02000+1334 LDS5181     old LDS6130.                                                                    
02003-0138 BAL   9     J  3333.                                                                Nsn2016 
02004-0831 HJ 3476     AB: A is AR Cet, probably a semi-regular variable.                              
02005-0240 BRG   8     The companion to 2MASS J02002975-0239579 has yet to be tested for               
                       common proper motion, but since its color and brightness are                    
                       consistent with expectation and its separation is small (~0.32"), it            
                       is counted as a physical companion here.                                Jnn2012 
02005-6246 HJ 3479     B is CPD-63@142.                                                                
02006+2753 J  3257     A is an Algol-type binary, X Tri, P = 0.97d.                                    
02011+3518 STF 197     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
02011-1741 LDS5362     NLTT 6759/6757                                                          Chm2004 
02012-0729 GWP 250     ABL   1.                                                                Tob2012b
02012-3000 CUS   1     Assuming a primary mass of 1.02 +/- 0.19 Msun, the derived flux ratio           
                       (~0.028 in H and K) gives a mass of ~0.5 Msun for the secondary.        Cus2012 
02013+1227 BPM  45     [PM2000]   74159 + [PM2000]   74128.                                    Gvr2010 
02013-0752 GWP 251     ABL   2.                                                                Tob2012b
02015+1830 BPM  46     [PM2000]   74328 + [PM2000]   74271.                                    Gvr2010 
02019+7332 JNN 252     GJ 3125. Estimated age 30-300 Myr; masses 0.12 +/- 0.07 and 0.06 +/-            
                       0.04 Msun; a ~5.0 au.                                                   Jnn2014 
02019+2415 POU 157     ID uncertain. Nothing at Pourteau's coordinates.                        Pou1933 
02020+7054 BU  513     48 Cas. A is a spectroscopic binary, same period as the visual pair.            
                       Suspected sub-periods of 39 yr (Baize) and 26 yr (Muller) are not       Baz1941b
                       confirmed by later measures.  The radial velocities of the primary may  Mlr1949c
                       show a trace of a period of about 4 yr (Heintz).                        Hei1981e
                       See Baize & Petit catalog of doubles with variable component.           Baz1989d
                       Masses and bolometric magnitudes are derived for the two components             
                       based on assumed spectral types and available parallaxes.                       
                       1980.7205: This measure was incorrectly attributed to ADS 1958 in               
                       McAlister et al. (1983).                                                McA1983 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.96 +/- 0.42, 3.07, and 2.00 Msun, respectively.  Mlk2012 
02020+0246 STF 202     alp Psc = Alrescha. Both components are listed as Alpha CVn variables           
                       of small amplitude, and both may have variable RV.                      Sca1983f
                       See Baize & Petit catalog of doubles with variable component.           Baz1989d
                       Absolute quadrant for 1998.657 determined by triple-correlation                 
                       techniques                                                              Pru2002b
                       Chevalier identified this star as alp Psc, but gave an incorrect        Che1911 
                       declination, leading to its initial designation as 02020+0320 CHE 32.   Hrt2012b
           PWL   1     AC: SHY 132. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
           STF 202     AB: H 2  12.                                                            MEv2010 
02021+0355 OSV   1     LDS5363.                                                                        
02021-1321 GAL 317     Object #59 in Gallo's original list.                                    Gal1912b
02022+7530 STF 185     Primary is V779 Cas, an Algol type eclipsing binary, P = 6.35340d.      Zas2012 
02022-1441 GWP 253     ABL   4.                                                                Tob2012b
02022-1808 GWP 252     ABL   3.                                                                Tob2012b
02022-4550 SHY 410     HIP   9495 + HIP   9672.                                                        
02022-6236 TOK  70     HIP 9499. A is SB, no orbit, dRV=70.7 (Nordstrom et al. 2004).          Nrd2004 
02023-2634 LDS  65     NLTT 6825/6826                                                          Chm2004 
02025-1410 GWP 254     ABL   5.                                                                Tob2012b
02026-1719 GWP 255     ABL   6.                                                                Tob2012b
02027-3019 HJ 3478     B is CD-30@717.                                                                 
02030+3317 STF 201     eps Tri = 3 Tri                                                                 
02031-0725 STF 209     B is BD-08@371.                                                                 
02031-1229 GWP 256     ABL   7.                                                                Tob2012b
02032+5514 BLL   4     A is a semi-regular variable, XX Per. B is BD+54@445.                           
02034+3919 MLB  10     AB: Also known as SMA  27.                                                      
02035+6408 HJ 1101     STI 337 (three Vat1926 measures from STI 337 merged 2008/06/25)                 
02035+1744 BPM  47     [PM2000]   75525 + [PM2000]   75508.                                    Gvr2010 
02037+2556 STF 208     10 Ari. Malkov et al. (2012) derive dynamical, photometric, and                 
                       spectroscopic masses 2.94 +/- 0.84, 2.35, and 1.29 Msun, respectively.  Mlk2012 
02038+7013 MLR 375     1983.0663: This autocorrelogram was remeasured; the new results are             
                       listed in the catalog.                                                  McA1987b
02038-0020 H 5 102     H V 102. 61 Cet. Spectrum composite; G5II-III+G5V.                              
02039+8221 HJ 2090     The measure in BDS by Cogshall belongs to some other pair.              Bu_1906 
                       1904.69, 243.9@, 3.52" (Van Biesbroeck).                                VBs1914 
02039+4220 STF 205     H III 5, SHJ 26. gam And = Almach. A quadruple system.                          
                       Star A (mag 2.3, K3II) forms with BC the pair STF 205, separation 10".          
                       Star B is SB, P = 2.67 d (Maestre & Wright, ApJ 131, 119, 1960).                
                       See discussion by Morgan et al. (1978).                                 BLM1978 
                       A,BC: H 3   5.                                                          MEv2010 
           STT  38     BC: See discussion by Morgan et al.                                     BLM1978 
                       BC: Poor agreement between two theta measures.                          Mlr1956d
                       BC: Additional notes may be found in Muller (1954).                     Mlr1954a
02039+1231 BPM  48     [PM2000]   75778 + [PM2000]   75779.                                    Gvr2010 
02039-4525 RST2272     Primary is SB2, P=0.851 y. Aa,Ab UR in speckle. Koen et al. (2002               
                       MNRAS 331, 45) find 311d photometric period.                            Tok2014d
02042+5257 HJ 2104     B is BD+52@501.                                                                 
02042+4641 ADM   1     HTP  32. HAT-P-32. Primary is exoplanet host star.                      Adm2013 
02042-1039 GAL 318     Object #62 in Gallo's original list.                                    Gal1912b
02044+1230 CHE  36     CHE  37.                                                                        
02046+2525 LTT 17328   Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from the Geneva           
                       Extrasolar Planet Search Programs home page.                            HaI2001 
02046+1757 GWP 257     XMI 235.                                                                Tob2012b
02051+7717 SHJ  22     47 Cas.                                                                         
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
           47 Cas      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02051-1737 BEU   3     PM = +1318-174.                                                                 
02053+2906 CHE  38     CD: Originally 02053+2907 CHE  38AB, until C component of 02053+2906            
                       found to be prmary of 02053+2907.                                               
           WAK  14     CE: Originally 02053+2907 WAK  14AC.                                            
02053-2803 LDS  67     NLTT 6979/6980                                                          Chm2004 
02054-5910 HJ 3481     B is CPD-59@185.                                                                
02055+7607 BU  785     49 Cas.                                                                         
02055+0056 LDS5365     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02056+1444 BPM  49     [PM2000]   76857 + [PM2000]   76899.                                    Gvr2010 
02057-2423 I   454     CPD-24@891. C is CPD-24@889.  AB,C = LDS  68.                                   
                       AB,C: SHY 135. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                       very high (near 100%) probability pair is physical.                             
           WSI   7     Aa,Ab: Tokovinin et al. (2014) derive a combined spectroscopic/                 
                       interferometric orbit of the Aa,Ab pair, as well as a new orbit of the          
                       AB pair. Resulting component masses for Aa, Ab, B, and C are 0.74,              
                       0.72, 0.57, and 0.78 Msun, respectively.                                Tok2014b
02058+1241 CHE  42     There are no obvious errors in applying the offset from Chevalier's     Che1910 
                       plate center, but there are no appropriate pairs near his coordinates,          
                       nor at coordinates found by reversing the sign of either or both                
                       offsets. The pair is likely lost.                                       Hrt2012b
02062-1808 GWP 258     ABL   8.                                                                Tob2012b
02065+5703 BAR  23     J 880.                                                                          
02068+2542 HO  312     11 Ari.                                                                         
02069-1126 SLW  99     Aka ABL   9.                                                                    
02070-1017 GAL 319     Object #63 in Gallo's original list.                                    Gal1912b
02070-4406 JNN 149     2MASS J02070176-4406380 and J02070198-4406444 are separated by only 7"          
                       and have similar estimated spectroscopic distances (13 and 21 pc,               
                       respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                       a physical pair.                                                        Jnn2012 
02074-5941 HJ 3484     B is CPD-60@183.                                                                
02076+1355 ZHN   2     BDK   4. G 73-26 + SDSS J020735.60+135556.3.   Distance 26 +/- 10 pc            
                       for primary, 35 +/- 5 pc for secondary. Estimated age of system 3-4             
                       Gyr. Mass of secondary estimated at 0.079-0.081 Msun.                   Fah2010 
02076-0037 LDS3346     NLTT 7066/7064                                                          Chm2004 
                       HJL  29.                                                                HJL1986 
02079+1343 GWP 259     XMI 236.                                                                Tob2012b
02080+2814 CHE  55     MLB 452.                                                                        
02080-0951 GAL 320     Object #64 in Gallo's original list.                                    Gal1912b
02081+1336 FAR  27     SKF  23.  Primary is white dwarf WD 0205+133.                           Far2006 
02082+1509 LDS5183     old LDS6131.                                                                    
02083+2543 ALP   6     2MASSW J0208183+254253                                                          
                       Further observations are required to determine the physical/optical             
                       nature of this triple.                                                  AlP2007 
02084+2819 KUI 118     G072-058. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 7087/7088                                                          Chm2004 
02085-0641 HDS 285     Possible sub-diffraction-limited component, but the astrometry is not           
                       consistent between the two observations.                                Hor2011b
02087-0026 STF 218     Same as STF 220.                                                                
02089+4927 BWL   9     Colors and/or astrometry are inconsistent with a late-type common               
                       proper motion companion based on visual inspection of the field from            
                       2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3136.                     Bwl2015 
02090+5745 STI1791     AB. WDS designation changed from 02099+5744 when it was determined              
                       that TDS2135 comprised the primary of this wider pair.                          
02091+5104 STF 213     C easily seen 8" north following. Magnitude about 10.5, not 12.5.       B__1963b
02091+4341 LDS3349     NLTT 7117/7118                                                          Chm2004 
02091+4048 STF 215     A is an eclipsing binary, BX And.                                               
02091+1511 GWP 260     XMI 237.                                                                Tob2012b
02093-1958 GWP 261     ABL  10.                                                                Tob2012b
02094+2556 H 6  69     H VI 69. 14 Ari. STTA 23.                                                       
                       AC: HJL1012.                                                            HJL1986 
02094-1011 HJ 2116     Richard Jaworski, in analysis of SuperCOSMOS data, has determined that  Jaw2005 
                       component C is the galaxy NGC 833, D is the galaxy NGC 835, E is the            
                       galaxy NGC 838 and F is the galaxy NGC 839. Thus, in the pairing "CD"           
                       both components are galaxies and not stars.                                     
02095+3459 MKT   4     bet Tri.                                                                        
                       Hummel et al. (1995) visual orbit based on astrometry from Mark III     MkT1995 
                       interferometer. Additional spectroscopic data yield component masses,           
                       luminosities, radii, effective temperatures, and distance.                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1995).                                                   MkT1995 
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.11 +/- 0.18, 5.26, and 1.82 Msun, respectively.             Mlk2012 
02096+4251 ES   48     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
02097+2021 STF 221     AB: H 3  68.                                                            MEv2010 
02097+0857 GWP 262     XMI 238.                                                                Tob2012b
02098-4052 TOK 427     HIP 10096 is SB2 according to GCS. The separation corresponds to a              
                       period of ~5yr.                                                         Tok2015c
02099+3449 HU 1034     Not seen 1948, 1951. No observations since that time.                           
02103+3322 STF 219     SEI  24.                                                                Nsn2017a
02104+3911 HJ 1109     C is a nebula.                                                                  
02104-5049 ESG   1     Gl 86. Magnitudes are K magnitudes of Lagrange et al. (2006).                   
                       Lagrange et al. (2006) give two possible orbital solutions, based on    Lgr2006 
                       different assumed masses (70 Mjup and 0.5 Msun) for the secondary.              
                       Semi-major axes converted from au (47.58 and 18.42 au, respectively)            
                       to arcseconds assuming an Hipparcos-based distance of 10.9 pc.                  
                       JHK photometry of primary from 2MASS, that of secondary transformed             
                       from NACO to 2MASS filters.                                                     
                       2001.7454: PA is measured in zenith mode. If data collected in                  
                       equatorial mode, PA = 112.1.                                            Rbr2011d
                       Farihi et al. (2013) derive a mass of 0.59 +/- 0.01 Msun and                    
                       Teff = 8180 +/- 120K for the white dwarf companion to GJ 86. Monte              
                       Carlo simulations yield the following orbital constraints:                      
                       P = 120-481y, T0 = 1933-2067, e = 0.00-0.61, i = 114.7-122.6deg,                
                       a = 2.57-6.47" (27.8-69.8 au) Omega = 63.7-76.1deg, omega=0-358deg.             
                       The upper ranges of P and a are considered less likely.                 Far2013 
           GJ 86       A: Combined solution, based on reduction of Hipparcos intermediate              
                       astrometric data together with spectroscopic elements from Queloz       Que2000 
                       et al. (2000).                                                          HaI2001 
02106+1027 GWP 263     XMI 239.                                                                Tob2012b
02107-1507 FAR  28     Primary is white dwarf WD 0208-153.                                     Far2006 
02109+3902 STF 222     59 And.                                                                         
                       H 4 129.                                                                MEv2010 
02109+1341 STF 224     H N 105; BDS 1146 is identical.                                                 
02110+0317 GWP 264     XMI 240.                                                                Tob2012b
02112+2604 BRT3260     Originally published as BRT 127.                                        Brt1928 
02114+1848 GWP 265     XMI 241.                                                                Tob2012b
02115+5739 BU  874     5 Per.                                                                          
02117-0531 GWP 266     ABL  11.                                                                Tob2012b
02117-1927 GWP 267     ABL  12.                                                                Tob2012b
02122+4440 RUC   2     Aa,Ab. GZ And. Spectral type of Ab component estimated at M3-4V.        Ruc2007 
           HJ 2117     A is a W UMa-type binary, GZ And.                                               
02123-0908 GWP 268     ABL  13.                                                                Tob2012b
02124+3018 STF 227     iot Tri = 6 Tri. A is a spectroscopic binary, P = 14.73d. B is also an          
                       SB, P = 2.24d. One component is variable: TZ Tri.                               
           TZ Tri      Koresko et al. (1998) PTI solution has period fixed at spectroscopic    Krs1998 
                       value of Kaye et al. (1995).                                            Eat1995b
           STF 227     H 2  34.                                                                MEv2010 
02124+1249 LDS1126     NLTT 7300/7301                                                          Chm2004 
02124-0223 HDO  56     Not found. There must be a large error in the Hd place. Burnham         Bu_1909 
                       could not find it anywhere in the vicinity.                                     
02124-0455 GWP 269     ABL  14.                                                                Tob2012b
02124-7023 R    15     HLN   3.  B is CPD-70@131.                                                      
02125-0804 BRT 357     Also known as LDS3357.                                                          
02127+1614 GWP 270     XMI 242. SLW 100.                                                       Tob2012b
02128+7941 S   405     STTA 22. A is a Delta Scuti-type variable and spectroscopic                     
                       binary, P = 4.12d. B is BD+78@71.                                               
                       AB: H 5  84.                                                            MEv2010 
02128+0309 GWP 271     XMI 243.                                                                Tob2012b
02128-0224 STF 231     66 Cet. B is BD-03@335.                                                         
                       Aka SHJ  29 = H 4  25.                                                          
                       AB: NLTT 7323/7321                                                      Chm2004 
                       HIP 10305. A is SB2, period 94.788d, resolved by speckle (TOK 39).              
                       A is evolved. B = HIP 10303.                                            Tok2011a
02129+5712 STTA 24     AB and AC: Optical pair, based on study of relative motion of the               
                       components using the method of apparent motion parameters.              Kiy2008 
02129-0349 GWP 272     ABL  15.                                                                Tob2012b
02130+0851 MCA   5     xi 1 Cet = 65 Cet. Also a spectroscopic binary.                                 
                       A 1985.8375 measure attributed to this pair by Mcalister actually               
                       actually belonged to 02157+2503COU  79.                                 McA1987b
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin & Herbig (1981).                                                Grf1981b
                 5     1985.8375: A measure at this date, belonging to 02157+2503 = COU  79,           
                       was erroneously attributed to MCA 5 in McAlister et al. (1987). This    McA1987b
                       measure has been moved to COU 79 and averaged with a re-reduced                 
                       measure from these data published by Hartkopf et al. (1996).            Hrt1996a
02131+5805 SHY 145     AC: HIP  10332 + HIP  12685.                                                    
02132+4414 CHR   5     60 And. A spectroscopic binary.                                                 
                       The negative results obtained during 1976 - 1980 are apparently due to          
                       a large magnitude difference.                                           Hrt1984 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Griffin & Herbig (1981).                                                Grf1981b
02132+4030 SHY 136     AB: HIP  10339 + HIP  10321. B component is V450 And.                           
           HEL   5     Ba,Bb: V450 And. Helminiak et al. (2016) resolve this SB and BY Dra             
                       type variable, and derive a combined astrometric/spectroscopic orbit.           
                       The secondary is shown to be an M-type star, rather than brown dwarf.           
                       Resulting best-fit masses are 1.141 and 0.279 Msun (median values               
                       1.113 +/- 0.065 and 0.277 +/- 0.021 Msun), respectively. Best-fit               
                       parallax is 37.24 mas (median 37.34 +/- 0.55 mas).                      Hel2016 
02133+3649 JNN  18     Estimated age 30-300 Myr; masses 0.26 +/- 0.06 and 0.09 +/- 0.03 Msun;          
                       a ~2.8 au.                                                              Jnn2014 
02135+5926 STI 351     STI1807                                                                         
02135-0502 GWP 273     ABL  16.                                                                Tob2012b
02135-2546 HJ 2120     B is CD-26@800.                                                                 
02136+5104 BAG   1     Aa,Ab: 6 Per. A is a long-period spectroscopic binary, now resolved by          
                       speckle interferometry.                                                         
                       SB1, P = 4.5 yr. Halbwachs (1981) predicts maximum separation 0".047.   HJL1981 
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Christie (1936).                                                        Crs1936 
           STT 555     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
02136-0945 GWP 274     ABL  17.                                                                Tob2012b
02137-0302 H 6 110     H VI 110. B is BD-03@341.                                                       
02138-1933 RSS  54     CPD-20@248                                                                      
02140+4729 STF 228     Spectral types and masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       Scardia says the quadrant unambiguous for their 2004 theta values of            
                       105.8; this does not agree with other determinations of magnitude               
                       difference, however.                                                    Sca2005a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.34 +/- 0.36, 2.52, and 2.47 Msun, respectively.             Mlk2012 
02140+1652 GWP 275     XMI 244.                                                                Tob2012b
02142+0555 GWP 276     XMI 245.                                                                Tob2012b
02142-1811 GWP 277     ABL  18.                                                                Tob2012b
02144+3454 HU  807     Motion in separation, with little angular change. Close 1950-1960.              
02144-1441 GWP 278     ABL  19.                                                                Tob2012b
02145+6631 MCA   6     55 Cas. Composite spectrum star: B9V + G0II-III, delta m = 0.2 mag      Bnu1984 
                       (Markowitz 1969)                                                        Mrz1969 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.70 +/- 1.31, 6.94, and 2.57 Msun, respectively.             Mlk2012 
02145+5912 STI1812     SMA  31.                                                                        
02145-1103 LDS5373     SLW 102.                                                                        
02146-0142 GWP 279     ABL  20.                                                                Tob2012b
02147+3024 STF 232     H 2  35.                                                                MEv2010 
02147+1657 GWP 280     XMI 246.                                                                Tob2012b
02149+5829 STF 230     B spectrum B9IV.                                                                
02149+1353 GWP 281     XMI 247.                                                                Tob2012b
02150+5903 MLR 447     Also known as TDS2174.                                                          
02152-3507 SHY 415     HIP  10483 + HIP  10385.                                                        
02154+1126 GWP 282     XMI 248.                                                                Tob2012b
02155+5231 GC 2695     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin & Radford (1977).                                               Grf1977c
02155+1220 GWP 283     XMI 249.                                                                Tob2012b
02156+4223 GIC  29     G133-079/G134-019.                                                              
                       NLTT 7438/7440                                                          Chm2004 
02157+6740 ENG  10     B is BD+66@193.                                                                 
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
           SHY  10     BC: HIP  10529 + HIP  11167.                                                    
02157+2503 COU  79     21 Ari. Couteau & Morel (1982) computed masses disagree with spectral   Cou1982d
                       type. Authors suggest 3rd component (mass ~1 Msun) as possible                  
                       explanation. 1985.8375: This measure was erroneously attributed to              
                       02130+0851 = MCA 5 by McAlister et al. (1987). The data were re-reduced McA1987b
                       by Hartkopf et al., giving similar results. The measure has now been    Hrt1996a
                       replaced by the mean of the two separate reduction results.                     
                       1986.567: The separation of this partially resolved pair was                    
                       calculated under the assumption of zero or otherwise known magnitude            
                       difference. Pair passed periastron earlier than predicted; now the              
                       orbit is definitive                                                     Tok1985 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.09 +/- 0.30, 3.04, and 1.17 Msun, respectively.             Mlk2012 
02157+1046 STF 237     AB: HJL  30.                                                            HJL1986 
02157-0217 GWP 285     ABL  21.                                                                Tob2012b
02157+1657 GWP 284     XMI 250.                                                                Tob2012b
02158-1814 HTG   1     Orbit poorly covered, period rather indeterminate.                      Hei1978c
                       Additional notes may be found in Burnham (1894).                        Bu_1894 
02159+1416 GWP 286     XMI 251.                                                                Tob2012b
02159+0638 A  2013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.60 +/- 0.37, 1.51, and 0.79 Msun, respectively.             Mlk2012 
02160-0929 BRG  10     This likely triple system has only been observed in one epoch, hence            
                       it remains unconfirmed. The brightnesses and colors of all components           
                       are however consistent with expectation for a physical triple.          Jnn2012 
02160-1626 GWP 287     ABL  22.                                                                Tob2012b
02161+1651 GWP 288     XMI 252.                                                                Tob2012b
02161+1630 BPM  50     [PM2000]   83035 + [PM2000]   83004.                                    Gvr2010 
02162-2302 I   457     ADS 1744a.                                                                      
02163-0949 STF 242     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
02164-0731 SLW 106     = GWP 289 = ABL  23.                                                            
02164-1233 SLW 105     = ABL  24.                                                                      
02164-1632 GWP 290     ABL  25.                                                                Tob2012b
02165-2227 LDS3364     NLTT 7520/7519                                                          Chm2004 
02165-5131 DUN   6     phi Eri. B is CPD-52@284.                                                       
           SHY 137     AC: HIP  10602 + HIP   9685.                                                    
           SHY 137     AD: HIP  10602 + HIP   7699.                                                    
           SHY 133     CD: HIP   9685 + HIP   7699.                                                    
           SHY 143     CE: HIP   9685 + HIP  12225.                                                    
           SHY 130     DF: HIP   7699 + HIP   6485.                                                    
02167-0430 GWP 291     ABL  26.                                                                Tob2012b
02167-3100 LDS  71     NLTT 7535/7528                                                          Chm2004 
02167-6324 TOK  71     HIP 10621. NOMAD: PM(B)=(0,-30), PM(A)=(18,60).                                 
                       D is HIP 10754.                                                         Tok2011a
02168+4346 GNS   1     Based on 2MASS and AstraLux images, Ginski et al. (2012) conclude the           
                       companion is a background object.                                       Gns2012 
02169+5703 STTA 25     B is BD+56@470.                                                                 
02169+0448 GWP 292     XMI 253.                                                                Tob2012b
02169-2322 BRG  11     The companion to 2MASS J02165488-2322133 has not yet been confirmed to          
                       share a common proper motion, but the color and brightness of it are            
                       well consistent with a physical companion, hence it is counted as such          
                       in the statistics.                                                      Jnn2012 
02171+3413 DOR  66     del Tri = 8 Tri. A is a double-lined spectroscopic binary, P = 10.02d.          
                       Proper motion +1154 -245.                                                       
           MKT   5     Aa,Ab: PM = +1154 -245. del Tri.                                                
                       Hummel et al. 1995) visual orbit based on astrometry from Mark III      MkT1995 
                       interferometer. Additional spectroscopic data yield component masses,           
                       luminosities, radii, effective temperatures, and distance.                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1995).                                                   MkT1995 
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.57 +/- 3.14, 1.92, and 1.05 Msun, respectively.  Mlk2012 
02172+5838 YSC  87     Ba,Bb: Originally 02171+5839 YSC  87, but found to correspond to B              
                       component of 02172+5838.                                                        
02172-2849 LDS3365     NLTT 7557/7558                                                          Chm2004 
02173+3351 VIG   1     Primary is gam Tri. The B and C components are background stars, the D          
                       component ambiguous.                                                    Vig2012 
02174+2845 STF 239     HJL  32.                                                                HJL1986 
                       Aka H 4  40 = SHJ  31.                                                          
02174+2708 GIC  30     AC: G035-037/G036-007.                                                          
02176+2214 STF 244     HJL  33.                                                                HJL1986 
02176-5400 RSS  55     CD-54@487                                                                       
02178+5638 A  1272     V438 Per, a W UMa type eclipsing binary, P = 3.50939d.                  Zas2012 
02179+1941 TOK  72     HIP 10710. Primary is astrometric binary (Makarov & Kaplan 2005)        Mkr2005 
02179+1614 GWP 293     XMI 254.                                                                Tob2012b
02180+5616 UC   29     Primary appears to be a close pair.                                     Cbl2010c
02180+3116 A   959     Primary is eclipsing binary of W UMa type, period 0.31069d.             Zas2017b
02180+1958 GWP 294     XMI 255.                                                                Tob2012b
02180+0145 GC 2770     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Harper (1935).                                                          Hrp1935 
                       Combined astrometric/spectroscopic orbit by Fekel et al. (2007). For    Fek2007 
                       primary, derive mass = 1.15 Msun, radius = 1.64 +/- 0.07 Rsun,                  
                       Luminosity = 3.0 +/- 0.1 Lsun. Spectral types are G0IV and ~M0V.                
                       SB1. Combined orbit including RV data and Hipparcos Intermediate                
                       Astrometric data. Semimajor axis derived from photocentric a0 plus              
                       stellar evolutionary model. Derived properties for A and B:                     
                       M/Msun = 1.20 + 0.53, L/Lsun = 2.76 + 0.04, dm = 4.60 mag,                      
                       log age = 9.65.                                                         WaX2015b
02180-1229 LDS  73     NLTT 7592/7593                                                          Chm2004 
02181+5731 BU 1170     7 Per = chi Per                                                                 
                       S   409 = H 6  19.                                                              
02182+5715 STI1836     BKO 165.                                                                        
02182+3920 A   207     Scardia et al. (2001) orbit preliminary as all the orbital elements     Sca2001d
                       are still rather uncertain. Hipparcos parallax (0".01200 +/- 0.00311)           
                       seems to be overestimated and leads to a mass sum 0f 0.46 Msun,                 
                       unacceptable for a system of type F5. Scardia (1982) classified the     Sca1982a
                       star as type F9. Dynamical parallax is 0".0065; the corresponding mass          
                       sum is 2.87 Msun.                                                               
02184+5758 STI1839     STI1844.                                                                        
02184-0636 GWP 295     ABL  27.                                                                Tob2012b
02186+4017 STF 245     ALI1193.                                                                        
           EGG   2     Aa,Ab: This system has spectral type F2 from SIMBAD and parallax of             
                       10.26 +/- 2.92 mas from van Leeuwen (2007). A previous orbit was        VlF2007 
                       calculated by Cvetkovic (2008) with period of 109 years and semimajor   Cve2008c
                       axis of 0.344 arcsec. However, our new observation shows that the               
                       system has a much shorter period and smaller semimajor axis. However,           
                       our orbit yields roughly the same total mass, with large uncertainty.           
                       The system appears to have executed nearly a full orbit since the               
                       first speckle observations taken of it in 1985 by McAlister et al.              
                       (1987). More data will be needed to confirm this orbital trajectory,            
                       but if correct, the smaller period makes the system much more                   
                       attractive for future study.                                            Hor2015b
02186-2940 B    34     AV For, Algol (EA) type eclipsing binary, P = 1.8797 d.                 Zas2011 
02187+3429 STF 246     H III 42, BDS 1165.                                                             
                       HJL  34.                                                                HJL1986 
                       H 3  42.                                                                MEv2010 
02187+0412 BU  437     Some observations erroneously ascribed to STF 247, even Struve's                
                       discovery, seems to belong to this pair, whose delta-m = 2 is less              
                       than Burnham's estimate.                                                Hei1992a
02188+0840 GWP 296     XMI 256.                                                                Tob2012b
02188+1440 GWP 297     XMI 257.                                                                Tob2012b
02190+2839 HJ 1115     10 Tri.                                                                         
02191-0651 HJ  327     AC: The C component is the galaxy NGC 883.                                      
02193-0259 JOY   1     Aa,Ab: The primary is omi Cet = VZ Cet = 68 Cet = Mira, prototype of            
                       the Mira-type variables. "Orbits" have been computed for the visual             
                       pair, but are most likely false. B has in the past been identified as a         
                       Cepheid, VZ Cet; however, it appears that the component seen as                 
                       variable is the Joy component, recently determined to be a White Dwarf. Skl2010 
                       Recent papers (in particular 1995 PhD thesis by Harold L. Chambers II)          
                       suggest that the visible companion is not the star itself, but the              
                       accretion disc around it (material captured from Mira's stellar wind).          
                       Rapid fluctuations of brightness are described by Warner (1972 MNRAS            
                       159, 95).                                                                       
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Aa,Ab: Pair seen but not measured.                                      Cou1958c
                       Aa,Ab: Additional notes may be found in Couteau (1963).                 Cou1963a
           H 6   1     H VI 1. C is BD-03@355.                                                         
02198-2352 HJ 2130     B is CD-24@1022.                                                                
02200-2213 BRT1373     CD-22@784.                                                                      
02201-1703 GWP 298     ABL  28.                                                                Tob2012b
02204+2456 POU 175     Also known as KU    9.                                                          
02204+1617 BPM  51     [PM2000]   85486 + [PM2000]   85504.                                    Gvr2010 
02204+0135 GWP 299     XMI 258.                                                                Tob2012b
02205+1733 BPM  52     [PM2000]   85552 + [PM2000]   85616.                                    Gvr2010 
02209-0954 GWP 300     ABL  29.                                                                Tob2012b
02209-5632 RST  51     CD-57@470.                                                                      
02210-1650 GWP 301     ABL  30.                                                                Tob2012b
02211+4246 STF 248     Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Combined spectroscopic/visual solution, yielding masses, etc.           Trr1995a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.39 +/- 0.49, 1.78, and 0.85 Msun, respectively.             Mlk2012 
02212+5651 BU 1171     Not seen in 1951 with 82-inch (Van Biesbroeck).                         VBs9999 
02212+3653 GIC  31     AB,C: NLTT 7710/7708                                                    Chm2004 
02213-1057 HJ 3495     B is BD-11@445.                                                                 
02215-1251 GWP 302     ABL  31.                                                                Tob2012b
02215-1354 GWP 303     ABL  32.                                                                Tob2012b
02216+2338 STF 254     POU 178.                                                                        
02219+0824 GWP 304     XMI 259.                                                                Tob2012b
02220+0445 TOK 231     Primary is SB1, P= 79.700 d. Companion at 53" is possibly a white       Tok2012c
                       dwarf (Tokovinin & Lepine 2012)                                         Tok2014d
02220-0034 GWP 305     ABL  33.                                                                Tob2012b
02222-0348 GWP 306     ABL  34.                                                                Tob2012b
02224+5551 BU  875     9 Per. Variable, V474 Per.                                                      
02225+2830 FAR  29     Primary is white dwarf WD 0219+282.                                     Far2006 
02225-0536 GWP 307     ABL  35.                                                                Tob2012b
02225-2349 LAF  27     TOK  40.                                                                        
                       Astrometric binary with 26.5 yr orbit has massive secondary with q~1.   Tok2012a
                       Tokovinin (2013) derived a combined spectroscopic/interferometric               
                       solution, including echelle spectroscopy and speckle interferometry.            
                       The B component is a close binary (tentative period 3.7d); masses of A          
                       and Ba+Bb are nearly equal.                                             Tok2013a
                       Astrometric binary with large acceleration, where the massive                   
                       companion B is in fact a close pair of M dwarfs.                        Tok2013b
           kap For     Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit based on   Gon2002a
                       combination of ground-based catalogs with Hipparcos.                            
02226+1531 LDS3375     G004-016. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 7795/7794                                                          Chm2004 
02229+5835 BLL   7     A is the semi-regular variable, S Per.                                          
02229+4129 TRN  10     The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.7451 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
           HD  14633   Rodgers (1974 M.S. Thesis, Univ. Toronto) made a preliminary orbital            
                       analysis (P =15.3 d) but the variations appear to be more complicated           
                       than originally claimed (Bolton & Rodgers 1978 ApJ 222, 234).           Msn1998a
02229-1718 GWP 308     ABL  36.                                                                Tob2012b
02229-5106 EHR   1     CPM pair.                                                               Ehr2010 
02230+0443 GWP 309     XMI 260.                                                                Tob2012b
02231+7021 MLR 377     A premature orbit has been published.                                           
                       Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995)            Ruy1995 
02231+0246 GWP 310     XMI 261.                                                                Tob2012b
02232-2952 BU  738     T incorrectly listed as 1953.489 by Scardia et al. (1990); should be    Sca1990a
                       1953.849 (erratum noted in Inf. Circ. 112, 1990)                        Sca1990b
                       Parabolic orbit.                                                        Fin1969b
                       sigma = areal constant in the true orbit = 0.0199 arcsec^2/yr                   
                       q = periastron distance in the true orbit = 0".4991                             
02233+2230 LDS3378     NLTT 7840/7842                                                          Chm2004 
02233+1525 AG   38     LDS 879. B is BD+14@387.                                                        
                       AB: NLTT 7845/7843                                                      Chm2004 
                       AB: SHY 417. Bayesian  analysis by Shaya & Olling (2011) indicates      Shy2011 
                       very high (near 100%) probability pair is physical.                          .  
                       HIP 11137. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: HJL  35.                                                            HJL1986 
02233+1452 GWP 311     XMI 262.                                                                Tob2012b
02236-1056 RST4203     Also known as OL  111.                                                          
02238+4920 STF 256     Also known as STF 243.                                                          
02239+5751 MLR 656     Also known as HDS 311.                                                          
02239+5522 BU 1373     The primary is the Cepheid variable V440 Per.                           Evs2016a
02239+3330 STF 258     Also known as STF 253.                                                          
02242+1016 CHR 199     First detected as an occultation binary by Evans.                       Evn1980 
02244-2253 LDS3382     NLTT 7922/7928                                                          Chm2004 
02245-0145 STF 265     HJL  36.                                                                HJL1986 
02246+5959 STF 255     STI 360.                                                                        
02246+2537 ALP   7     2MASSI J0224367+253704                                                          
                       Further observations are required to determine the physical/optical             
                       nature of this pair.                                                    AlP2007 
02246-4050 GC 2912     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Barker et al. (1967).                                                   Evn1967 
02247+4008 LDS3381     NLTT 7887/7890                                                          Chm2004 
02249+5153 ES  764     B is BD+51@567.                                                                 
02249+3039 UC  733     AC: Candidate on Tokovinin list, now reconfirmed as CPM. The primary            
                       hosts an exoplanet.                                                     Tok2013c
02250-1501 GWP 312     ABL  37.                                                                Tob2012b
02252+1217 BRT1170     1deg error in WDS designation, apparently an error in transcribing              
                       coordinates from the original source.                                           
02253-0802 GWP 314     ABL  39.                                                                Tob2012b
02253-1242 GWP 313     ABL  38.                                                                Tob2012b
02255-1834 GWP 315     ABL  40.                                                                Tob2012b
02256+5017 BUP  31     65 And.                                                                         
02257+6133 STF 257     The primary is SB1 V559 Cas, P = 1.58 d.                                        
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
02257+0846 GWP 316     XMI 263.                                                                Tob2012b
02257-2119 HJ 3500     HIP 11324. B = HIP 11323. Both components are below the MS, the true            
                       parallax should be 12.6 mas (as for the B-component in Hipparcos).      Tok2011a
02258-1038 HJ 2140     Identical with HJ 2134, 4 minutes west.                                         
02259+1747 JNN  19     LP 410-22.                                                                      
02260+4228 LDS3383     Aka SLN  57.                                                                    
02260-1520 H 3  80     H III 80. A is a variable of the Alpha CVn type, AB Cet, and a                  
                       spectroscopic binary.                                                           
02262+3428 HDS 318     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.48 +/- 0.19, 1.81, and 1.80 Msun, respectively.             Mlk2012 
02262-0833 GWP 318     ABL  42.                                                                Tob2012b
02262-1602 GWP 317     ABL  41.                                                                Tob2012b
02263+0618 VIG   2     The B component appears to be a faint background star.                  Vig2012 
02265+5417 STF 260     HJL  37.                                                                HJL1986 
02268+5853 HD  14947   Garmany & Stencel (1992 A&AS 94, 211) include this star in Per OB1.     Msn1998a
02268+1034 STTA 27     B is BD+09@322. A is VW Ari, a Delta Scuti-type variable.                       
02269+3733 ADM   2     WSP  33. WASP-33. Primary is del Sct-type variable and exoplanet host.  Adm2013 
02270-0326 GWP 319     ABL  43.                                                                Tob2012b
02272+0309 GWP 320     XMI 264.                                                                Tob2012b
                       HIP 11417. SB, no orbit. NOMAD: PM(B)=(-12,-68), V=14.73.               Nrd2004 
                       Primary is SB2, P=5.997d, but the mass ratio is unknown.                Tok2014d
02273+5433 LAW  10     LSPM J0227+5432. Law et al (2008) derive a distance of 18.6 +9.5/-3.4   Law2008 
                       pc and a projected separation of 13.2 +7.2/-2.2 au. Estimated spectral          
                       types are M4.5 and M5.                                                          
02273-0304 GWP 321     ABL  44.                                                                Tob2012b
02274+3059 INN   1     Rotation periods 12.1d (AG Tri, 13.7d wrong) and 4.7d.                  Skf2013 
02274+1807 GWP 322     XMI 265.                                                                Tob2012b
02278+0426 A  2329     Using the Hipparcos parallax value of 60.22 +/- 1.75 mas, the orbital           
                       elements of Andrade (2007) yield a mass sum of 1.25 +/- 0.14 Msun.      Ana2007 
                       Masses of the two K7V components are estimated at 0.63 +/- 0.01 and             
                       0.62 +/- 0.01 Msun.                                                             
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.37 +/- 0.12, 1.25, and 0.65 Msun, respectively.             Mlk2012 
02279+4710 BWL  10     AB: Primary is a probable member of the AB Dor moving group.            Bwl2015 
02280+0248 GWP 324     XMI 266.                                                                Tob2012b
02280-0520 GWP 323     ABL  45.                                                                Tob2012b
                       WDS designation corrupted at some point to 02280-0303. Corrected.               
02280-3349 SHY 140     HIP  11477 + HIP  11448.                                                        
02281+3251 ES 2407     GCB 6.                                                                          
02282+5423 STF 267     B is BD+53@530.                                                                 
02282+2952 STF 269     STT  41. May also be H 1  21.                                                   
02284-0404 GWP 325     ABL  46.                                                                Tob2012b
02286+5521 ES  872     There is a difference of 18 degrees in the measured angles. The Espin           
                       measure appears correct.                                                Es_1910b
02286-0704 A   447     WSP  77.                                                                        
02287+1850 GWP 326     XMI 267.                                                                Tob2012b
02287-3114 TOK  73     HIP 11537. The V-photometry is affected by small separation. B is red           
                       in the V-K color, variable? Astrometric binary in HIPPARCOS (Makarov            
                       and Kaplan), possibly new triple?                                       Mkr2005 
                       PMS star (Torres et al. 2006).                                          TrC2006 
                       SIMBAD: PMS star and X-ray source 1RXS J022843.6-311332.                Tok2011a
                       Companion is partially resolved in 2MASS images, for that reason the            
                       star is not found in the 2MASS point-source catalog. Pre-main-sequence          
                       star according to SIMBAD.                                               Tok2012a
02288+3215 WOR   2     Tamazian et al. derive a dynamical mass sum of 1.40 +/- 0.25 Msun       Tam2005 
                       and classify the stars as K6-7V and M0V. Absolute magnitudes of                 
                       the two components are estimated at +8.0 and +8.6, leading to                   
                       individual masses of 0.65 and 0.61 Msun, in good agreement with                 
                       the dynamical mass sum.                                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.46 +/- 0.20, 1.25, and 0.55 Msun, respectively.             Mlk2012 
02288-0826 GWP 327     ABL  47.                                                                Tob2012b
02290-0302 GWP 328     ABL  48.                                                                Tob2012b
02291+6724 STF 262     iot Cas. The primary is an unresolved binary, also an Alpha CVn                 
           CHR   6     type variable, P = 1.74 d, and an astrometric, spectroscopic, and               
                       spectrum variable (Rakos 1962; Klock, AJ 70, 176, 1965). The RV         Rak1962 
                       variation has not been confirmed.                                               
                       Heintz (1962) also detected this pair as a submotion to the visual      Hei1962 
                       orbit of the AB pair with a period of 52 years and an amplitude of              
                       0".11. Star C (mag. 8.4, dG4) is probably physical, but Hopmann         Hop1960b
                       (1960) computed a hyperbolic orbit for it, as there is some RV                  
                       difference between C and A.   q = periastron distance in the true               
                       orbit = 6".7056. All hyperbolic orbits were rejected from the                   
                       Fourth and subsequent orbit catalogs.                                   Wor1983 
                       Soderhjelm gives Aa,Ab,B,C quadruple solution (AB in HIP). High         Sod1999 
                       mass-sum, strangely well-behaved speckle obs at  Delta m=4?                     
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Drummond et al. (2003) give solution for Aa,Ab incorporating motion of  Dru2003 
                       the AB pair. The authors conclude that the motion of B relative to              
                       the CHR pair appears to be rectilinear. Masses of the CHR components            
                       are derived.                                                                    
                       1985.8540: This autocorrelogram was remeasured; the new results are             
                       listed in the catalog.                                                  McA1987b
           STF 262     AB: H 1  34.  AC: H 3   4.                                              MEv2010 
                       AC: Hyperbolic orbit.                                                   Hop1960b
02291+2331 VBS   6     The inclination must be high.                                                   
02294+5532 STF 268     A is a spectrum variable and shell star.                                        
02296+6039 STF 263     A is a possible Beta Cep variable, V528 Cas.                                    
02297-0030 GWP 329     ABL  49.                                                                Tob2012b
02297+0134 GWP 330     XMI 268.                                                                Tob2012b
02297-0955 GAL 321     Object #69 in Gallo's original list.                                    Gal1912b
02305+2514 STF 271     AB: H N  12.                                                            MEv2010 
02307-0407 GWP 331     ABL  50.                                                                Tob2012b
02308+5533 STF 270     AB: HJL  38.                                                            HJL1986 
                       Is there a wobble in the PA of AB?                                      Tok2014d
02309+0158 GWP 332     XMI 269.                                                                Tob2012b
02310+1358 GWP 333     XMI 270.                                                                Tob2012b
02310+0823 GIC  32     G004-024/G073-059.                                                              
02313-1310 GAL 322     Object #70 in Gallo's original list.                                    Gal1912b
02315+0106 SHY 422     BC: HIP  11736 + HIP  12728.                                                    
02318+8916 STF  93     alp Umi = 1 UMi = Polaris. Cepheid variable and spectroscopic binary,           
                       P = 30y. A close companion has been suspected. The close pair,                  
                       measured three time from 1937-1939 by R.H. Wilson using an eyepiece     WRH1941b
                       interferometer, was not seen again until Evans et al. (2006) resolved   Evs2006 
                       it with HST.  Wilson's measures agree with the combined astrometric/            
                       spectroscopic solution by Gerasimovic (1936), although both orbit and   Ger1936 
                       measures are called into dispute by the more recent orbit of Wielan et  Wln2000 
                       al. (2000), whose solution includes mass estimates, etc.                        
                       An earlier orbit by Wyller (1957) was rejected from Fourth Orbit        Wye1957 
                       Catalog ("amplitude below noise level")                                 Wor1983 
                       Component B = BD+88@@@7. See discussion of this system by Roemer.       Re_1965 
                       The C component was observed by Burnham in the late 19th century, then  Bu_1894 
                       not seen again until the early 21st century by Daley and Ashcroft.      Dal2006a
                       The extremely large magnitude makes the pair too close for most large           
                       astrometric surveys.                                                            
                       The D component has also been recently recovered in 2MASS data.         TMA2003 
                       According to Jim Daley, the R-I color for C is 0.56 and for D it is             
                       0.67. The V-I color for D is 1.08.                                      Dal2006b
                       AB: H 4   1.                                                            MEv2010 
02318-0021 GWP 334     ABL  51.                                                                Tob2012b
02319+5742 BU 1314     V425 Per. Variable in light and radial velocity.                                
02319+0108 LDS9132     Old LDS6132. Primary is confirmed quasar: Z = 1.26.                             
02320+1822 STF 273     H N 106.                                                                MEv2010 
02320-1955 BRT 297     LDS3400.                                                                        
02321-1515 GWP 335     ABL  52.                                                                Tob2012b
                       sig Cet. B is BD-15@@447.                                                       
                       SHY 141. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
02323+4630 BRT 330     Since precise position has been corrected from previous precise         WSI2002 
                       position null detection not relevant.                                           
02324-1849 GWP 336     ABL  53.                                                                Tob2012b
02327+6127 STI 368     Both visual components were observed and appeared to be single.         Msn1998a
           MZA   8     EL and EM pairs were originally 02326+6128 MZA   8AB and AC, until              
                       match of E component of 02327+6127 to primary of 02326+6128 noticed.            
02327+0704 GWP 337     XMI 271.                                                                Tob2012b
02328+0021 GRV1174     SLW 119.                                                                        
02328-3421 LDS9133     Old LDS6133.                                                                    
02329+3433 GC 3048     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
02329+1502 TOK  12     Estimated period of visual pair 160y.                                   Tok2006 
                       Primary is SB2, P=19.4161d (Katoh et al. 2013 AJ 145, 41)               Tok2014d
02330+4852 HJ 2144     B is BD+48@694.                                                                 
02331-7738 BVD  25     B is CPD-78@59.                                                                 
02332-2207 DON  35     CD-22@863.                                                                      
02333+5219 STT  42     Distance small, measures often discordant.                                      
                       1982.7604: This autocorrelogram was remeasured; the new results are             
                       listed in catalog.                                                      McA1987b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.00 +/- 1.28, 4.13, and 2.19 Msun, respectively.  Mlk2012 
02333-1933 GWP 338     ABL  54.                                                                Tob2012b
02333-7554 HJ 3522     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
02335+5732 HJ 2143     B is BD+56@657.                                                                 
02338-2814 HJ 3506     ome For.                                                                        
02340-1812 BRG  13     There is insufficient motion between the two epochs of observation of           
                       2MASS J02335984-1811525 to establish common proper motion of the                
                       binary, but the components are nearly equal brightness and color, and           
                       reside at a relatively small separation of ~0.85" hence it is almost            
                       certainly a physical pair.                                              Jnn2012 
02342+0916 GWP 339     XMI 272.                                                                Tob2012b
02342+0139 LDS9134     Old LDS6134.                                                                    
02343+4017 AG   42     STF 275.                                                                        
02344+3542 J  1810     ALI 35.                                                                         
02344+2040 A  2218     Identification error in ADS. Pair is BD+20 426, not BD+19 375.          Cou1970c
02344-4259 HJ 3510     Spectrum: G3/5III/IV.                                                           
02347-0752 BUP  32     77 Cet.                                                                         
02350-1522 GWP 340     ABL  55.                                                                Tob2012b
02351-1046 GAL 323     Object #71 in Gallo's original list. Aka J  1452.                       Gal1912b
02352+0407 TOK 649     Resolved using ANDICAM2. Primary SB?                                    Tok2014d
02353+4017 A  1818     Baize suspected another close pair in the region.                               
02353-0334 MUG   2     Followup spectroscopy confirmed the B component is a dwarf; estimated   Mug2005 
                       mass is 0.286 +- 0.017 Msun. Primary is planet host star. Colors of B   Egn2007 
                       component consistent with M1-M4 dwarf with mass 0.31 +/- 0.02 Msun.     Met2009 
                       HIP 12048. The B component estimated mass 0.29Msun.                             
                       2001.7454: PA is measured in zenith mode. If data collected in                  
                       equatorial mode, PA = 183.7.                                            Rbr2011d
           79 Cet      A: Combined solution, based on reduction of Hipparcos intermediate              
                       astrometric data together with spectroscopic elements from Marcy et al. CPS2000b
02354-0228 GWP 341     ABL  56.                                                                Tob2012b
02355+5948 HIP  12062  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Latham et al. (2002). They derived component masses 0.96 and 0.45 Msun  Lat2002 
                       and an estimated semimajor axis of 35.47 mas.                           Ren2013 
02356+6106 RAO   7     Primary is close astrometric binary; also SB?                           Tok2014d
02356+3719 STF 279     AB: H N  47.                                                                    
02358+3441 AG  304     15 Tri. B is BD+34@471.                                                         
02359+6338 CTT   3     The B component is BD+62@423.                                                   
02359+1515 GWP 342     XMI 273.                                                                Tob2012b
02359+0536 STF 281     nu Cet = 78 Cet                                                                 
                       The A component is a 714d spectroscopic binary. B is not a binary, so           
                       this is a physical triple.                                              Grf2015a
02359-2830 SWR   4     CPM pair                                                                Skf2004 
02360-0750 BUP  33     80 Cet.                                                                         
02360-1312 GWP 343     ABL  57.                                                                Tob2012b
02360-2331 GIZ   1     GJ 1048.  Discovered by Gizis et al. (2001) on 2MASS images. The A      Giz2001 
                       component is K2V; conclude secondary is L1, mass ~0.077 Msun.                   
                       Seifahrt et al. (2004) combine 2MASS measure with earlier UK Schmidt    Sef2004 
                       near-IR southern survey data to show stars have similar proper motion,          
                       so are likely physical companions.                                              
02361+0653 GKI   1     AB: This object was misidentified as HD 61660 by McAlister (1978).      McA1978c
           PLQ  32     AC: GJ 105. Proper motion of A +1811 +1451 (FK5). Spectroscopic binary          
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       HIP 12114. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
02362-1656 GWP 344     ABL  58.                                                                Tob2012b
02363-0500 GWP 345     ABL  59.                                                                Tob2012b
02363-6329 B  1435     Spectral type F6?                                                               
02366+1231 GWP 346     XMI 274.                                                                Tob2012b
02366+1227 MCA   7     31 Ari. This system has a small Delta m (~0.1 in the blue, 0.3 in the           
                       red) as determined from lunar occultation measures by Africano et al.   Afr1978 
                       Measures in 1982.7659, 1984.7046, and 1988.6544 were based on           Hrt1994 
                       reprocessing of archival video data.                                    Hrt2000a
                       Martin et al. (1998) derive component masses 11.001 +/- 1.969 and               
                       9.407 +/- 1.707 Msun.                                                   Mig1998 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 19.08 +/- 2.57, 2.95, and 1.13 Msun, respectively.            Mlk2012 
02368+1723 BPM  53     [PM2000]   95004 + [PM2000]   94927.                                    Gvr2010 
02368-1929 ARA 523     BRT1374.                                                                Brt1935b
02369+5953 STF 277     V791 Cas, a Beta Lyr type eclipsing binary, P = 2.88680d.               Zas2012 
02370+2439 STFA  5     30 Ari. STTA 29. A is 1.1d SB1; AB has estimated period of 34,000y.     Tok2006 
                       B is BD+24@375.                                                                 
                       HJL  39.                                                                HJL1986 
                       SHY 142. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       H 5  49.                                                                MEv2010 
                       Primary is SB2, P=1.109d. B is exoplanet host, P=335d. A is F6III, but          
                       on the MS.                                                              Tok2014d
           RAO   8     BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral            
                       types of B and C as F8V and M1V.                                        Rbr2015a
02370-3435 MUG  12     Primary is GJ 9088 = lam 2 For. Spectral type of comoving secondary             
                       estimated as M5-6, confirmed by follow-up spectroscopy. Mass of                 
                       secondary ~0.11 Msun.                                                   Mug2014 
02371+6232 MLR  31     No significant movement since first resolution.                         Drd2009 
02371+1740 GWP 347     XMI 275.                                                                Tob2012b
02371-0926 ITF  62     BD: Originally 02368-0926ITF  62.                                               
02371+0055 LDS5388     Error in WDS designation - incorrect precession of Luyten coordinates?  Luy1984 
02371-2951 LDS3405     NLTT 8520/8519                                                          Chm2004 
02374-5233 EHR   2     Primary is eta Hor. Physical/optical nature ambiguous.                  Ehr2010 
           TOK 186     Aa,Ab: The Marion et al. (2014) measure is in good agreement with the   Mrn2014 
                       Hartkopf et al. (2012) discovery observation, but hints at a            Tok2014a
                       significantly eccentric and/or inclined orbit. A face-on, circular              
                       orbit with a semimajor axis of 3.6au would have a period of ~3.7y,              
                       which is in line with the 3.0y astrometric period found by Goldin &             
                       Makarov (2007).                                                         Gln2007 
02376+2250 LDS1132     NLTT 8503/8502                                                          Chm2004 
02378+1737 BPM  54     [PM2000]   95638 + [PM2000]   95705.                                    Gvr2010 
02380+1418 GWP 348     XMI 276.                                                                Tob2012b
02381-0541 SLW 126     Aka ABL  60.                                                                    
02382+4604 A  1278     A premature orbit has been computed.                                            
02382-1123 STF 288     H 3  79.                                                                MEv2010 
02383-3012 UC  766     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02386+0327 KUI   9     HR 775 in Cetus. Some scatter in measured position angles.                      
02387-5257 COO  14     Spectrum: F8IV/V + G/K.                                                         
           SHY 424     AC: HIP  12326 + HIP  12361.                                                    
02388+3325 STF 285     H 1  21.                                                                MEv2010 
02389+1526 AG   43     HU 1043.                                                                        
02389-5450 HJ 3520     B is CPD-55@444.                                                                
02390+6235 STTA 28     B is BD+61@445.                                                                 
02390+1452 STF 287     H N 107.                                                                MEv2010 
02392-0016 GWP 350     ABL  62.                                                                Tob2012b
02392-0933 GWP 349     ABL  61.                                                                Tob2012b
02394-0318 GWP 351     ABL  63.                                                                Tob2012b
02396-1152 FIN 312     eps Cet = 83 Cet. Pourbaix gives combined solution for this resolved            
                       SB2, yielding orbital parallaxes and component masses.                  Pbx2000b
                       Arenou give combined solution of astrometric orbits and DSBs. Paper             
                       includes masses and distances.                                          Are2000 
                       Systematic errors are clearly present and the period remains in doubt.  Fin1954c
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.68 +/- 0.35, 2.39, and 2.40 Msun, respectively.             Mlk2012 
                       Docobo & Andrade (2013) derive a dynamical parallax of 41.43 +/- 0.68           
                       mas and component masses 1.37 +/- 0.09 and 1.03 +/- 0.08 Msun. See              
                       paper for extensive notes on this system.                               Doc2013d
02398-1522 GWP 352     ABL  64.                                                                Tob2012b
02398-3354 LDS3413     HIP 12411. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
02399+0009 A  1928     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.83 +/- 0.56, 2.33, and 1.05 Msun, respectively.             Mlk2012 
02399-2429 TOK 205     A faint companion near the detection limit is found, our measures are           
                       uncertain. The estimated long period P ~ 100 yr suggests that the               
                       Hipparcosacceleration of 17 mas yr-2 is spurious.                       Tok2012a
                       The tentative resolution on 2011.84 at 78deg, 0".34, dK=3.8 is not              
                       confirmed here, with new good-quality images. The star has constant RV          
                       so could be single.                                                     Tok2013b
02401+1148 FAR  30     Primary is white dwarf WD 0237+115.                                     Far2006 
02401+0255 UC  771     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
02402+0436 HDS 347     Mean motion indicates P ~ 90 yr, rho increasing.                        Msn1999b
02405-1341 GAL 324     Object #74 in Gallo's original list.                                    Gal1912b
02406+3420 WNO  43     Aa,Ab: Identified as WNO  13 by Routley.                                USN1972 
           GIC  33     AB = G074-039/G074-040. AC = G074-039/G074-041.                                 
                       AB: NLTT 8633/8634                                                      Chm2004 
02407+6117 STF 284     A is a Beta CMa-type variable, V482 Cas.                                        
           CHR 208     Both visual components were observed: A was resolved (CHR 208Aa,Ab),            
                       B appeared to be single.  Gies & Bolton (1986) found a large scatter    Gie1986 
                       in radial velocities (but could not find a suitable period), and this           
                       suggests that at least one component may be a spectroscopic binary.     Msn1998a
02407+2704 STF 289     33 Ari. A spectroscopic binary.                                                 
                       HJL  41.                                                                HJL1986 
                       H 4   5.                                                                MEv2010 
02407+2637 STT  43     Scardia et al. (2001) orbit considered preliminary because the arc of   Sca2001d
                       the observed orbit is only 90 degrees and is placed completely around           
                       aphelion. The Hipparcos parallax of 0".01385 +/-  0.00125 gives a mass          
                       sum of 3.1 Msun, an overestimate for a star of type F7V. The dynamical          
                       parallax of 0".0149 agrees well with the measured one.                          
02410+6539 STF 282     AB: HJL  40.                                                            HJL1986 
02410+3905 A  1820     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
02410-2506 LDS3414     NLTT 8688/8689                                                          Chm2004 
02412-0042 STF 295     84 Cet. A is a Delta Scuti-type variable.                                       
02413+2659 L    55     Since precise position has been corrected from previous precise         WSI2013 
                       position null detection not relevant.                                           
02413-0432 BWL  12     Colors and/or astrometry are inconsistent with a late-type common               
                       proper motion companion based on visual inspection of the field from            
                       2MASS, SDSS, DSS1, and/or DSS2. Primary is G 75-35.                     Bwl2015 
02413-5725 BRG  14     2MASS J02411909-5725185 is yet to be confirmed as a common proper               
                       motion binary, but the color and brightness of the companion are well           
                       consistent with it being bound.                                         Jnn2012 
02414+3629 HJ  328     Aka ALI 269.                                                                    
02415+4053 COU1511     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.86 +/- 1.13, 2.54, and 1.05 Msun, respectively.             Mlk2012 
02415+1115 GWP 353     XMI 277.                                                                Tob2012b
02418-5300 JFF   1     Aka CAB   6.                                                                    
02420+4248 HJ 1123     B is BD+42@588, spectrum B9IVp(Hg,Mn,Eu).                                       
02420-1824 GWP 354     ABL  65.                                                                Tob2012b
02421+1351 LDS3416     NLTT 8720/8721                                                          Chm2004 
02421-0134 OL    9     Since precise position has been corrected from previous precise         WSI2004b
                       position null detection not relevant.                                           
                       Aka RST4211.                                                                    
02422+4242 HJ 1124     Aka BKO 172.                                                                    
02422+4012 MCA   8     12 Per. SB2 resolved by speckle interferometry by McAlister (1977).     McA1977 
                       Elements P = 331.0d, T, e, and longitude of periastron for McAlister    McA1978a
                       solution are from the spectroscopic orbit by Colacevich (1941).         Cla1941 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Colacevich (1941).                                                              
                       Martin et al. (1998) derive component masses 1.125 +/- 0.169 and                
                       1.389 +/- 0.193 Msun.                                                   Mig1998 
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Bagnuolo et al. (2006) solution combines speckle data with data from    Bgn2006 
                       the CHARA Array. Authors derive orbital parallax 41.19 +/- 0.21 mas,            
                       masses 1.382 +- 0.019 and 1.240 +- 0.017 Msun, and a magnitude                  
                       difference 0.409 +/- 0.013 mags in K' (2136 nm). Values for omega and           
                       Omega are switched in their Table 3.                                            
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.59 +/- 3.80, 2.58, and 1.07 Msun, respectively.             Mlk2012 
02422-2445 LDS3418     NLTT 8753/8759                                                          Chm2004 
02423+1639 BPM  55     [PM2000]   98625 + [PM2000]   98718.                                    Gvr2010 
02423+1415 GWP 355     XMI 278.                                                                Tob2012b
02424+3837 EVT   1     Aa,Ab: Exo-planet host                                                  Tok2014d
02424+2001 BLA   1     Aa,Ab: mu Ari = 34 Ari. Occultation binary, known to have variable              
                       radial velocity.                                                        Bag1984b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 3.64 +/- 0.47, 5.77, and 2.24 Msun, respectively.  Mlk2012 
02424+0247 GWP 356     XMI 279.                                                                Tob2012b
02424-0214 LDS9135     Old LDS6135.                                                                    
02424-1358 LDS3419     NLTT 8758/8757                                                          Chm2004 
02425+4016 STF 292     B is BD+39@611.                                                                 
                       H 4  64.                                                                MEv2010 
02425+1045 CHR 200     First detected as an occultation binary by Blow et al.                  Blw1982a
02426-5048 iot Hor     Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from Kurster      CPS2000e
                       et al. (2000).                                                          HaI2001 
           HD  17051   No comoving objects found within separation/magnitude range listed.             
                       However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                       background object.                                                              
02426-7947 TOK 362     This 0.6" pair with dK=1.1 is obvious and should have been resolved             
                       both by visual observers and by Hipparcos, yet there are no                     
                       indications of previous resolution in the literature. The declination           
                       of -79deg may have something to do with the missed companion, as the            
                       southern sky is less well surveyed for binaries.                        Tok2013b
02427+3932 J  2401     Jonckheere says is two faint condensations of a nebula. Galaxy           .      
                       UGC 2180.                                                               J__1962a
02427+1434 GWP 357     XMI 280.                                                                Tob2012b
02427-1513 GWP 358     ABL  67.                                                                Tob2012b
02428+4249 HJ 2155     B is BD+42@605.                                                                 
02431+0330 GWP 359     AB: XMI 281AB.                                                          Tob2012b
           GWP 360     AC: XMI 281AC.                                                          Tob2012b
02433+1926 BAG  20     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin et al. (1985).                                                  Grf1985b
                       Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       However, this is a Hyades non-member                                    Grf1988 
                                                                                               Grf2013c
02433+1718 BPM  56     [PM2000]   99282 + [PM2000]   99285.                                    Gvr2010 
02433+0314 STF 299     gam Cet = 86 Cet. AC is a CPM pair, according to Alden.                 Ald1924 
                       AB: Additional notes may be found in Muller (1946).                     Mlr1946a
02434-3756 TOK 187     Triple. The A-component is 0.955d SB2; the tertiary is resolved with            
                       speckle. As A is located some 1.7m above the main sequence, the object          
                       can be closer than indicated by the Hipparcos parallax of 24.6 mas.     Tok2012a
02434-6643 FIN 333     Probably an ambiguous case, although only one solution has been                 
                       tested.                                                                         
                       More speckle obs needed to define orbit.                                        
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 14.55 +/- 4.04, 2.67, and 1.20 Msun, respectively.            Mlk2012 
02435+2742 35 Ari      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Abt & Levy (1978).                                                      AbH1978 
02435+1611 BPM  57     [PM2000]   99396 + [PM2000]   99434.                                    Gvr2010 
02438-2754 BU  261     Aka HDO  59.                                                                    
02440-0601 TOK  75     HIP 12764. A is SB, no orbit, dRV= 2.5). Contradictory photometry of    Nrd2004 
                       B, it is too close in 2MASS (5"). NOMAD: PM(B)=(-99,-71) V=7.79 (??)            
                       Considering the brightness of B and  N*=15, it is almost certainly      Tok2011a
                       physical. A new triple system. See Bonavita & Desidera (2007).          Bnv2007 
02442+4914 STF 296     the Per = 13 Per. A premature orbit has been computed.                          
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Data appear equally well fit by rectilinear solution - see catalog.             
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AB: H 3  58.                                                            MEv2010 
02442-2530 FIN 379     Aa,Ab: More than one revolution apparently has occurred.                        
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.55 +/- 0.22, 2.20, and 1.02 Msun, respectively.  Mlk2012 
           BSO   1     HIP 12780. A is visual binary FIN 379, 0.1". B = HIP 12779.             Tok2011a
02443+5704 STF 293     AB: Additional notes may be found in van den Bos.                       B__1963b
02443+1600 GWP 361     XMI 282.                                                                Tob2012b
02445-1859 GWP 362     ABL  68.                                                                Tob2012b
02446+7912 BVD  26     Primary is V405 Cep.                                                            
02446+2928 STF 300     H 1  74.                                                                MEv2010 
02448+4231 LDS3424     NLTT 8830/8829                                                          Chm2004 
02448+1536 KIR   7     A close double dwarf pair,spectral types M5V and M5.5V.                 Kir1999 
02449+5456 ES   50     Initially assigned as TDS  94. Corrected 11/27/01.                              
02449+1007 TOK   1     Aa,Ab: mu Cet = 87 Cet. Considered somewhat uncertain by Tokovinin.             
                       Not resolved by McAlister on several occasions.                                 
                       A preliminary spectroscopic orbit with a period of 1202 days has been           
                       published by Abt (1965).                                                AbH1965 
02449-1336 GWP 363     ABL  69.                                                                Tob2012b
02451-1834 tau 1 Eri   Despite a large acceleration of 26 mas yr-2, no RV variability was              
                       found in the GCS from two measures.                                     Tok2012a
02452-4344 CPO  29     LDS  78.                                                                        
           BRG  15     Aa,Ab: 2MASS J02451431-4344102 is a member of an approximately equal-           
                       brightness binary with ~50" separation, in addition to being a close            
                       binary discovered with AstraLux.                                        Jnn2012 
02452-6700 GLI  18     Spectrum: F5/6III/IV.                                                           
02455-6342 HDO 306     gam Hor. A spectroscopic binary.                                                
02456-7114 HDS 357     Primary is CN Hyi, a W Uma type eclipsing binary, period 0.45611d.      Zas2012 
02457+4456 LDS5393     old LDS6136.                                                                    
                       AB: NLTT 8869/8870                                                      Chm2004 
           GIC  34     AC = G078-004/G078-003 = GJ 3178A+3179B.                                        
02457-3943 B  2077     Astrometric orbit for primary, P=2.303y (Golden & Makarov 2007). PM(A)  Gln2007 
                       moves almost towards B, so the increased separation is not reflex PM.   Tok2014d
02460-0457 BU   83     A premature orbit has been calculated.                                          
                       A: Dommanget (1972) astrometric orbit calculated from perturbations     Dom1972a
                       seen to rectilinear motion.                                                     
02461+1250 GWP 364     XMI 283.                                                                Tob2012b
02462+0536 RAO   9     AB: Primary is HIP 12925. A 13.8m star at 221.7deg, 494.3" appears to           
                       share common proper motion, but the probability of physicality is only          
                       36%. It is likely this star is another member of the Tuc-Hor moving             
                       group.  HIP 12925 and 12862 also appear to be a co-moving pair.         Tok2013c
                       AB: The primary is a spectroscopic binary.                              Tok2014d
                       Quadruple system with 3-tier hierarchy: a close spectroscopic pair              
                       with yet unknown period, Robo-AO companion D at 1".89, and CPM                  
                       companion C at 494" (Tokovinin & Lepine 2012). Yet another star,        Tok2012c
                       HIP 12862, at 0.9deg, also shares common PM and parallax. The stars             
                       are young and belong to the Tucana–Horlogium moving group (Zuckerman    .     
                       et al. 2011 ApJ 732, 61). Our photometry places D slightly above the            
                       MS. D was  independently discovered by Brandt et al. (2014) by high-    Bdt2014 
                       contrast imaging at Subaru. They measured it on 2012.0 at 252.9 deg     RAO2015 
                       and 1".893, in excellent agreement with Riddle et al. (2015).           Rbr2015d
           TOK 651     AC: Tuc-Hor moving group? Additional CPM companions at 725" and 1536".  Tok2014d
                       AD: Too wide to be a companion at 3271", but CPM, common parallax. F            
                       is a rapid rotator (Vsini=109km/s), on main sequence.                           
02462-0619 GWP 365     ABL  70.                                                                Tob2012b
02463+1427 GWP 366     XMI 284.                                                                Tob2012b
02464+0301 GWP 367     XMI 285.                                                                Tob2012b
02470-0952 A  2608     The northern pair, CD, is slightly fainter                              Hei1985a
02470-1320 RST3371     Variable: CU Eri.                                                               
02472+3611 ALI  38     No star seen at AC catalog location of the purported secondary                  
                       - probably a plate flaw.                                                        
02473+1812 BPM  58     [PM2000]  102021 + [PM2000]  102010.                                    Gvr2010 
02473+1803 GWP 368     XMI 286.                                                                Tob2012b
02473+1717 A  2222     CD: Aitken gives the magnitude of B as 13.8. I could not see it at all          
                       on the first two nights, glimpsed it on the fourth, and made a very             
                       uncertain measure on the third. Variable?                               B__1962d
02474-1733 GWP 369     ABL  71.                                                                Tob2012b
02475+1922 STF 305     A premature orbit has been computed.                                            
02476+5357 STF 301     A is a long-period spectroscopic binary, P = 675d.                              
02476+1014 HJ  655     Hipparcos identified the B component as a candidate for Hyades          HIP1998 
                       membership. However, re-reduction of the Hipparcos parallax places      VlF2007 
                       the B component elsewhere, so this is an optical pair.                  Grf2013c
02478-0411 GWP 370     ABL  72.                                                                Tob2012b
02479-0529 GWP 371     ABL  73.                                                                Tob2012b
02480-0108 GRV 993     SLW 134.                                                                        
02480-0940 GAL 325     Object #76 in Gallo's original list.                                    Gal1912b
02480-2836 RED  20     One companion is ~10" from CD-29 1020 = 2MASS J02481094-2835382.  To            
                       the SW at a milar distance is 2MASS J02480263-2835465. There are no             
                       USNO-B1 proper motions for the fainter stars, but comparison of                 
                       Digitized Sky Survey UKST and 2MASS images show little evidence of              
                       significant relative motion. IR colors are consistent with a K0/M3/M6           
                       triple at 60pc. System appears non-hierarchical, with projected                 
                       separations of ~600au between each component.                           Red2007a
02481-1244 GAL 326     Object #77 in Gallo's original list.                                    Gal1912b
02482+2704 LDS1138     HIP 13081. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
           LDS1138     NLTT 8997/8996                                                          Chm2004 
02483+1532 BPM  59     [PM2000]  102707 + [PM2000]  102652.                                    Gvr2010 
02486+1344 GRV 146     NI    4.                                                                        
                       Primary is BQ Ari, a W UMa type eclipsing binary, period 0.282335d.     Zas2011 
02487+3107 GJ 9102     1981.6875: HD 17433 was misidentified as Gliese 113 by Balega et al.    Bag1984b
                       (1984). It is uncertain whether this observation is of HD 17433 or of           
                       GJ 113 = HD 17382.                                                              
02488-0301 GWP 372     ABL  74.                                                                Tob2012b
02489+3823 ALD  10     First measure probably 90@ in error.                                    Ali1955 
02490-1029 BRG  16     The system is precisely at the 3 sigma threshold for statistically              
                       significant exclusion of the background star hypothesis. By chance,             
                       the AB astrometry is just below the criterion (2.7 sigma) and BC is             
                       just above (3.1 sigma), so in principle the BC pair is inconsistent             
                       with chance alignment, if the pair does share a common proper motion            
                       with  A. However, the proper motion of the system has of course been            
                       determined based on A, so until the AB physical connection has been             
                       demonstrated to the required accuracy, the 3.1 sigma confidence of the          
                       BC pair is irrelevant. Hence, we label the entire system as                     
                       undetermined for now, although it is obviously very likely that the             
                       whole system is indeed bound.                                           Jnn2012 
02491-1712 GWP 373     ABL  75.                                                                Tob2012b
02491-3224 B  1031     bet For                                                                         
02493+1728 STF 311     pi Ari = 42 Ari. A is a spectroscopic and occultation binary.                   
                       AB: H 1  64.                                                            MEv2010 
02494+4336 LDS3429     LDS9137. LDS6137.                                                               
                       NLTT 9035/9037                                                          Chm2004 
02495+5705 MCA   9     V480 Per.                                                                       
02496-0932 GWP 374     ABL  76.                                                                Tob2012b
02497+1209 CHR 201     First detected as an occultation binary by Evn1983a.                            
02498-0220 GWP 376     ABL  78.                                                                Tob2012b
02498-0346 GWP 375     ABL  77.                                                                Tob2012b
02498-2015 HJ 3533     B is BD-20@523.                                                                 
02498-2434 BU  877     gam 1 For. AB =? LDS  80. Separation and position angle (sf)                    
                       agree, as does the DM number from LDS catalog. The quoted primary               
                       magnitude of the LDS pair is much fainter, however - possibly a poor            
                       measure of CB instead?                                                          
02499+0856 STF 313     B component is EE Cet, a W UMa type eclipsing binary, P = 0.37992d.     Zas2012 
02499-0206 GWP 377     ABL  79.                                                                Tob2012b
02500+2716 MCA  10     Aa,Ab: 41 Ari. Aa is a spectroscopic binary and resolved                        
                       interferometer pair.                                                            
           STT  47     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
           H 5 116     AC: H V 116.                                                                    
                       AC: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
           H 6   5     AD: H VI 5. D is BD+26@470.                                                     
02501+1646 GWP 378     XMI 287.                                                                Tob2012b
02502+7255 HJ 2157     Also known as STF 298.                                                          
                       Primary is V793 Cas, an Algol-type eclipsing binary, period 1.652303d.  Zas2011 
02502+1343 SHY 426     HIP  13223 + HIP  13122.                                                        
02502+0641 AG   55     AB,C: HJL  42.                                                          HJL1986 
02502-3551 HJ 3536     eta 2 For                                                                       
02504+3551 LDS3430     Old LDS6138. LDS9138.                                                           
                       NLTT 9076/9097                                                          Chm2004 
02505+1113 BPM  60     [PM2000]  104291 + [PM2000]  104261.                                    Gvr2010 
02505-0414 GWP 379     ABL  80.                                                                Tob2012b
02506+3819 BUP  34     16 Per.                                                                         
02507+5554 STF 307     eta Per = 15 Per. A is a spectroscopic binary. B is BD+55@712.                  
02507+1910 TOK  76     HIP 13269. The 2MASS PSC companion at 17.2" is likely an artifact (not          
                       detected in J and H bands). A is an astrometric binary.                 Tok2011a
02507+1601 BPM  61     [PM2000]  104457 + [PM2000]  104476.                                    Gvr2010 
02508-3956 SHY 427     AB: HIP  13271 + HIP  13499.                                                    
02509+0331 PLQ  36     LDS3432.                                                                        
02510+1317 GWP 381     XMI 289.                                                                Tob2012b
02510+1329 GWP 380     XMI 288.                                                                Tob2012b
02510-2100 SEE  20     tau 2 Eri = 2 Eri                                                               
02511+6025 STF 306     Spectroscopic binary, also classified Oe5V and O7.5.                            
                       AC: See BDS 1430.                                                               
                       AG: G component = A component of 02512+6023.                                    
           STI 398     EF: previously 02512+6025STI 298AB, merged with STF 206 system.                 
                       fh: previously 02512+6025STI 298bc, merged with STF 206 system.                 
02512+6023 D  9001     See BDS 1431.                                                                   
02513+0303 HO  218     Position angle and distance changing rapidly but                                
                       period not established. Needs speckle.                                          
02514-1526 GWP 382     ABL  81.                                                                Tob2012b
02514-2139 DON  43     Gomez et al. (2016) derive dynamical parallax and component masses:             
                       8.24 +/- 0.22 mas, 1.110 +/- 0.014 Msun, 1.045 +/- 0.013 Msun.          Doc2016i
02516+6033 BU 1374     B component spectral type B0III                                         AbH2000 
                       CD: Also known as STI 400.                                                      
02517+5921 GIC  35     G246-014/G246-013.                                                              
02518+5819 BLL   8     A is a spectroscopic binary. B is BD+57@652.                                    
02518-2117 SEE  21     This very close visual system was discovered at a separation of 0".36   See1898b
                       and has closed steadily for over 90 years. It is unknown at this                
                       point whether the system is still approaching periastron or has                 
                       begun to widen.                                                         Hrt1993 
02520-5347 BRT2020     CD-54@578.                                                                      
02521+1536 GWP 383     XMI 290.                                                                Tob2012b
02521-6054 HJ 3540     CD-61@515.                                                                      
02522+1520 BPM  62     [PM2000]  105424 + [PM2000]  105482.                                    Gvr2010 
02525+2505 LDS1140     NLTT 9175/9176                                                          Chm2004 
02525-1246 LWR   4     EP Eri                                                                          
02527-1105 GWP 384     ABL  84.                                                                Tob2012b
02529+5300 STF 314     AB,C: H 1  38.                                                          MEv2010 
02531-1212 GAL 327     Object #78 in Gallo's original list.                                    Gal1912b
02532+4155 LDS9139     Old LDS6139.                                                                    
02532-1007 GWP 385     ABL  85.                                                                Tob2012b
02533+2714 ALP   8     2MASSI J0253202+271333                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
02536-0745 GWP 386     ABL  86.                                                                Tob2012b
02536-3826 TOK 652     Primary is psi For                                                      Tok2014d
02537+3820 BU  524     AB: 20 Per. Barnard gives this as 20 Per = BU 520.                      Bar1898b
                       Star A is a suspected variable of Delta Scuti type. A suspected                 
                       spectroscopic 3.5 yr period is not confirmed (Scarfe & Fekel 1978).     Scf1978 
                       A measure on 1979.5326 was incorrectly attributed to ADS 2200 by                
                       McAlister & Hendry (1982); it actually belongs to ADS 490.              McA1982d
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Aristidi et al. (1999) orbit includes mass determination.               Ari1999 
                       Docobo et al. (2001) orbit includes mass determination.                 Doc2001c
                       Calculated mass sum is 3.88 +/- 0.58 Msun, a bit high for a pair of             
                       mid-F dwarfs.                                                           Mut2010b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.88 +/- 0.60, 2.99, and 1.38 Msun, respectively.  Mlk2012 
           STF 318     AB,C: HJL  43.                                                          HJL1986 
                       AB,C: H 3  60.                                                          MEv2010 
02542+3644 ES 2555     ALI 274.                                                                        
02542-1225 GWP 387     ABL  87.                                                                Tob2012b
02543+5246 LAB   1     Aa,Ab: tau Per = 18 Per. Spectrum composite; G4III+A4V. A is a                  
                       long-period spectroscopic binary, resolved by speckle interferometry.   Lab1974 
                       Speckle observations have resolved the pair and invalidate an                   
                       astrometric solution by Kamper (1969).                                  Kam1969a
                       van de Kamp & Andersen orbit rejected from Fourth Orbit Catalog         Kam1969a
                       ("amplitude below noise level")                                         Wor1983 
                       The elements P, T, e, and longitude of periastron for the McAlister     McA1981c
                       (1981) orbit are from the orbit by Colacevich (1941).                   Cla1941 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Demircan & Selam (1992).                                                Dmr1992 
                       The 52" distant, visual double BC may be physical.                              
02544+0946 HJ  658     HIP 13543. B is a known close binary A 2341 of 1.3" separation,                 
                       partially resolved in the ANDICAM images in K and V bands.              Tok2011a
02544-0030 GWP 390     AB: ABL  88AB.                                                          Tob2012b
           GWP 391     AC: ABL  88AC.                                                          Tob2012b
02544+0635 GWP 388     XMI 291.                                                                Tob2012b
02544+1754 GWP 389     XMI 292.                                                                Tob2012b
02546+2819 COU 677     Previously combined with the nearby BRT 130.                                    
02546+1306 BPM  63     [PM2000]  107057 + [PM2000]  107037.                                    Gvr2010 
02548+4332 HJ 2162     Star C is A of HJ 2163, BDS 1479.                                               
02548+2916 BRT 130     1deg error in WDS designation, apparently an error in transcribing              
                       coordinates from the original source.                                           
02548-0640 GWP 393     ABL  89.                                                                Tob2012b
02548+1401 GWP 392     XMI 293.                                                                Tob2012b
02548-2754 HDO  58     Aka HDO  61.                                                                    
02549+1913 GWP 394     XMI 294.                                                                Tob2012b
02549-0709 JNN  21     The primary is an SB2 binary with an 11.8 day period (Torres et al.             
                       2002 AJ, 123, 1701). Since the angular confirmed to share a common              
                       proper motion) for the purpose of multiplicity statistics, although it          
                       is really a triple system. To estimate the mass of the primary for the          
                       purpose of deriving the mass ratio to the tertiary component detected           
                       in our images, we adopt the mass ratio of 0.58 derived from the                 
                       spectroscopic orbit and use the mass corresponding to an M3 spectral            
                       type for the primary.                                                   Jnn2012 
02550-1402 GAL 328     Object #81 in Gallo's original list.                                    Gal1912b
02552-0800 EGN   2     Pair likely unbound.                                                    Egn2007 
02552-4549 CPO 113     This is ESO 247-11, B is an interacting galaxies.                       Dam2010 
02553-0348 GWP 396     ABL  91.                                                                Tob2012b
02553-1209 GWP 395     ABL  90.                                                                Tob2012b
02555+0731 GWP 397     XMI 295.                                                                Tob2012b
02556+2652 STF 326     Parabolic orbit by Hopmann (1967).                                      Hop1967 
                       sigma = areal constant in the true orbit = 0.05215 arcsec^2/yr                  
                       q = periastron distance in the true orbit = 2".827                              
                       Data appear equally well fit by rectilinear solution - see catalog.             
02556+1311 HU 1047     Close, position angles scattered. No positive observations since 1937.          
02557-1223 GAL 329     Object #82 in Gallo's original list.                                    Gal1912b
02558+3429 LDS9140     BC: Old LDS6140.                                                                
                       NLTT 9308/9312                                                          Chm2004 
02558+1909 A  2342     Closing in with little angular change.                                          
02558-1606 GWP 398     ABL  92.                                                                Tob2012b
02559+1455 BPMA  3     [PM2000]  107836 + [PM2000]  107938.                                    Gvr2010 
02559-1521 LDS3441     NLTT 9361/9360                                                          Chm2004 
02560+1221 GWP 399     XMI 296.                                                                Tob2012b
02561+2003 HER   6     AC: Additional notes may be found in Herbig (1962).                     Her1962 
           CVN   6     Ca,Cb: COR   1Aa,Ab previously cataloged is actually this pair.                 
02562+2359 JNN 253     Estimated age 1000-10000 Myr; masses 0.07 +/- 0.02 and 0.07 +/- 0.01            
                       Msun; a ~0.4 au.                                                        Jnn2014 
02563+5852 STF 321     B is BD+58@531.                                                                 
02563-1816 GWP 400     ABL  93.                                                                Tob2012b
02564+1534 BPM  64     [PM2000]  108162 + [PM2000]  108210.                                    Gvr2010 
02564-1722 LDS3442     NLTT 9390/9388                                                          Chm2004 
02565+6322 MLB 390     Also known as STI 405.                                                          
02565+5526 LDS5401     Duplicity first noted by Ross: Ross 364-5.                              Ros1926 
02567+4248 LDS9141     old LDS6141. A is possibly the same as A of LDS2815.                            
                       AB: NLTT 9354/9355                                                      Chm2004 
02570+1244 BPM  65     [PM2000]  108547 + [PM2000]  108528.                                    Gvr2010 
02571-1244 GWP 401     MBL   1.                                                                Tob2012b
02572+1157 GWP 402     XMI 297.                                                                Tob2012b
02572+0153 A  2413     Component variable?                                                     Hln1963 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       According to Scardia et al. (2001), this orbit is now well defined and  Sca2001d
                       will certainly change little in the future; only the period is still            
                       slightly uncertain. The Hipparcos parallax is 0".02012 +/- 0.00150.             
                       This gives a mass sum of 2.1 Msun +/- 29%, agreeing very well with              
                       expected values for a system of type G0. Compared to the orbit                  
                       calculated by Scardia in 1980, the total mass of the system, whose      Sca1980e
                       uncertainty was then 55%, is now much better defined. The dynamical             
                       parallax is 0".0193, well in agreement with the measured parallax.              
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.64 +/- 0.52, 2.04, and 1.05 Msun, respectively.             Mlk2012 
02572-2458 BU  741     Rica (2012) derived a dynamical parallax of 45.0 mas (compared with     FMR2012g
                       44.51 +/- 2.09 mas from Hipparcos) and a mass sum (using the Hipparcos          
                       parallax) of 1.5 +/- 0.3 Msun.                                                  
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.46 +/- 0.44, 1.66, and 0.79 Msun, respectively.  Mlk2012 
02578+4431 STF 328     Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
02579+6400 STI 409     PTT 7.                                                                          
02579+0025 STF 332     HJL  44.                                                                HJL1986 
02581+6912 STF 317     BDS mentions a third star 15 sec f at 102.4@.                                   
02582+0310 GWP 403     XMI 298.                                                                Tob2012b
02583-0002 GWP 404     MBL   2.                                                                Tob2012b
02583-4018 PZ    2     the Eri = Acamar. A is a spectroscopic binary.                                  
02584-0135 A   208     C is BD-02@528.                                                                 
02585-1453 GWP 405     MBL   3.                                                                Tob2012b
02586+2408 BU 1173     Star C (mag. 13, 4.6") is probably physical.                                    
02586+1741 HO  498     Last star in a row of four. STT 49 20' n, 1.9m f.                       Ho_1899a
02586+1302 GWP 406     XMI 299.                                                                Tob2012b
02586-1628 GWP 407     MBL   4.                                                                Tob2012b
02588+4322 LDS2816     B is BD+42@664.                                                                 
02590-0746 GRV 996     SLW 141.                                                                        
02592+2120 STF 333     eps Ari. Variable velocity suspected.                                           
                       Rica (2012) derived a mass sum (using the Hipparcos parallax 9.81 +/-   FMR2012g
                       0.79 mas) of 7.4 +/- 1.8 Msun.                                                  
02594+6034 TRN  14     The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.7451 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
                       Position angle ambiguity solved by Jesus Maiz Apellaniz.                        
02595+3916 BRT2202     ALI 763.                                                                        
02596+3849 MLB1002     ALI 764.                                                                        
02596+0508 BAL2603     J 1811.                                                                         
02596-1436 LDS3445     NLTT 9570/9569                                                          Chm2004 
02596-2516 LDS3446     zet For                                                                         
                       NLTT 9579/9563                                                          Chm2004 
02598+3856 LAW  11     LSPM J0259+3855 = NLTT 9527. Law et al (2008) derive a distance of      Law2008 
                       18.8 +9.3/-3.4 pc and a projected separation of 17.6 +9.4/-2.8 au.              
                       Estimated spectral types are M4.5 and M5.5.