.                                                                        
03373-8517   R    39     Also appears to be R    48.                                                     
03374-8051   HJ 3607     B is CPD-81@89.                                                                 
03375+3107   GC 4314     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03376+1751   LDS3512     NLTT 11415/11416                                                        Chm2004 
03376-0103   GWP 486     ABL 150.                                                                Tob2012b
03377+7235   HJ 2190     C component is galaxy NGC 1343.                                                 
03377-0801   GWP 487     ABL 151.                                                                Tob2012b
03378+4046   COU1517     AB Per, an Algol type eclipsing binary, P = 7.1601d.                    Zas2012 
03378+1526   HD  22522   This star was misidentified as BD+17 0593 = SAO 93525 in the first              
                         speckle catalog.                                                        McA1984b
03379+8017   MLR 456     Also known as TDS2606.                                                          
03379+1950   LDS3515     G006-022. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         NLTT 11424/11425                                                        Chm2004 
03381-1133   OL  151     Aka HEI 315.                                                                    
03382-5947   DUN  14     B is CPD-60@261.                                                                
                         SHY 448. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03383+4448   S   430     STTA 37.  B is BD+44@759.                                                       
                         AB: HJL  50.                                                            HJL1986 
03388+5055   ES  953     Appears to be the lost HJ 2197.                                         Dam2015b
03388-1607   LDS3517     NLTT 11485/11486                                                        Chm2004 
03390+4232   RAO  47     Triple system consisting of an astrometric binary with period of 3 yr           
                         (Goldin & Makarov 2007) and Robo-AO tertiary B at 1".76. Considering    Gln2007 
                         the fast PM(A), the fixed position of AB during 1 year would appear to          
                         confirm it as a physical binary. B is located well below the MS,                
                         although its photometry has a large uncertainty. If it is a physical            
                         component with unusual colors, the system merits further study.         Rbr2015d
03392+5632   JNN 258     G 175-2. Estimated age 1000-10000 Myr; masses 0.60 +/- 0.10 and 0.38            
                         +/- 0.03 Msun; a ~24.7 AU.                                              Jnn2014 
03393+5632   JNN 258     Aa,Ab: Originally 03392+5632; merged with 03393+5632.                           
03395-1017   GWP 494     ABL 153.                                                                Tob2012b
03396+3747   GRV 185     Primary is V736 Per, Algol-type eclipsing binary, period 3.76674d.      Zas2013 
03396+2530   LDS9158     old LDS6158. This is the common proper motion pair Wolf 204,5.                  
03396+1823   TOK  14     AB has estimated period 5000y; primary is 8.7d SB2.                     Tok2006 
             LDS9159     AC: Old LDS6159.                                                                
                         NLTT 11499/11500                                                        Chm2004 
03397-0331   GWP 495     ABL 155.                                                                Tob2012b
03397-1612   GWP 496     ABL 154.                                                                Tob2012b
03397-2727   LDS 841     NLTT 11538/11539                                                        Chm2004 
03398+3328   ES  327     Also known as GJ 9119 B, this star is a wide companion to GJ 9119 A at          
                         about 14" as noted in e.g. the WDS catalog. It is however single in             
                         the separation range covered by the AstraLux data.                      Jnn2012 
03398+0515   J  1812     BAL 2608.                                                                       
03400+6352   STTA 36     A,BC: HJL  51.                                                          HJL1986 
                         A,BC: SHY 160. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                         very high (near 100%) probability pair is physical.                             
03401+3407   STF 425     H 2  52.                                                                MEv2010 
                         The B component was resolved at Palomar (0.580"). Genet et al. (2013)           
                         detect a wobble in the motion of AB, with P~107y, alpha~0.18"                   
                         suggesting M2~0.5 Msun                                                  Tok2014d
                         AB: known binary, which shows apparently a non-Keplerian motion. Rica           
                         Romero & Zirm (2014) proposed that the motion was caused by an unseen   RMR2014c
                         companion and calculated an astrometric orbit for it with P = 107 yr,           
                         eccentricity 0.61, and photocenter semimajor axis 0".179. Our                   
                         observations were able to resolve the predicted subsystem Aa,Ab. For            
                         the time of our observations the orbit predicts a companion position            
                         angle of 43.3 deg, in excellent agreement with the position angle of            
                         44 +/- 1.3 deg measured here. The ratio of the predicted displacement           
                         to the measured separation of 0".50 is r = 0.32 = q/(1+q). Hence, the           
                         mass ratio q = 0.47 (the contribution of the light from Ab to the               
                         photo-center is neglected). The mass of Aa is estimated at 1.16 Msun            
                         from its absolute magnitude, leading to 0.54 Msun for Ab. The absolute          
                         magnitude of Ab corresponds to a smaller mass of 0.33 Msun. This                
                         discrepancy, if confirmed, can be explained by Ab being a close pair            
                         of M-dwarfs, as happens in other known multiple systems, e.g., in kap   Tok2013a
                         For (Tokovinin 2013).                                                   Rbr2015d
03402-1936   GC 4392     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03403-0805   STF 433     B is BD-08@698.                                                                 
03404-1502   GWP 497     ABL 156.                                                                Tob2012b
03405-1925   GWP 498     ABL 157.                                                                Tob2012b
03406+2846   STF 427     H N  23.                                                                MEv2010 
                         V1268 Tau, Algol (EA) type eclipsing binary, P = 8.161235 d.            Zas2011 
03407+0643   A  1934     Companion not seen in 1934.                                                     
03409+1435   BPM  79     [PM2000]  137052 + [PM2000]  137046.                                    Gvr2010 
03409-1237   STF 436     B is BD-13@712.                                                                 
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
03413+4554   BU 1181     Motion in separation. The period may be fairly short. Needs speckle.            
                         Additional notes may be found in van den Bos (1963).                    B__1963b
                         Known triple system. Inner binary has been known for over a century     Bu_1894d
                         (Burnham 1894); its first orbit was computed by Riddle et al. (2015).   RAO2015 
                         They also detected a third component C which was confirmed by                   
                         examination of 2MASS images. The close binary is detectable in our Ks           
                         images, but the PSFs of the stars are overlapping and we are unable to          
                         make a consistent measurement with fitstars. We are able to extract             
                         the astrometry of the AC pair and consider it as likely physical.       Rbr2015d
03414-0934   GWP 501     ABL 159.                                                                Tob2012b
03414-1421   GWP 499     ABL 158.                                                                Tob2012b
03416+2655   LDS6095     Also known as GRV 187.                                                          
03418+6239   BLL  12     A is a semi-regular variable, U Cam. B is BD+62@594.                            
03418+5317   A   985     Primary is the eclipsing binary CV Cam, P = 0.97326 day.                Zas2010 
03419-5542   JNN  25     2MASS J03415581-5542287 and J03415608-5542408 are separated by only             
                         12" and have similar estimated spectroscopic distances (14 and 20 pc,           
                         respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                         a physical pair. 2MASS J03415581-5542287 is a close (~0.61") binary in          
                         our data, so the system is likely triple in reality, although common            
                         proper motion of all components has yet to be proven.                   Jnn2012 
03422+6313   BD Cam      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin (1984).                                                         Grf1984c
03422+5436   HJ 2198     B is BD+54@704.                                                                 
03423+3141   COU 691     A premature orbit has been computed.                                            
03424+3358   STF 431     40 Per = o Per. A spectroscopic binary. Spectrum of B: A1Vn.                    
                         H 3  39.                                                                MEv2010 
03424-1200   GWP 503     ABL 160.                                                                Tob2012b
03424-8001   HJ 3612     Spectrum: G0/2III/IV. B is CPD-80@94.                                           
03425+3256   HJ  336     Also known as STF 432.                                                          
03425+1416   BPM  80     [PM2000]  138169 + [PM2000]  138144.                                    Gvr2010 
03425+1216   JNN  26     Since the two epochs of observation were acquired over a baseline of            
                         only a few months, there is not yet sufficient motion to confirm                
                         common proper motion of the companion that was detected with AstraLux.          
                         However, the separation between components is rather small (~0.86"),            
                         and the fact that the companion is clearly detected in z' but too               
                         faint in i' implies that it must be very red, as expected for a real            
                         companion. Hence, we count it as a binary system for statistical                
                         purposes.                                                               Jnn2012 
                         Primary is an active M4.0Ve star, age 60-300 Myr. Bowler et al (2015)           
                         confirm B is physically bound and detect slight orbital motion. The             
                         projected separation is 19.8 +/- 0.9 AU. Spectral type of B is                  
                         L0 +/- 1, mass 35 +/- 8 Mjup.                                           Bwl2015 
03425+0202   BAL1260     HJL  52.                                                                HJL1986 
03426+1718   GC 4435     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03426-2445   RST2317     TDS2636.                                                                        
03427+1448   BPM  81     [PM2000]  138368 + [PM2000]  138396.                                    Gvr2010 
03427-2428   LDS3527     NLTT 11680/11682                                                        Chm2004 
03429+4747   BUP  46     del Per = 39 Per. A possible variable of the Alpha CVn type.                    
03430+4554   JNN 259     NLTT 11633. Estimated age 1000-10000 Myr; masses 0.28 +/- 0.03 and              
                         0.20 +/- 0.04 Msun; a ~21.8 AU.                                         Jnn2014 
03430+2515   LDS1148     NLTT 11651/11648.                                                               
03431+2541   STF 435     H 3  88.                                                                MEv2010 
03435-4549   PRB   1     Primary is WD 0341-45 = VY Hor, secondary (not found in Aladin) is              
                         BPM 31492. Possible CPM pair, according to Probst (1983).               Prb1983 
03438+4236   ENG  14     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03439+1640   GIC  44     AB = G006-029/G006-028 = GJ 9122AB.                                             
                         AB: NLTT 11693/11688                                                    Chm2004 
                         AB: SHY  17. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
03439-7100   HJ 3603     B is CPD-71@@218.                                                               
03440+3822   STF 434     B is BD+37@@821.                                                                
03440-1836   GWP 505     ABL 161.                                                                Tob2012b
03441+3207   DCH   3     HMW 72. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.527 mag, no periodicity found.  CHW2004 
03442+3207   STF 437     H 3  37.                                                                MEv2010 
03442-6448   LDS 104     bet Ret. A is a spectroscopic binary. B has separation of 1480". B is           
                         CPD-65@272.                                                                     
             bet Ret     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Jones (1928).                                                           Jon1928a
03443+3217   BU  535     38 Per = omi Per. Ellipsoidal and spectroscopic binary.                         
03443+3208   DCH   4     HMW 73. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 1.271 mag; multiple periods,              
                         average = 7.582d. Photometry may be contaminated by nearby star.        CHW2004 
03444+3210   DCH   5     HMW 10/78 = LLRL 10/45. Monitored for photometric variability                   
                         1998-2003  by Cohen et al. (2004). Range of variability dI = 0.030 mag          
                         for A component, 4.816 mag for B. No periodicity found for either               
                         component. Photometry of B may be contaminated by nearby companion.     CHW2004 
03444+3207   DCH   7     HMW 136. Monitored for photometric variability 1998-2003 by Cohen et            
                         al. (2004). Range of variability dI = 0.789 mag, no periodicity found.  CHW2004 
03444+3206   DCH   6     HMW 39. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.251 mag; multiple periods,              
                         average = 9.667d.                                                       CHW2004 
03444+2812   A  1826     Not seen on three nights 1964-1982.                                             
03444+1637   BPM  82     [PM2000]  139475 + [PM2000]  139465.                                    Gvr2010 
03445+3212   DCH   8     HMW 13 = LLRL 12. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.048 mag, no                    
                         periodicity found.                                                      CHW2004 
03445+3211   DCH  10     HMW 86. Monitored for photometric variability 1998-2003 by Cohen et             
                         al. (2004). Range of variability dI = 0.318 mag, no periodicity found.  CHW2004 
03445+3210   DCH   9     HMW 75 = LRLL 40. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.337 mag, nonperiodic.  CHW2004 
03445+3209   DCH  12     HMW 12 = LLRL 29. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.181 mag; multiple              
                         periods, average = 2.237d.                                              CHW2004 
03445+3208   DCH  13     HMW 42 = LRLL 86. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.097 mag; multiple              
                         periods, average = 6.532d.                                              CHW2004 
03445-1322   GAL 354     Object #99 in Gallo's original list.                                    Gal1912b
03446+3210   STF 439     AB,C: H 3  38.                                                          MEv2010 
             BU  880     AB: HMW 1 = LRLL 1. Monitored for photometric variability 1998-2003 by          
                         Cohen et al. (2004). Range of variability dI = 0.455 mag, no                    
                         periodicity found.                                                      CHW2004 
03446+3209   DCH  11     AB: HMW 27/28 = LLRL 16/33. Monitored for photometric variability               
                         1998-2003 by Cohen et al. (2004). Range of variability dI = 0.097 mag           
                         for A, 1.462 mag for B. Multiple periods seen for A, average = 2.656d.          
                         Photometry of B may be contaminated by nearby companion.                CHW2004 
03446+3209   HER  20     CD: HM 107 = LLRL 165. Monitored for photometric variability 1998-2003          
                         by Cohen et al. (2004). Range of variability dI = 0.328 mag, no                 
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03446+3208   HER   7     Additional notes may be found in Herbig (1962).                         Her1962 
03446+3207   DCH  14     HMW 11 = LRLL 6. Monitored for photometric variability 1998-2003 by             
                         Cohen et al. (2004). Range of variability dI = 0.094 mag; multiple              
                         periods, average = 1.687d.                                              CHW2004 
03446+2754   STTA 38     Optical with BU 1041BC, which is BD+27@558, at 03 44.7 +27 55.                  
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             BU 1041BC   The B component has both an astrometric and a spectroscopic orbit       Gln2007 
                         which are not associated with the optical BC pair.                      Grf2015c
03446-5416   HJ 3592     See claimed A was a close pair in 1897, but no trace of it was seen     See1898c
                         subsequently by van den Bos, Dawson, and Innes.                         Daw1918a
03447+3211   HER  21     HM 98 = LRLL 166. Monitored for photometric variability 1998-2003 by            
                         Cohen et al. (2004). Range of variability dI = 0.960 mag, no                    
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+3210   DCH  15     HMW 99 = LRLL 221. Monitored for photometric variability 1998-2003 by           
                         Cohen et al. (2004). Range of variability dI = 2.136 mag, no                    
                         periodicity found.                                                      CHW2004 
03447+3209   DCH  16     HMW 14 = LRLL 9. Monitored for photometric variability 1998-2003 by             
                         Cohen et al. (2004). Range of variability dI = 0.109 mag; multiple              
                         periods, average = 2.539d.                                              CHW2004 
03447+3208   DCH  17     HMW 111 = LLRL 52. Monitored for photometric variability 1998-2003 by           
                         Cohen et al. (2004). Range of variability dI = 0.187 mag, no                    
                         periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+2449   ITO   7     Pleiades HII 405.                                                               
03447+2414   LDS6103     A component is Pleiades star Melotte 22 HII 430.                                
03448+4602   BAG   8     Combined astrometric/spectroscopic solution by Balega et al. (2002),    Bag2002b
                         including determination of component masses.                                    
                         The Balega (2002) orbit predicts a separation of 0.055" in mid-2006,    Bag2002b
                         opening rapidly to 0".197 in late 2007. Perhaps T0 is not quite                 
                         correct?                                                                Hrt2009 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.54 +/- 0.13, 1.54, and 0.79 Msun, respectively.             Mlk2012 
03448+2417   HL    6     Primary is Pleiades star Celaeno = 16 Tau.                                      
03448-7002   LFR   1     SHY 450. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
03449+2407   HL    7     Primary is Pleiades star Electra = 17 Tau.                                      
03452+4235   ES 2601     nu Per = 41 Per                                                                 
03452+2450   HL    8     Primary is Pleiades star 18 Tau.                                                
03452+2428   HJ 3251     Primary is Pleiades star Taygeta = 19 Tau = 19 Pleiadum.                        
                         A is a spectroscopic and occultation binary.                                    
03454+2402   HL   10     Primary is Pleiades star.                                                       
03454-2752   BU 1003     A premature orbit has been computed. Motion direct and increasing as            
                         the pair closes in. However, there are no measures in the last twenty           
                         years.                                                                          
03457+2438   YAM   1     Pleiades cluster member. Primary is the BY Dra type variable V855 Tau.  Yam2013 
03457+0603   HJ 2204     29 Tau. A is a spectroscopic binary.                                            
03458+2422   HL   11     Primary is Pleiades star Maia = 20 Tau.                                         
03458+2309   STF 444     Spectroscopic binary, P = 7.15d.                                                
03459+2433   HL   12     Primary is Pleiades star Asterope = 21 Tau.                                     
03459+2402   HL   13     Primary is Pleiades star.                                                       
03460+7302   MLR 457     Same as HDS 476.                                                                
03460+2432   HL   14     Primary is Pleiades star 22 Tau.                                                
03460+1721   BPM  83     [PM2000]  140561 + [PM2000]  140577.                                    Gvr2010 
03461-1522   GWP 508     ABL 163.                                                                Tob2012b
03461-1708   GWP 507     ABL 162.                                                                Tob2012b
03461-6405   HJ 3600     B is CPD-64@271.                                                                
03462+2434   POU 309     LDS6108.                                                                        
                         Both components are Pleiades variables. A = Melotte 22 HII 879 = V813           
                         Tau, while B = Melotte 22 HII 883 = V789 Tau.                                   
03462+1710   HJ 3252     This star has a possible wide companion at about 8" as noted in the             
                         WDS. It is however single in the separation range covered by the                
                         AstraLux data.                                                          Jnn2012 
03463+2411   BU  536     In the Pleiades. The motion so far is retrograde and rectilinear.       Hzg1958 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Both elliptical orbit and rectilinear trajectory were calculated by             
                         Popovic & Pavlovic (1995). See also rectilinear catalog.                Pop1995d
03463+2357   HL   15     Primary is Pleiades star 23 Tau.                                                
03463-1235   GAL 355     Object #103 in Gallo's original list.                                   Gal1912b
03464+7523   STF 418     Same as PRZ   4. Coordinates of PRZ   4 correct and retained.                   
03464+2435   ITO   8     AB: Pleiades HII 996.  Primary is the BY Dra-type variable V1045 Tau.   Ito2011 
             LDS6110     AC: Possibly common with LDS6108.                                               
03464+1143   LEP 119     LHS 1589 = NLTT 11793. Lepine et al. determine a photometric distance   Lep2007b
                         of 81 +/- 18 pc; masses are estimated at 0.25 and 0.20 Msun.                    
03465+2508   ITO   9     Pleiades HII 1015.                                                              
03465+2426   ITO  10     Pleiades HII 1032.  Primary is V1171 Tau. Both companions are                   
                         background stars.                                                       Yam2013 
03465+2415   CHR  12     Pleiades cluster member.                                                        
                         1985.8488: This measure is from reanalysis of archival data.  Not               
                         listed as an SB by Abt et al. (1965), but it may show measurable        AbH1965b
                         velocity variation at some phases of a possibly eccentric orbit.        Msn1993b
                         Aa,Ab: Observed 20 times 1982-1998 and resolved 4 times 1983-1989,              
                         with separations decreasing from 0.236" to 0.160". Motion indicates a           
                         ~40-year period orbit.                                                  Hrt2009 
03466+2950   BRT 233     MLB 683.                                                                        
03466+2458   MET  34     Pleiades cluster member. The companion is a background star.            Yam2013 
03466+2255   RDR   2     Primary is an F6 Pleiades member (HII 1132). Based on common motion             
                         over 4 years, Rodriguez et al. (2012) conclude the B component is               
                         either a companion to the primary or (less likely) a nearby comoving            
                         Pleiades member. Assuming they comprise a physical pair, the companion          
                         is a brown dwarf, with mass estimated at 0.06 +/- 0.01 Msun,                    
                         temperature 2600 +/- 100K.                                              Rdr2012b
03467+2402   LDS6111     A component is a Pleiades variable = Melotte 22 HII 1124 = V814 Tau.            
03467-1231   GAL 356     Object #104 in Gallo's original list.                                   Gal1912b
03470+4126   STF 443     HIP 17666. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 11792/11791                                                    Chm2004 
                         Proper motion of A +596 -1249. Proper motion of B +594-1259. B is a             
                         single-lined spectroscopic binary, P = 48.65d. A common proper motion           
                         companion, G095-059, mag. 13.4, lies more than 2 degrees away.                  
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AB: HJL  53.                                                            HJL1986 
03470+2431   CHR 124     Occultation binary. Has variable radial velocity. Pleiad.                       
03471+2449   BU  537     Variable, V534 Tau.                                                             
03473+2424   BOV  18     Geissler et al (2012) conclude companion is an M8 brown dwarf, the              
                         first substellar companion discovered around a Pleiades star.  Mass             
                         estimates range from 0.052 to 0.063 Msun, depending on distance, etc.   Gei2012 
                         Pleiades cluster member. The companion shares common proper motion.     Yam2013 
03473+2348   HL   18     Primary is Pleiades star.                                                       
03473+2344   HL   19     Primary is Pleiades star.                                                       
             BOV  17     CF: 03471+2343BOV  17 = HL  19C, system merged.                                 
03474+2435   HL   20     Primary is Pleiades star.                                                       
03474+2355   STF 450     POU 311. Primary is Pleiades star.                                              
03474+2255   HD 23610    Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                         Cluster Melotte 22 #1407.                                                       
03475+2417   HL   22     Primary is Pleiades star.                                                       
03475+2406   STFA  8     Primary is Pleiades star Alcyone = 25 Tau = eta Tau = V647 Tau.                 
                         STTA 42.                                                                        
                         A is an occultation and spectroscopic binary.                                   
                         B, at 03 47.4 +24 07, is an occultation binary.                                 
                         C is V647 Tau.                                                                  
                         BC: HJL1029.                                                            HJL1986 
                         BD: HJL1028.                                                            HJL1986 
                         CD: HJL1027.                                                            HJL1986 
03476+2337   HL   24     Primary is Pleiades star.                                                       
03478+3501   ES  235     Primary is eclipsing binary of Algol type, period 1.92873d.             Zas2014 
03478+3212   HR 1164     Orbit determined by fitting revised Hipparcos intermediate astrometric          
                         data. Derived component masses 1.44 +/- 0.09 and 1.15 +/- 0.08 Msun.    Ren2010 
03479+3336   STF 448     HJ 5457. A is a spectroscopic binary. Also, one component is variable.          
03479+2555   BRT2520     Heintz finds no pair in the field, and believes identity with J 27      Hei1985a
                         (03470+2855) is possible.                                                       
03479+2407   BU  538     AB. Identification of a 2000.8 measure by Lampens et al. (2007)         Lmp2007 
                         originally attributed to 03481+2409 COU  80 was corrected by the                
                         author; it actually was of this pair.                                           
03480+6840   KUI  13     See discussion by van de Kamp & Chao-Yuan Yang.                         Kam1967 
             WNO  16     AD: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
03480+4032   TOK 240     Primary is an exoplanet host, P=1565d                                   Tok2014d
03480-7048   HJ 3606     B is CPD-71@223.                                                                
03481+2409   COU  80     Pleiad.                                                                         
                         Identification of a 2000.8 measure by Lampens et al. (2007) originally  Lmp2007 
                         attributed to this pair was corrected by the author; it actually was            
                         of 03479+2407 BU  538AB.                                                        
03482+2419   CHR 155     Included in the Pleiades cluster survey of Abt et al. (1965), who did   AbH1965b
                         not detect variable RV. Pearce & Hill (1975 Pub DAO, 14, 319) did               
                         notice velocity variation at the 1% level, and Liu et al. (1997) found  Liu1997 
                         the system to be a SB2, although large velocity difference may imply a          
                         closer companion than this.                                             Msn1993b
03482+2219   EQ Tau      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                         estimate the mass of the contact pair at 1.752 Msun and the minimum             
                         mass of the wider component at 0.49 Msun.                                       
03483+2325   HL   25     Pleiades H 722. Primary was misidentified as SAO 76125 in the first             
                         speckle catalogue.                                                      McA1984b
03483+1109   STF 452     30 Tau.                                                                         
                         H 3  66.                                                                MEv2010 
03483-0943   GWP 517     ABL 164.                                                                Tob2012b
03484+5202   HU  546     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.17 +/- 0.43, 1.53, and 1.20 Msun, respectively.             Mlk2012 
03486+3039   SHY 453     HIP  17796 + HIP  18204.                                                        
03486-3737   DUN  16     f Eri. One component is a possible Beta Lyrae-type system.                      
03489+6445   STT  62     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.82 +/- 0.52, 2.75, and 1.20 Msun, respectively.             Mlk2012 
03489+2351   HL   27     Primary is Pleiades star 26 Tau.                                                
03490+5120   LDS9160     Old LDS6160. NLTT 11871/11873.                                                  
03491+4358   V376 Per    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03492+3651   J  2721     BRT 2586. ALI 288.                                                              
03492+2408   CHR 125     Aa,Ab: Pleione, 28 Tau = BU Tau. Shell star and suspected long-period           
                         spectroscopic binary (Hoffleit 1982) . Pleiades cluster member.         Hof1982 
                         Frequently unresolved, probably due to large Delta m.                   Msn1993b
                         For their measure, Roberts et al. reports that the "The close                   
                         proximity of the two star's PSFs prevented accurate measurement of the          
                         astrometry and photometry."                                             Rbr2007 
                         Aa,Ab: Observed 3 times 1987-1991 (all observations noted as weak),     Rbr2007 
                         then unresolved until a 2002 (0.24") measure at 900nm                   Hrt2009 
             RBR   4     AF: 2002.0924: PA is measured in zenith mode. If data collected in              
                         equatorial mode, PA = 119. Confirmation of the pair should establish            
                         the correct value for theta.                                            Rbr2007 
03492+2403   STF 453     Primary is Pleiades star Atlas = 27 Tau = Melotte 22 #2168                      
                         Position angles scattered. Distances range from "single" to 0.6". Some          
                         question duplicity. A is a long-period spectroscopic binary.                    
             MKT  12     Aa1,Aa2: Hipparcos astrometric solution assumed circular orbit (e =             
                         omega = 0).                                                             HIP1997d
                         Pan et al. (2004) orbit is based on Mark III and PTI measures. A        PTI2004 
                         distance to the Pleiades of 135 +/- 2 pc is determined. Masses for the          
                         components are calculated as 4.90 +/- 0.28 and 3.65 +/- 0.08 Msun.              
                         Zwahlen et al. (2004) orbit is based on published Mark III and PTI      Zwa2004 
                         measures, plus additional Mark III and NPOI astrometric data and                
                         ELODIE echelle spectra. This combined spectroscopic/interferometric             
                         solution yields masses of 4.74 +/- 0.25 and 3.42 +/- 0.25 Msun; the             
                         distance 132 +/- 4 pc found agrees with "traditional" Pleiades                  
                         distances obtained through MS fitting techniques.                               
                         Aa1,Aa2: Malkov et al. (2012) derive dynamical, photometric, and                
                         spectroscopic masses 5.68 +/- 0.79, 6.68, and 3.31 Msun, respectively.  Mlk2012 
03493+5707   S   436     STTA 39. B is BD+56@847.                                                        
                         HJL1030.                                                                HJL1986 
03493-1656   GWP 519     ABL 165.                                                                Tob2012b
03494+5214   ES  770     B is BD+51@781.                                                                 
03494+2423   STTA 40     AB: LDS6116. B is BD+23@560. A is Pleiades star and occultation double          
             HL   30     BC: Primary is Pleiades star.  Also known as STU   2BC.                         
             HL   30     BD: Also known as STU   2BD.                                                    
03495+5239   STF 446     Also known as STF 454. Another classification: B0Ib. The primary is             
                         slightly variable; the system is a member of the cluster NGC 1444.1             
03495+1255   AG   74     Primary is V1128 Tau, a 10th magnitude W UMa type eclipsing binary,             
                         with period 0.3053725d.                                                 Zas2011 
03496+6318   CAR   1     Also known as MOAI 1.                                                           
                         1995.948: Theta corrected from published value of 213 deg (Aristidi,            
                         private communication)                                                          
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.76 +/- 0.61, 3.36, and 1.82 Msun, respectively.             Mlk2012 
03496+3859   HU 1067     A RW Aur-type variable, XY Per. Both components may vary.                       
                         dm estimates on a number of nights. quadrant reversed on 1936 Jan 17,           
                         indicating primary is responsible for variation. Beyer (AN 263, 71,             
                         1937) established the irregular character of the variation.             VBs1954 
03496-0220   YR   23     Triple. The RV amplitude of 9.5 km s-1 and double lines seen in GCS             
                         cannot be caused by the visual system YR 23 with estimated period of            
                         ~50 yr which could however be responsible for dmu.                      Tok2012a
03497+2343   HL   32     Primary is Pleiades star.                                                       
03497+2320   YAM   2     BC: Pleiades cluster member. The companion is a background star.        Yam2013 
                         Pair initially 03495+2323 YAM 2; merged with 03497+2320 LDS6118.                
03498+2421   HL   33     Primary is Pleiades star.                                                       
03498+2342   ITO  11     Pleiades HII 2462.                                                              
03499+2313   ITO  12     Pleiades HII 2506.                                                              
             YAM   3     Pleiades cluster member. The companion is probably a background star.   Yam2013 
03500+2351   STT  64     A is a spectroscopic binary, P = 16.72d, spectrum B9.5VpSiSrCr. Pleiad          
03501+4458   CHR 126     A spectroscopic binary.                                                         
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         P'edoussaut et al. (1987).                                              Ped1987 
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Pedoussaut et al. (1987).                                               Ped1987 
03501+0637   TOK  80     HIP 17936. The magnitude difference in the 2MASS PSC dK=1.8 is                  
                         suspect (5" separation), dK=3.4 is measured with ANDICAM.               Tok2011a
03502-1335   FAR  32     NLTT 11972. Primary is white dwarf WD 0347-137.                         Far2006 
03503+2535   STT  65     One star variable?                                                      Wor1967b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.15 +/- 0.39, 3.39, and 3.91 Msun, respectively.             Mlk2012 
03503-0131   SHY 164     AE: HIP  17950 + HIP  16933. E component = A component of 03503-0131.           
                         AB: Hipparcos identified the pair as a candidate for Hyades membership. HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
03504+7120   HJ 2200     gam Cam                                                                         
03505-1219   GAL 357     Object #105 in Gallo's original list.                                   Gal1912b
03506+2431   YAM   4     Pleiades cluster member. Primary is V1174 Tau.                          Yam2013 
03506-4234   EGN   3     Pair bound, with projected separation 73AU. Mass of secondary                   
                         0.15 +/- 0.01 Msun; spectral type M4-M6.                                Egn2007 
03507-1206   GAL 358     Object #106 in Gallo's original list.                                   Gal1912b
03508+4546   FMR  63     Typographical error in initial WDS designation (03508+4946)                     
03510+1414   JLM   1     Erroneously labelled as JML 1; changed upon request of discoverer.              
03511+3548   BRT3238     ALI 51.                                                                         
03511+1551   BPM  84     [PM2000]  144054 + [PM2000]  144088.                                    Gvr2010 
03513+2621   A  1830     The few observations do not define the nature of the motion.                    
03514+2538   HEI   9     Primary is eclipsing binary of Algol-type, period 1.26292 d.            Zas2012 
03514-1610   GWP 523     ABL 166.                                                                Tob2012b
03517+7030   HJ 1139     B is BD+70@263.                                                                 
03517+2433   LDS5437     A component is a Pleiades variable = Melotte 22 HII 3096 = V1054 Tau.           
                         B component is flare star V383 Tau.                                             
03518+3453   ARN  58     Also known as GRV 196.                                                          
03518-0306   GWP 524     ABL 167.                                                                Tob2012b
03520+2440   BOV  27     AB: Assuming a Pleiades parallax of 7.43 +/- 0.17 mas (distance 134.6           
                         pc; Soderblom et al. 2005, AJ 129, 161), Schaefer et al. (2014) find a          
                         total mass of 1.42 +/- 0.10 Msun. The revised Hipparcos parallax of             
                         8.32 +/- 0.13 (120.2 pc; van Leeuwen 2009, A&A 497, 209) gives a total          
                         mass of 1.01 +/- 0.05 Msun, which is not consistent with the                    
                         corresponding photometric masses of the components.                     Sfr2014 
03520+0632   KUI  15     31 Tau.                                                                         
                         AB: Additional notes may be found in Van Biesbroeck (1954) and          VBs1954 
                         Couteau (1955).                                                         Cou1955c
03525+3546   ES 2334     BRT 3239. ALI 52.                                                               
03525-0403   GWP 525     ABL 168.                                                                Tob2012b
03526-0829   RST4762     The few measures do not define the motion.                                      
03527-0522   HJ  338     30 Eri.                                                                         
03529+3532   ES 2459     BRT 3240.                                                                       
03529-0633   GWP 528     ABL 169.                                                                Tob2012b
03530+1158   BPM  85     [PM2000]  145369 + [PM2000]  145423.                                    Gvr2010 
03530-1332   GWP 529     ABL 170.                                                                Tob2012b
03534+1743   BPM  86     [PM2000]  145657 + [PM2000]  145663.                                    Gvr2010 
03535+3538   ES 2460     Identical to ALI 54 and BRT 3237                                        Hei1983a
03535-1229   GAL 359     Object #107 in Gallo's original list.                                   Gal1912b
03535-1440   GWP 531     ABL 171.                                                                Tob2012b
03536+2718   OCC9003     The OCC2010 solution is ambiguous and one is arbitrarily "T" coded              
                         until the true solution is determined.                                          
03536+2146   OL  184     TDS2678. Appears to be the same as 03549+2148 OL  200. IDS notes that           
                         OL  200 is possibly identical to 03559+2146 HU  815, but they appear            
                         to be different pairs.                                                          
03537+5316   A  1293     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.00 +/- 0.24, 1.94, and 1.05 Msun, respectively.             Mlk2012 
03539-1751   GWP 532     ABL 172.                                                                Tob2012b
03541+3153   STF 464     zet Per = 44 Per. A is a spectroscopic binary.                                  
                         AD: H 6  96.                                                            MEv2010 
03543-0257   STF 470     32 Eri. A is a spectroscopic binary.                                            
                         AB: H 2  36.                                                            MEv2010 
03544+0116   TOK  81     RoboAO finds a companion to B (233deg, 3.05", dI=5.88mag), but it is            
                         thought to be optical.                                                  Tok2014d
03544-0649   A   461     Less than 0.1" in 1954 - 1961. It appears that a revolution has been            
                         completed.                                                                      
03544-4021   FIN 344     Spectroscopic binary.                                                           
                         1989.9438: This is the first observation of this system since those of          
                         Finsen in the 1960's, and is considerably closer than any of his                
                         results.  It is known that in some instances Finsen's rho values                
                         appeared systematically larger than those of speckle; further                   
                         observations of this system will determine whether such is again the            
                         case.                                                                   Hrt1993 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.24 +/- 0.59, 4.58, and 4.88 Msun, respectively.  Mlk2012 
03545+3203   LEI   6     Member of Taurus-Auriga molecular cloud.                                Dae2015 
03545+0510   STTA 41     A is a Delta Scuti-type variable, V479 Tau. B is BD+04@@600.                    
                         A,BC(60") is probably physical.                                                 
             A  1831     BC: Less than 0.1" in 1954 - 1955 with 82-inch.                                 
                         A premature orbit has been computed. Motion direct.                             
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03546+2507   HAT   1     30' error in WDS designation.                                                   
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
03546+2131   LDS1149     Old LDS6161. LDS9161.                                                           
03547+5200   TOR   5     Formerly known as PAN   2.                                                      
03547+1529   BPM  87     [PM2000]  146665 + [PM2000]  146678.                                    Gvr2010 
03547-1811   GWP 533     ABL 173.                                                                Tob2012b
03548-3542   TOK  82     HIP 18305. NOMAD: PM(B)=(-89,+19), V=11.48(??).                                 
                         PM(A)=(+108,+218).                                                      Tok2011a
03549-1426   GAL 360     Object #109 in Gallo's original list.                                   Gal1912b
03553-0237   BRT1928     BAL 25.                                                                         
03553-1921   GWP 534     ABL 174.                                                                Tob2012b
03554+3103   HO  325     A is a RW Aur-type variable, X Per, and also a long-period                      
                         spectroscopic binary.                                                           
03557-2236   I   722     CD-22@1398.                                                                     
03558+5225   TOR   6     Formerly known as PAN   3.                                                      
03558+5224   STF 462     HJ 2206.                                                                        
03561-4509   CPO 121     LDS 108.                                                                        
03561-4746   HU 1361     HIP 18402. B is definitely physical, but it is too red in the                   
                         (Kabs,V-K) CMD. Infrared companion? Nothing on B in SIMBAD.             Tok2011a
03562+5939   ENG  16     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             HDS 497     AD: CfA: P=12625d=34.6y? Abt & Willmarth (2006): RV=-22.18 const.       AbH2006 
03563-1935   GWP 535     ABL 175.                                                                Tob2012b
03564+4404   LDS5186     NLTT 12174/12173                                                        Chm2004 
03565-3642   BAS   2     This is the X Ray source EUVE J0356-36.6.                                       
03566+5042   S   440     43 Per. A is a spectroscopic binary. B is BD+50@861.                            
                         AB: H 5  41.                                                            MEv2010 
03571-0828   RST4764     Rapid retrograde motion.                                                        
03572-0706   OSW   7     Typographical error in WDS - initially entered as 03572-0025, with dec          
                         portion copied from OSW 8.                                                      
03573-1054   GWP 536     ABL 176.                                                                Tob2012b
03575-0110   BU  543     A premature orbit has been computed. A is a flare suspect.                      
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         NLTT 12237/12236                                                        Chm2004 
03576+5712   ES 1820     Doubtful this system is physically bound, since relative motion is              
                         larger than pm of A.                                                    Kiy2012 
03578+4932   KU   82     B is BD+49@1068.                                                                
03579+4001   STF 471     eps Per = 45 Per. A is a Beta Lyrae-type binary.                                
                         AB: H 2  22.                                                            MEv2010 
03580-1331   HJ 3608     gam Eri = 34 Eri = Zaurak. Variable?                                            
                         The faint pair, presumeably the original system, was recovered in       Dal2009 
                         2009, which appears to have common proper motion. All subsequent                
                         measures of the HJ 3608 were of a more distant pair with linear                 
                         motion relative to the primary, presumeably optical.                            
03583+2757   ARG  58     AG 75.                                                                          
03583-1659   GWP 537     ABL 177.                                                                Tob2012b
03584+2538   LDS5459     Also known as LDS9162.                                                          
                         NLTT 12251/12250                                                        Chm2004 
03586-0239   BU 1042     B is BD-03@651.                                                                 
03587+1646   LDS5462     GWP 538. Luyten's original 1960 measure listed theta = 144deg, 90deg    Luy1984 
                         different from the angle found by Bernal. Agreement on coordinates,     ABl2012a
                         separation, and magnitude difference led to the conclusion Luyten made          
                         a trigonometry error in his reduction.                                          
03590+3547   TRN  16     The image rotator was in an unknown state, so two possible theta                
                         values are listed for the 2001.7342 observation - one for zenith up             
                         and one for north up.                                                   Trn2008 
03590+0947   HU   27     The value of omega for Ling's (2001) orbit was incorrectly given as     Lin2001b
                         263.1 in IAU Inf. Circ. 144.                                                    
                         Ling (2004) derived an orbital parallax 0".01239 and a mass sum of      Lin2004a
                         1.94 +/- 0.82 Msun.                                                             
03590-0056   HEI 215     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
03591-0656   LDS3545     NLTT 12296/12294                                                        Chm2004 
03591-2312   FAR   3     FAR  33. Primary is white dwarf WD 0357-233.                            Far2005b
03592+8020   JNN  27     A companion to 2MASS J03591438+8020019 was detected on two separate             
                         occasions with AstraLux, in both cases the detection is rather                  
                         tentative, but since it is detected twice with consistent properties            
                         we count it as a genuine detection. However, due to the poor quality            
                         of the fit and the fact that the two epochs of observation are only             
                         separated by 3 months, we do not try to acquire two epochs of                   
                         astrometry, but merely quote the astrometry as the mean (and standard           
                         deviation) of the two epochs.                                           Jnn2012 
03596-1019   HU   29     Motion in a highly-inclined orbit.                                              
03597+4809   STT  68     A is an Algol-type binary, IQ Per. B is BD+47@921.                              
03597-1147   GWP 540     ABL 178.                                                                Tob2012b
03597-1301   GAL 361     Object #110 in Gallo's original list.                                   Gal1912b
03598+1133   STF 478     LDS5464.                                                                        
03599+1325   LDS1150     Aka LDS5465.                                                                    
04005+1935   KOH   1     Metchev & Hillenbrand say pair probably physical, based on proximity.   Met2004b
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04005-4145   DON  58     B is above the MS in (V,V-K). Tuc-Hor moving group? (Kiss et al., 2011          
                         MNRAS 411, 117)                                                         Tok2014d
04005-5120   TOK  83     HIP 18713. NOMAD: PM(B)=(+44,+43). PM(A)=(+162,-39).                    Tok2011a
04007+2023   BD+19  641  Hyades vB 9                                                                     
                         SB with P > 7 yr according to Griffin et al. (1988).                    Grf1988 
04008+1812   BUP  49     A is a spectroscopic binary. B is BD+17@664.                                    
04008+0505   A  1937     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.32 +/- 1.76, 2.84, and 2.00 Msun, respectively.             Mlk2012 
04009+2312   STF 479     H N 93.                                                                         
04009-1027   STF 487     B is BD-10@814.                                                                 
04021-3429   BU 1004     HIP 18824. See Allen et al. (2000) for information on metallicity,      AlC2000 
             LDS3551     age, galactic orbital parameters, etc.                                          
             BU 1004     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             LDS3551     AD: Holberg et al. (2013): D at 64" is CPM, WD(DA9.9)                   Hbg2013 
04022+2808   STF 481     AD: Declination difference 11.18".                                              
                         AD: Component D is 04039+2808VBS   9.                                           
04024-2832   DAW  79     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.29 +/- 0.72, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04025+0638   HDS 510     Cvetkovic et al. (2016) estimate spectral types K2 and K3, masses 0.81          
                         and 0.79 Msun. Dynamical parallax is 13.24 +/- 0.28 mas.                Cve2016b
04025-6121   LDS 109     Jenkins et al. (2010 A&A 515, 17): RV(A) var with P>6.5yr, M2min=66     CPS2002b
                         Mjup. However, Jones et al. (2002) do not detect RV variation.          Tok2014d
04029+1228   BPM  88     [PM2000]  152895 + [PM2000]  152883.                                    Gvr2010 
04031-1149   GAL 362     Object #113a in Gallo's original list.                                  Gal1912b
04032+2553   DCH  45     HBC 356/357 = V1067 Tau.                                                        
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04033+3516   OSO  16     Not a common proper motion pair, based on comparison with POSS2 red             
                         plates. PM of A = +1732 -1356.                                          Oso2004 
04033+1820   BPM  89     [PM2000]  153212 + [PM2000]  153228.                                    Gvr2010 
04036-3611   WHI   5     Listed as possibly resolved by White et al. (1991).                     Whi1991 
04037-1545   A  2913     1989.9413: This system closed steadily from its discovery at 0".45 in           
                         1915 to 0".22 in 1959; this is the first observation in 30 years so it          
                         is unknown whether the pair has passed through periastron.              Hrt1993 
04038+3758   ES 2085     A is V380 Per.                                                                  
04038-4429   LCL 120     AB: B is CD-44@1388.                                                            
                         AB: Additional notes may be found in Herschel (1847).                   HJ_1847a
             SHY 458     AC: HIP  18958 + HIP  18888.                                                    
04039+2808   VBS   9     An Algol-type binary, RW Tau.                                                   
                         This is the D component of 04022+2808.                                          
04040+3932   L    51     Not found in Heintz at IDS position.                                    Hei1987a
04042+2324   OSO  17     Not a common proper motion pair, based on comparison with POSS2 red             
                         plates                                                                  Oso2004 
04043-1231   GAL 363     Object #116 in Gallo's original list.                                   Gal1912b
04044+2406   MCA  13     36 Tau. A is an occultation binary, first detected by Dunham et al.     Dnh1973 
                         Now resolved by speckle interferometry.                                         
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 16.02 +/- 8.21, 11.83, 2.92 Msun, respectively.    Mlk2012 
04044+2025   RED   1     1996.0656: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981)                                         Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04045+1512   BPM  90     [PM2000]  154069 + [PM2000]  154068.                                    Gvr2010 
04046+5504   HO  221     Both A and B are above the MS. AC: reflex PM(A), likely optical.        Tok2014d
04047+2205   STT 558     AB: 37 Tau.                                                                     
04047-0303   LDS3555     NLTT 12486/12488                                                        Chm2004 
04049-3527   CHR 224     AC. Surprisingly, no record of this wide companion to the 0".8 pair             
                         I 152 is listed in the WDS, despite 17 observations spanning 90+ years          
                         since Innes' discovery in 1896.  Misidentification appears ruled out,   I__1897b
                         since both the Innes pair and the new component are seen on two                 
                         separate occasions.                                                     Hrt1996b
04050+3705   KU   83     AB: HJL  55.                                                            HJL1986 
04050-0600   BFR   4     BD-06 813 + 2MASS J04050209-0600409. Baron et al. (2015) estimate               
                         spectral types K0 and M6.5 +/- 1, distances 68 +/-10 and 86 +2/-37 pc,          
                         masses 0.925-1.014 and 0.096-0.114 Msun.                                BFr2015 
04053+2201   CHR 158     Aa,Ab: 39 Tau. Variable?                                                        
                         Aa,Ab: Observed 7 times 1985-1998, then resolved at 0.22" in 1988       McA1993 
                         (note: "uncertain"), unresolved in 2002 (3.6m AO), and finally          Rbr2005 
                         resolved at 0".41 in late 2003                                          Hrt2009 
04056+1255   BPM  91     [PM2000]  154891 + [PM2000]  154924.                                    Gvr2010 
04057+2248   COU 151     Metchev & Hillenbrand say the AB pair is probably physical, based on            
                         proximity.                                                              Met2004b
04058+7117   LDS1589     NLTT 12426/12424                                                        Chm2004 
04059+3438   ES  238     A measure in 1946 gives distance as 7.2".                                       
04063+3548   BRT3241     ALI 57.                                                                         
04063+1952   BAG   4     A preliminary circular orbit is determined                              Bag2001 
04064+4325   A  1710     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.73, 2.49, and 0.95 Msun, respectively.             Mlk2012 
04065+1422   S   443     B is BD+13@643.                                                                 
04066+2018   BNV   2     V1300 Tau. DAE 17. Member of Taurus-Auriga molecular cloud.             Dae2015 
                         Primary is F8-G1, mass = 1.14 +/- 0.05 Msun, age = 25 +25/-10 Myr,              
                         Teff = 5970-6100K. Secondary is M8-L1, mass = 32 +18/-14 Mjup,                  
                         Teff = 2537 +95/-182K.                                                  Bnv2014 
04066-6019   R    40     B is CPD-60@292. Spectral type of B may be G8.                                  
04067+1309   BPM  92     [PM2000]  155660 + [PM2000]  155680.                                    Gvr2010 
04067+0324   HJ 2221     A component: V = 11.8; B-V = +0.9; Spectral type: K-M.                          
                         B component: V = 13.5; B-V = +0.8; Spectral type: M                     FMR2000a
04068+5035   HU  547     Variable of unknown type.                                                       
04069+3327   STT  71     A is an Algol-type eclipsing binary, AG Per, P = 2.03d.                         
04070-1000   SHY 165     AB: HIP  19206 + HIP  21489.                                                    
             HDS 521     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 1.68 +/- 0.48, 2.13, and 1.96 Msun, respectively.  Mlk2012 
04070-2200   HU 1363     1994.8069: Quadrant determined by speckle imaging analysis.             Hor1996 
04072+2731   TOK 241     Makarov & Kaplan (2005) note as astrometric companion to A, but there   Mkr2005 
                         is RV data for A to support this astrometric sub-system.                Tok2014d
04075-5234   TOK  15     Astrometric binary in Hipparcos catalog. Estimated period of visual             
                         pair 6y. Primary is 2.5d SB1. G-solution in HIPPARCOS.                  Tok2006 
                         Triple system, consisting of 2.5d SB and 0".1 tertiary companion                
                         discovered by Tokovinin (2006) and previously revealed by Hipparcos     Tok2006 
                         acceleration and RV trend. It is not resolved here; apparently it               
                         closed in.                                                              Tok2013b
04076+3804   STT 531     A: V491 Per. CPM with BD+37@882 (50 Per), 12' distant.                  Cou1955c
                         Premature orbits have been calculated. Motion retrograde.                       
                         G039-001. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
             ALC   1     AE: Also known as BU  545CA.                                                    
                         AE: SHY  19. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         E: 50 Per = V582 Per.                                                           
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04077+1510   STF 495     A is a Delta Scuti-type variable. A = Hyades vB 11, B = Hyades vB 12.           
                         AB pair, with rho = 3".8 is outside our detection window.               Msn1993a
04077+1413   LDS5187     old LDS6164.                                                                    
04078+6220   ES 2603     SZ Cam                                                                          
             STF 485     The classification is from Chocol (1980 Bull. Astron. Inst. Czech. 31,          
             CHR 209     321).  The discovery of speckle companion CHR 209 Ea,Eb with a period           
             WSI  20     of some 60 y confirms the third body model advocated by  Mayer et al.           
             HZG   2     (1994 A&A 288, L13) based on the appearance of the spectrum and                 
             HLM   3     variations in the time of light curve minimum (they suggest a third             
                         body period of 50.7 y).  Another light curve solution is given by               
                         Harries et al. (1998 MNRAS 295, 386).  The B component was also                 
                         observed and appeared to be single. Classification of the B component           
                         is from the WDS.                                                        Msn1998a
                         This complex multiple system has had numerous identification errors             
                         due to various difficulties. The diagram of Lewis in his catalog of     L__1906b
                         the Struve pairs, which seemed a good first step, was hampered by the           
                         quadrant error of the pair he designated Ca. This quadrant error was            
                         repeated in the ADS, IDS, and in earlier editions of the WDS. In the            
                         ADS (where this pair is listed as #2984, but note that #2989 is part            
                         of this system, too) the errors multiplied. The pair Holmes AF (WDS             
                         designation HLM   3AF) is apparently the same as STF 485Ac. Inspection          
                         of scanned images of this region of the sky have allowed the                    
                         Hertzsprung pairs (HZG   2) whose components are given within                   
                         quotation marks in the ADS to be identified. Of the HZG pairs, the              
                         "CD" pairing is the same as STF 484AC and the "CE" pairing is the               
                         same as STF 484AB. The ADS note to the "AJ" pairing of HZG   2 is a             
                         typographical error. The correct position angle is 77 degrees, which            
                         corresponds to the AD (now AO) pair. Below outlines the changes from            
                         the WDS 2001.0 to the current version.                                          
                                                                                                         
                         ES 2603Aa ---> ES 2603AB                                                        
                         STF 485Ab ---> STF 485AC                                                        
                         STF 485Ac ---> STF 485AD                                                        
                         STF 485AB ---> STF 485AE                                                        
                         STF 485BE ---> STF 485EF                                                        
                         STF 485   ---> STF 485EG (formerly STF 485B to STF 484A)                        
                         STF 484AB ---> STF 484GH                                                        
                         STF 484AC ---> STF 484GI                                                        
                         STF 485Bb ---> STF 485EC                                                        
                         HLM   3AF ---> STF 485AD                                                        
                         STF 485AD ---> STF 485AO                                                        
                         STF 485   ---> STF 485AL (formerly STF 485A to HLM   3A)                        
                         HLM   3AB ---> HLM   3LM                                                        
                         HZG   2AC ---> STF 484AI                                                        
                         HZG   2AD ---> STF 484AG                                                        
                         HZG   2AE ---> STF 484AH                                                        
                         HZG   2AG ---> HZG   2AN                                                        
                         HZG   2BC ---> STF 484EI                                                        
                         HZG   2BE ---> STF 484EH                                                        
                         HZG   2CD ---> STF 484GI                                                        
                         HZG   2CE ---> STF 484HI                                                        
                         HZG   2JK ---> HZG   2OP                                                        
                         HZG   2   ---> HZG   2JK                                                        
                         SLV   3   ---> STF 485AF                                                        
                         CHR 209Ba ---> CHR 209Ea,Eb                                                     
             CHR 209     Ea,Eb: The primary of this pair is the Beta Lyrae-type O9/B0 eclipsing          
                         system SZ Cam, with a period of 2.698d. The Gorda et al. (2007) orbit   Grd2007a
                         is based on changes in the period of SZ Cam to determine P, omega, e,   Grd2007b
                         and T, and speckle measures to derive i, Omega, and a. They derive a            
                         distance of 1125 +/- 135 pc, which exceeds by 30% the 800pc distance            
                         to the open cluster NGC 1502; they conclude that SZ Cam is not a                
                         member of the cluster. The mass of the eclipsing pair (Ea) is 28.5              
                         +/- 0.5 Msun, that of the third body (Eb) 23.4 +/- 2.4 Msun.                    
                         Eb is also a close binary.                                                      
             STF 484     GH: STI 492.                                                                    
04079+1750   DAE  18     V1302 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04080+4311   AG  308     B is BD+42@897.                                                                 
04080+0119   HJ 2223     BAL 1262.                                                                       
04082+1957   DAE  19     V1196 Tau.                                                              Dae2015 
04083+1327   BPM  93     [PM2000]  156773 + [PM2000]  156823.                                    Gvr2010 
04087+2553   OCC 777     Griffin (2013) notes that the magnitude and parallax of this pair               
                         suggest a star of luminosity class III, rather than the published               
                         spectral type of G8II. He derived a spectroscopic orbit of P=2224.4             
                         +/- 2.3 days, e=0.477 +/- 0.009.                                        Grf2013g
04088+1126   LDS5188     LDS5508.                                                                        
04089+2911   BU 1232     Only elements P, T, and a in the Starikova (1980) orbit have been       Sta1980b
                         amended from the orbit of Muller (1978).                                Mlr1978a
                         Griffin et al. (1988) find this to be a SB but doubt its                Grf1988 
                         membership in the Hyades in spite of its inclusion by                   Sym1965 
                         Wayman et al. (1965).                                                   Msn1993a
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, this is a Hyades non-member                                    Grf1988 
                                                                                                 Grf2013c
04089+2306   STF 494     H N  17.                                                                MEv2010 
04090-5153   HJ 3625     B is CPD-52@499.                                                                
04091+2901   KOH   3     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04091+2839   HO  326     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 9.61 +/- 4.45, 2.43, and 1.10 Msun, respectively.             Mlk2012 
04091-1624   SKF 950     GWP 556.                                                                Tob2012b
04092+2105   ALP  11     2MASSI J0409095+210439                                                          
                         Physical companionship of B component to this ultracool dwarf ruled             
                         out based on I-J color, using I-band photometry taken at WIYN in                
                         August 2002. C component seen as elongated; its physical companionship          
                         also ruled out.                                                         AlP2007 
04093+1835   LDS1154     NLTT 12637/12636                                                        Chm2004 
04093-0756   A   469     Only elements P and T in the Starikova (1984) orbit have been amended   Sta1984 
                         from the orbit of Baize (1981).                                         Baz1981b
                         Typographical error in semimajor axis for Brendley & Mason (2007)       USN2007b
                         orbit corrected from 2".435 to 0".2986.                                         
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 8.49 +/- 6.33, 3.80, and 2.09 Msun, respectively.             Mlk2012 
04094+2328   POU 412     LDS5509.                                                                        
04094+0546   LAW  12     LSPM J0409+0546 = NLTT 12648. Law et al (2008) derive a distance of     Law2008 
                         19.9 +9.1/-3.8 pc and a projected separation of 4.9 +2.7/-0.7 AU.               
                         Estimated spectral types are M4.5 and 04094-0125   BAL 290     J  3334.                                                                Nsn2016 
04095-0742   BRT 533     Not found by Heintz at IDS position.                                    Hei1990b
04095-1729   ENG  17     B is BD-17@806.                                                                 
04096+3139   HO  327     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
04096-6023   R    41     B is CPD-60@297.                                                                
04096-8151   RST2345     A semi-regular variable, U Men. Hipparcos suspected non-single.                 
04097+1154   BPM  94     [PM2000]  157774 + [PM2000]  157781.                                    Gvr2010 
04097+0006   GRV 207     HJL  56.                                                                HJL1986 
04099+2446   ITO  16     V1306 Tau. Young member of Taurus-Auriga molecular cloud.               Dae2015 
04100+8042   STF 460     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 7.24 +/- 2.42, 5.27, and 4.54 Msun, respectively.             Mlk2012 
04100+0944   LDS1155     LIT  10.                                                                        
04102-0217   FIL  10     BAL  27.                                                                        
04105+5751   HDS 529     Pair originally X coded due to lack of resolution, however, elsewhere   Msn1999b
                         it is noted as a "very close double" so uncertain. Ambiguity from old   MCK1956 
                         reference recently found.                                               Dam2015 
04107+3808   WNT   2     IRAS 04073+3800 = Parsamian 13. Weintraub (1992) suggests that both     Wnt1992 
                         the northern and southern components are double, with separations of            
                         about 5" and 8", respectively.                                                  
04107-0452   A  2801     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.83 +/- 0.33, 2.34, and 1.05 Msun, respectively.             Mlk2012 
04108-1252   PHB   1     LP 714-37                                                                       
                         Phan-Bao et al. (2005) derive distance 18.1 +/- 2.2 pc, spectral types  PhB2005 
                         M5.5 and M7.5, masses 0.11 +/- 0.01 and 0.09 +/- 0.005 Msun.                    
                         Phan-Bao et al. (2006) derive spectral types, absolute K-band mags,     PhB2006 
                         masses of components as follows:                                                
                         A   M5.5 +/- 0.5    9.11 +/- 0.25   0.11 +/- 0.01 Msun                          
                         B   M8.0 +/- 0.5   10.05 +/- 0.30   0.09 +/- 0.01 Msun                          
                         C   M8.5 +/- 0.5   10.35 +/- 0.30   0.08 +/- 0.01 Msun                          
04111-1826   UPT   1     No change in angle; distance decreased 2" in 70 years.                  B__1951a
04112+2630   STF 502     LDS5514 (both AB and BC).                                                       
04112+1538   CHR 202     First detected as an occultation binary by Radick & Lien.               Rad1982a
04113+0531   ENG  18     45 Tau.  Hyades vB 14.  CPM companion with rho = 124".1 is outside              
                         detection window. An additional component was noted as spectroscopic    Grf1988 
                         by Griffin et al. (1988).                                               Msn1993a
04119+2338   CHR  14     Observed under poor seeing conditions. Griffin & Gunn (1981) found a    Grf1981d
                         2.4-day SB.                                                             Msn1993a
04120-0916   A   471     Motion increasing, but only three measures since 1933.                          
04123+6908   HJ 1141     A 13.3 magnitude star is 20" preceding.                                         
04125+3538   HJ  341     ALI 59. BU gives 1880 position +35 25.                                          
04125-3609   HJ 3628     B is CD-36@1632.                                                                
04128+1937   KOH   4     V1307 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04130+5237   PRV   1     GJ 164. Discovered by Palomar 5m/STEPS astrometry and confirmed                 
                         using HST/NICMOS, the combined solution by Pravdo et al. (2004)                 
                         yielded an absolute parallax of 0".0820 +/- 0".008, spectral types of           
                         M4.5V and M6-8V and masses 0.170 +/- 0.015 and 0.095 +/- 0.015 Msun.            
                         Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                      Prv2004 
                         Combined AO+STEPS analysis of this M dwarf binary yields a total mass           
                         0.343 +/- 0.026 Msun, individual masses 0.257 +/- 0.020 and 0.086 +/-           
                         0.007 Msun. Metallicity is at least solar.                              Mtc2008 
                         Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                              
                         GJ 164 = LHS 1642. A known close binary system with a well-determined           
                         orbit (Pravdo et al. 2004; Martinache et al. 2009). Its separation is   Prv2004 
                         smaller than 100 mas at all times, and it therefore remains unresolved  Mtc2009 
                         by AstraLux. We do detect one other point source in the field of view,          
                         but it is a suspected background contaminant based on its blue color,           
                         with dz'= 5.8 +/- 0.1 mag and di' = 5.3 +/- 0.1 mag.                    Jnn2014 
04132+5032   CHR  15     Ross 29.  Van Maanen (1941) suspected this star to be a binary, but     Maa1941 
                         these are the first measurements of a companion.                        McA1987b
04132+2258   HU  302     A premature orbit has been computed.                                            
04135+2816   KSA 102     Primary is variable star V1096 Tau.                                             
04135+1813   BPM  95     [PM2000]  160209 + [PM2000]  160214.                                    Gvr2010 
04135-2554   LDS3564     NLTT 12805/12807                                                        Chm2004 
04136+0743   A  1938     46 Tau. Hipparcos astrometric solution adopted some elements from the   HIP1997d
                         orbit of Heintz.                                                        Hei1984b
                         Combined spectroscopic/astrometric solution of SB1. Calculated masses           
                         1.38 +/- 0.26 and 0.82 +/- 0.21 Msun.                                   Mut2010b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.17 +/- 0.14, 2.77, and 2.55 Msun, respectively.             Mlk2012 
04139+0916   BU  547     47 Tau.                                                                         
                         Spectral types of primary and secondary assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
04140+8216   LUH   7     LHS 1643 + WISE J041328.73+821854.7. Companion is likely not physical,          
                         based on proper motion.                                                 Luh2012b
04140-1222   GAL 364     Object #120 in Gallo's original list.                                   Gal1914 
04142+2813   GHE   1     Aa,Ab: V773 Tau.  Orbital elements and dynamical mass determinations            
                         were published by Tamazian et al. (2002).                               Tam2002 
                         Aa,Ab: The combined solution by Boden et al. (2012) yields a mass and   Bod2012 
                         luminosity for the Ab component of 2.35 +/- 0.67 Msun and 2.6 +/- 0.6           
                         Lsun. This mass is higher than expected, and suggests the Aa,Ab pair            
                         may instead be a multiple system.                                               
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04142-4608   RST2338     Half-period solution equally good, but gives large mass-sum.                    
                         More speckle obs needed (the only existing one erroneous?).                     
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.72 +/- 0.26, 2.26, and 1.07 Msun, respectively.             Mlk2012 
04143-2742   SWR   7     CPM pair                                                                Skf2004 
04144+1523   BPM  96     [PM2000]  160726 + [PM2000]  160650.                                    Gvr2010 
04144-1015   STF 516     39 Eri.                                                                         
                         AB: H N  24.                                                            MEv2010 
04144-6228   HJ 3638     alp Ret. Possible spectroscopic binary.                                         
04145+2851   GRV 208     2MASS J04143060+2851298 and J04143109+2851518, both from the Riaz et            
                         al (2006) sample, are separated by only 23" and although the estimated  Ria2006 
                         spectroscopic distances of 55 and 72 pc are not fully equal, they are           
                         consistent to within the 37% error. In addition, they have very                 
                         similar proper motions (e.g. Roser et al. 2010) and thus probably form  Rsr2010 
                         a physical pair.                                                        Jnn2012 
04148+2813   GHE   2     FO Tau.  Orbital elements and dynamical mass determinations were                
                         published by Tamazian et al. (2002).                                    Tam2002 
04148+2753   GHE   3     HBC 368 = V1098 Tau = LkCa 3. Torres et al. (2013) find that both               
                         components of this 0".5 pre-MS pair are spectroscopic binaries, with            
                         periods for Aa,Ab and Ba,Bb of 12.942 and 4.068d, respectively.         Trr2013 
04148+2648   DAE  21     CX Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148+2646   DAE  20     FP Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148-6212   HJ 3641     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
04149+5824   LDS9165     Old LDS6165.                                                                    
04149+4825   STT  73     mu Per = 51 Per. A is a Beta Lyrae-type system.                                 
                         The elements P, T, and e of Alden (1925) were adopted from the          Ald1925 
                         spectroscopic orbit of Cannon (Pub. DAO Ottawa 2, 365, 1915).                   
             H 6  20     H VI 20. SHJ 364.                                                               
04152+5052   AG  309     B is BD+50@944.                                                                 
04153+2044   KOH   6     Metchev & Hillenbrand say the pair is probably physical, based on               
                         proximity.                                                              Met2004b
                         V1199 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04153-0739   STF 518     A: omi 2 Eri = 40 Eri = omi Eri                                                 
                         LDS 114 = STFB 1. Proper motion of A -2224 -3423.                               
                         C is a flare star, DY Eri, and a strong X-ray source.                           
                         AE: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         BC: NLTT 12868/12869                                                    Chm2004 
                         BC at 83" is physical, and is a Delta Scuti star showing coronal X-ray          
                         emission.                                                                       
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         HIP 19849. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         BC: Additional notes may be found in Worley (1956).                     Wor1956b
04155+2048   RED   2     1996.1230: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04155+0611   STTA 45     AB: H VI 98. A is V774 Tau. B is BD+05@613, and a suspected variable.           
                         AB: SHY  21. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: H 6  98.                                                            MEv2010 
                         Toyota et al. (2009) monitored the RV of both the A and B components            
                         every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                         echelle (precision ~10 m/s). Standard deviations of the RVs of both             
                         components are <40 m/s and velocities show no periodic variation.               
                         These results rejects the association of a planet of mass > 1.8 Mjup            
                         with either star.                                                       Toy2009 
04157+2049   TOK 659     Hyades, vB162.  primary is SB2, P=55.130d                               Tok2014d
                         The 55.1-day SB of Griffin & Gunn (1981) is outside our detection       Grf1981d
                         window.                                                                 Msn1993a
04158+4524   STF 512     HJL  58.                                                                HJL1986 
04158+3100   KOH   7     V952 Per. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04158+1524   BUP  51     A: 48 Tau = V1099 Tau                                                           
04159+3142   STT  77     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 4.90 +/- 3.64, 2.97, and 1.10 Msun, respectively.  Mlk2012 
             STTA 43     AB,C: HJL  59.                                                          HJL1986 
04162+1648   RED   3     1995.8821: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers possible binary.                Red1997 
04163+0710   WSI 97      This is a single-lined nearby binary. Using the radial velocities               
                         measured by D. Latham (2012, private communication), we computed a              
                         combined orbit (the previous visual orbit reported by Riddle et al.     RAO2015 
                         (2015) had a wrong period). The inclination is close to 180deg and had          
                         to be fixed in order to match the RV amplitude.                         Tok2015c
04163-6057   GLE   1     Variable: TT Ret. A premature orbit has been computed.                          
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04164+0710   WSI  97     Provisionally designated WSI9102.                                       Tok2010 
04165+0041   J  1458     BAL 971.                                                                        
04165-5918   JSP  56     eps Ret                                                                         
                         The companion is a possible white dwarf.                                Cvn2006 
                         Companion confirmed as DA white dwarf.                                  Cvn2007 
                         Optical spectroscopy suggests the companion is a mid- to late-B                 
                         (B3-B9) dwarf.                                                          Mug2007b
04166+2447   LDS1158     NLTT 12896/12897                                                        Chm2004 
04170+1941   HO  328     Only elements P and T in the Starikova (1980) orbit were amended from   Sta1980b
                         the orbit of Heintz (1978).                                             Hei1978a
                         Additional notes may be found in Van Biesbroeck (1954) and              VBs1954 
                         Couteau (1963).                                                         Cou1963a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 6.92 +/- 2.37, 2.74, and 1.20 Msun, respectively.             Mlk2012 
04171+6408   STF 503     BD is +63  489a.                                                                
04171+0409   BAL2119     J 1814.                                                                         
04173+4613   STTA 44     B is BD+45@904.                                                                 
04173+2035   LDS5535     HJL1032.                                                                HJL1986 
04176+2833   SAR   2     HBC 371 = LkCa 5.                                                               
04176+1658   LDS3568     This cannot be the close 3079-d or 5.609-d spectroscopic binaries of    Grf2012b
                         Griffin. The 3079-d pair has an estimated separation of 0.06", but              
                         delta-mag may be considerable.                                                  
04176+1657   HD  27130   Hyades vB 22.  The 5.6-day SB of Griffin et al. (1985) is outside our   Grf1985b
                         detection window.                                                       Msn1993a
04177-6315   RMK   3     the Ret                                                                         
04179+5847   STF 511     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.60 +/- 1.54, 3.37, and 2.09 Msun, respectively.             Mlk2012 
04179-3348   I   270     ups 4 Eri = 41 Eri. Duplicity of AB doubtful.                                   
                         A is a spectroscopic binary, and possible variable.                             
04180+1815   HD  27149   Hyades vB 23. The 75.6-day SB of Batten & Wallerstein (1973) is         Bte1973 
                         outside our detection window.                                           Msn1993a
04180-0031   SKF 848     Pair originally published as BVD 45, but with incorrect sign given to   Bvd2010b
                         declination. Pair later "rediscovered" and published with correct               
                         declination; this latter discoverer designation has been maintained.            
04181+0446   TOB9003     Measured as BAZ   3 = STF1063 but with an error of -3h in RA!           Tob2010 
                                                                                                 Dam2012 
04181-1448   LDS9166     Old LDS6166.                                                                    
                         NLTT 12975/12973                                                        Chm2004 
04182+5018   b Per       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hill et al. (1976).                                                     HlG1976 
04182+2248   STF 520     Measured separation too large, estimated at probably 0.30".             Cou1955c
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 14.33 +/- 9.16, 3.42, and 1.20 Msun, respectively.            Mlk2012 
04183-3000   LDS3571     NLTT 12992/12990                                                        Chm2004 
04184+2135   MCA  14     51 Tau. Hyad (vB 24). B is BD+21@619. A is a long-period spectroscopic          
                         binary, resolved by speckle interferometry. Analysis of the                     
                         spectroscopic/interferometric orbit is given by McAlister (1977).       McA1977 
                         1978.1490:  Theta was incorrectly given as 325.5 degrees                McA1980b
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         A new orbit with a period of 11.3 years was determined by Dombrowski    Dmb1991 
                         (1991).                                                                 Msn1993a
                         Torres et al. (1997) derive a combined spectroscopic/astrometric        Trr1997a
                         solution, yielding an orbital parallax 0.01792 /- 0.00058 and masses            
                         1.80 +/= 0.13 and 1.46 +/- 0.18 Msun.                                           
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Deutsch & Lowen (1971).                                                 Deu1971 
                         Aa,Ab: Martin et al. (1998) derive component masses 1.756 +/- 0.343             
                         and 0.953 +/- 0.247 Msun.                                               Mig1998 
                         Pourbaix (2000) gives a combined solution for this resolved SB2,        Pbx2000b
                         yielding orbital parallaxes and component masses.                               
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.96 +/- 0.47, 2.99, and 1.45 Msun, respectively.  Mlk2012 
04184-2347   RST2344     BRT2832.                                                                Brt1947 
04185+2817   HAT   4     AB: Additional notes may be found in Herbig (1962).                     Her1962 
04186+1606   BPM  97     [PM2000]  163490 + [PM2000]  163456.                                    Gvr2010 
04187+2819   SKN   1     Measure of 1990.725 made by the VLA at radio wavelengths.               Skn1993 
04187-5252   SHY 462     AB: HIP  20109 + HIP  20074.                                                    
04188+2820   KSA 104     Primary is variable star V1023 Tau.                                             
04189+0146   STTA 49     B is BD+01@734.                                                                 
04190-0725   STF 527     H 2  80.                                                                MEv2010 
04192+6135   STF 513     Same as STF 507.                                                                
04192+1100   BPM  98     [PM2000]  163846 + [PM2000]  163809.                                    Gvr2010 
04193-4416   HJ 3643     B is CD-44@1505.                                                                
04195+3800   HDS 552     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.74 +/- 0.86, 2.77, and 1.45 Msun, respectively.             Mlk2012 
04195+2808   DAE  23     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04196+3355   HJ  674     The discovery observation of 220 deg may be in error. The AC2000                
                         catalog include one measurement for 1924.381: 22.3 deg and 16.1".               
                         Proper motion of B is mu(AR) = +0.004+-0.007, mu(DEC) = -0.022+-0.002   FMR2000b
04196-2847   SHY 463     HIP  20184 + HIP  19926.                                                        
04197+1416   GIC  45     G008-027/G008-026 = Melotte 25 VA 174 + 170.                                    
04198+1538   BLM   1     gam Tau = 54 Tau. SB resolved by speckle interferometry.                        
                         This object was misidentified as HR 1349 by McAlister (1978).           McA1978c
                         Observed under rather poor seeing conditions. Morgan et al. (1982)      BLM1982 
                         also report a large magnitude difference.                               Msn1993a
04199+3145   J   934     Jonckheere gives the 1950 position: 04 17.0 +31 43.                     J__1958 
                         Couteau corrects the position.                                          Cou1953a
04199+1631   STT  79     Hyad (vB 29). SB according to Griffin et al. (1988).                    Grf1988 
                         1978.6183: The date of this observation was given incorrectly as                
                         1977.6183 by McAlister & Fekel (1980).                                  McA1980b
                         Observed under poor seeing conditions.                                  Msn1993a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.57 +/- 1.41, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04200+1402   BUP  53     57 Tau. A is a Delta Scuti-type variable, V483 Tau.                             
04201+1953   LDS1164     LDS9167 (old LDS6167).  NLTT 13024 = LP 414-169                         Chm2004 
                         NLTT 13024/13026                                                        Chm2004 
04202+3336   FAR   4     Primary is white dwarf WD 0416+334 = GD 60. Aka SKF 316.                Far2005b
04203+1833   LDS5540     Companion at 264" agrees with Luyten's astrometry, but star at 307" is  Luy1984 
                         in much better magnitude and proper motion agreement. This pair added           
                         as AC pair, until proper identification can be determined.                      
04204+3434   BU 1382     54 Per.                                                                         
04204+2721   SHJ  40     phi Tau = 52 Tau. STTA 48 = H 5  13. B is BD+26@712.                            
04205-0119   RST4769     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.54 +/- 0.98, 3.17, and 2.00 Msun, respectively.             Mlk2012 
04206+2429   COU 704     Probably the A component of POU 442.                                            
04207+1514   JNN 261     LP 475-7. Estimated age 1000-10000 Myr; masses 0.45 +/- 0.04 and 0.21           
                         +/- 0.03 Msun; a ~7.4 AU.                                               Jnn2014 
04208+3009   KOH   8     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04209+1352   BAS   3     Hyad - Melotte 25 VA 201 = vB 34.                                               
                         This binary, unresolved by visual and IR speckle interferometry is not          
                         the 3.06-day SB of Northcott & Wright (1952 JRASC, 46, 11).                     
                         The combined spectroscopic/interferometric solution by Konacki et al.   Knc2004 
                         (2004) uses data from the Palomar Testbed Interferometer and assumes            
                         the eccentricity = 0.0 and the K-band brightness ratio = 1.0. Results           
                         include P = 3.0591080 +/- 0.000011 d, T = 44497.185696 +/- 0.0026 MJD,          
                         derived masses 1.38 +/- 0.13 and 1.39 +/- 0.13 Msun, spectral types             
                         F6V, and diameters 0.25 mas.                                                    
                         The 3-day SB is outside our detection window.                           Msn1993a
                         This cannot be the close 3.06-d spectroscopic binary of Griffin.        Grf2012b
                         Aa,Ab is resolved with PTI, orbit (Konacki & Lane 2004). The B          Knc2004 
                         component is a white dwarf (Barstow et al. 2001), DA3.1; mass 0.98      Bas2001 
                         Msun.  Shaya & Olling (2011): co-moving HIP 1996 at 0.75pc, prob.       Shy2011 
                         0.96: another Hyades star?                                              Tok2014d
             HD  27483   Mel 25 VA 201: Malkov et al. (2012) derive dynamical, photometric, and          
                         spectroscopic masses 3.04 +/- 6.10, 2.70, and 3.17 Msun, respectively.  Mlk2012 
04209-1156   GAL 365     Object #125 in Gallo's original list.                                   Gal1914 
04210+5015   S   445     STTA 47. B is BD+49@1161.                                                       
04211+5532   STTA 46     B is BD+55@869.                                                                 
04215+1704   BPM  99     [PM2000]  165579 + [PM2000]  165489.                                    Gvr2010 
04215-2055   LDS9168     Old LDS6168.                                                                    
                         AC: NLTT 13102/13095                                                    Chm2004 
                         AC: SHY 167. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04215-2544   BU  744     Star A is SB1, P = 4.0 d, tho this may be spurious,                     Wor1983 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 3.42 +/- 1.00, 2.96, and 1.35 Msun, respectively.  Mlk2012 
04216-1559   LDS9169     Old LDS6169.                                                                    
                         NLTT 13109/13110                                                        Chm2004 
04217+1046   TOK  84     HIP 20366. Small PM(A)=(-31,-12). NOMAD: PM(B)=(+39,-63), V=13.95.      Tok2011a
04218+1949   KNT   2     LDS2228. The variable U Tau.                                                    
04218+1929   SIG   1     LP 415-20 = Bryja 262.  Spectral types M7.0, M9.5. Probable Hyades              
                         member. Estimated orbital period 23 +7/-6 yrs.                          Sig2003 
                         Konopacky et al. (2010) derive a distance of 21. +/- 5. pc and a                
                         system mass of 0.09 +/- 0.06 Msun.                                      Kon2010 
04219+5749   BRG  34     XO-3. Bergfors et al. (2013) estimate spectral types F5V and G0-M2.5V.  Brg2013 
04219+1530   CHX   1     IRAM 04191+1522. Primary is a Class 0 protostar, resolved into 7.8"             
                         pair in 1.3mm continuum observations at Submillimeter Array (SMA).      ChX2012 
                         Chen et al. quote position angle as "SE/NW"; followup check on Aladin           
                         by cataloguer suggests angle approximately 290deg.                              
04220+2826   ISM   1     RY Tau, a T-Tauri star.                                                         
04220+2818   ITO  21     V987 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04220+2658   SMN   9     FS Tau.                                                                         
                         Measure of 1989.5 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
                         Tamazian et al. (2002) solution includes a mass determination based on  Tam2002 
                         an estimated distance.                                                          
                         AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
04220+1932   GHE   6     Components A, Ba, and Bb of this system are also commonly designated            
                         as N, Sa, and Sb, respectively, due to the north-south orientation of           
                         the wider pair.                                                                 
                         AB: Measure of 1982.5 made by the VLA at radio wavelengths.             Scw1984 
                         Measure of 1983.75 made by the VLA at radio wavelengths.                Scw1986 
                         Measures of Johnston et al. and Loinard et al. made by the VLA at       Jnt2003 
                         radio wavelengths.                                                      Loi2003 
                         AB: Rho and theta errors for Ghez et al. (1995), Furlan et al. (2003),  Ghe1995 
                         and Roddier et al. (2000) measures have been added/updated as noted by  Fun2003 
                         Koehler et al. (2008). Koehler et al. derive a preliminary orbit for    Rod2000 
                         the AB pair, yielding a system mass of 5.57 +0.11/-0.29 Msun.           Koh2008b
                         A,Ba: The 2000.886 Duchene et al. (2002) theta value was corrected by   Dch2002 
                         Duchene et al (2006). Also, the Duchene et al. (2006) theta value for   Dch2006 
                         2005.801 was changed by 90deg to correct for the orientation of the             
                         camera (Schaefer, priv. comm. cited by Koehler et al. 2008)             Koh2008b
             KRS   2     Ba,Bb: Tamazian derives a total system mass of 2.82 +/- 0.74 Msun,      Tam2005 
                         consistent with the IRC model of Koresko et al. (1997).                 Krs1997 
                         T Tau Sa-Sb orbit gives range 1991-2001 for T, 0.09-0.87 for e,                 
                         11-60 for i. Values for P and a are lower limits.                       Sfr2006 
                         Duchene et al. (2006) derive masses for the Ba and Bb components of     Dch2006 
                         2.73 +/- 0.31 and 0.61 +/- 0.17 Msun, respectively.                             
                         Ba,Bb: The 2000.886 Duchene et al. (2002) theta value was corrected by  Dch2002 
                         Duchene et al (2006)                                                    Dch2006 
                         The 2002.829 Schaefer et al. (2006) measure is a reanalysis of data     Sfr2006 
                         from Beck et al. (2004).                                                Bck2004 
                         Koehler et al. (2008) derive a system mass of 2.96 +0.15/-0.24 Msun     Koh2008b
                         and individual masses of 2.13 +0.14/-0.20 and 0.83 +0.10/-0.11 Msun             
                         for the Ba and Bb components, respectively.                                     
                         Ba,Bb: The Schaefer et al. (2014) orbit, combined with a VLBA parallax          
                         of 6.90 +/- 0.09 mas (147.6 +/- 0.6pc; Loinard et al. 2007, ApJ 671,            
                         546) yields a total mass for Ba+Bb of 2.70 +/- 0.22 Msun.               Sfr2014 
                         Ba,Bb: Csepany et al. (2015) generated new orbital parameters for T             
                         Tau N-S (KRS   2Ba,Bb), but their grid search yields a wide range of            
                         possible solutions (P 475-27000y, a 0.57-16.8", etc.)                   Cse2015b
04220+1405   HD  27628   Hyades vB 38 = V775 Tau. The 2.14-day SB of Abt (1961) is outside our   AbH1961 
                         detection window.                                                       Msn1993a
             BUP  54     60 Tau. A is a specroscopic binary and variable, V775 Tau.                      
04221+2826   KSA 105     V1071 Tau = LkCa 21. Young member of Taurus-Auriga molecular cloud.     Dae2015 
04221-2849   BWL  15     Pair is a 0".7 equal-flux K7V2 binary. Torres et al. (2006 A&A 460,             
                         695) found strong Halpha emission and lithium absorption. Age is                
                         consistent with that of the Pleiades, so an age range of 50-200 Myr             
                         is adopted for this system.                                             Bwl2015 
04221+1934   KOH   9     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04224+1118   PAT   5     The 3-year SB of Griffin et al. (1988) is outside our detection         Grf1988 
                         window.                                                                 Msn1993a
                         The double-lined spectroscopic solution of this 1043.5-d pair           Grf2012b
                         determined by Griffin.                                                          
04226+2538   STF 528     chi Tau = 59 Tau                                                                
                         H 4  10.                                                                MEv2010 
                         The secondary is SB2 (F8+G6), with period 17.6 days for Ba,Bb; RV               
                         residuals indicate the presence of a more distant Bc companion. Based           
                         on spectroscopic observations obtained at CfA 1988-2004, Torres (2006)          
                         derived an orbit for Bab,Bc with period 9.447 +/- 0.017 yr. Mass for            
                         the A component is determined to be 2.60 +/- 0.5 Msun. Inclination              
                         angle for the Ba,Bb orbit is 53.5 +/- 0.5deg, yielding masses 1.19 and          
                         1.02 Msun for Ba and Bb. Bc appears to be over-massive; based on                
                         infrared excess this could be well explained as an equal-mass binary            
                         composed of late-type stars of masses ~0.70 Msun (spectral type ~K4).           
                         Total mass of B is 3.6 Msun.  Torres estimates the Bab,Bc semi-major            
                         axis at about 83.6 mas and the magnitude difference dV~3.3mag                   
                         (dK~1.5mag), making the pair potentially resolvable by speckle                  
                         interferometry.                                                         Trr2006b
04227+1503   STT  82     Hyades vB 40A. The primary is SB1, P = 4.00 d (Sanford 1921).           San1921 
                         Primary is SB2, P=4.0002d (Griffin 2012)                                Grf2012b
                         Also a wider companion (LDS 1166 AC, rho = 62", M = 17.8).                      
                         The 255.5-year binary, ADS 3169 = STT 82 AB is outside our detection            
                         window, although part of a peak is seen at the edge of the window at            
                         the expected position angle, according to the orbit in the Worley &             
                         Heintz (1983) orbit catalog. A wider companion (LDS 1166AC, rho = 62",  Wor1983 
                         M = 17.8) and the 4d SB are also outside our detection window.          Msn1993a
                         A component of pair determined to be a 4.0-d spectroscopic binary.      Grf2012b
04228+1647   HD  27685   Hyades vB 39. Spectroscopic binary with P > 7 yr, according to Griffin  Grf1988 
                         et al. (1988).                                                          Msn1993a
04230+1732   CHR 262     del 1 Tau = 61 Tau. The primary is a long-period spectroscopic and              
             BUP  55     occultation binary.                                                             
                         This system, first announced in Mason et al. but considered of          Msn1993a
                         uncertain veracity, has been included. While its status is not                  
                         definitive, subsequent confirmation or suspected duplicity (by another          
                         technique) makes the discovery measurement somewhat more probable.              
                         1991.8995: This is a particularly unexpected result, given the four             
                         previous epochs at which our observations have shown no indications of          
                         duplicity.  All four of the earlier observations were reanalyzed using          
                         the same procedures employed here, but no additional supporting                 
                         evidence of duplicity was found.  If this additional component is               
                         confirmed,  vB 41 will be the second K0 giant binary that has been              
                         resolved in the Hyades (HR 1411 being the other).  The common proper            
                         motion companion at a separation of 195".5 is far outside our window            
                         of observation, and the 530-day spectroscopic component of Griffin &            
                         Gunn (1977) would have an angular separation below the diffraction      Grf1977d
                         limit of the KPNO 4-m telescope.                                        Msn1993a
                         Aa,Ab : If real, this pair could be the 530.1-d spectroscopic binary    Grf2012b
                         of Griffin.                                                                     
04231-0117   BU  402     Aka OL  201.                                                                    
04232+7510   MLR 459     Also known as TDS 138.                                                          
04232-1135   GAL 366     Object #127 in Gallo's original list.                                   Gal1914 
04233+1123   STF 535     A premature orbit has been computed.                                            
                         Ruymaekers & Nys (1995) noted discrepancies in the orbit of Popovic     Ruy1995 
                         (1982), and calculated elements from their Thiele-Innes elements.       Pop1982a
04233-0500   HJ  342     Same as STF 539 and H IV 117.                                                   
                         AB: H 4 117.                                                            MEv2010 
04233-2138   B  2571     CPD-21@545.                                                                     
04234+1940   V988 Tau    Hyades vB 43. Hipparcos astrometric solution adopted some elements      HIP1997d
                         from the orbit of Griffin et al. (1985).                                Grf1985b
                         The 1.6-year SB of Griffin et al. is outside our detection window.      Msn1993a
04234+1647   HD  27749   Hyades vB 45.  The 8.418-day SB of Abt & Levy (1985) is outside our     AbH1985 
                         detection window.                                                       Msn1993a
04235+2059   CHR  16     An occultation binary, now resolved.                                            
04236+4226   STT  80     1977.7420: The date of this observation was given incorrectly as                
                         1978.7420 by McAlister & Fekel (1980).                                  McA1980b
04237+1538   MET   3     Metchev & Hillenbrand say the pair is probably optical, based on                
                         proximity.                                                              Met2004b
04238-0414   BUG   7     SDSS J042348.57-041403.5                                                        
                         Estimated spectral types are L6.5 + T2, effective temperatures 1490             
                         +/- 100 and 1250 +/- 80 K. Masses are estimated at 0.039-0.062 and              
                         0.029-0.051 Msun, and the orbital period (assuming the semi-major axis          
                         = 1.26 * rho) is ~19yr.                                                 Bug2006a
04239+0928   HU  304     66 Tau.                                                                         
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.81 +/- 1.40, 6.11, and 4.43 Msun, respectively.             Mlk2012 
04239-1102   GAL 367     Object #128 in Gallo's original list.                                   Gal1914 
04240+2418   STF 534     62 Tau.                                                                         
                         AB: H 4 109.                                                            MEv2010 
04241+1727   BUP  56     del 2 Tau = 64 Tau. Hyades vB 47. A is spectroscopic binary.                    
04242+1445   HDS 564     1991.8992: Noted as a possible spectroscopic binary by Griffin et al.   Grf1988 
                         (1988), it is uncertain whether the system we detect here is also               
                         producing the radial velocity variation.                                Msn1993a
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         The spectroscopic solution of this ~42000-d pair determined by Griffin, Grf2012b
                         its gamma velocity "removing any remaining doubt about the systems      Grf2013c
                         credentials as a Hyades member."                                                
04244+3419   STF 533     AB: H 4  72.                                                            MEv2010 
                         Primary is V590 Per, a Beta Lyr type eclipsing binary, P = 5.6866d.     Zas2012 
04245+5051   TOK 245     AC: The physical nature of C is not certain: CPM, but the PM is small.  Tok2014d
04245+2244   BU 1235     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.22 +/- 2.00, 2.88, and 1.35 Msun, respectively.             Mlk2012 
04245+1653   PAT   6     Noted as a possible spectroscopic binary by Griffin et al.              Grf1988 
                         (1988).                                                                 Msn1993a
                         Hyades vB 52. Mass of B 0.49 Msun (Metchev & Hillenbrand 2009).         Met2009 
04246+3358   STT  81     AB: 56 Per.                                                                     
04247+0442   HJL1115     Hyades vB 140. The 156.4-day SB of Griffin et al. (1985) is outside     Grf1985b
                         our detection window.                                                   Msn1993a
                         A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
04247-0845   STF 544     Primary is SB1, P=1248d = 3.41y. RV(B)=var?                             Tok2014d
04247+0442   HJL1115     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
23456+1309   HJL1116     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                         (2016) yields masses 1.686 +/- 0.021 and 1.390 +/- 0.034 Msun.          HJL2016 
04248-5037   RST1273     HIP 20606. Both components A,B are above the MS, young? B is too red in         
                         the (Kabs,V-K) CMD, infrared companion? Planetary companion to A = HD           
                         28254 is detected with RV. No relevant references in SIMBAD.            Tok2011a
                         A is exoplanet host, P=1116d.  Roell et al. (2012 A&A 542, A92) list B          
                         as physical, confirmed by Naef et al. (2010 A&A 532, A15).              Tok2014d
04249-3445   I    59     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
04251+8603   WFC  23     HJL  57.                                                                HJL1986 
04252+2545   TOK 247     Not Hyades member: different PM and RV. (Griffin 2013).                 Grf2013c
04252-6415   HJ 3656     B is CPD-64@333.                                                                
04253-0932   GAL 368     Object #129 in Gallo's original list.                                   Gal1914 
04254+2218   STF 541     A: kap 1 Tau = 65 Tau = K Tau                                                   
                         A,CD: H 6   8.                                                          MEv2010 
                         AB: HJL1034.                                                            HJL1986 
             STF 541     04253+2215STF 541CD and 04254+2218STFA  9AB were found to                       
             STFA  9     be the same wide pair, so designations for these two                            
                         multiple systems were combined, as follows:                                     
                         04253+2215STF 541AB   --> 04254+2218STF 541CD                                   
                         04253+2215STF 541AB,C --> 04254+2218STF 541A,CD                                 
                         04253+2215STF 541AB,D --> 04254+2218STF 541B,CD                                 
                         04254+2218STFA  9AB   --> 04254+2218STF 541AB                                   
                         04254+2218STFA  9Aa   --> 04254+2218STF 541AE                                   
                         04254+2218STFA  9Bb   --> 04254+2218STF 541BF                                   
                         A : kap 1 Tau = 65 Tau = K Tau. Occult. binary, Hyades member (vB 54)           
                         B : kap 2 Tau = 67 Tau. Delta Scuti variable, Hyades cluster member.            
                         CD : J 2722. This faint pair is between kap 1 and kap 2 Tau.                    
                         Pairs STFA  9AB (rho = 339"), STFA  9Aa (rho = 141") and STFA  9Bb              
                         (rho = 107") are all far outside our detection window.                  Msn1993a
04255+1756   KUI  17     del 3 Tau = 68 Tau. A is spectroscopic binary and variable, V776 Tau.           
             H 6 101     H VI 101. There is a wide faint pair noticed by John Herschel, 320@             
                         Class VI.                                                               H__1867 
                         The B, C, D, and E components all fall outside our detection window.    Msn1993a
04256+1556   FIN 342     Aa,Ab: Hyad (vB 57). HR 1391 = 70 Tau.                                          
                         Combined spectroscopic/astrometric solution. Orbital parallax 0.02144   Trr1997b
                         +/- 0.00067, masses 1.363 +/= 0.073 and 1.253 +/- 0.075 Msun.                   
                         Quadrant determinations made at several epochs by McAlister et al.      McA1988 
                         (1988) have shown that this system is best represented by an eccentric          
                         orbit of period 6.3 years, rather than a circular 13-year orbit.                
                         1977.7421  Theta was incorrectly given as 6.0 degrees by McAlister &            
                         Fekel 1980).                                                            McA1980b
                         This resolved spectroscopic binary (with P = 6.28 yr) is discussed by   McA1988 
                         McAlister et al. (1988) and by Dombrowski (1991).                       Dmb1991 
                         The published measure for 1988.6582 (McAlister et al. 1990) is          McA1990 
                         is spurious. The data leading to this measure are actually the same as          
                         those for HR 1331 (= McA 14) for the same epoch. These two stars were           
                         observed in immediate sequence but with different microscope                    
                         objectives, and the final reductions calculated two results from the            
                         same data set, but with different scale factors; the HR 1331 measure            
                         for 1988.6582 is the correct one.  Reanalysis of the correct data for           
                         FIN 342 gives the 25 mas result shown here. Peterson (1992, private             
                         communication) pointed out the inconsistency of our originally                  
                         published measure with respect to our previous orbital analysis of              
                         this Hyades binary (McAlister et al. 1988).                             Hrt1992b
                         Pourbaix gives combined solution for this resolved SB2, yielding                
                         orbital parallaxes and component masses.                                Pbx2000b
                         Aa,Ab : New spectroscopic solution determined by Griffin.               Grf2012b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 2.50 +/- 0.47, 2.48, and 1.13 Msun, respectively.  Mlk2012 
04257+6340   HJL1033     SHY 464. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
04257-0214   BU  403     Linear elements fit nicely at present, but this is a physical pair and          
                         an orbit can be computed at some future date.                                   
04258+1800   COU2682     Spectroscopic binary with P > 15 yr, according to Griffin et al.        Grf1988 
                         (1988).                                                                 Msn1993a
                         The spectroscopic solution of this 15650-d pair determined by Griffin.  Grf2012b
04258+1733   RED   4     1996.1449: RHy ID and coordinates from Reid (1992).                     Red1992 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04259+1852   BU 1185     Hyad (vB 58).                                                                   
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1982.7579: This autocorrelogram was remeasured; the new results are     McA1987b
                         listed here.                                                                    
                         The 27.67-year binary (see Dombrowski 1991) ADS 3210  was observed at   Dmb1991 
                         a time when atmospheric seeing was rated as poor.  Also noted as a SB   Grf1988 
                         in Griffin et al. (1988).                                               Msn1993a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.01 +/- 0.36, 2.00, and 0.98 Msun, respectively.             Mlk2012 
04260+4515   ES  567     B is BD+44@946.                                                                 
                         Measures attributed to BC are all AC. Component designation changed.            
04261+1531   PAT   7     SB with P > 7 yr according to                                           Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         The spectroscopic solution of this 5688-d pair determined by Griffin.   Grf2012b
04261-1059   GAL 369     Object #130 in Gallo's original list.                                   Gal1914 
04263+3443   HU  609     Only elements P and T have been amended from the orbit of               Sta1978c
                         Heintz (1967).                                                          Hei1967d
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 12.01 +/- 10.65, 3.16, and 1.20 Msun, respectively.           Mlk2012 
04263+2249   BUP  58     ups Tau = 69 Tau. A is an occultation binary.                                   
04263+2128   TOK  16     Hyades vB 62. Primary is 8.55d SB1 (Griffin & Gunn 1978); estimated     Grf1978b
                         period of visual pair 9300y. Unresolved by Patience et al.              Tok2006 
                         The SB  is outside our detection window.                                Msn1993a
04263+1538   HD  28052   Hyades vB 141. A CPM companion with rho = 134".4 is outside our         Msn1993a
                         detection window.  Also, noted as a 14.24-year SB by Abt (1965).        AbH1965 
04263+1537   BUP  59     71 Tau. A is a long-period spectroscopic binary,                                
                         P = 5200d, and occultation pair. V777 Tau.                                      
                         Peirce noted a close companion to A component (1868.13, 70deg) which            
                         he said was "much closer than 80 Tau". His 1868.13 separation                   
                         measure for 80 Tau (= 04301+1538 STF 554) was 0".75.                    Pei1882 
04263+1400   HJ 3256     LDS5558.                                                                        
04264+2249   HD  28024   Hyades vB 60. A CPM companion with rho = 110".2 is outside our                  
                         detection window.                                                       Msn1993a
04264+1651   HD  28068   Hyades vB 63. A spectroscopic binary B with P ~ 7 yr, according to      Grf1985b
                         Griffin et al. (1985).                                                  Msn1993a
04268+1525   LDS2236     LDS5559.                                                                        
04268+1052   PAT   8     1991.8990: This K dwarf is noted as a binary with a period in excess            
                         of 16 years in Griffin et al. (1988), and it is likely that we have     Grf1988 
                         detected the spectroscopic companion.                                   Msn1993a
                         The spectroscopic solution of this 6950-d pair determined by Griffin.   Grf2012b
04268+0843   HJ  678     This is not BD+08  690, according to Heintz.                            Hei1992a
04268-0143   UC 1168     Candidate on Tokovinin list, now reconfirmed as CPM.                    Tok2013c
                         AB is CPM according to Hartkopf et al. (2013).  A is on Keck RV         UC_2013b
                         program, RV trend.                                                      Tok2014d
04269+2607   LEI   2     Measure of 1987.8 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
             SMN  10     Ca,Cb: Called FV Tau-c by Simon, therefore given component designation          
                         of Ca,Cb. Relationship to LEI  02 uncertain.                            Smn1992 
                         Measure of 1987.8 made by triangulation of multiple measures and was            
                         in a red filter.                                                                
                         aka COR   3Ca,Cb                                                                
                         FV Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04270+1907   STF 546     HJL  60.                                                                HJL1986 
                         H 2  54.                                                                MEv2010 
04270-7238   B  2091     Composite spectrum: G8III+(A/F).                                                
04271+2542   THB   1     Preliminary orbital elements give total mass 2.8 +/- 1.5 Msun.          Thb1995b
                         Tamazian et al. (2002) solution includes mass determination based on    Tam2002 
                         estimated distance.                                                             
                         DF Tau orbit by Schaefer et al. (2006) gives range 1974-2022 for T,     Sfr2006 
                         0.05-0.76 for e. Values for P and a are lower limits.                           
                         Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                         mass 1.17 +/- 0.13 Msun. The orbital period of 43.7y closely matches            
                         the 44yr timescale of photometric variations; this is consistent with           
                         a suggestion by Lamzin et al. (2001 A&A 372, 922) that the variability          
                         is caused by the circumstellar accretion rate onto the primary being            
                         modulated by the orbital motion of the companion.                       Sfr2014 
04271+1812   STF 545     AB: H 4  74.                                                            MEv2010 
04275+1113   BU 1186     A is variable.                                                                  
04275-1707   HU  440     Primary is HH Eri, eclipsing binary (Algol), P=8.5d.                    Tok2014d
04275-2427   I   413     Baize (1993) value of omega incorrectly listed as 96.0, same as Omega.  Baz1993b
04276+1927   RED   5     1995.6986: RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al.(1981).                                         Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04277+2631   GIC  47     LDS1171.  G008-035/G039-014.                                                    
                         NLTT 13302/13303                                                        Chm2004 
04278+1001   STF 549     AB: H 4  75.                                                            MEv2010 
04280+2137   BUP  60     A is a spectroscopic and occultation binary.                                    
04281-1033   GAL 370     Object #131 in Gallo's original list.                                   Gal1914 
04282+5303   RUC   3     AO Cam. Spectral type of resolved companion later than M5V.             Ruc2007 
04282+0600   LDS9170     Old LDS6170.                                                                    
04283-1400   GAL 371     Object #132 in Gallo's original list.                                   Gal1914 
04284+1622   RCH   2     Measure of 1998.921 made by triangulation of multiple measures.         Rch2002 
04284-6543   HJ 3662     B is CPD-65@@345.                                                               
04285+1742   GUE   5     The spectroscopic solution of this 7022-d pair determined by Griffin.   Grf2012b
04285+1458   BPM 100     [PM2000]  170962 + [PM2000]  171001.                                    Gvr2010 
04285+0505   HJ 2233     BAL 2614.                                                                       
04286+1944   HD  28291   Hyades vB 69.  The 41.66-day SB of Griffin et al. (1985) is outside     Grf1985b
                         our detection window.                                                   Msn1993a
04286+1911   BUP  61     eps Tau = 74 Tau                                                                
04287+2714   KON   2     Estimated masses 0.15 and 0.06 Msun. Primary spectral type M5.25        Kon2007b
04287+2613   HDS 576     Cvetkovic et al. (2014) derive spectral types M0 and  M0, masses 0.46           
                         and 0.46 Msun. Dynamical parallax is 25.86 +/- 0.27 mas.                Cve2014 
04287+1552   STFA 10     AB: the 2 Tau = 78 Tau. Hyades vB 72 = HR 1412.                                 
                         Pair appears in an appendix list, not part of discoverer's regular              
                         numbering sequence. B is BD+15@631.                                             
                         Also variable, probably of  Delta Scuti type.                                   
                         The 140.7-day SB of Ebbighausen (1959 Pub. DAO, 11, 235) is outside             
                         our detection window.                                                   Msn1993a
             MKT  13     Aa,Ab: Data from lunar occultation, spectroscopy, and Mark III                  
                         astrometry are combined by Torres et al. to generate orbital elements.  Trr1997c
                         Distance and component masses and absolute magnitudes are derived from          
                         these elements.                                                                 
                         Period is fixed for the Armstrong et al. (2006) orbit. The resulting    MkT2006 
                         component masses are 2.15 +/- 0.12 Msun and 1.87 +/- 0.11 Msun.                 
                         Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                         astrometric data. Derived component masses are 2.03 +/- 0.87 and                
                         1.78 +/- 0.76 Msun.                                                     Ren2010 
                         Aa,Ab: Combined spectroscopic/astrometric solution, using data from             
                         Mark III interferometer plus high-resolution spectroscopy from ELODIE,          
                         HERMES, and CfA. Torres et al. (2011) determine an orbital parallax of  Lmp2011 
                         20.90 +/- 0.14 mas and component masses 2.86 +/- 0.06 and 2.16 +/-              
                         0.02 Msun. Effective temperatures for both components are 7800 +/-              
                         170K, absolute magnitues are 0.33 +/- 0.03 and 1.44 +/- 0.03 mag.               
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 4.46 +/- 0.29, 3.81, and 2.00 Msun, respectively.  Mlk2012 
             MCA  15     Ba,Bb:The primary of 04286+1558 was found to be the B component of              
                         physical pair 04287+1552; systems were merged.                                  
                         the 1 Tau = 77 Tau. Hyad (vB 71). Physical companion to the 2 Tau.              
                         A spectroscopic, occultation, and interferometric binary.                       
                         First detected as an occultation binary by White.                       Wit1979 
                         1979.698, 1979.857:  possible third component                           Heg1983 
                         This is a long period interferometric companion in addition to the              
                         spectroscopic component suggested by Griffin & Gunn (1977) to have a    Grf1977d
                         period of about 16 years.  An estimate of Delta m = 0.76 was made by    Dmb1991 
                         Dombrowski (1991).                                                      Msn1993a
                         Masses and distance of the 2 Tau are derived from spectroscopic                 
                         elements, adopting astrometric elements from Pan et al. (1992)          MkT1992e
                         Combined spectroscopic/astrometric solution by Torres et al. (1997).    Trr1997c
                         Distance (from relative proper motions and orbital parallax of the 2            
                         Tau) 47.6 +/- 1.9 pc, masses 2.91 +/= 0.88 and 1.31 +/- 0.14 Msun.              
                         Ba,Bb : New spectroscopic solution determined by Griffin.               Grf2012b
                         Ba,Bb: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                         4.14 +/- 0.35 and 2.88 Msun, respectively.                              Mlk2012 
             BPMA  7     BC: [PM2000]  171052 + [PM2000]  171309.                                Gvr2010 
04288+1617   BPMA  8     [PM2000]  171281 + [PM2000]  171421.                                    Gvr2010 
04289+3022   STF 548     AB: B=HIP 20907 is bluer than A, below the MS. A is 1.7mag above. But           
                         they are physical: CPM, parallax, same RV! Primary is SB1, P=460.7d.    Tok2001 
                         A,B have same RV (Tokovinin & Gornya 2001), both rotate fast            Tok2014d
04290+1610   HU 1080     Hyad (VB 75); RV possibly variable, as noted by Wilson (1948).          WOC1948 
                         The spectroscopic solution of this 14697-d pair determined by Griffin.  Grf2012b
                         B is also a close 21.3-d pair.                                                  
04290+1338   SIG   2     LP 475-855. Spectral types M7.5, M9.5. Probable Hyades member.                  
                         Estimated orbital period 86 +20/-19 yrs.                                Sig2003 
04292-1206   LDS3591     NLTT 13376/13372                                                        Chm2004 
04293+1733   HD  28394   Hyades vB 77.  The 238.9-day SB of Griffin et al. (1985) lies outside   Grf1985b
                         our detection window.                                                   Msn1993a
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Griffin et al. (1985).                                                  Grf1985b
04294+2701   KON   3     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M6.0          Kon2007b
04294-3335   HJ 3652     Primary is CT Eri, a Beta Lyr type eclipsing binary, P = 0.63420d.      Zas2012 
04295+2617   SMN  11     Measure of 1990.25 made by triangulation of multiple measures and was           
                         in a red filter.                                                                
                         AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
             WHT   2     AC: Primary is the Orion-type variable FW Tau. Multi-epoch astrometry           
                         by Kraus et al. (2014) confirm the AC pair is co-moving, and estimate           
                         mass of the companion at 10 +/- 4 Mjup for a system age of 1-5 Myr.     KsA2014 
             HER   8     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04295+1752   BGH   2     LDS 2244. Variable, V921 Tau. B is +17@  734.                                   
                         HJL1035.                                                                HJL1986 
04295+0025   BAL 972     RST 5206.                                                                       
04296+0350   BAL2121     J 2725.                                                                         
04297+2633   HAT   6     AB: Additional notes may be found in Herbig (1962).                     Her1962 
                         DI Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
             ITO  13     BC: B component is the Orion-type variable DH Tau = HBC 38. Colors of           
                         both B and C are consistent with T Tauri stars. The B component has a           
                         lower effective temperature than A (2700-2800K, vs 3580K), and is               
                         redder. The stars are probably early and late M stars; mass of the              
                         companion is estimated at 30-50 Mjup.                                   Ito2005 
                         Kraus et al. (2014) estimate mass of the companion at 18 +/- 4 Mjup.    KsA2014 
04298-0949   LDS3592     NLTT 13393/13392                                                        Chm2004 
04299+2607   HER   9     Aka IQ Tau. Additional notes may be found in Herbig (1962).             Her1962 
04300+8320   HR 1304     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Prieur et al. (2006).                                                   Pru2006 
04300-6955   OGL 193     LMC157.7.150   + LMC157.7.333                                           Pli2012 
04301+1814   JOY   2     A RW Aur-type variable, UX Tau.                                         Her1962 
04301+1538   STF 554     80 Tau. Hyad. Star A is SB1, P = 30.5d                                  Hei1981e
                         Spectral types and masses of components assigned by ten Brummelaar et           
                         al., based on adaptive optics observations.                             TtB2000 
04302+3516   TTH   1     HBC 40 = LkHA 101. Herbig Ae/Be star imaged at multiple wavelengths             
                         shows evidence of a companion at ~180 mas to the East-Northeast of the          
                         primary. Derived physical parameters for A and B for three possible             
                         distances are:                                                                  
                            160pc: L/Lsun =  1300 and  340   R/Rsun = 1.9 and 1.0                        
                            340pc: L/Lsun =  5900 and 1500   R/Rsun = 4.1 and 2.1                        
                            800pc: L/Lsun = 30000 and 8500   R/Rsun = 9.7 and 5.0                Tth2002 
04302-0303   PRB   2     Primary is WD 0427-03 = NLTT 13402, secondary is LP 655-33. Possible            
                         CPM pair, according to Probst (1983).                                   Prb1983 
04302-6753   TOK  85     HIP 20998. Not observed, but J-K=2.92 for B in the 2MASS PSC, hence             
                         optical.                                                                Tok2011a
04303+1950   PAT  10     Noted as a probable SB in                                               Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         Member of the Hyades (vB 81) and "probable SB" according to Griffin et  Grf1988 
                         al. (1988). This WDS pair PAT 10 was resolved by speckle.               Tok2012a
                         The spectroscopic solution of this 4023-d pair determined by Griffin.   Grf2012b
04306+1612   LDS2246     Hyades vB 82. A is possibly variable. B is BD+15@640.                           
                         The primary was noted as a possible occultation binary by Peterson      Pts1981a
                         et al. (1981).                                                          Msn1993a
                         HJL1036.                                                                HJL1986 
04306+1545   HD  28545   Hyades vB 182.  The 358.4-day SB of Griffin & Gunn (1981) is outside    Grf1981d
                         our detection window.                                                   Msn1993a
04306+1542   BUP  62     81 Tau = LDS2247. Hyades vB 83.  B is BD+15@638.                                
                         AB: HJL1037.                                                            HJL1986 
             ARN  36     The CPM B companion with rho = 161".8 is outside our detection window,          
                         as are C and D.                                                         Msn1993a
                         D component is primary of 04309+1547 TDS2876. Pair does not appear to    .      
                         be physical, so systems not merged.                                             
04306+1344   HD  28556   Hyades vB 84. A CPM companion with rho = 111".9 lies far outside our            
                         detection window with a large Delta m of 5.8.                           Msn1993a
04306+1343   BUP  63     83 Tau.                                                                         
04307+2601   SMN  12     Measure of 1990.77 made by triangulation of multiple measures and was           
                         in a red filter.                                                        Smn1992 
04307-1627   HJ 3653     B is BD-16@879.                                                                 
04308+1609   PAT  11     Hyades. The 0".3 binary PAT 11 was not resolved by speckle. The GCS did         
                         not detect RV variability despite large scatter of 4.8 km s-1 in their          
                         three measures.                                                         Tok2012a
04309+2442   SMN  13     ZZ Tau. Sfr2003 astrometry for 1995.081 and 1996.124 was based on               
                         interpolation of one-dimensional data by Simon.                         Smn1996a
                         The first ZZ Tau orbit by Schaefer et al. (2006) gives range 1994-1999  Sfr2006 
                         for T, 0.35-0.88 for e, 115-134 for i, 111-129 for Omega, 268-336 for           
                         omega.  Values of P and a are lower limits.  The second orbital                 
                         solution includes a lunar occultation measure by Simon et al. (1995).   Smn1995 
                         Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                         mass of 0.83 +/- 0.16 Msun.                                             Sfr2014 
04309+1547   TDS2876     D component of 04306+1542. ARN  36AD does not appear to be physical,            
                         so systems not merged.                                                          
04309-0849   KO    2     CPM pair; A = LP 655-23 (spec early M), B = 2MASS J0430516-084901               
                         (M8.0V). Mean separation (1953-2000) 0.328 +/- 0.004 arcmin. Data               
                         sources: Palomar Sky Survey red (1953.2), UK Schmidt blue (1982.8), UK          
                         Schmidt red (1985.9), 2MASS (1998.7), DENIS I (1998.9), UK Schmidt              
                         near-IR (2000.0). Masses of components estimated at 0.26 +/- 0.04 and           
                         0.086 +/- 0.004 Msun.                                                   Cab2007b
                         A known component of the wide binary Konigstuhl 2AB with a separation           
                         of 20" (Caballero 2007), 2MASS J04305203-0849193 is single closer in,   Cab2007b
                         in the AstraLux images.                                                 Jnn2012 
04310+7724   MLR 461     Also known as TDS 142.                                                          
04310-6911   OGL 194     LMC156.6.7     + LMC156.6.6                                             Pli2012 
04311+0647   STT  84     HJL  61.                                                                HJL1986 
04311-4522   TOK 208     Possibly triple. The new companion at 1".6 should not produce RV                
                         variability by 3.8 km s-1.                                              Tok2012a
04312+5858   STI2051     A is an astrometric binary. B (mag. 12.44, 8", DC) is a white dwarf,            
                         in slow retrograde motion about the mass-center. A very large proper            
                         proper motion brought this pair close to a 13th magnitude star which            
                         was measured as the C component by Pauwels & Lampens.                   Pws1993 
                         Also known as HDS 584.                                                          
04312+0621   LDS9171     Old LDS6171.                                                                    
04313-6959   OGL 195     LMC157.7.2247  + LMC157.7.2249                                          Pli2012 
04314+4001   STF 552     H N  44.                                                                MEv2010 
04314-0934   GAL 372     Object #136 in Gallo's original list.                                   Gal1914 
04314-1339   STF 560     B is BD-13@905.                                                                 
04315+1706   SAR   3     HBC 392 = V1074 Tau. SB2.                                               Sar1998 
                         Member of Taurus-Auriga molecular cloud.                                Dae2015 
04316+1743   HD  28634   This is a 2.31-year spectroscopic binary, according to Griffin et al.   Grf1985b
                         (1985).                                                                 Msn1993a
             vA 627      VVO 394. Hipparcos astrometric solution adopted some elements from the  HIP1997d
                         orbit of Griffin et al. (1985). Hyad.                                   Grf1985b
                         Perturbation orbit by McArthur et al. (2011) is based on HST FGS        AST2011 
                         astrometry, plus radial velocities from Griffin et al. (1985). Derived  Grf1985b
                         masses are 0.83 +/- 0.05 and 0.42 +/- 0.05 Msun.                                
04316-7037   OGL 196     LMC158.1.29    + LMC158.1.122                                           Pli2012 
04317+2330   POU 458     LDS 886 = LDS1173.                                                              
04317+1814   HER  10     AB: Additional notes may be found in Herbig (1962).                     Her1962 
04317+1538   WOR  16     The A component is a known Hyad.                                                
             LDS1174     The C component may or may not be a physical companion, possibly                
                         sharing CPM only as a member of the cluster.                                    
04318+2424   CHN   3     Formerly known as LEI  15.                                                      
04319-0851   HJ 2234     B is BD-09@917.                                                                 
04320+5355   STF 550     1 Cam. A spectroscopic binary.                                                  
                         AB: H N  67.                                                            MEv2010 
04320+1822   CHN   4     Formerly known as LEI  16.                                                      
                         AB: Additional notes may be found in Herbig (1962).                     Her1962 
             HER  11     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04320-6939   OGL 197     LMC157.5.2454  + LMC157.5.2477                                          Pli2012 
04322+3630   AG   80     ALI 293.                                                                        
04322+1820   KSA 107     Primary is variable star V827 Tau.                                              
04322+1757   MSR   1     HBC 397 = V1075 Tau.                                                    Msr2005 
04323+2422   KON   4     Estimated masses 0.07 and 0.06 Msun. Primary spectral type M6.5         Kon2007b
04323-6918   OGL 198     LMC156.7.3411  + LMC156.7.3620                                          Pli2012 
04324+0128   HDO 307     Aka BAL 1273.                                                           Hei1983a
04325+2420   HAT   7     Additional notes may be found in Herbig (1962).                         Her1962 
04325+2044   RED   6     1996.0902  RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers possible binary.                Red1997 
04325+1732   LEI   3     Aa,Ab: GG Tau.                                                                  
                         Tamazian (2002) solution includes mass determination based on an        Tam2002 
                         estimated distance.                                                             
                         Aa,Ab: Kohler (2011) derives orbits both coplanar and not coplanar              
                         with the disk; only his "most plausible" orbit is tabulated in the              
                         orbit catalog. Elements are as follows: P = 403 +67/-32 y, a = 0".429,          
                         i = 132.5 +1.0/-2.5 deg, Omega = 131 +13/-8 deg, e = 0.44 +0.02/-0.03,          
                         T = 2463400 +1470/-5420, omega = 19 +9/-10.                             Koh2011 
             CHN   5     AB: formerly known as LEI   3.                                                  
             DIF   1     Ab1,Ab2: Di Folco et al. estimate spectral types for Ab1 and Ab2 of M2V         
                         and M3.5V, respectively. Assuming the close pair is coplanar with the           
                         outer diskof the system, the stars were separated by 5.1AU in Dec 2012. DiF2014 
04326+2628   GIC  48     LDS1176 = G008-040/G039-021.                                                    
                         NLTT 13455/13456                                                        Chm2004 
                         HD 283702. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
04326-0313   H 6  64     H VI 64. Probably a variable of Delta Scuti type,                               
                         DZ Eri. B is BD-03@810.                                                         
04327+2553   GHE  11     Aa,Ab: Measure of 1990.77 made by triangulation of multiple measures            
                         and was in a red filter.                                                Smn1992 
             JOY   3     AB: A RW Aur-type variable, UZ Tau.                                             
                         Measure of 1990.77 made by triangulation of multiple measures and was           
                         in a red filter.                                                        Smn1992 
                         AB: Additional notes may be found in Herbig (1962).                     Her1962 
04327+1855   DAE  26     V1203 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04327+1803   SAR   4     HBC 403 = V1076 Tau.                                                            
04328+1600   CHR 152     This is probably the spectroscopic system found by Griffin et al.       Grf1988 
                         (1988) to have a period in excess of 15 years.                          Msn1993a
                         The spectroscopic solution of this 9377-d pair determined by Griffin.   Grf2012b
04329+0007   LDS 121     BC: NLTT 13492/13491 = LSPM J0432+0006. Law et al (2008) derive a       Law2008 
                         distance of 16.5 +8.2/-2.7 pc and a projected separation of                     
                         76.2 +38.7/-11.8 AU. Estimated spectral types are M4.5 and M5.5.                
04330-3817   BU  747     RZ Cae, Algol (EA) type eclipsing binary, P = 2.486955 d.               Zas2011 
04331+2410   GHE  13     Ab1,Ab2: Second and third Schaefer et al. (2006) orbits for Elias 12    Sfr2006 
                         Na-Nb include a lunar occultation measure by Simon et al. (1995)        Smn1995 
                         Schaefer et al. (2012) derive spectral types, Teff, luminosities, and           
                         masses for the Aa, Ab1, and Ab2 components (assuming a distance of              
                         140pc for M and L) as follows:                                                  
                            Aa:  K7       4060K  1.05 +/-0.20 Lsun  1.040+/-0.016 Msun (Mtotal)          
                            Ab1: M2       3560   0.447+/-0.058      0.564+/-0.018                        
                            Ab2: M2-M2.5  3560   0.356+/-0.038      0.476+/-0.017                Sfr2012 
                         Aa,Ab: V807 Tau. Young member of Taurus-Auriga molecular cloud.         Dae2015 
             HAT   9     AB: Additional notes may be found in Herbig (1962).                     Her1962 
             GHE  12     Ba,Bb: GH Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04331-1208   STF 564     The pair GAL 145 is identical                                           Hei1983a
04331-4646   SKF1205     The pair also show matching radial velocities, but primary is a SB1.    TrC2006 
04332+2434   SAR   5     HBC 405 = V830 Tau.                                                             
04332-6829   OGL 199     LMC155.5.3403  + LMC155.6.576                                           Pli2012 
04333+6847   LDS9172     Old LDS6172.                                                                    
04333+5921   TOR   7     Formerly known as PAN   4.                                                      
04333+5248   MLR 695     Aa,Ab: Also known as HDS 591.                                                   
             ES 2607     B is BD+52@844.                                                                 
04333+2505   LDS5190     old LDS6173.                                                                    
04334+4304   SHJ  44     57 Per. STTA 50 = H 6  99.                                                      
04335+7232   HJ 2228     AB: A is a spectroscopic binary.                                                
             LDS1595     AC: Initially merged with AB under mistaken belief was same pair.               
04335+1801   STF 559     H N 132.                                                                MEv2010 
04336+2610   GHE  14     Aa,Ab: IS Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04336+2421   POU 460     AB: Haro 6-22. Both components variable (A: 13.9-15.5, B: 14.1-16.1)            
                         according to Wenzel (1957 Nach. astr. Zentralst. 11,28)                 Her1962 
                         A is GK Tau. B is GI Tau.                                                       
04336-6249   HJ 3670     B is CPD-63@343.                                                                
04337+1824   DAE  27     V1323 Tau.                                                              Dae2015 
04337+1752   CHN   7     Formerly known as LEI  17.                                                      
                         HN Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04338+1451   rho Tau     Hipparcos astrometric solution assumes circular orbit (e = omega = 0);  HIP1997d
                         Hyades VA 725 = vB 95.  1.337-year SB according to Abt (1965).          AbH1965 
04339-0644   BU  881     46 Eri. A is variable EH Eri, P = 3.8d, small amplitude.                        
04340+1510   CHR  17     This rapidly moving system within the wide binary ADS 3317 is probably  Grf1988 
                         the spectroscopic system with P ~13 yr found by Griffin et al. (1988).  Msn1993a
                         New spectroscopic solution determined by Griffin.                       Grf2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.34, 1.66, and 0.95 Msun, respectively.             Mlk2012 
04340-5503   B  2092     alp Dor. Hyad (vB 96).                                                          
                         High mass-sum, illustrative solution only, speckle/spectroscopic orbit          
                         needed, cf. Griffin et al. (1988).                                      Grf1988 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 5.51 +/- 1.51, 4.25, and 2.69 Msun, respectively.  Mlk2012 
             HJ 3668     AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
04342+2612   SMN  14     Measure of 1990.77 made by triangulation of multiple measures and is            
                         in a red filter.                                                        Smn1992 
04343+1830   SAR   6     HBC 407 = V1077 Tau.                                                            
04344+6928   HJ 1145     Aka TDS2898.                                                            Skf2016a
04344+1630   OL  107     The ES pair formerly listed at 04350+1631 (= ADS 3313)                          
                         is identical to this pair.                                              Hei1980a
04345-6859   OGL 200     LMC156.4.9     + LMC156.4.130   + LMC155.1.775                          Pli2012 
04345-6958   OGL 201     LMC157.2.3089  + LMC157.2.3113                                          Pli2012 
04346-6948   OGL 202     LMC157.3.2891  + LMC157.3.2890                                          Pli2012 
04346-7015   OGL 203     LMC151.5.4     + LMC151.5.38    + LMC151.6.4891                         Pli2012 
04348+3206   SEI  49     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
04349-7651   HJ 3691     B is CPD-77@176.                                                                
04350-1246   GAL 373     Object #143 in Gallo's original list.                                   Gal1914 
04352+1822   SAR   7     TAP 51  = V1078 Tau.                                                            
04352-0944   STF 570     B is BD-10@958.                                                                 
                         H 3 100.                                                                MEv2010 
04353+2254   KSA 108     Primary is variable star FF Tau.                                                
04353+2232   HER  23     HAT  11.                                                                        
04354+1045   RED   7     Identification with GCS2 uncertain.                                             
                         1996.8130  RHy ID and coordinates from Reid (1992).                     Red1992 
                         LP ID from Luyten et al. (1981).                                        Luy1981 
                         Candidate Hyades member; Reid considers definite binary.                Red1997 
04356+2408   HRM   1     AB = DCH  56. IRAS 04325+2402.                                                  
04356+1206   TOK  17     Hyades vA 771.                                                                  
                         Primary is 1.9d SB2. Estimated period of visual pair 400y.              Tok2006 
04357+2411   CHN   8     Formerly known as LEI  19.                                                      
04357+1953   L     4     First resolved by Lewis in 1902, this system was unconfirmed for        GrO1932A
                         several decades despite numerous attempts, notably those of Aitken              
                         with the 36inch between 1910 and 1922. In the ADS, Aitken concluded     A__1932b
                         "It is very doubtful whether the star is double". The system was                
                         subsequently removed from the WDS, until its resolution by Prieur et            
                         al. over 90 years after its discovery.                                  Pru2002b
04357+1010   CHR  18     Aa,Ab: 88 Tau. A is an Alpha CVn-type variable, and spectroscopic               
                         binary, now resolved by speckle interferometry.                                 
                         B is BD+09@606.                                                                 
                         1997.071: Absolute quadrant determined by triple-correlation                    
                         techniques                                                              Pru2002b
             88 Tau      Lane et al. (2007) combine PHASES astrometry with speckle and radial    Lne2007 
                         velocity data to derive an orbit for the Aa,Ab components of the                
                         nearby sextuple 88 Tau, as well as the Aa1,Aa2 and Ab1,Ab2 subsystems.          
                         The parallax of the system is determined at 0".01973 +/- 0".00034,              
                         with semimajor axes for Aa,Ab; Aa1,Aa2; and Ab1,Ab2 of 12.17 +/- 0.17,          
                         0.0689 +/- 0.0012, and 0.0997 +/- 0.0021 AU, respectively. Other                
                         derived quantities for the four components are as follows:                      
                                Star     Mass (Msun)        M_K (mag)      Spec Type                     
                                Aa1    2.06  +/- 0.11     0.69 +/- 0.26      A6m                         
                                Aa2    1.361 +/- 0.073    2.20 +/- 0.28      F5V                         
                                Ab1    1.069 +/- 0.069    2.31 +/- 0.27      G2-3:V                      
                                Ab2    1.057 +/- 0.068    2.00 +/- 0.27      G2-3:V                      
             SHJ  45     STTA 52.                                                                        
                         AB: H 6  31.                                                            MEv2010 
04358-6655   OGL 204     LMC152.7.209   + LMC152.7.891                                           Pli2012 
04359+2352   KOH  15     V1324 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04359+2254   LEI  21     Primary is variable star HP Tau.                                                
04359+1631   BU  550     alp Tau = 87 Tau = Aldebaran. A is an unclassified variable.                    
             STFB  2     AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         Incorrectly listed as STFA  2.                                                  
             STFA  2     AC: H 6  66.                                                            MEv2010 
04359-0332   LDS9174     Old LDS6174.                                                                    
04360-0337   STF 571     AB: H 3  95.                                                            MEv2010 
04361+5525   HIP  21433  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Tokovinin et al. (1994). They derived component masses 0.88 and 0.24    Tok1994c
                         Msun and an estimated semimajor axis of 28.68 mas.                      Ren2013 
04362+0814   A  1840     Observations suggest eccentricity >0.80 and period 150-200y.            Mlr1956a
                         Star C (mag. 9, 6") is probably physical.                                       
04363+5502   RAO  35     Triple, consisting of a 2.6 day spectroscopic binary (Gorynya &                 
                         Tokovinin 2014 MNRAS 441, 2316) and the Robo-AO and 2MASS companion at          
                         5".7. The field is crowded and PM(A) is small. Our photometry places B          
                         slightly above the MS. The star is young and active according to                
                         Guillout et al (2009 A&A 504, 829) and we retain B as likely physical.  Rbr2015d
04363+4722   S   451     STTA 51. B is BD+47@1012.                                                       
04363-0321   BUP  64     nu Eri = 48 Eri. A is a Beta CMa-type variable.                                 
04363-6655   OGL 205     LMC152.7.23    + LMC152.7.88                                            Pli2012 
04364+3413   HU  610     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Baize (1961).                                              Baz1961b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.70 +/- 1.07, 2.11, and 0.95 Msun, respectively.             Mlk2012 
04365-0559   LDS9175     Old LDS6175.                                                                    
04365-0611   LDS 843     Aka LDS9175.                                                                    
04366+1930   LDS3597     The primary is a BY Draconis-type variable.                                     
04366+1845   RUC   4     RZ Tau. Spectral type of resolved companion M3-5V or possibly later.    Ruc2007 
04367+4116   58 Per      Wyller orbit rejected from Fourth Orbit Catalog                         Wye1957 
                         ("not confirmed by subsequent observations")                            Wor1983 
04367+4105   STF 563     H 3  65.                                                                MEv2010 
04367+1155   LDS1181     Hyades vB 210.                                                                  
                         NLTT 13608/13606                                                        Chm2004 
04367-6733   OGL 206     LMC153.7.3072  + LMC153.7.3092                                          Pli2012 
04368+2708   GIC  49     LDS1180 = G008-044/G039-027 = GJ 171.2AB. A component is the variable           
                         V833 Tau = Melotte 25 301.                                                      
                         NLTT 13601/13599                                                        Chm2004 
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
04368-6205   HJ 3679     A is a long-period variable, R Dor.                                             
04372+3108   KOH  16     V961 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04372+1108   GIC  50     LDS1182 = G083-024/G083-023.                                                    
04372-6658   OGL 207     LMC152.7.3126  + LMC152.7.3127                                          Pli2012 
04373+1748   BPM 101     [PM2000]  178584 + [PM2000]  178531.                                    Gvr2010 
04373-6853   OGL 208     LMC155.1.4867  + LMC155.1.5999                                          Pli2012 
04373-6905   OGL 209     LMC149.7.8     + LMC149.7.35    + LMC149.5.668                          Pli2012 
04374+0034   STTA 53     B is BD+00@801.                                                                 
                         Pair appears in an appendix list, not part of the discoverer's                  
                         regular numbering sequence.                                                     
                         SHY 465. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
04375+1509   CHR 153     1991.9021: Reprocessing of archival speckle data have confirmed this            
                         already strong detection and have shown a change in theta of 15 deg in          
                         2.7 yr.  CHR 153 cannot be the 2-yr  spectroscopic system of Griffin    Grf1988 
                         et al. (1988). In the Hyades.                                           Msn1993a
                         The preliminary orbital solution is clearly in error as the visual      Ole2003b
                         companion shows only linear motion. It can be another member of the     Hrt2012a
                         Hyades or a wide pair in projection. The acceleration could be          Hrt2012a
                         produced by the 1.8 yr SB companion.                                    Tok2012a
                         This is not the 734.2-d spectroscopic binary of Griffin but a more      Grf2012b
                         distant companion.                                                              
04376-0228   WAL  32     After analysis of proper motions, radial velocities, etc. conclude              
                         that A (= 51 Eri) and C (= GJ 330) comprise a wide physical binary and          
                         are members of the young bet Pic moving group. Distance is ~30pc and            
                         estimated orbital period is ~60,000y; pair form a very fragile system.  Fgl2006 
                         C component is GJ 3305; A and C are members of bet Pic moving group.    Zuc2001b
             BU   88     AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             KAS   1     Ca,Cb: Better known as GJ 3305, this binary is part of the beta Pic             
                         moving group (Zuckerman et al. 2001), and is also bound to 51 Eri in a  Zuc2001b
                         wide orbit (Feigelson et al. 2006) with a projected separation of 66".  Fgl2006 
                         The binarity of GJ 3305 was first reported by Kasper et al. (2007),     Kas2007b
                         and has been observed with AstraLux on several occasions.               Jnn2012 
                         Ca,Cb: Montet et al (2015) derive a combined spectroscopic/astrometric          
                         orbital solution, yielding masses 0.67 +/- 0.05 and 0.44 +/- 0.05               
                         Msun, luminosities 0.112 +/- 0.007 and 0.043 +/- 0.005 Lsun, and an             
                         age of 37 +/- 9 Gyr.                                                    Mtt2015 
04379-6701   OGL 210     LMC152.2.1     + LMC152.2.31                                            Pli2012 
04379-6915   OGL 211     LMC149.7.39    + LMC149.7.80                                            Pli2012 
04380-1302   STF 576     B is BD-13@938.                                                                 
04381+1457   LDS5582     LDS6138.                                                                        
04382+2813   BEU   6     GJ 3304 = G039-029.  Daemgen et al. (2007) derive a distance of 14.5    Dae2007 
                         +/- 3.8 pc, a separation of 11.4 +/- 3.4 AU, and a predicted orbital            
                         period of 76 +36/-35 yr. Spectral types are M4.0 +/- 0.5  and M4.5 +/-          
                         0.5; masses are 0.23 +0.10/-0.07 and 0.20 +0.07/-0.05 Msun.                     
                         Estimated age 60-300 Myr; masses 0.28 +/- 0.06 and 0.19 +/- 0.05 Msun;          
                         a ~13.4 AU.                                                             Jnn2014 
04382+1603   PAT  12     Aa,An. CPM companion (rho = 140".5) is outside our detection window.    Msn1993a
04382+1602   BUP  65     89 Tau.                                                                         
04382+1231   BUP  66     Hyades vB 104. 90 Tau. A is a spectroscopic binary.                             
                         Two CPM companions (rho = 44" and 120") fall outside detection window.  Msn1993a
             MRN   2     Aa,Ab: Marion et al. (2014) estimate the companion to this Hyades               
                         member as K4V.  Assuming a face-on, circular orbit with a semi-major            
                         axis of 11.1 mas (0.52 AU), the minimum period would be ~84d.           Mrn2014 
04382-1315   TOK 660     Resolved using ANDICAM2. PM(A) is small, B is considered physical from          
                         photometry and low crowding                                             Tok2014d
04382-1418   KUI  18     53 Eri.                                                                         
04384+2611   ITO   6     AC: Itoh et al. (2008) estimate that if the AC pair is physical, the            
                         H-band magnitude of C suggests a mass of order 1 Mjup. Followup                 
                         astrometry and spectroscopy is needed to confirm its companionship.     Ito2008b
04385+2656   STF 572     AB: One component is a spectroscopic binary.                                    
04385+2611   SMN  15     Measure of 1990.77 made by triangulation of multiple measures                   
                         and is in a red filter.                                                 Smn1992 
04385+1752   BPM 102     [PM2000]  179567 + [PM2000]  179474.                                    Gvr2010 
04386-0921   TOK 387     HIP 21265 is an X-ray source and an SB2 according to GCS (only one              
                         observation). It is resolved here at 56mas, which corresponds to a              
                         period of ~5yr.                                                         Tok2015c
04387-6822   OGL 212     LMC148.5.112   + LMC148.5.706                                           Pli2012 
04388+2147   JNN 262     G 8-48. Estimated age 300-1000 Myr; masses 0.12 +/- 0.04 and 0.10 +/-           
                         0.03 Msun; a ~21.9 AU.                                                  Jnn2014 
04388-2702   TOK 661     CA: Resolved using ANDICAM2. Tuc-Hor moving group. PM(C) is small,              
                         physical from ptm only.                                                 Tok2014d
04388-7015   OGL 213     LMC151.4.44    + LMC151.4.45                                            Pli2012 
04389+1406   HD  29461   Hyades vB 106.  This is SB with P ~ 10 yr according to Griffin et al.   Grf1988 
                         (1988).                                                                 Msn1993a
04389+1406   MET  41     This optical companion cannot be 3760d spectroscopic binary of Griffin  Grf2012b
04389-1207   HDS 599     Cvetkovic et al. (2014) derive spectral types A1 and  F2, masses 2.28           
                         and 1.56 Msun. Dynamical parallax is 15.50 +/- 0.75 mas.                Cve2014 
04390+2149   LDS1183     NLTT 13673/13674                                                        Chm2004 
04391+0752   BUP  67     B is BD+07@680.                                                                 
04392+2553   TMR   1     IRAS 04361+2547.                                                                
04393+3331   JNN 263     Estimated age 1000-10000 Myr; masses 0.32 +/- 0.16 and 0.20 +/- 0.10            
                         Msun; a ~2.6 AU.                                                        Jnn2014 
04393+2221   LKCA 15     Sallum et al. (2015) resolve three planetary companions to LkCa 15.             
                         Companion b has a best-fit orbital semi-major axis 14.7 +/- 2.1 AU,             
                         that of companion c is 18.6 +2.5/-2.7 AU. Companion d is only seen in           
                         the L' band, so less information can be gleaned.                        Sll2015b
04393+1555   STFA 11     A: sig 2 Tau = 92 Tau. A is a spectroscopic binary.                             
                         B: sig 1 Tau = 91 Tau. B is BD+15@665, SB and occultation binary.               
04394-6938   OGL 214     LMC150.4.33    + LMC150.4.139                                           Pli2012 
04395-1141   GAL 374     Object #147 in Gallo's original list.                                   Gal1914 
04395-4507   I  1489     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.49 +/- 0.82, 1.60, and 0.79 Msun, respectively.             Mlk2012 
04396-2115   BU 1236     AC: SHY 467. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04397+0952   GIC  51     LDS1184.  AB = G083-028/G083-029 = GJ 9162AB.                                   
04397-6722   OGL 215     LMC153.3.3746  + LMC153.3.4025                                          Pli2012 
04399+5305   BU 1043     3 Cam. A is an eclipsing binary of the W UMa-type.                              
04399+1940   RED   8     1996.0929  RHy ID and coordinates from Reid (1992). Candidate Hyades    Red1992 
                         member; Reid considers possible binary.                                 Red1997 
04400+5328   BU 1295     2 Cam.                                                                          
                         The high-eccentricity solution for AB by Valbousquet (1980) is          Val1980b
                         questioned by Heintz (1962) on grounds of a mass discrepancy.           Hei1962 
                         The equinox-1900 position was incorrectly given as 04320+5310 in                
                         McAlister & Hendry (1982).                                              McA1982d
             STF 566     A is the D component of 04404+5328.                                             
04400+3534   HJ  681     ALI 64.                                                                         
04400+2556   KON   5     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M5.75         Kon2007b
04403-6924   OGL 216     LMC149.2.6     + LMC149.2.26                                            Pli2012 
04404+5328   D     4     AD: D component is primary of 04400+5328BU 1295AB. AD not physical, so          
                         systems not merged.                                                             
04404+1631   CHR 154     1991.9021, 1993.2045: The spectroscopic orbit for HD 29608 (Griffin et  Grf1985b
                         al. 1985) is that of a much closer system, not the companion to this            
                         Hyades star observed and confirmed here.                                Msn1993a
04404-1940   STN   9     54 Eri. A semiregular variable, DM Eri. No very positive observations           
                         as a visual double. Needs speckle.                                              
04406-4152   HDO 190     AB: alp Cae. A is a Delta Scuti-type variable.                                  
                         AB: Physical/optical nature undefined.                                  Ehr2010 
04407+2519   KON   6     Estimated masses 0.15 and 0.08 Msun. Primary spectral type M5.5         Kon2007b
04407-2812   TOK 209     Resolved with NICI, uncertain measure. Not resolved with speckle.       Tok2012a
                         Direct motion by 16deg since first resolution at Gemini on 2011.80;             
                         estimated period is 15 yr.                                              Tok2013b
04408-3951   RSS   5     This previously uncataloged double star was a Hipparcos double entry            
                         system.  The first measure is determined from the individual positions          
                         listed by Rousseau et al.                                               Rss1996 
04408-6741   OGL 217     LMC146.8.31    + LMC146.8.30                                            Pli2012 
04409+0058   STF 583     AB: H 2  81.                                                            MEv2010 
04410-6935   OGL 218     LMC150.4.7439  + LMC150.4.8170                                          Pli2012 
04413+3242   JNN 264     Estimated age 300-1000 Myr; masses 0.54 +/- 0.04 and 0.40 +/- 0.06              
                         Msun; a ~58.9 AU.                                                       Jnn2014 
04414+2715   KOH  20     V1328 Tau.                                                              Dae2015 
04413+2054   LWR   5     V834 Tau                                                                        
04415-4328   Anon        EQ 0439-4333. ID as EQ 0439-4333 is uncertain, as it was based on a             
                         Simbad search using epoch-1950 coordinates 043955-433318 from White et  Whi1991 
                         al. (1991).                                                                     
04416-4302   WHI   6     Possibly resolved.                                                      Whi1991 
04417+2302   KSA  29     Primary is of spectral type M8.5 and shows evidence of a circumstellar          
                         disk and active accretion. The Ab companion is estimated as type                
                         M9.5-L0, mass 5-10 Mjup. Todorov et al. (2010) also resolved the B              
                         component into a 0.23" pair.                                            Tod2010 
04418+2658   KOH  21     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04419-6714   OGL 219     LMC146.5.3639  + LMC146.5.3827                                          Pli2012 
04421+2523   LEI  24     The measures and component designations of the Ba and Ca pair were              
             GHE  15     assigned incorrectly and were correctly re-assigned 5/22/02. The                
                         designations LEI  24Ba <---> GHE  15Ca were flipped and the                     
                         designation LEI  25Aa became LEI  24Aa.                                         
04422+3731   STF 577     CfA: SB? Not clear if it is A or B.                                     Tok2014d
04422+2257   MCA  16     Aa,Ab: tau Tau = 94 Tau. Occultation binary and short-period SB.                
                         Hough suspected duplicity due to a slow occultation. Finally resolved           
                         by McAlister in 1980.                                                   McA1983 
                         1983.9337, 1983.9391: Interferometric observations are incompatible     Jef1963 
                         with the large delta m reported by Jeffers et al. (1963).               Bnu1984 
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 12.44 +/- 4.14, 7.48, and 6.92 Msun, respectively. Mlk2012 
             S   455     STTA 54 = H 6   7.                                                              
04422+0259   A  2424     Position angles uncertain.                                                      
04423+8103   LDS1596     NLTT 13589/13587                                                        Chm2004 
04423+0932   TOB 369     Aka GWP 610.                                                                    
04423-2943   LDS 126     NLTT 13802/13804                                                        Chm2004 
04423-6657   OGL 220     LMC145.7.3953  + LMC145.7.4003                                          Pli2012 
04426+2516   KSA 111     Primary is variable star DP Tau.                                                
04427-2147   LDS3608     NLTT 13805/13809                                                        Chm2004 
04428-7030   OGL 221     LMC144.7.6     + LMC144.7.441                                           Pli2012 
04429+1843   LDS2266     BC: HJL1038.                                                            HJL1986 
                         RV(A)=+14.5, not Hyades member! On Lick RV program.  B is SB2,          HJL2012b
                         P=56.445d (Halbwachs et al. 2012)                                       Tok2014d
04430+5712   A  1014     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                         the orbit of Baize (1958).                                              Baz1958 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.48, 2.37, and 1.10 Msun, respectively.             Mlk2012 
04431+3356   HJ  348     Also known as STF 580.                                                          
04431-0725   A   476     KP Eri, Algol (EA) type eclipsing binary, P = 7.447126 d.               Zas2011 
04431-6844   OGL 222     LMC148.2.7773  + LMC148.2.7774  + LMC148.2.7791                         Pli2012 
04432-5436   TOK  87     HIP 21960.                                                                      
04432-6723   OGL 223     LMC146.3.22    + LMC146.3.117                                           Pli2012 
04433+5931   A  1013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.20 +/- 2.40, 3.42, and 1.82 Msun, respectively.             Mlk2012 
04434+1558   BPM 103     [PM2000]  183754 + [PM2000]  183745.                                    Gvr2010 
04436-0848   STF 590     55 Eri. B is a Delta Scuti-type variable, DW Eri., BD-09@969. Spectral          
                         type F4IIIpSr. Both components are spectroscopic binaries.                      
                         H 3  99.                                                                MEv2010 
04441+1739   LDS2268     NLTT 13828/13829.                                                               
04441+0205   HL    1     This is a measure of HL 04441+0204 and A 3006 04440+0204                        
04442-6959   OGL 224     LMC143.8.7618  + LMC143.8.8368                                          Pli2012 
04443+2017   KOH  22     V1205 Tau.                                                              Dae2015 
04444+1952   KOH  23     V1333 Tau.                                                              Dae2015 
04444+1109   BUP  68     Hyades vB 111.  A may be variable. Two CPM companions with rho = 74".7          
                         and rho = 10".0, both outside our detection window.                     Msn1993a
04445+3953   COU1524     Primary is eclipsing binary V592 Per (period 0.71572 day).              Zas2010 
04448-6946   OGL 225     LMC143.6.9637  + LMC143.6.10050                                         Pli2012 
04449+2717   KOH  24     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04449+1757   LDS2271     LDS5590.                                                                        
04450+1605   BPM 104     [PM2000]  185037 + [PM2000]  185149.                                    Gvr2010 
04453-6943   OGL 226     LMC143.6.9561  + LMC143.6.9815                                          Pli2012 
04454+2955   NI   12     BVD  47.                                                                        
04454+2421   POU 477     Also known as GRV 215.                                                          
04454-5949   FIN  89     A is the Mira-type variable, T Dor.                                             
04454-7006   OGL 227     LMC143.8.7703  + LMC143.8.7822                                          Pli2012 
04455-0512   HJ   27     B is BD-05@1021.                                                                
04455-2226   DON  77     CD-22@1801.                                                                     
04455-7018   OGL 228     LMC144.3.38    + LMC144.3.177                                           Pli2012 
04458+3515   ES 2410     ALI 65.                                                                         
04459+1911   AG  311     B is BD+18@714.                                                                 
04460+1616   BPM 105     [PM2000]  185978 + [PM2000]  185928.                                    Gvr2010 
04460+1142   BUP  69     A is possibly a spectroscopic binary.                                           
04464+4221   COU2031     1985.740:  The separation of this partially resolved pair was                   
                         calculated under the assumption of zero or otherwise known magnitude            
                         difference.                                                             Tok1985 
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 2.53 +/- 0.35, 2.85, and 1.05 Msun, respectively.             Mlk2012 
                         Combined spectroscopic/interferometric orbit. Resulting masses are              
                         1.75 +/- 0.08 and 1.32 +/- 0.08 Msun. Spectral types are estimated as           
                         G3IV and F6V.                                                           Doc2014i
04465+1528   HD  30246   Hyades vB 142.                                                          Grf1988 
                         Noted as a SB in Griffin et al. (1988).                                 Msn1993a
04465+1528   MET  42     This optical companion cannot be 989.8-d SB of Griffin.                 Grf2012b
04466+4002   BRT2206     ALI 1040.                                                                       
04468+1745   PAT  15     This pair is noted as a slow spectroscopic binary in Griffin et al.     Grf1988 
                         (1988).                                                                 Msn1993a
04468+1744   LDS1187     LDS5601.                                                                        
04468+0901   PAT  16     This pair is a spectroscopic binary with P ~ 7 yr according to Griffin  Grf1988 
                         et al. (1988).                                                          Msn1993a
                         Hyades. The 0".1 pair PAT 16 was not resolved with speckle; its                 
                         estimated period is 7 yr.                                               Tok2012a
                         The spectroscopic solution of this 2446-d pair determined by Griffin.   Grf2012b
04468-2618   VIG   6     The B component appears to be a faint background star.                  Vig2012 
04469+1700   DAE  35     DQ Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04469-1117   JNN  28     2MASS J04465175-1116476 has a companion that has not yet been tested            
                         for common proper motion. Since the brightness and color match                  
                         expectations, the system counts as an unconfirmed binary.               Jnn2012 
04469-4630   LDS9177     Old LDS6177.                                                                    
04469-6036   TOK 388     First resolution of HIP 22229 at 0".043, dI=1.2. The measure is                 
                         uncertain, but the elongation is confirmed with 2-ms exposure and is            
                         not seen in other observed stars, so it is not caused by vibration.             
                         This is a triple system containing an eclipsing binary AL Dor (Algol)           
                         with an eccentric orbit (Bulut & Demirkan, 2007 MNRAS, 378, 179). The           
                         separation implies an orbital period of the outer system ~5yr.          Tok2015c
04470-6954   OGL 229     LMC143.2.264   + LMC143.2.1526                                          Pli2012 
04472+2027   KU   85     Also known as STF 593.                                                          
04472+1332   LDS1188     LDS5603.                                                                        
04472-1715   ARG  11     B is BD-17@951, spectrum G2/3V.                                                 
04476+1816   PAT  17     This pair is a spectroscopic binary with P >5 yr according to Griffin   Grf1988 
                         et al. (1988).                                                          Msn1993a
                         The spectroscopic solution of this 4822-d pair determined by Griffin.   Grf2012b
04476-0534   GRE   1     IRAS 04451-0539 = PDS 11.                                               Gre1992 
04477+4014   A  1545     Primary is V593 Per, a Beta Lyr type eclipsing binary, P = 3.2437d.     Zas2012 
04477-6945   OGL 230     LMC143.3.10488 + LMC143.3.11560                                         Pli2012 
04478+3643   GAA   2     AW Per. This Cepheid is an SB with an orbital period of ~40 yr. First           
                         discovered by Miller & Preston (1964 PASP 76, 47), it took several              
                         years to derive the first orbit from radial velocity data (Evans 1989           
                         AJ 97, 1737). It is likely that this companion is itself a binary, as           
                         argued by Evans and by Evans et al. (2000 AJ 120, 407), because the             
                         magnitude difference between the Cepheid and its companion is not               
                         consistent with equal masses and predictions from evolutionary tracks.          
                         Unfortunately, Gallenne et al. (2015) note they did not have enough             
                         angular resolution and sensitivity to detect this third companion. The          
                         properties of the brightest companion were studied based on IUE                 
                         spectra by Evans (1994 ApJ 436, 273; 1995 ApJ 445, 393), who found its          
                         spectral type to be B8.3V. This is in agreement with their detection            
                         with a flux ratio f = 1.22 +/- 0.30%, i.e., a spectral type in the              
                         range B6-B9V (using d = 853 pc from a P-L relation and K = 4.63 mag     .   
                         for the Cepheid). They estimate the companion mH = 9.6 +/- 0.3 mag      .     
                         (using for the Cepheid at theirgiven phase mH = 4.84 +/- 0.01 mag from  .     
                         Monson & Pierce (2011 ApJS 193, 12). Massa & Evans (2008 MNRAS 383,             
                         139) also determined the angular separation of the component for                
                         another epoch, which will allow an estimate all the orbital elements,           
                         (see also Gallenne et al. 2013 EAS Pub. Ser. 64, 197). Gallenne et al.          
                         (2015) derived a maximum sensitivity limit at 3sigma of 0.62%, i.e.,            
                         dmH> 5.5 mag, so can therefore exclude any additional components with   .     
                         a spectral type earlier than B9V.                                       GaA2015 
                         Spectroscopic binary orbit with P = 13954d determined.                  Grf2016c
04478+2925   CHN  10     Additional notes may be found in Herbig (1962).                         Her1962 
                         DS Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04478-3043   LDS3620     NLTT 13968/13970                                                        Chm2004 
04479+2755   KOH  26     V1337 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04479+1902   LDS3619     LDS5604.                                                                        
04480+5645   BU 1387     4 Cam.                                                                          
04480+5307   STF 587     H 4  73.                                                                MEv2010 
04480-4154   TOK 490     AD: D component is the primary of 04490-4128 RST1285.                           
04481+7810   MLR 464     Also known as TDS 148.                                                          
04483-7036   OGL 231     LMC137.8.142   + LMC137.8.140                                           Pli2012 
04485+1056   HJ  684     CD: Also known as STF 601.                                                      
04486+1748   STF 598     HJL  62.                                                                HJL1986 
04486-6648   OGL 232     LMC138.6.5554  + LMC138.6.5870                                          Pli2012 
04487+2106   HD 284787   Hyades vB 115.  This pair is a spectroscopic binary SB with P ~ 4 yr    Grf1988 
                         according to Griffin et al. (1988).                                     Msn1993a
04487-6830   OGL 233     LMC141.4.9     + LMC141.4.22                                            Pli2012 
04488+5308   STF 586     Same position, and in field of, STF 587.                                        
04488-6124   JSP  60     AC, 180deg, 8" 14th mag noted.                                          Hln1966 
04488-6902   OGL 234     LMC142.4.13828 + LMC142.4.14777                                         Pli2012 
04489-6951   OGL 235     LMC136.7.1220  + LMC136.7.2869                                          Pli2012 
04491+1408   BPM 106     [PM2000]  189268 + [PM2000]  189301.                                    Gvr2010 
04491+0513   STTA 55     B is BD+04@755.                                                                 
04492+2448   HD 283882   Hyades vB 117.  The 11.93-day SB of Griffin & Gunn (1978) is outside    Grf1978b
                         our detection window.                                                   Msn1993a
04492-3505   TOK 210     The companion is close to the detection limit, but it is considered to          
                         be real. The measurement is uncertain.                                  Tok2012a
                         Retrograde motion by 5deg since resolution on 2011.78; period is about          
                         20y. Measurements are uncertain because of large dm. The "blue" color           
                         of the companion is caused by measurement error.                        Tok2013b
04492-6736   OGL 236     LMC139.2.2     + LMC139.2.1                                             Pli2012 
04492-6901   OGL 237     LMC142.4.13837 + LMC142.4.14005                                         Pli2012 
04493+3235   CHR  19     A spectroscopic binary with P = 7.05d.                                          
                         Fekel et al. (2013) derive a new spectrosopic orbit with P=7.051d and           
                         e (adopted) = 0.0. Estimated masses are 1.95 and 1.2 Msun. Differences          
                         between early DAO and more recent data suggest the possibility of a             
                         3rd component in the system. It in uncertain whether this corresponds           
                         to the never-confirmed speckle companion, however.                      Fek2013a
04493+2934   RAS  18     Magnetic star; primary is A0 silicon star. Companions A8-F0.            Ras2014 
                         LSC  31. V473 Tau.                                                              
04494+4828   JNN 265     G 81-34. Estimated age 30-300 Myr; masses 0.27 +/- 0.14 and 0.18 +/-            
                         0.09 Msun; a ~13.5 AU.                                                  Jnn2014 
04497+1554   HJ 3261     96 Tau. BU  551A,BC.                                                            
04498+0658   STT 560     pi 3 Ori = 1 Ori. Obviously an optical pair. A spectroscopic binary             
                         and possibly a variable of Delta Scuti type.                                    
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
04499+2230   LDS9178     Old LDS6178. G085-017. See Allen et al. (2000) for information on       AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 14005/13996                                                        Chm2004 
04500+2230   KOH  27     V1341 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04501+6632   STF 584     May be H 2  92.                                                         Bu_1906 
04501-6635   OGL 238     LMC138.4.30    + LMC138.4.63                                            Pli2012 
04502-0413   SLW 172     GWP 619.                                                                Tob2012b
04502-3113   B  1474     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.59 +/- 1.09, 1.93, and 0.91 Msun, respectively.             Mlk2012 
04503+0657   H 6  83     H VI 83.                                                                        
04503-4119   HJ 3697     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
04503-6649   OGL 239     LMC138.3.160   + LMC138.3.161   + LMC138.3.468                          Pli2012 
04504+1712   HD  30676   Hyades vB 119                                                           Grf1988 
                         This pair is noted as a SB in Griffin et al. (1988).                    Msn1993a
04505+0103   A  2622     A premature orbit has been computed.                                            
04505-3834   GC 5916     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
04506+1505   CHR  20     Hyad (vB 120). Preliminary circular orbit, speckle/spectroscopic                
                         orbit needed, cf. Griffin et al. (1988).                                Grf1988 
                         1991.9023: This may be the spectroscopic system found by Griffin et             
                         al., but more observations are needed to determine the orbital motion.  Msn1993a
                         New spectroscopic solution determined by Griffin.                       Grf2012b
                         This is a Hyades binary for which Griffin (2012) published an SB2       Grf2012b
                         orbit. We combined his RVs with the speckle data, resulting in a very           
                         accurate period. The combined orbit corresponds to a mass sum of 2.1            
                         Msun and an orbital parallax of 22mas, in good agreement with the HIP2          
                         parallax of 23.69 +/- 0.87mas.                                          Tok2015c
04506-6711   OGL 240     LMC139.4.89    + LMC139.4.1334                                          Pli2012 
04507-4540   HJ 3699     old LDS6179.                                                                    
04508+1613   HD  30738   Hyades vB 121                                                                   
                         The 5.751-day SB of Griffin & Gunn (1978) is outside our detection      Grf1978b
                         window.                                                                 Msn1993a
04508-4013   I  1492     Variable, Y Cae.                                                                
04509+3746   TOK 249     Cmp? Crowded field (N*=81), small PM, hence B can be optical.           Tok2014d
04509-5328   DUN  18     iot Pic                                                                         
             SHY 172     AC: HIP  22531 + HIP  22562.                                                    
             SHY 173     BC: HIP  22534 + HIP  22562.                                                    
04511-2731   TOK  88     HIP 22538. The original Hipparcos gives parallax 13.9 mas. A is X-ray           
                         source 1RXS J045103.5-273115.                                           Tok2011a
04512+1104   BU  883     Hyad (vB 122).                                                                  
                         Mass-sum calls for sp subsystem, but RV-ampl <1km/s according to                
                         Griffin et al. (1988).                                                  Grf1988 
                         AO photometric analysis by ten Brummelaar et al. (2000) includes mass           
                         determination.                                                          TtB2000 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.58 +/- 0.49, 2.36, and 2.24 Msun, respectively.  Mlk2012 
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
04512-2213   BRT1378     CD-22@1851.                                                                     
04512-6843   OGL 241     LMC134.7.16981 + LMC134.7.17012                                         Pli2012 
04513-6804   FIN 362     Only one observation, with many negative results. Duplicity                     
                         questionable. Needs speckle.                                                    
04514+1850   BUP  70     97 Tau = LDS1190. A is a Delta Scuti-type variable, V480 Tau.                   
                         B is BD+18@742.                                                                 
04515+5550   LDS5615     relative motion of AB is 0.1"/yr, too fast. optical?                    Tok2014d
04515-3454   FIN 320     Appears to have completed a revolution if the quadrants are correct.            
                         Period about 40y.                                                               
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 4.50 +/- 1.29, 3.59, and 2.19 Msun, respectively.             Mlk2012 
                         Docobo & Andrade (2013) derive a dynamical parallax of 13.78 +/- 0.41           
                         mas and component masses 1.85 +/- 0.21 and 1.58 +/- 0.18 Msun. See              
                         paper for extensive notes on this system.                               Doc2013d
04515-6653   OGL 242     LMC138.3.7274  + LMC138.3.7555                                          Pli2012 
04515-6933   OGL 243     LMC136.5.13108 + LMC136.5.13830                                         Pli2012 
04516-6841   OGL 244     LMC134.7.20843 + LMC134.7.21738                                         Pli2012 
04518+3047   JOY   4     A is the RW Aur-type variable, UY Aur.                                  Her1962 
                         Hioki et al. (2007) calculate a period of 1640 +/- 90 yr and a total    Hio2007 
                         mass of 1.73 +/- 0.29 Msun.                                                     
04518+1339   BU  552     Hyad (vB 124).                                                          Wor1963a
                         The primary is 143d SB (Griffin et al. 1985).                           Grf1985b
                         The spectroscopic system of Griffin et al. would be too close for us            
                         to resolve by speckle interferometry.                                   Msn1993a
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Turner et al. (1986). They derived component masses 1.42 and 0.55 Msun  TrD1986 
                         and an estimated semimajor axis of 15.67 mas.                           Ren2013 
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.67 +/- 1.47, 2.30, and 1.00 Msun, respectively.  Mlk2012 
                         A faint component (about mag. 13, 45") is unobserved since 1906; its            
                         physical nature is unknown.                                                     
04519-3414   BVD  48     AC: SHY 470. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
04519-6058   JSP  62     CD-61@974.                                                                      
04519-6635   OGL 245     LMC138.4.6967  + LMC138.4.6968                                          Pli2012 
04521-6706   OGL 246     LMC138.1.8041  + LMC138.1.8261                                          Pli2012 
04525-3631   LDS9180     Old LDS6180.                                                                    
04526+4302   ES 1526     BC: BRT 111                                                                     
04526-2646   LDS3625     NLTT 14126/14125                                                        Chm2004 
04527-2546   TOK 662     With plx(A), B is on the MS, likely physical.                           Tok2014d
04527-6936   OGL 247     LMC136.4.307   + LMC136.4.140                                           Pli2012 
04527-7043   OGL 248     LMC137.1.262   + LMC137.1.650                                           Pli2012 
04531-0117   S   457     B is BD-01@743.                                                                 
04533+1401   BPM 107     [PM2000]  194282 + [PM2000]  194455.                                    Gvr2010 
04534-0925   RST4256     BRT 2834.                                                                       
04535-5551   LDS 131     See note to 05287-6527 SHY  27AD.                                               
04538-6831   OGL 249     LMC134.3.20577 + LMC134.3.20575                                         Pli2012 
04540-6943   OGL 250     LMC136.3.223   + LMC136.3.524                                           Pli2012 
04540-7022   OGL 251     LMC137.3.14145 + LMC137.3.18362                                         Pli2012 
04541+8125   MLR 490     Also known as TDS 152.                                                          
04541+6621   alp Cam     Fullerton (1990) presents high quality profiles that indicate the       Ful1990 
                         presence of line profile variations; his associated radial velocity             
                         measurements do not confirm any of the periods suggested by Zeinalov &          
                         Musaev (1986 SvAL 12, 125) and Musaev & Snezhko (1988 SvAL 14, 68).     Msn1998a
04542+4935   STF 603     AB: H N  77.                                                            MEv2010 
04543+0722   STF 612     HD 31208. See Allen et al. (2000) for information on metallicity,       AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: HJL  64.                                                            HJL1986 
04544-6720   OGL 252     LMC132.6.11391 + LMC132.6.12002                                         Pli2012 
04545-0314   RST5501     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 3.79 +/- 1.45, 3.77, and 1.20 Msun, respectively.             Mlk2012 
04547+1221   TOK 251     A is exoplanet host, P=466d. RV(A)=+12.1, not Hyades                    Tok2014d
04547-0257   J  1348     GCB 7. BRT 370.                                                                 
04548+1126   MCA  17     6 Ori.                                                                          
04549+1009   ENG  19     7 Ori = pi 1 Ori. B is BD+09@682.                                               
04549+0836   STT  90     V1834 Ori, Algol (EA) type eclipsing binary, P = 1.51058 d.             Zas2011 
04549-6934   OGL 253     LMC136.4.18656 + LMC136.4.18660                                         Pli2012 
04551+5516   BU 1187     5 Cam.                                                                          
04551+3535   MLB 923     Not found by Heintz at IDS position.                                    Hei1985a
04551-6718   OGL 254     LMC132.4.88    + LMC132.4.1271                                          Pli2012 
04552+1827   DAE  39     V1349 Tau.                                                              Dae2015 
04552-6656   OGL 255     LMC131.7.14509 + LMC131.7.14673                                         Pli2012 
04552-6908   OGL 256     LMC135.3.30074 + LMC135.3.30071                                         Pli2012 
04552-7923   HJ 3733     B is CPD-79@163.                                                                
04554-7109   OGL 257     LMC130.7.31    + LMC130.7.349   + LMC130.7.1118                         Pli2012 
04555+1711   BPM 108     [PM2000]  197155 + [PM2000]  197180.                                    Gvr2010 
04556+3018   MSR   3     HBC 426 = V396 Aur.                                                     Msr2005 
04557+1742   DAE  40     V1350 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04557-6637   OGL 258     LMC131.4.8     + LMC131.4.7                                             Pli2012 
04558+3033   BNS   1     HBC 78 = MWC 93 = AB Aur                                                        
04558-3100   LDS3628     NLTT 14212/14213                                                        Chm2004 
04558-6741   OGL 259     LMC132.1.137   + LMC132.1.297                                           Pli2012 
04558-7056   OGL 260     LMC130.6.29    + LMC130.6.186                                           Pli2012 
04559+0440   LDS9181     Old LDS6181.                                                                    
             EGN   4     Aa,Ab pair bound. Ab component is likely an early M dwarf with mass             
                         0.43 +/- 0.02 Msun                                                      Egn2007 
                         Aa,Ab: A is on Keck program, RV var.                                    Tok2014d
04560+3021   SFN   1     Aa,Ab: Steffen (2000, 2001) combined solutions each yield values for    Sfn2000 
                         the masses, as well as an orbital parallax.                             Sfn2001 
                         Simon et al. (2013) derive masses 0.86 +/- 0.11 and 0.55 +/- 0.05 Msun          
                         and distance 187.7 +/- 3.9 pc for this pre-MS binary.                   Smn2013 
             KSA  31     HBC 427 = V397 Aur.                                                     Msr2005 
04560-6938   OGL 261     LMC128.5.315   + LMC128.5.772                                           Pli2012 
04560-7040   OGL 262     LMC129.8.308   + LMC129.8.309                                           Pli2012 
04561-7116   OGL 263     LMC130.8.10926 + LMC130.8.11364                                         Pli2012 
04562+2554   GIC  52     G039-042/G039-041.                                                              
                         NLTT 14180/14179                                                        Chm2004 
04563+5206   STF 608     AB,C: HJL  65.                                                          HJL1986 
04563+2415   LDS6148     Also known as GRV 220.                                                          
04564+1331   BU  553     omi 2 Ori = 9 Ori                                                               
04564-0510   SHJ  48     62 Eri. B is BD-05@1093.                                                        
                         AB: H 6 106.                                                            MEv2010 
04566+0422   TOB9004     Measured as BAL2622 but actually an anonymous pair added here.          Tob2010 
                                                                                                 Dam2012 
04566-6629   DON  89     Variable.                                                                       
04566-7027   OGL 264     LMC129.7.22    + LMC129.7.188                                           Pli2012 
04567+3917   HU 1091     V560 Aur, Algol (EA) type eclipsing binary, P = 1.528311 d.             Zas2011 
04567-7106   OGL 265     LMC130.7.12419 + LMC130.7.12474                                         Pli2012 
04568+1825   BPM 109     [PM2000]  199012 + [PM2000]  199066.                                    Gvr2010 
04569-6721   OGL 266     LMC132.3.14233 + LMC132.3.14300                                         Pli2012 
04570+1716   BPMA  9     [PM2000]  199271 + [PM2000]  199591.                                    Gvr2010 
04570+1517   MET   4     Metchev & Hillenbrand say the C component is probably optical, based            
                         on proximity.                                                           Met2004b
04572+3838   ES 2338     ALI 780.                                                                        
04573+5345   D     5     7 Cam. A premature orbit has been computed for AB. The primary is SB1,          
                         P = 3.884 d (Lucy & Sweeney).                                           Lcy1971 
                         Drummond linear elements have been modified.                            Dru2014 
             STF 610     AB,C: Star C (mag. about 11.3, 26") may be physical.                            
04573+1524   HEI  38     KOH  36.                                                                        
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04573-7055   OGL 267     LMC130.6.14234 + LMC130.6.16118                                         Pli2012 
04574+0100   A  2624     Aa,Ab : Hipparcos identified the pair as a candidate for Hyades         HIP1998 
                         membership. However, it is not.                                         Grf1988 
                                                                                                 Grf2013c
04574+0100   SHY 471     AB: HIP  23044 + HIP  23266. B component = A component of 05003+0100.           
04575-2358   LDS3630     NLTT 14263/14262                                                        Chm2004 
04576+1356   BPM 110     [PM2000]  200066 + [PM2000]  200068.                                    Gvr2010 
04576-0545   STF 624     B is BD-05@1103.                                                                
04576-6950   OGL 268     LMC128.6.11701 + LMC128.6.11986                                         Pli2012 
04578+2357   BU 1045     99 Tau.                                                                         
04580-2248   I   473     CD-22@1917.                                                                     
04580-6735   OGL 269     LMC124.7.79    + LMC132.2.17928                                         Pli2012 
04581+0141   STF 622     A,BC: H 1  68.                                                          MEv2010 
04582+8015   OSO  18     GD 288. Not a common proper motion pair, based on comparison with               
                         POSS2 red plates                                                        Oso2004 
04582+2503   BU 1390     98 Tau. A is a spectroscopic binary.                                            
04582+1423   BPM 111     [PM2000]  201029 + [PM2000]  201109.                                    Gvr2010 
04584-6739   OGL 270     LMC124.8.20199 + LMC124.8.20752                                         Pli2012 
04585-2749   RST 117     CPD-28@715.                                                                     
04585-6834   OGL 271     LMC126.6.46772 + LMC126.6.46857                                         Pli2012 
04587-7053   OGL 272     LMC130.3.25    + LMC130.3.4226                                          Pli2012 
04588-7027   OGL 273     LMC129.2.10    + LMC129.7.17168                                         Pli2012 
04589+6435   GNO   1     Distance is estimated at about 10.5 +/- 1.4 pc, giving a projected              
                         component separation of ~5 AU. Estimated orbital period ~70 yr, for an          
                         assumed age of 1 Gyr.  Spectral types are estimates at T8.5 and T9;             
                         total system mass ~25 Mjup.                                             Gno2011 
04590+1433   SHJ  49     STTA 58 = H 5 113. B is BD+14@795. Probably same as BDS 2461, H V 57.           
                         AB: H 5  57.                                                            MEv2010 
04590-1623   BU  314     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.87 +/- 0.28, 2.66, and 2.36 Msun, respectively.  Mlk2012 
                         AB,C: Optical pair, based on study of relative motion of the                    
                         components using the method of apparent motion parameters.              Kiy2008 
04591+6322   HU 1090     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 12.31 +/- 4.18, 2.27, and 1.10 Msun, respectively.            Mlk2012 
04591+1123   BPM 112     [PM2000]  202364 + [PM2000]  202525.                                    Gvr2010 
04593+3753   STF 616     ome Aur = 4 Aur                                                                 
                         AB: H 2  14.                                                            MEv2010 
04595-4927   HJ 3715     Primary is VW Pic, a W UMa type eclipsing binary, P = 0.42576d.         Zas2012 
04595-6802   OGL 274     LMC125.6.10758 + LMC125.6.10639                                         Pli2012 
04595-6958   OGL 275     LMC128.2.17    + LMC128.2.402                                           Pli2012 
04596+3135   HO  222     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         However, radial velocity classifies this as not a Hyades member.        Grf2013c
                         The colors from Tycho photometry are also not consistent with a         Fab2000a
                         physical pair.                                                                  
04597+1555   BUP  73     Hyades vB 128                                                                   
                         A CPM companion with rho = 106".4 is outside our detection window.      Msn1993a
04597-6940   OGL 276     LMC128.4.12    + LMC128.4.92                                            Pli2012 
04598-1016   63 Eri      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                         Intermediate Astrometric Data with spectroscopic elements by                    
                         Vennes et al. (1998).                                                   Ven1998 
04599+5327   A  1303     A premature orbit has been computed.                                            
                         T corrected from 200.74 to 2000.74 by Ruymaekers & Nys (1995)           Ruy1995 
05001-6217   B  1942     Composite spectrum: G5/8III + F/G.                                              
05001-6953   OGL 277     LMC128.2.32346 + LMC128.2.32381                                         Pli2012 
05002+1811   GIC  53     LDS1198. G083-047/G083-048.                                                     
05003+3924   CHR 159     5 Aur.                                                                          
05004+6925   STF 606     B is BD+69@289.                                                                 
05005+0506   STT  93     Hyperbolic orbit by Janova (1966).                                      Jnv1966 
                         sigma = areal constant in the true orbit = 0.00576 arcsec^2/yr                  
                         q = periastron distance in the true orbit = 0".366                              
05006+0337   STF 627     B is BD+03@736.                                                                 
05007-0204   VIG   7     Optical/physical nature of the six faint companions (B-G) is undefined. Vig2012 
05007-6856   SKF1044     OGL 278. LMC126.1.9 + LMC126.1.100                                      Pli2012 
05008+3913   STF 621     Same as AG   83.                                                                
05008+3811   SEI  52     Secondary not seen on POSS plate; may be either variable star or flaw           
                         on AC Potsdam plate.                                                            
05009-7052   OGL 279     LMC130.4.19979 + LMC130.4.21083                                         Pli2012 
05010-6948   OGL 280     LMC128.3.14335 + LMC128.3.14552                                         Pli2012 
05012+3430   COU1229     Primary is V410 Aur, a W UMa type eclipsing binary, P = 0.36636d.       Zas2012 
05015+3733   BRT2207     ALI 523.                                                                        
05015-7107   OGL 281     LMC122.7.267   + LMC122.7.1784                                          Pli2012 
05016+6105   HU 1093     Primary is possible astrometric pair?                                   Tok2014d
05016-7056   OGL 282     LMC122.6.146   + LMC122.6.918                                           Pli2012 
05017+2640   A  1844     Masses and bolometric magnitudes are derived for the two components     Msn1999a
                         of this system by Maosn et al. (1999), based on assumed spectral types          
                         and available parallaxes.                                                       
                         Visual separations systematically too small.                                    
                         AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 1.83 +/- 0.31, 2.12, and 1.00 Msun, respectively.  Mlk2012 
             S   461     STTA 59 = STFA 12.                                                              
             BAG  21     Ca,Cb: SB2, P=186.28d                                                   Tok2014d
05017+2050   HU  445     Quadrant uncertain, Delta m at least 0.3.                               B__1963b
                         Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                         orbit of Baize (1957).                                                  Baz1957a
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.15 +/- 0.04, 1.78, and 1.05 Msun, respectively.             Mlk2012 
05020+4349   BU  554     AB: eps Aur = 7 Aur. Strand orbit rejected from Fourth Orbit Catalog    Str1959 
                         ("amplitude below noise level")                                         Wor1983 
             eps Aur     A is a enigmatic supergiant eclipsing system. Also a spectroscopic and          
                         eclipsing binary                                                        Fin1970b
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Heintz & Cantor (1994).                                                 Hei1994b
05020+0137   STF 630     A,BC: H 3  52.                                                          MEv2010 
05021+6910   BU  313     The AB component, BU 313 AB, originally in the BDS and IDS, was                 
                         removed by Worley following multiple unresolved observations. The new           
                         Hipparcos binary (AB), is almost certainly not the Burnham AB star,             
                         which was seen at 10", 250 deg, and had a Delta-M of 5.0.                       
                         AC: Burnham (BDS) notes 1874 observation made with 6-in telescope but           
                         says no 10" companion was found during subsequent searches with either          
                         the 36-inch or 40-inch.                                                 Bu_1906 
05022+3116   RUC   5     V402 Aur. Spectral type of resolved companion later than M5V.           Ruc2007 
05023-1932   LPM 201     NLTT 14407/14408                                                        Chm2004 
05023-5605   LDS 135     B is CPD-56@767.                                                                
                         Primary is SB1; Jenkins et al. (2010 A&A 515, 17) estimate P(Aa,Ab)             
                         ~6.5y, M2min=55 Mjup.                                                   Tok2014d
05023-6821   OGL 283     LMC125.1.12039 + LMC125.1.12040                                         Pli2012 
05024+1628   BPM 113     [PM2000]  207217 + [PM2000]  207230.                                    Gvr2010 
05024-6454   GLI  32     B is CPD-65@416.                                                                
05025+4105   MKT   6     zet Aur. Eclipsing binary (K4IB + B5V).                                         
                         This object was misidentified as rho Aur by McAlister (1978).           McA1978c
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Wright (1970).                                                          Wri1970 
                         Bennett et al. (1996) orbit is combined solution, using astrometry      MkT1996 
                         from the Mark III interferometer, spectroscopy from HST Goddard High            
                         Resolution Spectrograph, and published photometry to determine masses,          
                         radii, etc. Positions of component stars on theoretical H-R diagram             
                         are compared to current evolutionary models.                                    
                         Errors to individual measures are given as "error ellipses"; these              
                         values are tabulated below, together with filters used. The columns             
                         include date (BY), major and minor axes of the ellipse (in mas),                
                         ellipse orientation (deg), and filter effective wavelengths (nm):               
                              1989.7857   1.63    0.31    98.1   800,550,450                             
                              1989.7994   0.56    0.14    86.9   800,550,450                             
                              1989.8213   0.58    0.12    84.5   800,550,450                             
                              1989.8240   0.73    0.15    78.6   800,550,450                             
                              1989.8350   0.50    0.12    85.3   800,550,450                             
                              1989.9281   0.48    0.17    96.1   800,550,450                             
                              1989.9363   1.24    0.27    86.1   800,550,450                             
                              1990.7029   1.14    0.16   104.0   800,550,500                             
                              1990.8124   0.56    0.17    97.5   800,550,500                             
                              1990.8179   0.69    0.14    91.7   800,550,500                             
                              1991.7488   2.00    0.20   111.9   800,550,500                             
                              1991.7871   0.65    0.12    92.4   800,550,500                             
                              1991.8364   0.32    0.09    94.1   800,550,500                             
                              1991.9048   0.21    0.07    86.4   800,550,500                             
                              1992.0855   1.31    0.15    90.4   800,550,500                             
                              1992.0965   1.50    0.25    73.5   800,550,500                             
                              1992.7700   0.63    0.14    99.5   800,550,500                             
                              1992.7946   0.65    0.11    98.5   800,550,500                             
                              1992.7974   0.44    0.08   104.2   800,550,500                             
                              1992.8932   1.82    0.24   111.3   800,550,500                             
                              1992.9206   1.39    0.27    99.0   800,550,500                             
                              1992.9452   1.23   0.23    101.9   800,550,500                             
                         Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                         8.40 +/- 3.79 and 10.96 Msun, respectively.                             Mlk2012 
05025-2115   DON  91     Good period, indeterminate a/e/i, more obs needed!                      Hei1978c
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05027-3309   HJ 3718     B is CD-33@2076.                                                                
05028-4909   RST 120     AB: Physical/optical nature undefined.  Primary is eta 1 Pic.           Ehr2010 
             EHR   6     AC: Physical/optical nature undefined.                                  Ehr2010 
05028-7020   OGL 284     LMC121.6.34935 + LMC121.6.34941                                         Pli2012 
05029+1433   BPM 114     [PM2000]  208075 + [PM2000]  208110.                                    Gvr2010 
05031+4933   BU  315     ID uncertain. Listed as BD+49 1288 in ADS, but no obvious 10" pair at   A__1932a
                         those coordinates. X-coded measures of a 45" pair refer to a wide               
                         companion to BD+49 1288.                                                        
05031+2523   MSR   5     HBC 429 = V836 Tau.                                                     Msr2005 
                         Young member of Taurus-Auriga molecular cloud.                          Dae2015 
05031-6944   OGL 285     LMC120.6.45262 + LMC120.6.45347                                         Pli2012 
05033+2125   LAW  13     Ba,Bb: LSPM J0503+2122 = NLTT 14406. Law et al (2008) derive a          Law2008 
                         distance of 13.7 +6.5/-2.5 pc and a projected separation of                     
                         4.4 +2.3/-0.7 AU. Estimated spectral types are M4.5 and M5.5.                   
                         Ba,Bb: LP 359-186. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.03           
                         and 0.16 +/- 0.01 Msun; a ~8.3 AU.                                      Jnn2014 
05033-1722   B  2583     LPM 202. L 736-49.                                                              
05034+6027   S   459     bet Cam = 10 Cam. STTA 57 = H 6  36.                                            
05034-7104   OGL 286     LMC122.7.14740 + LMC122.7.14741                                         Pli2012 
05035+1449   BPM 115     [PM2000]  209034 + [PM2000]  208947.                                    Gvr2010 
05036+6305   STF 618     LDS 889. STTA 56. D is BD+62@721.                                               
                         AB: HJL  66.                                                            HJL1986 
05037-0232   J   307     Reality of BC is in doubt.                                                      
05037-6834   OGL 287     LMC118.6.42400 + LMC118.6.42472                                         Pli2012 
05038+1457   BPM 116     [PM2000]  209491 + [PM2000]  209477.                                    Gvr2010 
05039-6738   OGL 288     LMC124.1.32825 + LMC124.1.32850                                         Pli2012 
05042-6956   OGL 289     LMC120.7.16863 + LMC120.7.18028                                         Pli2012 
05043+4013   ES 1718     Espin incorrectly identified this pair as BD+40 1144 in 1919, but       Es_1919 
                         corrected this to +40 1158 in 1925. Error in transcribing to catalog;   Es_1925a
                         WDS designation originallyVIG   7 05041+4023, corrected when matched with      .
                         05043+4013TDS3056.                                                              
05043+2319   J  1816     POU 523.                                                                        
05043-6946   OGL 290     LMC120.6.17556 + LMC120.6.17583                                         Pli2012 
05044+6237   HU 1094     Stein measure 1901.3, 289@, 4.2", 9.5-9.9. For this position            A__1932a
                         Hussey finds no such pair.                                              Hu_1905b
05044-3529   JC    9     gam 1 Cae. The secondary is variable (IBVS 2736, 1985).                         
05044-6706   OGL 291     LMC115.8.111   + LMC115.8.177                                           Pli2012 
05045+1622   BPM 117     [PM2000]  210663 + [PM2000]  210510.                                    Gvr2010 
05045-2402   LDS3638     NLTT 14472/14466                                                        Chm2004 
05046+5852   STF 625     A,BC: H 2  53.                                                          MEv2010 
05047+7404   STT  89     Judged single by Hussey, Burnham, and Aitken, and not inserted in ADS.          
                         Rediscovered by Kuiper in 1935 (PASP 47, 230). Obvious in 1938.         Baz1942b
05047-0925   GAL 375     Object #161 in Gallo's original list.                                   Gal1914 
05047-2017   WHC   2     CPD-20@742.                                                                     
05049+1520   BPMA 10     [PM2000]  211239 + [PM2000]  211233.                                    Gvr2010 
05050-6740   OGL 292     LMC116.8.65    + LMC116.8.164                                           Pli2012 
05051+0608   HD 32662    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05053+6923   HJ 2244     B is BD+69@295.                                                                 
05054-6905   SKF1072     OGL 293. LMC119.5.40836 + LMC119.5.40603                                Pli2012 
05055-5728   SHY  22     HIP  23693 + HIP  23708.                                                        
05056+2304   STT  97     See long note in BDS. Single in 1889.                                   Bu_1906 
                         Recovered in 1976 by McAlister.                                         McA1978b
                         Primary is V1154 Tau, an Algol-type eclipsing binary, period 1.76788d.  Zas2011 
05056-7056   OGL 294     LMC122.3.16    + LMC122.3.89                                            Pli2012 
05057+0628   PAT  18     This pair is a spectroscopic binary with P ~ 2 yr, according to         Grf1988 
                         Griffin et al. (1988).                                                  Msn1993a
                         The spectroscopic solution of this 631.08-d pair determined by          Grf2012b
                         appears to be a closer pair.                                                    
                         Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                         It appears to match on grounds of proper motion and photometry but      Grf1988 
                         still appears slightly off based on radial velocities.                  Grf2013c
05061+5858   STFA 13     A: 11 Cam. B: 12 Cam =  BD+58@805. B is a spectroscopic binary,                 
                         P = 80.2d, spectrum K0III.                                                      
05062-6247   TOK  91     HIP 23742. ANDICAM confirms the 2MASS PSC photometry of B in K-band.            
                         B is well below the MS in the CMDs.                                     Tok2011a
05063+3738   ES 2339     Aka BRT2587 and ALI 528.                                                        
05063+3722   SEI  60     ALI 527.                                                                        
05064-1649   GAL 376     Object #164 in Gallo's original list. Aka POC9001.                      Gal1914 
05064-6700   OGL 295     LMC115.7.14821 + LMC115.7.14818                                         Pli2012 
05066-6830   OGL 296     LMC118.4.12    + LMC118.4.529                                           Pli2012 
05067+5136   BU 1046     9 Aur. A is a spectroscopic binary.                                             
             H 6  35     AC: H VI 35.                                                                    
05067+3748   SEI  61     ALI 529.                                                                        
05067+1427   GC 6239     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                         Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                         (2013). Periods match "tolerably well," other common elements less so.          
05067-6725   OGL 297     LMC116.6.12552 + LMC116.6.14377                                         Pli2012 
05068-0439   STF 642     66 Eri. A is a spectroscopic binary.                                            
05069-6718   OGL 298     LMC116.5.13203 + LMC116.5.16702                                         Pli2012 
05069-6728   OGL 299     LMC116.6.12514 + LMC116.6.14626                                         Pli2012 
05070+1650   HJ 3267     LDS1199. Possibly the same as STF 672.                                          
05070-3939   HJ 3725     B is CD-39@1789.                                                                
05071-7042   OGL 300     LMC121.1.12614 + LMC121.1.12789                                         Pli2012 
05074+2715   DOO  30     J 3259.                                                                         
05074+1839   A  3010     104 Tau.                                                                        
                         Two orbit solutions (Eggen 1956). Observations of this close pair       Egg1956 
                         are so scattered that both orbits are highly conjectural.                       
                         A measure on 1977.9196 was incorrectly attributed to ADS 3701 in                
                         McAlister & Hendry (1982); it actually belongs to ADS 4020.             McA1982b
                         Visual and speckle observations at 0".1 sep ruled out as spurious by            
                         constant RV (Duquennoy & Mayor 1991).                                   Duq1991 
                         Precise velocities are stable to better than 100 m/s over 388 days,     Nid2002 
                         so there are no "hot jupiters" and a 2-year period is excluded with     Tok2010b
                         high confidence.                                                                
                         104 Tau is a G4V dwarf at 16 pc resolved into equal components at 0.1"          
                         by R. Aitken in 1912. The WDS contains 16 resolutions of this pair.     A__1927a
                         Apart from Aitken himself, it has been resolved on multiple occasions           
                         by R.H. Wilson in 1934-1971, by W. Finsen (1953-1955) and by others,    WRH1941a
                         although in other instances those observers found it to be single.      Fin1953d
                         The measures suggest a near-circular orbit seen face-on with a semi-            
                         major axis on the order of 0.1" or 1.5 AU. Assuming a mass sum of 2             
                         Msun, the orbital period should be around 1.3 yr; in fact, two orbits           
                         with periods 1.19 yr and 2.38 yr were published by Eggen (1956). This   Egg1956 
                         binary should be an easy target for speckle interferometry at 4-m               
                         telescopes. It was observed 10 times from 1976.9 to 1980.7 with                 
                         speckle and, surprisingly, found unresolved on all occasions,                   
                         excluding any short-period orbits. Later, however, two measures were            
                         made by the author at a 1-m telescope with a phase-grating                      
                         interferometer. The first resolution in 1984.8 at 0.04" was tentative   Tok1985 
                         (below the diffraction limit), but the second in 1985.7 was secure,     Tok1988 
                         being an average of two observations. It was followed by the speckle            
                         resolution at 4-m telescope in 1988.17, after which the pair            Mca1993 
                         disappeared again. It was found unresolved in 2012.                     Tok2012b
                         The star is well studied. Two statistical surveys of binaries within            
                         25 pc consider it to be single (Duquennoy & Mayor 1991; Raghavan et     Duq1991 
                         al. 2010). Heintz & Borgman (1984) state that measures cannot be        Rag2010 
                         fitted by any orbit and conclude: "Although this alleged visual binary  Hei1984i
                         (ADS 3701) has three published orbits, it is probably spurious".                
                         Several independent RV studies have shown that this star is not a               
                         spectroscopic binary. Precise RVs measured by Nidever et al. (2002)     Nid2002 
                         are stable to better than 100 m s-1 over 388 days, excluding orbital            
                         periods from one to two years with high confidence. Data with lower             
                         precision show a constant RV of +21 km/s over many years (Duquennoy &           
                         Mayor 1991; Abt & Willmarth 2006; Raghavan et al. 2010). The star is    AbH2006 
                         located about 1m above the main sequence, supporting the thesis of an           
                         equal-component binary. If the orbit is seen face-on, the RV variation          
                         would be small, especially if the components are of equal brightness            
                         (blended lines move in opposite directions, the centroid stays                  
                         constant). However, the lines in this star remain narrow and the                
                         speckle non-resolution during 3.8 yr firmly excludes a face-on orbit.           
                         Remember that 104 Tau is bright (no identification errors possible)             
                         and that the components are supposedly equally bright, hence easy to            
                         resolve by speckle. If this star is single (as everything seems to              
                         suggest), we cannot dismiss its multiple resolutions with micrometer,           
                         eyepiece interferometer, and speckle as spurious; occasional image              
                         doubling (or at least elongation) must be real.                         Tok2012b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 0.65 +/- 0.09, 2.12, and 1.02 Msun, respectively.             Mlk2012 
                         In the WDS summary line this carries an "X" code (non double), but              
                         still retains all the historical measures.                                      
05074-6641   OGL 301     LMC115.4.42    + LMC115.4.508                                           Pli2012 
05076+1631   BPM 118     [PM2000]  215983 + [PM2000]  215874.                                    Gvr2010 
05076+0928   STT 561     AB: 16 Ori. A is a spectroscopic binary.                                        
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05076-7018   OGL 302     LMC121.3.45664 + LMC121.2.45533                                         Pli2012 
05076-8852   HJ 4047     1900: 06 56.4.                                                                  
05078+3024   JOY   5     RW Aur, prototype of its class.                                         Her1962 
05078+1622   BPM 119     [PM2000]  216289 + [PM2000]  216084.                                    Gvr2010 
05078-0505   BUP  74     bet Eri = 67 Eri. STF 647.                                                      
05079+6849   HJ 1152     BDS 2479 has an error of 30', making it identical with HJ 1152                  
                         (Van Biesbroeck).                                                       VBs1914 
05079+2142   S   466     105 Tau. B is BD+21@764. A is a spectroscopic and occultation binary.           
                         H 6 105.                                                                MEv2010 
05079+1519   BPM 120     [PM2000]  216579 + [PM2000]  216575.                                    Gvr2010 
05079+0830   STT  98     14 Ori. One component, probably the primary, is SB; the RV range in the         
                         combined light is 22 km/s.                                                      
                         According to Eggen, the system shares common proper motion with         Egg1963 
                         ADS 3712 = STF 643 (mags. 9.5-9.5, 3", K2), which is 6' distant.                
05080-2648   MUG  13     Spectral type of comoving secondary estimated as M4-5, mass 0.17 Msun.  Mug2014 
05080-6934   OGL 303     LMC120.4.70309 + LMC120.4.70525                                         Pli2012 
05081+3701   COU1530     Also known as HDS 673.                                                          
05081+2416   EDG   2     103 Tau. A is a spectroscopic and occultation binary.                           
             H 5 114     H V 114.                                                                        
05083+7538   JNN 266     G 248-32. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.15           
                         +/- 0.03 Msun; a ~3.1 AU.                                               Jnn2014 
05083-0840   STF 649     AB: H 4  43 = H N  46.                                                  MEv2010 
05084+5525   GC 6249     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05085+1418   LDS5662     LDS6166.                                                                        
05085-1036   GAL 377     Object #165 in Gallo's original list.                                   Gal1914 
05085-4113   HJ 3728     NLTT 14574/14573                                                        Chm2004 
                         HIP 23926. B = HIP 23923. A is above the MS, evolved (despite sp. type          
                         G3V). The pair was observed with NICI in 2010. Both A and B have large          
                         PM, PM(A)=(-77,+284). The original Hipparcos parallax of B is 8.5mas,           
                         obviously wrong. IRAS source.                                           Tok2011a
                         Moutou et al. (2011 A&A 527, A63): exoplanet around A, P~2800d +drift   Tok2014d
05085-7058   OGL 304     LMC114.6.224   + LMC114.6.480                                           Pli2012 
05087+3703   SEI  78     ALI 302.                                                                        
05087+1251   BPM 121     [PM2000]  218040 + [PM2000]  218004.                                    Gvr2010 
05087-6846   MLO  13     AC: Identification uncertain.                                                   
05088-6800   OGL 305     LMC117.3.18237 + LMC117.3.18886                                         Pli2012 
05090+1238   BPM 122     [PM2000]  218603 + [PM2000]  218372.                                    Gvr2010 
05092-6701   OGL 306     LMC115.2.14607 + LMC115.2.14813                                         Pli2012 
05093+0950   BUP  75     13 Ori. Hyades vB 130.                                                          
                         Two CPM companions with rho = 88".6 and rho = 168".0, both outside              
                         our detection window.                                                   Msn1993a
05094-6857   OGL 307     LMC111.5.43680 + LMC111.5.44857                                         Pli2012 
05096+2947   STTA 61     HJL1040.                                                                HJL1986 
                         SHY 474. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         AB: Primary is SB2, P=1469.4d (Halbwachs et al. 2012)                   HJL2012b
05097+1536   STT  99     15 Ori. Round (Hussey). May not be double.                                      
05097-7009   OGL 308     LMC113.5.47798 + LMC113.5.47799                                         Pli2012 
05098+2802   BU 1047     BC: Van Biesbroeck in 1953 noted "no evidence of change in 65 years."           
                         However, the pair is now apparently in rapid motion in a highly-                
                         inclined orbit.                                                         Wor1967b
                         BC. The star was noted as a spectroscopic binary by Griffin et          Grf1988 
                         al. (1988).                                                                     
                         Hipparcos identified the pair as a non-Hyades member, however, the      HIP1998 
                         results invesigating proper motion, photometry and radial velocity      Grf1988 
                         yield a more ambiguous finding. The jury is still out!                  Grf2013c
             STF 645     A,BC: HJL  67.                                                          HJL1986 
                         A,BC: H 3  90.                                                          MEv2010 
05099-6715   OGL 309     LMC116.4.13354 + LMC116.4.13836                                         Pli2012 
05100+4009   ES  169     Aka BRT 112.                                                                    
05100+3754   SEI  81     ADS 3729a.                                                                      
05100+1054   J   323     A is probably variable.                                                 J__1952 
05100-0704   STF 651     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05100-6722   OGL 310     LMC108.6.14    + LMC116.3.15651                                         Pli2012 
05101+2733   BGH  21     NLTT 14576/14572                                                        Chm2004 
                         HJL1041.                                                                HJL1986 
                         SHY 175. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                         high (near 100%) probability pair is physical.                                  
                         Secondary is SB1, P=2273.8d (Halbwachs et al. 2012)                     HJL2012b
05101-0204   BAL 296     1deg error in IDS led to similar error in WDS designation.                      
05101-2341   WSI 121     Both 2MASS J05100427-2340407 and J05100488-2340148 are binaries in the          
                         AstraLux images, so since they are separated by only 27" on the sky             
                         and have very similar proper motions (e.g. Roser et al. 2010), this is  Rsr2010 
                         likely a quadruple system in reality. Common proper motion remains to           
                         be confirmed for both of the close components.                          Jnn2012 
05101-6929   OGL 311     LMC111.8.8839  + LMC119.8.34937                                         Pli2012 
05101-7008   OGL 312     LMC113.5.48001 + LMC113.5.48018                                         Pli2012 
05102+1400   S   468     Also known as STF 650.                                                          
05102+0439   GWP 650     This is also known as V1396 Ori (ZZ Cet type var).                              
05103+3718   STF 644     One component is a spectroscopic binary.                                        
                         AB: H 1  45.                                                            MEv2010 
                         AB: Additional notes may be found in van den Bos (1963).                B__1963b
05103-0736   A   484     Position angles uncertain but near 130@-310@.                                   
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.20 +/- 0.18, 2.28, and 1.10 Msun, respectively.             Mlk2012 
05104+3741   SEI  84     Also known as ALI 531.                                                          
05105-1854   HJ 3727     CPD-19@760.                                                                     
05108-6716   OGL 313     LMC108.5.27    + LMC108.5.171                                           Pli2012 
05108-6740   OGL 314     LMC108.8.34    + LMC108.8.462                                           Pli2012 
05111+3718   BLL  13     B is BD+37@1072.                                                                
05112-0833   RUC  18     Multiple system including contact binary ER Ori. Pribulla & Rucinski            
                         (2006) estimate the mass of the contact pair at 2.510 Msun and the      Pbl2006 
                         minimum mass of the wider component at 0.93 Msun.                               
05113-6707   OGL 315     LMC107.8.492   + LMC107.8.1389                                          Pli2012 
05114-0101   BAL 297     Duplicity suspected by Baillaud but no measure.                         Bal1943 
05115+5305   HJ 2251     HJ gives position angle as 319.9@.                                              
05115-5519   HJ 3738     B is CPD-55@759.                                                                
05115-6753   OGL 316     LMC109.5.9247  + LMC109.5.9566                                          Pli2012 
05117+0031   HU   33     One component is a spectroscopic binary. Variable, V1085 Ori.                   
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 5.26 +/- 4.75, 9.35, and 2.57 Msun, respectively.             Mlk2012 
05119-0907   BUP  76     B is BD-09@1093.                                                                
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05119-4253   HJ 3734     LDS 137.                                                                        
05119-6830   OGL 317     LMC110.5.14459 + LMC110.5.14649                                         Pli2012 
05120+0650   STTA 62     B is BD+06@865.                                                                 
                         Pair appears in an appendix list, not part of the discoverer's regular          
                         numbering sequence.                                                             
05121-6511   TOK  92     HIP 24221.                                                              Tok2011a
                         A is SB without orbit, dRV=56.7                                         Nrd2004 
05123-1152   STF 655     iot Lep = 3 Lep                                                                 
                         AB: H 3  67.                                                            MEv2010 
05123-6708   LDS 140     Aka MLO  15.                                                                    
05126-1727   S   470     B is BD-17@1046.                                                                
05130+1242   BPM 123     [PM2000]  226150 + [PM2000]  226362.                                    Gvr2010 
05130-6941   OGL 318     LMC112.4.1006  + LMC112.4.1258                                          Pli2012 
05130-7028   JNN  32     There is a companion to 2MASS J05130132-7027418 in the AstraLux images          
                         which has a brightness and color that is consistent with a physical             
                         companion. It counts as an unconfirmed binary here, since it has not            
                         yet been tested for common proper motion.                               Jnn2012 
05131-5959   HJ 3743     Large parallax error in HIP! Primary is possible SB.                    Tok2014d
05133+0252   STF 654     rho Ori = 17 Ori. A is long-period spectroscopic binary, P = 1031.4d.           
                         A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                         Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                         Bertiau (1957).                                                         BFC1957 
                         AB: H N  21.                                                            MEv2010 
05134+3829   CHR 256     mu Aur = 11 Aur. Hipparcos stochastic double solution.                          
05134+2411   POU 586     POU 588.                                                                        
05134+0341   TOK 211     The 1".25 companion discovered with NICI is hardly the one that                 
                         produced the acceleration of 17 mas yr-2.                               Tok2012a
05135+1608   BPM 124     [PM2000]  227301 + [PM2000]  227493.                                    Gvr2010 
05135+0158   STT 517     Star C (mag. 13, 7") may be physical.                                           
                         Trajectory appears quasi-linear.                                        Mlr1956a
05135-5534   HJ 3742     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05136-7025   OGL 319     LMC113.3.8348  + LMC113.3.9695                                          Pli2012 
05137-0856   MLL   2     Aka BRT3264.                                                                    
05138-1641   GAL 378     Object #171 in Gallo's original list.                                   Gal1914 
05139+3958   HU 1100     ES 280.                                                                         
                         J  3306.                                                                Nsn2016 
05139-5648   HJ 9001     Previously known as HJ 5450a.                                                   
05140+5126   HU  821     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05140-6827   OGL 320     LMC110.4.6684  + LMC110.4.7756                                          Pli2012 
05142+2535   BRT3263     Originally published as BRT 136.                                        Brt1928 
05142-6701   OGL 321     LMC107.2.166   + LMC107.2.193                                           Pli2012 
05143+6949   STF 638     H 2  92.                                                                MEv2010 
05143+1953   KIR   1     AB. Using data from 2MASS and IRTF, Kirkpatrick et al (2001) derive     Kir2001b
                         spectral types K4V and M6V, conclude is probably a physical pair with           
                         separation 225 AU.                                                              
05143-1550   GJ 193      The acceleration is due to the 2.2 yr SB with estimated axis of 55 mas          
                         and q > 0.14. The companion is too faint and close to be resolved with          
                         NICI or speckle. The system is triple with a faint common-proper-motion         
                         (CPM) companion at 14".6.                                               Tok2012a
                         Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                         Intermediate Astrometric Data with spectroscopic elements by Nidever            
                         et al. (2002). They derived component masses 0.98 and 0.22 Msun and     Nid2002 
                         an estimated semimajor axis of 57.81 mas.                               Ren2013 
05143-1723   FEN   3     Aka OL  127.                                                                    
05145+1707   BPM 125     [PM2000]  229086 + [PM2000]  229142.                                    Gvr2010 
05145-0812   STF 668     bet Ori = 19 Ori = Rigel. The companion is a spectroscopic binary and           
                         suspected visual double, although it remains unconfirmed. Magnitudes            
                         of B and C very uncertain. Changed from IDS values (10.4 for B, C, and          
                         BC). AD pair first mentioned by Mitchel in 1846 (Sidereal Messenger,            
                         May 1847) but no astrometry included.  See extensive notes by Burnham.  Bu_1906 
             bet Ori     1975.631: Possible binary (450 and 656 nm).                             Bla1977a
                         1975.636: Possible binary (400, 500, 600, and 750 nm).                  Bla1977a
             STF 668     A,BC: H 2  33.                                                          MEv2010 
05145-6957   HJ 3754     B is CPD-70@376.                                                                
05146+7628   HU 1097     B may be variable.                                                              
05147+3707   SEI 115     Primary not seen on POSS plate; may be flaw on AC Potsdam plate.                
05147-0704   STF 667     H 1  54.                                                                MEv2010 
05149+3309   HJ  694     Aka HJ  361.                                                                    
05150+3813   BRT2208     ALI 788.                                                                        
05150+0108   OL   95     The south following of two faint stars.                                 B__1963b
05151-3639   HJ 3740     B is CD-36@2133.                                                                
05152+0826   STF 664     Same as CHE  79. Verified by DAL04.                                             
05152-1404   LDS3648     Luyten gives a separation of 130", but this appears to be a             Luy1978 
                         typographical error; if identification is correct, rho ~13"; this               
                         secondary corresponds to a high proper motion CPM companion.                    
05153+4710   A  1031     A 1998.8317 measure by Mason et al. (2001) was actually of STT 98.      Msn2001b
05154+3241   STF 653     14 Aur. A is the Delta Scuti-type variable KW Aur, and is also a                
                         spectroscopic binary.                                                           
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
                         AC: H 4  19.                                                            MEv2010 
05154-6700   OGL 322     LMC107.2.14205 + LMC107.3.195                                           Pli2012 
05155+2217   COU 158     108 Tau.                                                                        
05155-7001   OGL 323     LMC112.1.64694 + LMC112.1.64780                                         Pli2012 
05156+7857   LDS1604     NLTT 14588/14589                                                        Chm2004 
05156-6139   JSP9002     Previously known as JSP  71a.                                                   
05156-7049   OGL 324     LMC105.5.15    + LMC105.5.761                                           Pli2012 
05157-4927   GC 6457     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05160-7002   OGL 325     LMC103.8.32853 + LMC103.8.32837                                         Pli2012 
05160-7214   JAO   3     Also known as LHS1749. Parallax = 46.08 +/- 1.40 mas.                   Rdl2010 
05162-1121   CHR 225     It in uncertain whether the pair resolved here is the known G8III+A0V           
                         composite spectrum binary (Hoffleit & Warren 1991). The small apparent  Hof1991 
                         change in theta over the 4-year span between observations does not              
                         appear consistent with our estimated period of ~15 or so years;                 
                         however, the magnitude difference between the components is small, so           
                         we are unable to rule out a 180 deg quadrant flip or perhaps an                 
                         eccentric orbit.                                                        Hrt1996b
                         Docobo et al. (2014) use the spectroscopic elements of Carquillat &             
                         Prieur (2007), together with speckle data and the Hipparcos parallax,   Crq2007 
                         to derive the remaining orbital elements. The resulting masses are              
                         1.92 +/- 0.26 and 2.50 +/- 0.29 Msun.                                   Doc2014h
05163+3419   TRN  17     Aa,Ab is an AO artifact as per Turner and Roberts.                      Trn2010 
                         Aa,Ab: Additional notes may be found in Turner et al. (2008).           Trn2008 
             SEI 136     AB: AE Aur. Nova remnant, probably not double.                                  
                         The companion indicated by the Potsdam Astrographic catalogue is non            
                         existing. There's the remark: Very doubtful.                            VBs1960 
05164-1531   GAL 172     J  1468.                                                                J__1962a
05164-7124   OGL 326     LMC106.5.13    + LMC106.5.66                                            Pli2012 
05165+3635   SEI 137     SEI 138.                                                                        
05165-2106   DON  97     Variable dm?                                                            Hln1965 
05165-6947   OGL 327     LMC103.6.11600 + LMC103.6.11652                                         Pli2012 
05167+4600   ANJ   1     Aa,Ab: 13 Aur = alp Aur = Capella.  Composite spectrum; G5IIIe+G0III.           
                         AKA "The Interferometrist's Friend."                                            
                         Separations from Anderson (1920) have been modified as described in     AnJ1920 
                         Merrill (1922).                                                         Mrr1922 
                         Measures of Kulagin made by a transit interferometer; quadrants were            
                         flipped for all his measures.                                           Kul1970 
                         See discussion in Labeyrie et al. (1974).                               Lab1974 
                         Combined spectroscopic/interferometric orbit by Heintz (1974):          Hei1974a
                         P = 104.0237 d, a = 0.0547", eccentricity neligibly small. Ascending            
                         node revised according to Heintz's astrometry                                   
                         1969.1348: This position angle was incorrectly published as 303.0               
                         degrees in Balega & Tikhonov (1977).                                    Bag1977 
                         1978.915, 1978.929, 1979.082: Observations on these three dates                 
                         overlap in two papers by Koechlin et al. (1979, 1983), with only        Koe1979 
                         slight changes.  Values from the later paper are given in the catalog.  Koe1983 
                         1984.9309, 1985.1062, 1985.1994: Estimates of the position angle and            
                         angular separation are deduced from the elongation of the central               
                         speckle peak in the autocorrelation.                                    Bnu1986 
                         Colors and spectral types determined by speckle photometry are                  
                         given by Bagnuolo & Sowell (1988).                                      Bgn1988 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         Observations by Hummel et al. (1994) were made through narrow band      MkT1994 
                         filters centered at 800, 550, and 450 nm. Colors were derived from all          
                         1988-1992 data, so are listed at the mean epoch of 1991.9.  This paper          
                         also includes a new orbit. Finally, errors are given as "error                  
                         ellipses"; these values are tabulated below.  Columns include date              
                         (BY), major and minor axes of the ellipse (in mas), and ellipse                 
                         orientation (in degrees).                                                       
                              1988.7973     0.95     0.11      96.                                       
                              1988.8000     0.42     0.03      93.3                                      
                              1988.8028     0.22     0.03      85.7                                      
                              1988.8055     0.15     0.02      88.2                                      
                              1990.9411     0.09     0.02      86.6                                      
                              1990.9548     0.13     0.05      88.6                                      
                              1991.7159     0.73     0.08     124.1                                      
                              1991.7214     0.37     0.06     179.6                                      
                              1991.7241     0.23     0.05     156.5                                      
                              1991.7871     0.07     0.01      93.7                                      
                              1991.8364     0.07     0.02      91.6                                      
                              1991.8665     0.04     0.01      94.5                                      
                              1991.8857     0.06     0.02      88.4                                      
                              1991.8939     0.10     0.05     149.3                                      
                              1991.9021     0.16     0.05      77.9                                      
                              1991.9733     0.10     0.03      87.6                                      
                              1991.9870     0.09     0.02      77.5                                      
                              1992.0006     0.50     0.07      83.0                                      
                              1992.0417     0.24     0.05      73.4                                      
                              1992.0445     0.09     0.02      83.8                                      
                              1992.0691     0.25     0.05      74.6                                      
                              1992.0855     0.22     0.02      93.5                                      
                              1992.0965     0.10     0.02      78.5                                      
                              1992.7399     0.33     0.05     111.1                                      
                              1992.7426     0.42     0.04     118.5                                      
                              1992.7454     0.21     0.06     110.6                                      
                              1992.7481     0.40     0.09     121.2                                      
                              1992.7508     0.62     0.08     121.3                                      
                              1992.7536     0.71     0.16     103.9                                      
                              1992.7563     0.76     0.12     121.9                                      
                              1992.7755     0.05     0.01     105.9                                      
                              1992.8357     0.19     0.02     118.1                                      
                              1992.8658     0.09     0.04      78.1                                      
                              1992.8658     0.14     0.04      91.8                                      
                              1992.8686     0.09     0.02      69.5                                      
                              1992.8686     0.14     0.07      92.9                                      
                              1992.8823     0.07     0.02      88.8                                      
                              1992.8932     0.11     0.02     116.4                                      
                              1992.9206     0.43     0.07      98.8                                      
                              1992.9452     0.15     0.03     113.0                                      
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Hummel et al. (1994).                                                   MkT1994 
                         Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                         orbital parallaxes and component masses.                                        
                         Branham (2008) derives combined interferometric/spectroscopic orbit,    Bnh2008 
                         using a semidefinite programming technique. The resulting masses are            
                         3.049 +/- 0.513 and 2.569 +/- 0.432 Msun; he also determines a value            
                         for the parallax of 74.85 +/- 1.53 mas.                                         
                         Aa,Ab: Following an extensive review of historical spectroscopic and            
                         astrometric measurements of Capella, Torres et al. (2009) derived a     Trr2009 
                         new combined-solution orbit, assuming a circular orbit. They determined         
                         an orbital parallax of 76.67 +/- 0.17 mas (distance 13.042 +/-                  
                         0.028 pc), an age of 540-590 Myr, and the following physical                    
                         parameters for the two components:                                              
                         Mass (Msun):       2.466 +/- 0.018     2.443 +/- 0.013                          
                         Radius (Rsun):     11.87     0.56      8.75      0.32                           
                         Teff (K):          4920      70        5680      70                             
                         Luminosity (Lsun): 79.5      4.8       72.1      3.6                            
                         Mv (mag):          0.315     0.017     0.186     0.016                          
                         Aa,Ab: Weber & Strassmeier (2011) derived new spectroscopic elements,   WbS2011 
                         assuming the period determined by Torres et al. (2009). The new         Trr2009 
                         solution yielded masses of 2.573 +/- 0.009 and 2.488 +/- 0.008 Msun.            
                         Aa,Ab: A combined solution by Torres et al (2015) yields the following  Trr2015 
                         physical parameters for Aa and Ab:                                              
                             mass (Msun):       2.5687 +/- 0.0074     2.4828 +/- 0.0067                  
                             Teff (K):          4970       50         5730       60                      
                             Radius (Rsun):     11.98      0.57       8.83       0.33                    
                             log g (cgs):       2.691      0.041      2.941      0.032                   
                             Luminosity (Lsun): 78.7       4.2        72.7       3.6                     
                             a(AU):                      0.74272 +/- 0.00069                             
                             Distance (pc):              13.159      0.015                               
                             Age (Myr):                  590-650                                         
                             [Fe/H}:                     -0.04       0.06                                
             HJ 2256     AF: H VI 30.                                                                    
                         AF: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
             SHY  23     AM: HIP  24608 + HIP  26779.                                                    
             SHY  23     AN: HIP  24608 + HIP  26801.                                                    
             ST    3     Capella HL, the distant (723") double companion to Capella with                 
                         common proper motion. A premature orbit has been computed.                      
             HJ 2256     AF: H 6  30.                                                            MEv2010 
05171-7128   OGL 328     LMC106.6.13434 + LMC106.6.13435                                         Pli2012 
05172+3320   STF 666     H 2  48.                                                                MEv2010 
05173+5335   ES 2610     A is R Aur, variable 6.5-13.8. B is BD+53@880, F8V.                             
05174+3500   SEI 155     J   184.                                                                Nsn2016 
05175+2008   STF 674     A is the Algol-type binary CD Tau, eclipsing SB2, P = 3.44d.                    
                         AB has estimated period of 11000y.  B has spectral type dK2.            Tok2006 
05175-3454   KIR  12     omi Col.                                                                        
05175-7031   OGL 329     LMC104.7.15822 + LMC104.7.16197                                         Pli2012 
05176-0651   H 5  25     tau Ori = 20 Ori. H V 25.                                                       
05176-1513   S   473     B is BD-15@1000.                                                                
05177-1809   SEE  49     See's 1897 angle should read 196.7.                                     B__1953a
05179+3724   SEI 162     The discrepant measure by Scheiner (1908) is apparently due to a        Sei1908 
                         typographical error in the AC Potsdam Astrographic Catalog, as the              
                         correct position of the secondary is off by exactly 24" in dec.                 
                         Matches to other AC plates from 1929 and 1930 agree well with the               
                         Aladin image, as well as more recent observations.                              
05181-3402   TOK  61     Aa,Ab: Estimated masses 1.04 and 0.15 Msun; sep 43.6 AU, period 260 y.  Tok2010c
             HJ 3745     HIP 24711. B = HIP 24712.                                               Tok2011a
05181-7654   TOK 663     Resolved using ANDICAM2. B is not in PPMX.                              Tok2014d
05182+3739   BU 9002     Previously known as BU 885 1/2.                                                 
05182+3322   STT 103     16 Aur. A is a long-period spectroscopic binary. P = 434.8d.                    
                         Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                         Christie (1936).                                                        Crs1936 
05182-6809   OGL 330     LMC102.7.16903 + LMC102.7.16902                                         Pli2012 
05183-7143   OGL 331     LMC106.7.13197 + LMC106.7.13239                                         Pli2012 
05184-3108   LDS3651     NLTT 14861/14860                                                        Chm2004 
05185+3800   SEI 171     ALI 536.                                                                        
05185-6933   OGL 332     LMC103.5.107911+ LMC103.5.110011                                        Pli2012 
05186+4020   SMA  50     IDS and old-WDS location in error. Nothing at 05194+4020 (Heintz),      Hei1987a
                         but probably identical to a pair at this location.                              
                         SLE  64.                                                                        
05187+3331   ES   59     A pair found many years ago with the 3in refractor. The distant double          
                         comes was found with the 13in reflector at the Oxford Univ. Obs. and            
                         the comes C with the 17 1/4. AB was measured by Burnham in 1882.        Es_1902a
05187+0359   STF 682     BAL 2143.                                                                       
                         HIP 24774. The B-companion could possibly be a semi-resolved binary.            
05187-7122   OGL 333     LMC106.5.14568 + LMC106.5.14749                                         Pli2012 
05188+5250   STF 657     Same as STF 660.                                                                
05188-1808   SEE  50     A is a spectroscopic binary.                                                    
05189-6810   OGL 334     LMC102.7.22886 + LMC102.7.22769                                         Pli2012 
05189-6948   OGL 335     LMC103.6.38675 + LMC103.3.2                                             Pli2012 
05189-6957   OGL 336     LMC103.7.31356 + LMC103.7.31945                                         Pli2012 
05190-2829   BUG   8     2MASS J05185995-2828372                                                         
                         Estimated spectral types are L6: + T4:, effective temperatures ~1600            
                         and ~1330 K. Masses are estimated at 0.042-0.077 and 0.031-0.074 Msun,          
                         and the orbital period (assuming the semi-major axis = 1.26 * rho) is           
                         ~10yr.                                                                  Bug2006a
05191+4009   H 5  88     H V 88.                                                                         
05191+4006   STFB  3     lam Aur = 15 Aur                                                                
                         AC and AD: Optical pairs, based on study of relative motion of the              
                         components using the method of apparent motion parameters.              Kiy2008 
                         AD: H 5  22.                                                            MEv2010 
05191-6803   OGL 337     LMC102.3.50    + LMC102.3.51                                            Pli2012 
05192+3548   SEI 179     A is an irregular variable, V348 Aur.                                           
05192+2008   STF 680     Spectrum composite; G8II-III+G1IV-V (BSC).                                      
05192+1212   BPM 126     [PM2000]  237882 + [PM2000]  238008.                                    Gvr2010 
05192-0304   A    53     HIP 24819. See Allen et al. (2000) for information on metallicity,      AlC2000 
                         age, galactic orbital parameters, etc.                                          
                         AB: NLTT 14867/14868                                                    Chm2004 
05192-1800   FEN   4     Aka ARA 331.                                                                    
05193-1045   STF 688     BDS 2665, H III 94 same star. B is BD-10@1152.                                  
                         H 3  94.                                                                MEv2010 
05193-1831   S   476     AB: B is BD-18@1056.                                                            
05193-2845   LDS3653     NLTT 14889/14887                                                        Chm2004 
05194+3359   HO   18     18 Aur.                                                                         
05196-0107   BAL 303     RST 4779.                                                                       
05197+3526   SEI 186     SEI 187.                                                                        
05197+2511   STF 679     HJL  68.                                                                HJL1986 
05199-0723   JNN  34     2MASS J05195412-0723359 and J05195513-0723399, both from the Riaz et            
                         al. (2006) sample, are separated by only 16" and have comparable        Ria2006 
                         estimated distances (59 and 70 pc), as well as quite similar proper     Rsr2010 
                         motions (e.g. Roser et al 2010), and thus likely form a physical pair.  Jnn2012 
05200+4546   GIC  54     G096-032/G096-031.                                                              
                         NLTT 14857/14855                                                        Chm2004 
05201+3236   SEI 194     J 1089.                                                                         
05201-7100   OGL 338     LMC105.3.5578  + LMC105.3.5594                                          Pli2012 
05202-6810   OGL 339     LMC102.2.30    + LMC102.2.37                                            Pli2012 
05203+2510   STF 683     Chevalier's measure was incorrectly identified as STF 694, so never     Che1910 
                         added to the WDS; correct ID was determined based on his coordinates.   Hrt2012b
05204-0802   STF 692     AB,C: H 4  87.                                                          MEv2010 
05206-1031   GAL 379     Object #176 in Gallo's original list.                                   Gal1914 
05206-7024   OGL 340     LMC104.3.8821  + LMC104.3.9924                                          Pli2012 
05207+5848   GIC  46     G191-030/G191-029 or GJ 3342A/3343B.  A 1hr typographical error in RA           
                         led to this pair being initially entered in the WDS as 04205+5852.              
                         LDS6183.                                                                        
05207+3726   SEI 201     Fullerton et al. (1991) describe profile and radial velocity            Ful1991 
                         variations that suggest that this star is a short-period, radial                
                         pulsator.  Underhill (1995 PASP 107, 513) also discusses radial                 
                         velocity measurements.                                                  Msn1998a
05209+2402   STF 686     POU 650.                                                                        
05210+7113   HJ 1154     The ADS incorrectly added the CD component of 05061+5858 (STFA 13) as   A__1932a
                         an additional component of this pair.                                           
05213-6835   OGL 341     LMC101.3.42767 + LMC101.3.42931                                         Pli2012 
05217+3322   LDS6184     NLTT 14919/14920                                                        Chm2004 
05217+1854   KU   87     B is BD+18@832.                                                                 
05217+1240   STT 105     Not seen since 1971. Needs speckle.                                             
                         Additional notes may be found in van den Bos (1963).                    B__1963b
05218+3231   HU  614     A is the Mira-type variable UV Aur.                                             
05218-2446   HJ 3752     Spectrum composite; G7II-III+A7IV-V.                                            
                         AC: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05219+4203   AG  314     B is BD+41@1166.                                                                
05222+2008   J   144     OL  204.                                                                        
05222+0524   STT 106     HJL  69.                                                                HJL1986 
05223-7109   OGL 342     LMC105.2.15955 + LMC105.2.16304                                         Pli2012 
05224-6934   OGL 343     LMC103.4.118812+ LMC103.4.118814                                        Pli2012 
05225-7044   OGL 344     LMC105.4.45008 + LMC105.4.45010                                         Pli2012 
05226+7914   STF 634     STTA 60.  B is BD+79@168.                                                       
                         AB: Optical pair, based on study of relative motion of the components           
                         using the method of apparent motion parameters.                         Kiy2008 
05226+0236   A  2641     Only elements P and T have been amended by Starikova (1978) from the    Sta1978c
                         orbit of Baize (1957).                                                  Baz1957b
                         Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                         masses of 1.27 +/- 0.35, 1.39, and 0.95 Msun, respectively.             Mlk2012 
05228+4755   GIC  55     G096-035/G096-034. See Allen et al. (2000) for information on           AlC2000 
                         metallicity, age, galactic orbital parameters, etc.                             
                         NLTT 14943/14940                                                        Chm2004 
05228+0333   STF 696     23 Ori. B is BD+03@872.                                                         
                         H 4  84.                                                                MEv2010 
05229-4219   TOK  93     HIP 25148. A is SB without orbit, dRV= 3.7                              Nrd2004 
                         and also an astrometric binary (Makarov & Kaplan 2005).                 Mkr2005 
                         The companion at 66 mas is at the diffraction limit, the NICI                   
                         measurement is not accurate. The pair can be resolved by speckle.       Tok2012a
                         Aa,Ab: The tentative resolution at Gemini om 2011.70 is confirmed here,         
                         with 25deg of direct motion.                                            Tok2013b
05229-7143   OGL 345     LMC165.7.83    + LMC165.7.149                                           Pli2012 
05230-0850   JNN  36     This star has been classified as a probable T Tau star in Alcala et             
                         al. (1996 A&AS 119, 7).                                                 Jnn2012 
05230-1613   GAL 380     Object #177 in Gallo's original list.                                   Gal1914 
05231+3110   STF 691     B is BD+31@947.                                                                 
05231+0103   STF 700     H 1  75.                                                                MEv2010 
                         V1804 Ori, Algol (EA) type eclipsing binary, P = 2.22878 d.             Zas2011 
05232-2642   HIP  25180  Large RV amplitude (31.7 km s-1) hints at short orbital period, but             
                         only small dmu = 3 mas yr-1 is detected by Hipparcos. Triple?           Tok2012a
05232-3145   HJ 3757     Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
05232-7112   OGL 346     LMC164.8.18917 + LMC164.8.18916                                         Pli2012 
05233+3445   SEI 229     FOX 140.                                                                        
05233+3409   MLB1037     HJ  363.                                                                        
05233-0825   STF 701     H 2 102.                                                                MEv2010 
05234-7128   OGL 347     LMC165.6.20315 + LMC165.6.20368                                         Pli2012 
05235+5733   BU 1393     16 Cam. A is a spectroscopic binary.                                            
05235+1602   STF 697     B is BD+15@804.                                                                 
05237+6841   GIC  56     LDS5192. G248-038/G249-007.                                                     
05237+3606   SEI 233     SEI 234.                                                                        
05238-7018   OGL 348     LMC163.6.62323 + LMC163.6.62352                                         Pli2012 
05239+1743   BPM 127     [PM2000]  247544 + [PM2000]  247826.                                    Gvr2010 
05239-0052   WNC   2     A,BC: Primary is SB2, P=22.58d                                          Tok2014d
             A   847     BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                         spectroscopic masses 2.74 +/- 0.51, 2.47, and 1.13 Msun, respectively.  Mlk2012 
05239-6832   OGL 349     LMC160.6.38837 + LMC160.6.39333                                         Pli2012 
05240+3238   COU1090     Primary is V424 Aur, an Algol type eclipsing binary, P = 1.8368d.       Zas2012 
05240-0940   GAL 381     Object #178 in Gallo's original list.                                   Gal1914 
05243+0222   STF 702     BDS 2709, H I 75 same star.                                                     
05244+1723   S   478     111 Tau. A is a spectroscopic binary. B is BD+17@919.                           
                         Optical pair, based on study of relative motion of the components               
                         using the method of apparent motion parameters.                         Kiy2008 
             WNO  52     AC: HJL1043.                                                            HJL1986 
                         AC: GJ 202 + GJ 201. CPM pair.                                          Mkr2008 
                         AC: SHY  25. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                         high (near 100%) probability pair is physical.                                  
             S   478     AB: H 5 110.                                                            MEv2010 
05245-0224   MCA  18     eta Ori = 28 Ori. Quintuple; primary is a double-lined spectroscopic            
                         triple with periods 7.99 d (Aa1,Aa2) and 9.2 yr (Aa,Ab). The close              
                         pair eclipses, and shows an 8-hour pulsation in one of the components.          
                         Aa is also eclipsing binary (period 7.9904 day).                        Zas2010 
                         Aa,Ab.  McAlister (1976) orbit uses the elements P, T, e, and the       McA1976 
                         longitude of  periastron for the 9-year orbit, from a spectroscopic             
                         orbit by Ziska & Beardsley (1981), and assumes the orbit is edge-on;    Bey1981 
                         semi-major axis and node are based on a single speckle observation.             
                         The ascending node has been reversed.                                           
                         The visual companions are star B (mag. 4.8, 1.5") in slow retrograde            
                         motion, and C (mag. 9.4, 115").                                                 
                         See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1985.8542: This measurement of the Aab,c component of eta Ori,                  
                         overlooked in the original analysis of this run, was discovered during          
                         preparation of a paper on absolute quadrant determinations by Bagnuolo  Bgn1992 
                         et al. (1992)                                                           Hrt1992b
                         Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                         spectroscopic masses 25.82 +/- 24.95, 24.50, 22.65 Msun, respectively.  Mlk2012 
05245-0224   MCA 18      Aa,Ab has an SB1 orbit with P=9.44yr. The orbit given here uses only            
                         the speckle data, however.                                              Tok2015c
             H 6  67     H VI 67.                                                                        
05246+0149   S   479     B is BD+01@1003.                                                                
05246-0535   SKF 248     There is a possible companion at 7.8" noted in the WDS, but inside the          
                         AstraLux field of view, the star appears single.                        Jnn2012 
05247+6323   STF 677     AB: CfA: RV var? Can be a sub-system in A or B.                         Tok2014d
                         Now a 3 tier quadruple system since we resolved the secondary                   
                         component of the binary STF 677AB into a new 0".18 pair Ba,Bb and               
                         confirmed that the Robo-AO tertiary C at 7" is physical. We find C to           
                         be slightly below the MS, within errors. Although the relative motion           
                         of AC is fast, it is not directed away from PM(A) as would be the case          
                         for a distant background star; it is produced by the orbital motion of          
                         the inner binary AB. The presence of an inner subsystem in the binary           
                         AB was suspected previously from its variable RV (Nordstrom et al.              
                         2004). The estimated masses of Ba and Bb, 0.98 and 0.65 Msun,           Nrd2004 
                         respectively, remove the discrepancy between the mass sum of 3.05 Msun          
                         calculated for the AB system from its grade 4 orbit by Hartkopf et al.  Hrt2008 
                         (2008) and the expected mass sum. Although such discrepancies are not           
                         uncommon for low-quality orbits, in this case it serves as an indirect          
                         confirmation of Ba,Bb. Estimated period of Ba,Bb is ~20 yr.             Rbr2015d
05247+3723   BU  888     sig Aur = 21 Aur                                                                
05247+2009   J   145     OL  185.                                                                        
05248-1642   GAL 382     Object #179 in Gallo's original list.                                   Gal1914 
05248-5219   I   345     the Pic. A is a spectroscopic binary.                                           
                         Quoted errors in P and a for the Argyle et al. (2002) solution are      Ary2002b
                         +259/-54y, +0".20/-0".01, respectively.                                         
                         1989.9388: This system has also decreased in separation steadily                
                         since the 1920's, and was last resolved visually in 1983.               Hrt1993 
05249+1658   BPM 128     [PM2000]  249674 + [PM2000]  249613.                                    Gvr2010 
05249-7105   OGL 350     LMC164.7.34239 + LMC164.7.34339                                         Pli2012 
05250-0249   H 6  68     H VI 68. B is BD-02@1238.                                                       
05251+1212   BPM 129     [PM2000]  250160 + [PM2000]  250278.                                    Gvr2010 
05251+0621   BUP  78     gam Ori = 24 Ori = Bellatrix                                                    
05251-6818   OGL 351     LMC159.8.17075 + LMC159.8.17418                                         Pli2012 
05251-6833   OGL 352     LMC160.6.45288 + LMC160.6.46200                                         Pli2012 
05252+3451   STF 698     Spectrum composite; K1pIII-IV+F6V. B is BD+34@1030.                             
                         Same as WZ    9. Verified by Daley.                                     Dal2001b
                         AB: H 4 101.                                                            MEv2010 
05252+0155   STF 708     H 1  52.                                                                MEv2010 
05252-1119   STF 710     B is BD-11@1168.                                                                
05255-0033   A   848     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                         1977.9196: This measure was incorrectly attributed to ADS 3701 in               
                         McAlister & Hendry (1982), with an incorrect position angle.            McA1982b
05256+3652   SEI 246     Not found by Heintz at IDS position.                                    Hei1987a
                         Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
05256-6005   HJ 3764     CD-60@1161.                                                                     
05257-0909   DAE   2     NLTT 15049 = LP 717-36.  Daemgen et al. (2007) derive a distance of     Dae2007 
                         20.2 +/- 4.7 pc, a separation of 10.9 +/- 2.5 AU, and a predicted               
                         orbital period of 58 +/- 21 yr. Spectral types are M3.5 +/- 0.5 and             
                         M4.0 +/- 0.5; masses are 0.36 +/- 0.09 and 0.28 +0.11/-0.08 Msun.               
05257-6931   OGL 353     LMC161.1.5     + LMC161.1.38                                            Pli2012 
                         Also known as SKF1046.