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.                                                                   
00081+3240 HJ  610     SEI   2.                                                                Nsn2017a
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 = Alpheratz                                                    
                       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 
00206-2356 WSP  20     Planet-host star found to be close visual binary. Evans et al. (2016)           
                       find that the transiting hot Jupiter is probably orbiting the primary,          
                       and derive the following properties:                                            
                       A:      M = 1.089 +/- 0.047 Msun, R = 1.142 +/- 0.085 Rsun                      
                       planet: M = 0.378 +/- 0.022 Mjup, R = 1.28  +/- 0.15  Rjup              EvD2016 
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+3230 STF  29     SEI   4.                                                                Nsn2017a
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
00263-4218 CRU9004     alp Phe = Ankaa.                                                                
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
                       BC: The B component is of type G5V, with mass 0.87 +/- 0.03 Msun.               
                       Based on isochrone fitting, Wittrock et al. (2016) estimate the mass            
                       of the C component at 0.48 +/- 0.03 Msun, and type likely an M dwarf.   Wtt2016 
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 
                       YSC 170.                                                                        
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.                                                                        
                       SEI   9.                                                                Nsn2017a
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 
00511-7226 DBR 213     DBR 214.                                                                        
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 
00523-7224 DBR 236     DBR 237.                                                                        
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.                               
                       AD: The D component is the A component of 00568+6022.                   Mam2017 
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.                  
                       The A component is the D component of 00567+6043.                       Mam2017 
           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