03001+6244 STI 417     MLB 391.                                                                        
03001+3911 ALI 765     A is the eclipsing binary ST Per.                                               
03001+1139 BPM  66     [PM2000]  110407 + [PM2000]  110416.                                    Gvr2010 
03002-1110 BRT2627     J 1454.                                                                         
03006+4753 A  1529     Round 1951 - 1954.                                                              
03007+5700 KR   15     Heintz gives the correct identification and position.                   Hei1983a
03008+1527 BPM  67     [PM2000]  110893 + [PM2000]  110922.                                    Gvr2010 
03009+5940 STTA 31     B is BD+59@581.                                                                 
03009+5221 STF 331     Both components are spectroscopic binaries.                                     
                       H 3  36.                                                                MEv2010 
03011+4453 HJ 2167     AB: HJL  45.                                                            HJL1986 
03012-1816 GWP 408     ABL  94.                                                                Tob2012b
03013+6035 MLR 108     V1018 Cas, an Algol-type eclipsing binary, period 4.12781d.             Zas2011 
03013-0636 GWP 409     ABL  95.                                                                Tob2012b
03014+1607 BPM  68     [PM2000]  111250 + [PM2000]  111338.                                    Gvr2010 
03014+0615 HDS 385     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.20 +/- 0.32, 1.76, and 1.82 Msun, respectively.             Mlk2012 
03014-1409 GWP 410     ABL  96.                                                                Tob2012b
03015+6029 ALV   1     RAFGL 4029 IRS 1. Massive YSO, member of cluster of IR sources.         Alv2004 
03015+3225 STF 336     SEI  26.                                                                Nsn2017a
03019-1633 RST2292     AB: LDS3448.                                                                    
03021+0005 GAU   2     BAL 652.                                                                        
03023+4124 STF 337     B is below MS in both (V,V-K) and (J,J-K) CMDs: wrong plx(B)=39.9mas!           
                       Wrong PM(B) in HIP?                                                     Tok2014d
03023+1820 A  2414     A premature orbit has been computed.                                            
03023+0405 alp Cet     Menkar                                                                          
                       1975.634: Disk possible marginally resolved (0".014 +/- 0".005) at 400          
                       and 425 nm.                                                                     
                       1975.639: Disk possible marginally resolved at 460 nm.                  Bla1977a
03023-7154 FIN 360     the Hyi. Not seen for certain 1962-1969, and not observed since.                
                       Needs speckle.                                                                  
03024+4204 BRT1135     LDS2824.                                                                        
03025-1516 HJL1114     IR Eri. A combined interferometric/spectroscopic solution by                    
                       Halbwachs et al. (2016) yields masses 0.982 +/- 0.010 and 0.8819 +/-            
                       0.0089 Msun.                                                            HJL2016 
03027-0741 BU   11     rho 2 Eri = 9 Eri. Note: this is not p Eridani (= 01398-5612DUN   5).           
03030-0205 STF 341     Primary is possible SB? On Keck RV program, but only small RV var.      Tok2014d
03031-0049 GWP 413     ABL  97.                                                                Tob2012b
03032-0215 J  1455     BAL 21.                                                                         
03033-1848 GWP 414     ABL  98.                                                                Tob2012b
03034-0804 LDS5409     A possible wide companion to 2MASS J03032132-0805153 at 172" with               
                       similar proper motion is noted in WDS.                                  Jnn2012 
03035+2304 HDS 389     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.50 +/- 0.27, 1.91, and 1.79 Msun, respectively.  Mlk2012 
                       Primary is SB, P(AB)=2152d=5.89y.  Metchev & Hillenbrand (2009)         Met2009 
                       resolve AB and list two faint optical(?) companions at 4", dK~5.        Tok2014d
03036+3627 BUP  37     The COU 869Aa companion was suspected by Burnham.                       Bu_1913 
03036-1001 GWP 415     ABL  99.                                                                Tob2012b
03036-2536 BRG  17     One or both of the stars in this system must be highly variable. The            
                       magnitude differences between the primary and secondary vary from 5.14          
                       mag to 1.72 mag between different observations in Bergfors et al.       Brg2010 
                       (2010) and here. In contrast to the individual note on this system in           
                       Bergfors et al., we assume here that the designation LTT 1453 refers            
                       to the primary star.                                                    Jnn2012 
                       First noted as a likely binary by Makarov & Kaplan (2005), based on     Mkr2005 
                       significant differences between Hipparcos and Tycho proper motions,             
                       then later resolved as part of the Astralux Lucky imaging survey by             
                       Bergfors et al. (2010) and Janson et al. (2012). Their 2008 and 2010    Brg2010 
                       measures, together with measures from 2011 reveal a constant            Jnn2012 
                       separation but a P.A. changing by ~3 deg/yr.                            Bwl2015 
03039+1514 BPM  69     [PM2000]  112964 + [PM2000]  112917.                                    Gvr2010 
03041+3509 POP  11     Popovic coordinate offset was apparently in error.                      Pop1969c
03042+6142 LDS9142     Old LDS6142.                                                                    
03044+2118 JNN  23     The close (~0.40") companion to 2MASS J03042184+2118154 is counted as           
                       an unconfirmed binary companion, since it has not yet been tested for           
                       common proper motion.                                                   Jnn2012 
03045+3844 SMA  33     ALI 766.                                                                        
03046-5119 DUN  10     B is CD-51@706.                                                                 
                       SHY 433. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       HIP 14307 and 14313 form a 38" pair belonging to the FG-67 sample.              
           TOK 428     AC: AC is not co-moving. C=HIP14257 has different parallax              Tok2014d
           TOK 428     Ba,Bb: The component B is resolved here at 0".19. The estimated                 
                       period of Ba,Bb is ~25yr. No motion is seen in 2 months. The subsystem          
                       Ba,Bb is also manifested by asymmetric line profiles (Tokovinin, in             
                       preparation). The A component has never been observed at high angular           
                       resolution.                                                             Tok2015c
03047+6346 STF 335     B is BD+63@388.                                                                 
03048+5330 WRH  29     Aa,Ab: gam Per = 23 Per. SB2. Spectrum composite: G8III+A2V.            WRH1955 
                       1975.781: Uncertain angle readout                                       Bla1977a
                       Analyses of the spectroscopic/interferometric orbit are given by        McA1982a
                       McAlister (1982) and Popper & McAlister (1987). Elements P, T, e for    Ppp1987 
                       the McAlister (1982) orbit are from the spectroscopic orbit by                  
                       McLaughlin (1948).                                                      MLa1948 
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       McAlister (1982).                                                       McA1982a
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       1998.657: Absolute quadrant determined by triple-correlation technique  Pru2002b
                       The physical nature of visual companion B (57", mag. 11) is uncertain.          
                       Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                       5.80 +/- 88.31 and 4.72 Msun, respectively.                             Mlk2012 
03048-0603 GWP 416     ABL 101.                                                                Tob2012b
03049+3446 HU  812     Hussey position angle 1902: 199.4@. Probably wrong quadrant.            Hu_1905a
                       HIP 14342. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
03052-0156 GWP 417     ABL 102.                                                                Tob2012b
03052-3725 BRG  18     This target, like BRG  23, gives conflicting information about whether          
                       the AB pair is physically bound. The brightness and color are fully             
                       consistent with B being an M3.5 companion to the M2.0 primary.                  
                       Furthermore, the separation is only 0.2", and the whole field is                
                       otherwise empty. This indicates physical companionship. However, the            
                       deviation from the expectation of a background source is only 1.1               
                       sigma, and the companion has moved 3.6 times closer to the background           
                       expectation than its original position where the motion has a 14 sigma          
                       confidence. This, by contrast, suggests a chance alignment. Since the           
                       magnitude of motion is not inconsistent with what could be expected             
                       for orbital motion of a real physical pair, we keep it as binary in             
                       our analysis, but we note that further observations will be necessary           
                       in order to resolve this issue satisfactorily.                          Jnn2012 
03054+2515 STF 346     52 Ari. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                       spectroscopic masses 9.10 +/- 6.84, 6.89, and 3.39 Msun, respectively.  Mlk2012 
03054-1432 GWP 418     ABL 103.                                                                Tob2012b
03055+0234 BAL1630     OL  183.                                                                        
03056+1150 GIC  36     G005-013/G005-012.                                                              
03056-0238 GWP 419     ABL 104.                                                                Tob2012b
03058+3202 ES  326     BC: SEI  27.                                                            Nsn2017a
03059+1302 BPMA  4     [PM2000]  114294 + [PM2000]  114392.                                    Gvr2010 
03061+7925 STF 320     Spectroscopic binary? Spectrum composite; M1III+F7IV.                           
03063-1243 LDS3452     NLTT 9888/9881                                                          Chm2004 
03064+1545 ALP   9     2MASSW J0306268+154514                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in February 2003.          AlP2007 
03071+3757 BRT2203     ALI 513.                                                                        
03072-0520 GWP 423     ABL 105.                                                                Tob2012b
03073-1346 CRJ   7     Crepp et al. (2015) determine effective temperatures for the A and B            
                       components of 5680 +/- 40 and 978 +20/-43K. Spectral types are G3V and          
                       T5.5 +/- 1, masses 0.95 +/- 0.02 and >51.9 +3.6/-4.3 Mjup,                      
                       ages 4.6-10 Gyr.                                                        CrJ2015 
03074+5831 RAFGL 437   Shows subarcsecond monopolar nebula extending towards SE at PA                  
                       135 +/- 10deg.                                                          Alv2004 
03075-7859 HJ 3568     A is a spectroscopic binary.                                                    
03076-4702 TOK 206     The companion with q = 0.29 is resolved with NICI but unresolved with           
                       speckle,  being too faint in the optical.                               Tok2012a
03077+3637 ENG  11     B is BD+36@631.                                                                 
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
03078+2533 TOK 234     The B component was suspected of duplicity (0".253, 240.5deg,                   
                       dI=2.7mag) by RoboAO, but the pair was not accepted as real             Tok2014d
03078+1223 BPM  70     [PM2000]  115596 + [PM2000]  115589.                                    Gvr2010 
03078-2750 VIG   3     Optical/physical nature of the faint companion is undefined.            Vig2012 
03079-2813 LDS  86     AB: NLTT 9987/9985                                                      Chm2004 
03080-0135 GWP 425     ABL 107.                                                                Tob2012b
03080-0537 GWP 424     ABL 106.                                                                Tob2012b
03082+4057 LAB   2     Aa,Ab: bet Per = 26 Per = Algol, prototype of the Algol-type binaries.          
                       The eclipse phenomena, known since historical times (although the time          
                       of minimum brightness was first measured by Montanari on 8 Nov 1670)            
                       was first explained as an eclipsing binary by Goodericke as early as            
                       1782. According to R.G. Aitken, this was verified when it was noted as  A__1935f
                       the second spectroscopic binary based on photographic spectra                   
                       obtained by Prof. H.C. Vogel at Potsdam in November, 1889. Belopolsky           
                       discovered a variation in the radial velocity with a period of order            
                       1.8 years, later resolved by Labeyrie and his speckle camera in 1973;   Lab1974 
                       the magnitude difference is about 2.5.                                          
                       The binary, a radio and X-ray source, is triple (and possibly                   
                       quadruple, but the variation with the 32 yr period is more probably an          
                       apsidal rotation of the eclipsing pair).                                        
                       The spectroscopic data were discussed by Hill et al. (1970, 1971).      HlG1970 
                       ADS lists several distant, faint, and probably optical companions.      HlG1971 
                       Elements P, T, e, and omega for Labeyrie et al. (1974) orbit adopted    Lab1974 
                       from the spectroscopic orbit of Hill et al. (1971).                             
                       Analysis of the spectroscopic/interferometric orbit is given by                 
                       Bonneau (1979)                                                          Bnu1979 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Hipparcos astrometric solution adopts some elements from the orbits of  HIP1997d
                       Pan et al. (1993) and                                                   MkT1993a
                       Gatewood et al. (1995).                                                 Gat1995 
                       Peterson et al. (2011) orbits of both the outer (LAB   2Aa,Ab) and      Ptn2011 
                       inner (CSI   1Aa1,Aa2) are based on VLBI measures combined with                 
                       speckle and radial velocity data. Assuming masses of the primary and            
                       secondary of 3.70 and 0.79 Msun, respectively, they derive a mass for           
                       the tertiary of 1.51 +/- 0.02 Msun.                                             
           BU  526     AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
03084+4020 BRT2204     ALI 1031.                                                                       
03084+2620 OSO  14     G037-026. Not a common proper motion pair, based on color               Oso2004 
03084-2410 LDS  87     NLTT 10008/10007                                                        Chm2004 
03084-7033 HLN  19     DAM 782.                                                                        
03087+1736 COU2680     BD+17@499a.                                                                     
03087-1432 GWP 426     ABL 108.                                                                Tob2012b
                       Not a double star, but an edge-on galaxy: USNO-B1.0 proper motion is    Skf2012 
                       spurious.                                                                       
03088-0952 GWP 427     ABL 109.                                                                Tob2012b
03090+4415 STF 351     B is BD+43@637.                                                                 
03090+1740 COU 358     BD+17 501a. Mistaken identification with BD+17 501 led to earlier               
                       incorrect WDS designation as 03088+1801.                                        
03091+4937 BUP  38     iot Per. Proper motion of A +1263 -091.                                         
03092+0728 STFA  6     STTA 32. B is BD+06@487.                                                        
03094-3004 LDS3460     NLTT 10074/10076                                                        Chm2004 
03095+4544 HDS 404     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 0.90 +/- 0.09, 0.87, and 0.75 Msun, respectively.             Mlk2012 
03095+4451 ES 2596     kap Per = 27 Per. A is a spectroscopic binary.                                  
03096+0512 A  2030     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.41 +/- 0.32, 2.11, and 1.05 Msun, respectively.             Mlk2012 
03096-0054 CHE  75     Aka BAL 281.                                                                    
03098-1238 GWP 428     ABL 110.                                                                Tob2012b
03099-0654 UX Eri      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                       estimate the mass of the contact pair at 1.901 Msun and the minimum             
                       mass of the wider component at 0.59 Msun.                                       
03099-8332 HJ 3582     Spectral type of A : F2IIISrEuSi:   Estimated orbital period ~100,000y. XXX2017b
03101+0210 RST5197     Aka TDS2463.                                                                    
03101-6355 HJ 3559     B is CPD-64@231.                                                                
03104+0238 OL  177     Not found by Heintz at IDS position. Position corrected.                Hei1990b
03104-0004 GWP 429     ABL 111.                                                                Tob2012b
03105+5040 LDS9143     Old LDS6143.                                                                    
03107+2226 LDS3461     NLTT 10112/10110                                                        Chm2004 
03107-4023 LDS9144     Old LDS6144.  Recognized to be the same as LDS5414 by John Greaves.     Grv2006c
03108+3724 LDS9145     Old LDS6145.                                                                    
                       NLTT 10082/10091                                                        Chm2004 
03110+1648 SPF   1     L dwarf 2MASS J03105986+1648155 resolved into close components at L/T           
                       boundary. Approximate orbital period 72 +/- 4 years, distance 25 +/- 4          
                       pc, system mass ~30-60 Mjup. Spectral types of both components are              
                       estimated at L9 +/- 1.                                                  Spf2010 
03112+2225 H 5 117     Also known as STF 359.                                                          
03113+3937 BLL  10     ome Per = 28 Per                                                                
03117+8128 STF 327     A is a spectroscopic binary.                                                    
03118+3525 GIC  37     G095-014/G095-013.                                                              
03121-2859 HJ 3555     alp For = 12 Eri. The magnitude of B is uncertain and has been                  
                       suspected to vary. Another century is needed for apastron coverage.             
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       A is GJ 127. B is possible SB. Variability of RV(B) is based on                 
                       historic RV (Eggen, van den Bos)                                        Tok2014d
03121-6420 HJ 3562     B is CPD -64@231.                                                               
03122+3713 STF 360     A premature orbit has been calculated. Data appear equally well fit by          
                       rectilinear solution - see rectilinear elements catalog.                        
                       A is SB1, P=415d. B is possible long-period SB.                         Tok2014d
03123-2727 LDS  88     NLTT 10222/10227                                                        Chm2004 
03124-1157 GWP 432     AB: ABL 112AB.                                                          Tob2012b
           GWP 433     AC: ABL 112AC.                                                          Tob2012b
03124-4425 JC    8     Variable RV of AB, not explained by the visual motion, has been                 
                       reported (Eggen 1965), but Heintz's mass ratio does not support         Egg1965b
                       the presence of a fourth body.                                          Hei1979a
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.59 +/- 0.73, 2.18, and 3.82 Msun, respectively.  Mlk2012 
           HJ 3556     AB,C: Star C (mag. 9.2, 3.5") is in slow retrograde motion.                     
                       Heintz (1979) gives AB orbit, attempts AC orbit with P=987yr.           Hei1979a
                       The motion of AC is not directed away from PM(A), hence physical.       Tok2014d
03125-3449 LDS  89     LDS5418.                                                                        
03127+7133 STT  50     A premature orbit has been calculated.                                          
                       Bespalov (1961) has a = 1".618, Finsen & Worley (1970) assume this      Bsp1961 
                       is a misprint.                                                          Fin1970b
03128+3720 WZ    6     ES 2556.                                                                        
03128-0112 HJ  663     94 Cet.                                                                         
                       AB: B is PMS star and SB1 (P=2.026y). Planet (P= 1.2y=535.7d) around            
                       A. Is this true planet or Ba,Bb effect?                                 Tok2014d
           TOK 654     AF: CPM companion HD 20619 = GJ 135: 7.03V, G1.5, HD 20169 at 133'              
                       from AB (0.7 pc)                                                        Tok2014d
03130+3254 LDS9146     AB: Old LDS6146.                                                                
                       B is deeply below MS, blue in V-K and J-K. White dwarf?  WDS: too fast          
                       motion of AB, optical? Hyades cluster. CfA: RV var?                     Tok2014d
                       Hyades cluster. The 2MASS companion B can be physical.                  Tok2014d
                       Previous AD companion, TOK 655, is the same as the known AB pair. The   Dam2015d
                       Luyten measure was poor.                                                        
03130-0343 GWP 434     ABL 113.                                                                Tob2012b
03132+1710 BPM  71     [PM2000]  119048 + [PM2000]  119061.                                    Gvr2010 
03134-0852 GWP 438     ABL 114.                                                                Tob2012b
03135+4417 ES  559     Also known as LDS9147, LDS6147, and LDS2836. These were all recognized          
                       by John Greaves (personal corres.) to be the same pair.                         
                       NLTT 10231/10232                                                        Chm2004 
03136+3909 STF 364     HJL  46.                                                                HJL1986 
03141+5934 TRN  15     CC Cas. Classification in Mason et al. (1998) is from the tomographic   Msn1998a
                       analysis of Hill et al. (1994 A&A 282, 455).                                    
                       The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.7452 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
03141+0832 GIC  38     G079-015/G079-016.                                                              
03144-0227 GWP 440     ABL 115.                                                                Tob2012b
03146-0940 GWP 441     ABL 116.                                                                Tob2012b
03147-3533 GAA   4     TZ For, a detached eclipsing binary.  A combined spectroscopic/                 
                       interferometric orbit by Gallenne et al. (2016) yields a semimajor              
                       axis of 0.5564 +/- 0.0001 au, distance 185.9 +/- 1.9 pc, and the                
                       following component parameters:                                                 
                       mass (Msun):        2.057 +/- 0.001     1.958 +/- 0.001                         
                       radius (Rsun):      8.28  +/- 0.22      3.94  +/- 0.17                          
                       luminosity (Lsun):  1.57  +/- 0.02      1.36  +/- 0.03                  GaA2016 
03149-1400 HJ 3558     HJ 3551 is identical.                                                           
03150+0101 GIC  39     G077-035/G077-034. See Allen et al. (2000) for  information on          AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
03151+1618 HU 1055     The companions C, D, and E, given in the ADS, do not exist. They                
                       should be under ADS 2426.                                               B__1963b
03154-6930 R    22     Also appears to be R    27.                                                     
03158+5057 HU  544     A = V572 Per: eclipsing binary of Algol type, period 1.21317 days.      Zas2015
03158-0849 SHY 154     HIP  15197 + HIP  15244. Primary is zet Eri = Zibal.                            
03160+4853 LDS9148     Old LDS6148.                                                                    
                       NLTT 10355/10353                                                        Chm2004 
03160+3441 HO  503     A spectroscopic binary and ellipsoidal variable, V423 Per.                      
03162+1302 BPMA  5     [PM2000]  120872 + [PM2000]  120882.                                    Gvr2010 
03165-0642 GWP 443     ABL 117.                                                                Tob2012b
03165-3541 SHY 439     AB: HIP  15239 + HIP  15432.                                                    
           SHY 439     AC: HIP  15239 + HIP  15152.                                                    
           SHY 439     AD: HIP  15239 + HIP  15933.                                                    
           SHY 441     BC: HIP  15432 + HIP  15152.                                                    
03166+4943 ES  463     Aka OL  150.                                                                    
03166+3238 STF 370     According to Burling, the long unconfirmed system, 03064+3153HJ 5456,           
                       may also be this pair.                                                  Bur2005 
                       SEI  29.                                                                Nsn2017a
03167+4237 LDS9149     Old LDS6149.                                                                    
03167+2639 TOR   4     Formerly known as PAN   1.                                                      
03167-0332 TOK  78     HIP 15247. A is SB without orbit, dRV= 6.6.                             Nrd2004 
03168+7830 STF 345     Also known as STF 340.                                                          
03168+0501 A  2032     HIP 15253. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
03172+4522 PRV   2     GJ 3213. Pravdo et al. (2006) derive masses 0.370 +/- 0.034 and                 
                       0.195 +/- 0.021 Msun.                                                   Prv2006 
03174+0739 BU 1039     Hyades vB 1. BU 1039AB, with rho = 2".2 and Delta m = 6.0 is outside            
                       the detection window.                                                   Msn1993a
                       AC: HJL  47.                                                            HJL1986 
                       AC: SHY 155. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
03175+6540 STT  52     A premature orbit has been calculated.                                          
03175-0107 GWP 445     ABL 118.                                                                Tob2012b
03175-1222 J  1456     BRT2628.                                                                Brt1947 
03176-1412 GWP 446     ABL 119.                                                                Tob2012b
03177+6108 STI 441     03175+6108SMA  36                                                               
03177+3838 STT  53     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.51 +/- 0.99, 2.40, and 1.05 Msun, respectively.             Mlk2012 
03178-7029 R    28     Aka RSS  62.                                                                    
03180-6656 EHR   3     Physical/optical nature undefined.                                      Ehr2010 
03182-6230 BNU   2     Aa,Ab: zet 2 Ret. B has common proper motion, +1370 +660, and is                
                       CPD-63@217 = zet 1 Ret.                                                         
                       Aa,Ab: Likely a spurious pair. Last measured 1978 and unresolved by             
                       SOAR on 3 occasions 2008–2012.                                          Tok201
                       Aa,Ab is suspicious, 1 observation in WDS, not binary in Raghavan et    Rag2010 
                       al. (2010). Jones et al. (2002) do not detect SB with precise RV at     CPS2002b
                       the AAT.                                                                Tok2014d
           ALB   1     AB = LDS  92.  HIP 15371. See Allen et al. (2000) for information       AlC2000 
                       on metallicity, age, galactic orbital parameters, etc.                          
                       AB: SHY  16. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
03184-0056 AC    2     95 Cet. According to Eggen this pair shares common proper motion with   Egg1960 
                       BD -01 474 at 11'.                                                              
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03184-0708 LDS3473     HIP 15396. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 10536/10548                                                        Chm2004 
03184-2231 SEE  23     15 Eri. CD-22@1146. Motion direct.                                              
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.33 +/- 0.80, 3.35, and 1.20 Msun, respectively.             Mlk2012 
03185+4721 MET   1     V522 Per.                                                               Met2004a
03185+1511 LDS9150     Old LDS6150. HIP 15394. See Allen et al. (2000) for information on      AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
03186+0827 LUH   6     AC: LSPM J0318+0827S + 2MASS J03184214+0828002.                         Luh2012b
03187+1527 LDS9151     Old LDS6151. SLE  41.                                                           
03187-1834 HJ 3565     A is a spectroscopic binary.                                                    
03188-0028 ABT   3     BAL 656.                                                                        
03188-0321 GWP 447     ABL 120.                                                                Tob2012b
03189-0101 BU 1177     Gomez et al. (2016) derive dynamical parallax and component masses:             
                       10.03 +/- 0.77 mas, 0.906 +/- 0.033 Msun, 0.886 +/- 0.032 Msun.         Doc2016i
03190-1549 GWP 448     ABL 121.                                                                Tob2012b
03192-5306 HJ 3571     CD-53@674.                                                                      
03193-0232 GWP 449     ABL 122.                                                                Tob2012b
03194+6156 JNN 254     G 246-33. Estimated age 35-300 Myr; masses 0.29 +/- 0.11 and 0.17 +/-           
                       0.07 Msun; a ~10.8 au.                                                  Jnn2014 
03194+0322 STT 557     AB: kap 1 Cet = 96 Cet. Variable? A is a spectroscopic binary.                  
                       B is BD+02@521.                                                                 
03195-2145 JC    1     tau 4 Eri = 16 Eri. A is an irregular variable.                                 
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
03199-0321 GWP 450     ABL 123.                                                                Tob2012b
03200+6539 BUP  43     Shell star. Light and spectrum variable, BK Cam. May also be a long-            
                       period spectroscopic binary.                                                    
03200+3845 BRT2205     MLB 819. ALI 774.                                                               
03201-2851 LDS  93     van den Bergh reports a third star at 38@, 105.6".                      Bgh1958 
                       A is exoplanet host, P=592d. B = HIP 15526 hosts exoplanets with                
                       P=29.1d, 85.1d.                                                         Tok2014d
                       B is CD-29@1229.                                                                
                       NLTT 10636/10635                                                        Chm2004 
                       SHY 157. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
03202-1457 LDS3479     NLTT 10629/10617                                                        Chm2004 
03202-1632 GWP 452     ABL 124.                                                                Tob2012b
03203+1944 STF 376     H 2  76.                                                                MEv2010 
03203+1625 SLE  42     Hipparcos suspected non-single.                                                 
03206+0902 GIC  40     G079-029/G079-030 = GJ 9114AB.                                                  
                       HIP 15572. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       Primary is SB1, P=321.6d                                                Tok2014d
03207+8459 STF 319     Schiller measures 1910.87,331.1@,42.32",7.7-9.2.                        Shr1913 
03207+1736 HJ 3245     See BDS for components.                                                         
03210-0054 LDS5420     LDS5420A was B component of 03211-0054ITF  55AB, LDS5420B was ITF 55C           
                       Pairs merged; ITF 55AB --> 03210-0054ITF 55AD (with quadrant flip),             
                       ITF 55AC --> 03210-0054ITF 55BD (also with quadrant flip).                      
03211-2632 SWR   5     CPM pair                                                                Skf2004 
03212+2109 COU 259     tau 1 Ari = 61 Ari. A is an irregular variable.                                 
03213+4302 A  1706     LDS2842.                                                                        
03214+4320 VIG   4     Optical/physical nature of the faint companion is undefined.            Vig2012 
03216-0841 GWP 454     ABL 126.                                                                Tob2012b
03217+0845 STF 380     A premature orbit has been calculated.                                          
03219+4904 WEB   1     B is BD+48@892.                                                                 
03220+1715 LDS3483     G006-003. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 10701/10698                                                        Chm2004 
03220-1636 LDS3485     NLTT 10725/10724                                                        Chm2004 
03226-0210 GWP 456     ABL 127.                                                                Tob2012b
03226-3011 LDS3487     LDS5422.                                                                        
                       NLTT 10762/10761                                                        Chm2004 
03227+1717 BPM  72     [PM2000]  124803 + [PM2000]  124860.                                    Gvr2010 
03227+1037 GIC  41     BC: 03328+1040 UC  997.                                                         
03228-0042 GWP 457     ABL 128.                                                                Tob2012b
03229+2949 STF 379     H III 91, BDS 1688.                                                             
                       H 3  91.                                                                MEv2010 
03230-0548 GWP 458     ABL 129.                                                                Tob2012b
03232+4554 LDS9152     Old LDS6152.  HD 20835. See Allen et al. (2000) for information on      AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
03232-1404 GWP 459     ABL 130.                                                                Tob2012b
03233-0337 GWP 460     ABL 131.                                                                Tob2012b
03233-5000 HJ 3573     LDS  94. A is CD-50@1015, B is CD-50@1014 (Roman).                              
03234-0710 GWP 461     ABL 132.                                                                Tob2012b
03234-1015 HJ 2188     STF 387.                                                                        
03236+0453 BU 1178     A is a spectroscopic binary.                                                    
                       Greenwich measure of 1921 erroneous. No certain change since 1890.      B__1963b
03236-4005 I   468     glimpsed?                                                               I__1948a
                       Soderhjelm (1999) gives possible orbit from two widely spaced visual    Sod1999 
                       observations + Hipparcos data.                                                  
03236-8116 SHY 161     AC: HIP  15803 + HIP  17184.                                                    
03237-0609 GWP 462     ABL 133.                                                                Tob2012b
03238+2432 LDS1144     NLTT 10780/10781                                                        Chm2004 
03240-0007 GRV 997     = GWP 464 = ABL 135.                                                    Tob2012b
03240-2613 HJ 3572     B is CD-26@1270.                                                                
                       SWR   6. CPM pair                                                       Skf2004 
03242+2347 LDS 884     AB,C: NLTT 10804/10808                                                  Chm2004 
03242-1048 GWP 463     ABL 134.                                                                Tob2012b
03243+4952 BUP  44     alp Per = 33 Per = Mirfak                                                       
03244-1539 A  2909     There are many negative observations. Needs speckle.                            
                       HIP 15868. A is the close pair A 2909, 0.1". The 2MASS PSC companion            
                       at 17" is called C in the WDS.                                          Tok2011a
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 0.62 +/- 0.11, 2.10, and 1.01 Msun, respectively.  Mlk2012 
                       CfA: SB? P=9115d? =25y?  UR at SOAR from 2008.6 to 2012.9, in           Mlr1955a
                       contradiction with orbit of Muller (1955).                              Tok2014d
03245+4626 LDS9153     Old LDS6153.                                                                    
03248-1533 GWP 466     ABL 136.                                                                Tob2012b
03249+1552 BPM  73     [PM2000]  126226 + [PM2000]  126261.                                    Gvr2010 
03249-0356 GWP 467     ABL 137.                                                                Tob2012b
03253+1158 BPM  74     [PM2000]  126464 + [PM2000]  126473.                                    Gvr2010 
03256-1855 GWP 468     ABL 138.                                                                Tob2012b
03257+0551 JNN 255     AB: GJ 3224. Estimated age 300-1000 Myr; masses 0.25 +/- 0.06 and 0.14          
                       +/- 0.01 Msun; a ~6.3 au.                                               Jnn2014 
                       AC: Estimated age 300-1000 Myr; masses 0.48 +/- 0.25 and 0.45 +/- 0.24          
                       Msun; a ~48.1 au.                                                       Jnn2014 
03259+4540 COU1682     TDS2544.                                                                        
03261+1229 A   829     Probably ambiguous case, but only one solution has been tested.                 
03262+2950 ALP  10     2MASSW J0326137+295015                                                          
                       Further observations are required to determine the physical/optical             
                       nature of this pair.                                                    AlP2007 
03262-1817 GWP 469     ABL 139.                                                                Tob2012b
03263+1709 JNN 256     Estimated age 1000-10000 Myr; masses 0.24 +/- 0.03 and 0.16 +/- 0.03            
                       Msun; a ~20.6 au.                                                       Jnn2014 
03264+3520 HDS 430     Cvetkovic et al. (2016) estimate spectral types F7 and G8, masses 1.30          
                       and 0.97 Msun. Dynamical parallax is 15.60 +/- 0.44 mas.                Cve2016b
03265+5909 GIC  42     G246-036/G246-035.                                                              
03266+2843 CHR   9     Aa,Ab: This is UX Ari, an RS CVn type binary that is not eclipsing.             
                       Peterson et al. (2011) orbits of both the outer (CHR   9Aa,Ab) and      Ptn2011 
                       inner (UX Ari Aa1,Aa2) are based on VLBI measures combined with                 
                       speckle and radial velocity data. Assuming masses of the primary and            
                       secondary of 1.10 and 0.95 Msun, respectively, they derive a mass for           
                       the tertiary of 0.75 +/- 0.01 Msun.                                             
           TOK  13     AB: AB is CPM, estimated period 20,000y. Primary is 6.4d SB2.                   
                       The spectrum shows 3 components (Fekel, 1986 private communication),            
                       two of which are identified with the 6.44-day system described by               
                       Carlos & Popper (1971), while the third is possibly the component       Ppp1971 
                       listed here.                                                                    
                       Evolved or bad 2MASS photometry.                                        Tok2006 
03266+1406 BPM  75     [PM2000]  127254 + [PM2000]  127284.                                    Gvr2010 
03269+1609 BPM  76     [PM2000]  127466 + [PM2000]  127423.                                    Gvr2010 
03269-2344 RSS   4     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
03271+1845 CHR  10     Resolution of an occultation binary.                                            
03272+0944 HDS 433     1975.629: Marginally resolved at 450 nm?                                Bla1977a
                       Hierarchical quadruple, including 51y, 145d, and 7.14d pairs                    
                       (HDS 433AB; MKT 15Aa,Ab; and MKT 15Aa1,Aa2; respectively). The 7d pair          
                       is eclipsing.  Nemravova et al. (2016) combine spectroscopy,            Nem2016 
                       photometry, and interferometry to derive orbits of all three pairs,             
                       yielding the following component parameters:                                    
                       Parameter       Aa1              Aa2               Ab                           
                       Mass (Msun)     2.252 +- 0.027   2.125 +- 0.027    3.89 +- 0.25                 
                       Radius (Rsun)   1.700    0.035   1.618    0.039    2.81    0.28                 
                       Teff (K)        10700    160     10480    130     14190    150                  
                       Mbol (mag)      0.923    0.079   1.120    0.075   -1.14    0.22                 
                       (Note: Nemravova et al. refer to the pairs as AC; AB; and Aa,Ab.                
                       However, the HDS pair was assigned components A and B at discovery.)    HIP1997 
03276+5847 RAFGL 490   Extended emission seen in H-band, no subarcsecond structure resolved.   Alv2004 
03276+0954 J   305     May be the same as GJ 3226, which is not in the WDS. At the SIMBAD      Dam2017c
                       precise position of GJ 3226 a measure from Gaia-DR1 is 117.1 deg @              
                       1.530", quite close to the measures of J   305.                                 
03278+5627 STI1984     The relative motion is small but fairly certain; it is smaller than             
                       the proper motions of both components. Therefore, although the                  
                       component proper motions are of the same order, we consider this to be          
                       a physical pair.                                                        Kiy2012 
03278-2352 LDS3496     NLTT 11000/10999                                                        Chm2004 
03279+5625 MLB 116     Triple star with weak hierarchy. Motions of all components relative to          
                       each other are small. If we trust the relatively large pm for A from            
                       the WDS, the system is physically bound; however there is an                    
                       appreciable discrepancy between this pm and the value given by                  
                       Kharhenko & Rezer (2001, Kinemat. Fiz. Nebesn. Tel 17, 409). Therefore          
                       we are not yet able to determine with confidence whether or not the             
                       components are physically bound.                                        Kiy2012 
03279-1948 GC 4128     Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                       Cluster Melotte 25 #EGG21.                                                      
03280+2631 LDS1146     NLTT 10977/10976                                                        Chm2004 
03280+2028 STF 394     AB: H 3  77.                                                            MEv2010 
03282+5628 ES 1777     Relative and proper motions are of the same order, making it                    
                       impossible to judge whether the pair is physically bound.               Kiy2012 
03282-1335 GAL 330     Object #94 in Gallo's original list.                                    Gal1912b
03282-3551 I    58     chi 3 For                                                                       
03284+2248 BAG   2     Aa,Ab: 66 Ari. A is a spectroscopic and occultation binary.                     
                       Agreement is poor between this observation and the only other                   
                       measurement, by Balega (1988, private communication).                   Hrt1992b
03284-1425 GWP 470     ABL 140.                                                                Tob2012b
03286-1537 LDS3498     NLTT 11020/11021                                                        Chm2004 
                       Also known as GJ 3228A, this star has a wide binary companion at 16"    VVO1991 
                       separation (e.g., Weis 1991).                                           Jnn2012 
03289+4039 ES 2598     LDS6169.                                                                        
03289-2723 LDS9154     Old LDS6154.                                                                    
                       LHS1549-50.                                                                     
03291+0118 MET   2     RX J0329.1+0118                                                                 
03292-0226 GWP 471     ABL 141.                                                                Tob2012b
                       This is the galaxy LEDA 1092357.                                        Dam2017c
03294+4931 BU 1179     34 Per.                                                                         
                       Magnitude 11.6 of Burnham is underestimate; mine are similar to the             
                       photometric values of Kuiper (1.93)                                     Baz1954a
03294-6256 HJ 3580     kap Ret. LDS 100.                                                               
03295-1558 GWP 472     ABL 142.                                                                Tob2012b
03296+2431 SAR   1     HBC 347 = V1224 Tau.                                                            
03297+5955 HLM   2     Aka HLM  42.                                                                    
03297-0850 GAL 331     Object #95 in Gallo's original list.                                    Gal1912b
03298+8402 STF 343     STF 347.                                                                        
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
03300+5527 STF 390     Aka H N  66.                                                                    
03301+1258 BPMA  6     [PM2000]  129571 + [PM2000]  129567.                                    Gvr2010 
03301-1019 GWP 473     ABL 143.                                                                Tob2012b
03302+7402 LDS1572     G221-010/G221-011.                                                              
                       NLTT 10954/10953                                                        Chm2004 
                       Aka GIC  43.                                                                    
           FAR  31     NLTT 10954. Primary is white dwarf WD 0324+738.                         Far2006 
03304-1257 GWP 474     ABL 144.                                                                Tob2012b
03305+5418 LEP  15     NI    7.                                                                        
03305+2006 STF 399     AB: H 4  89 (aka, H IV 89)                                              MEv2010 
                       A component SB1, P=32.5y. Is AB a real physical pair, or just two               
                       members of Hyades?                                                      Tok2014d
03307-1926 HDS 441     Cvetkovic et al. (2016) estimate spectral types G2 and G5, masses 1.11          
                       and 1.05 Msun. Dynamical parallax is 24.78 +/- 1.48 mas.                Cve2016b
03309+7041 JNN 257     LHS 1553. Estimated age 1000-10000 Myr; masses 0.31 +/- 0.03 and 0.17           
                       +/- 0.02 Msun; a ~7.9 au.                                               Jnn2014 
03309+1256 5 Tau       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Harper (1924).                                                          Hrp1924 
03309-6200 TOK 190     The double-lined SB detected in GCS is resolved by speckle. Its                 
                       estimated orbital period of 4 yr explains the acceleration.             Tok2012a
03311+2744 STFA  7     STTA 34. B is BD+27@513.                                                        
                       HJL  49.                                                                HJL1986 
03311+1544 HDS 443     1997.7181  Large change in separation seen since Hipparcos epoch.       Msn1999b
03312+1947 STF 403     AB: H 1  55.                                                            MEv2010 
03313+6644 OSO  15     G246-038. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates. PM = +1193 -1066.                                     Oso2004 
03313+2734 SHY 445     BC: HIP  16410 + HIP  16742.                                                    
03313-5955 JSP  47     CD-60@724.                                                                      
03314+5842 STI1991     STI1997.                                                                        
03316+4752 STT  56     Primary also is classified B8.5VeShell.                                         
03317+1331 BPM  77     [PM2000]  130670 + [PM2000]  130734.                                    Gvr2010 
03318+3803 ES 2458     ALI 517 is the same pair.                                               Hei1980a
03319+3536 ES 2559     BRT 3235.                                                                       
03319-2537 VIG   5     The B component appears to be a faint background star.                  Vig2012 
03320+6735 STT  54     B is BD+67@@274.                                                                
03320+1820 LDS3501     NLTT 11140/11139                                                        Chm2004 
03321+4801 BAG  40     Primary is the rotationally variable star V396 Per.                             
03321+4340 COU1688     AB: A premature orbit has been calculated with very sparse data, since          
                       most of the observations are negative.                                          
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.58 +/- 1.35, 2.16, and 0.95 Msun, respectively.  Mlk2012 
           LDS9155     AC: Old LDS6155. HIP 16467. See Allen et al. (2000) for information on  AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
                       NLTT 11124/11125                                                        Chm2004 
03322+1133 AG   68     H IV 44. Also known as STF 409.                                                 
                       H 4  44.                                                                MEv2010 
03323-0705 STF 411     B is BD-07@619 (Roman).                                                         
                       B component spectral type F9IV                                          AbH2000 
03326+2844 JNN  24     This is a close triple system discovered with AstraLux, where in                
                       particular the tertiary component is difficult to fit for. Since the            
                       relative positions of the BC pair components are therefore clearly              
                       dominated by noise scatter in both separation and position angle, we            
                       set the error of each epoch to the scatter among the data points and            
                       make no assessment of orbital motion for the BC pair (although by               
                       contrast, clear orbital motion is seen of the pair with respect to the          
                       A component).                                                           Jnn2012 
                       Estimated age 10-20 Myr; masses 0.07 +/- 0.01 and 0.04 +/- 0.01 Msun;           
                       a ~8.7 au.                                                              Jnn2014 
03327+3540 CHR 261     This object is a new addition to older Hyades member lists added by             
                       Schwan (1991 A&A, 243, 386), although Griffin (1992 private comm.)              
                       doubts that this object is actually a cluster member. While its status          
                       is not definitive, subsequent confirmation or suspected duplicity (by           
                       another technique) makes the discovery measurement somewhat more                
                       probable.                                                               Msn1993a
03327-0553 GWP 476     ABL 145.                                                                Tob2012b
03328-0247 GWP 477     ABL 146.                                                                Tob2012b
03329-0927 BLA   2     eps Eri = 18 Eri = Ran. Macintosh et al (2003) made a K-band search for MBA2003 
           MBA   1     extrasolar planets in the dust surrounding eps Eri, using Keck, NIRC2,          
                       and AO. The relative motions for these 10 objects between 2001 Dec and          
                       2002 Aug were all well below expected motions for true companions,              
                       leading to conclusion all these faint companions are background stars.          
03332+4615 ES  560     NLTT 11174/11176                                                        Chm2004 
03334+2322 STT  57     STTA 35 = S   429.                                                              
03335+5846 STF 396     B is BD+58@618. Spectrum of A: Am(A3/A7/F0).                                    
03336-0735 GWP 478     ABL 147.                                                                Tob2012b
03336-1904 RSS  66     CPD-19@376                                                                      
03337+5752 CHR 117     Cf orbit in McAlister et al. (1992).  High-space-velocity binary.       McA1992 
                       See Balega et al. (2001) for further discussion of Li abundance.        Bag2001 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.47 +/- 0.38, 3.40, and 1.13 Msun, respectively.             Mlk2012 
03339+3205 HJ  334     STT 540.                                                                        
                       SEI  30.                                                                Nsn2017a
03339-3105 B    52     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.62 +/- 1.43, 2.46, and 1.20 Msun, respectively.             Mlk2012 
03342+4837 BU  787     Burnham notes: "Hussey measures a third star, 175.8deg, 12.70arcsec     Hu_1903b
                       (1898.70) 1n. I could not see this on one night with the 40-inch, but           
                       measured 11m star in nearly the same direction, 175.6deg, 36.78arcsec           
                       (1899.13) 1n."                                                          Bu_1906 
                       C does not exist.                                                       B__1960b
03342+4651 HDS 452     V578 Per, eclipsing binary of bet Lyr type, period 0.97077d.            Zas2016 
03343+6348 MLB 190     Also known as WFC  16.                                                          
03343+2625 OL  152     COU 687.                                                                        
03344+2428 STF 412     7 Tau. Only P, T, and a were redetermined by Vlaicu & Vasile (1961);    Vla1965 
                       the remaining elements were from the orbit of Luyten (1934).            Luy1934c
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.04 +/- 1.54, 4.91, and 2.09 Msun, respectively.  Mlk2012 
                       AB,C: H 4  88.                                                          MEv2010 
03344-1940 GWP 480     ABL 148.                                                                Tob2012b
03345+1948 STF 414     H III 78. STT  58.                                                              
                       H 3  78.                                                                MEv2010 
03346-1613 GAL 332     Object #96 in Gallo's original list.                                    Gal1912b
03346-3104 LDS3508     NLTT 11300/11288                                                        Chm2004 
03348+2126 BRT3261     AB: Also known as TDS2588.                                                      
                       AB: Additional notes may be found in Couteau (1952).                    Cou1952a
           J   932     AB,C: Additional notes may be found in Jonckheere (1949) and            J__1949b
                       Couteau (1952).                                                         Cou1952a
03349-1604 GAL 353     Object #97 in Gallo's original list. ARA  17.                           Gal1912b
03350+6002 STF 400     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.96 +/- 1.62, 2.62, and 1.30 Msun, respectively.  Mlk2012 
03350+3201 STF 410     A is an ellipsoidal variable, IX Per.                                           
03352+0543 TOK 657     CPM, common parallax, both on MS.                                       Tok2014d
03353+1549 BPM  78     [PM2000]  133139 + [PM2000]  133157.                                    Gvr2010 
03354+3948 MLB1064     ALI 1035.                                                                       
03355-3218 LDS3510     NLTT 11346/11349                                                        Chm2004 
03356+4253 LDS9156     Old LDS6156.                                                                    
                       AD: NLTT 11280/11270                                                    Chm2004 
03357-1644 GWP 484     ABL 149.                                                                Tob2012b
03361-0320 J  1457     HD 22393.                                                               J__1941a
03362+4220 A  1535     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.99 +/- 0.69, 2.06, and 0.95 Msun, respectively.             Mlk2012 
03368+2106 LDS3511     NLTT 11370/11371                                                        Chm2004 
03368+0035 STF 422     A premature orbit has been computed. The primary is a variable of the           
                       RS CVn type, V711 Tau., and also a spectroscopic binary, P = 2.8 d.             
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       H 3  45.                                                                MEv2010 
03369-4957 SEE  29     The astrometric orbit of the stars comprising the A component was               
                       generated by a fit to individual data points available in Hipparcos             
                       Intermediate Astrometry Data.                                           Mkr2007a
                       Primary is possible SB.                                                 Tok2014d
           TOK 207     Likely triple. The inner pair produces RV variability and acceleration,         
                       the outer companion at 2".7 is discovered with NICI.                    Tok2012a
03370-2808 LDS 840     NLTT 11423/11421                                                        Chm2004 
03372+3710 BRT3236     ALI 283.                                                                        
03373-8517 R    39     Also appears to be R    48.                                                     
03374-8051 HJ 3607     B is CPD-81@89.                                                                 
03375+3107 GC 4314     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03376+1751 LDS3512     NLTT 11415/11416                                                        Chm2004 
03376-0103 GWP 486     ABL 150.                                                                Tob2012b
03377+7235 HJ 2190     C component is galaxy NGC 1343.                                                 
03377-0801 GWP 487     ABL 151.                                                                Tob2012b
03378+4046 COU1517     AB Per, an Algol type eclipsing binary, P = 7.1601d.                    Zas2012 
03378+1526 HD  22522   This star was misidentified as BD+17 0593 = SAO 93525 in the first              
                       speckle catalog.                                                        McA1984b
03379+8017 MLR 456     Also known as TDS2606.                                                          
03379+1950 LDS3515     G006-022. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 11424/11425                                                        Chm2004 
03381-1133 OL  151     Aka HEI 315.                                                                    
03382-5947 DUN  14     B is CPD-60@261.                                                                
                       SHY 448. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
03383+4448 S   430     STTA 37.  B is BD+44@759.                                                       
                       AB: HJL  50.                                                            HJL1986 
03388+5055 ES  953     Appears to be the lost HJ 2197.                                         Dam2015b
03388-1607 LDS3517     NLTT 11485/11486                                                        Chm2004 
03390+4232 RAO  47     Triple system consisting of an astrometric binary with period of 3 yr           
                       (Goldin & Makarov 2007) and Robo-AO tertiary B at 1".76. Considering    Gln2007 
                       the fast PM(A), the fixed position of AB during 1 year would appear to          
                       confirm it as a physical binary. B is located well below the MS,                
                       although its photometry has a large uncertainty. If it is a physical            
                       component with unusual colors, the system merits further study.         Rbr2015d
03392+5632 JNN 258     G 175-2. Estimated age 1000-10000 Myr; masses 0.60 +/- 0.10 and 0.38            
                       +/- 0.03 Msun; a ~24.7 au.                                              Jnn2014 
03393+5632 JNN 258     Aa,Ab: Originally 03392+5632; merged with 03393+5632.                           
03395-1017 GWP 494     ABL 153.                                                                Tob2012b
03396+3747 GRV 185     Primary is V736 Per, Algol-type eclipsing binary, period 3.76674d.      Zas2013 
03396+2530 LDS9158     old LDS6158. This is the common proper motion pair Wolf 204,5.                  
03396+1823 TOK  14     AB has estimated period 5000y; primary is 8.7d SB2.                     Tok2006 
           LDS9159     AC: Old LDS6159.                                                                
                       NLTT 11499/11500                                                        Chm2004 
           JAO   9     Ba,Bb: Referred to as G 006-026BC by Jao et al. (2016), but the C       Jao2016 
                       component is the Luyten companion. Combined astrometric/spectroscopic           
                       solution yields component masses 0.474 +/- 0.053 and 0.436 +/- 0.049            
                       Msun, plus an orbital parallax  of 26.34 +/- 0.2 mas. There is an               
                       error in their Table 3: a" = 0.0225 +/- 0.0008" (Jao, private comm.)            
03397-0331 GWP 495     ABL 155.                                                                Tob2012b
03397-1612 GWP 496     ABL 154.                                                                Tob2012b
03397-2727 LDS 841     NLTT 11538/11539                                                        Chm2004 
03398+3328 ES  327     Also known as GJ 9119 B, this star is a wide companion to GJ 9119 A at          
                       about 14" as noted in e.g. the WDS catalog. It is however single in             
                       the separation range covered by the AstraLux data.                      Jnn2012 
03398+0515 J  1812     BAL 2608.                                                                       
03400+6352 STTA 36     A,BC: HJL  51.                                                          HJL1986 
                       A,BC: SHY 160. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                       very high (near 100%) probability pair is physical.                             
03401+3407 STF 425     H 2  52.                                                                MEv2010 
                       The B component was resolved at Palomar (0.580"). Genet et al. (2013)           
                       detect a wobble in the motion of AB, with P~107y, alpha~0.18"                   
                       suggesting M2~0.5 Msun                                                  Tok2014d
                       AB: known binary, which shows apparently a non-Keplerian motion. Rica           
                       Romero & Zirm (2014) proposed that the motion was caused by an unseen   RMR2014c
                       companion and calculated an astrometric orbit for it with P = 107 yr,           
                       eccentricity 0.61, and photocenter semimajor axis 0".179. Our                   
                       observations were able to resolve the predicted subsystem Aa,Ab. For            
                       the time of our observations the orbit predicts a companion position            
                       angle of 43.3 deg, in excellent agreement with the position angle of            
                       44 +/- 1.3 deg measured here. The ratio of the predicted displacement           
                       to the measured separation of 0".50 is r = 0.32 = q/(1+q). Hence, the           
                       mass ratio q = 0.47 (the contribution of the light from Ab to the               
                       photo-center is neglected). The mass of Aa is estimated at 1.16 Msun            
                       from its absolute magnitude, leading to 0.54 Msun for Ab. The absolute          
                       magnitude of Ab corresponds to a smaller mass of 0.33 Msun. This                
                       discrepancy, if confirmed, can be explained by Ab being a close pair            
                       of M-dwarfs, as happens in other known multiple systems, e.g., in kap   Tok2013a
                       For (Tokovinin 2013).                                                   Rbr2015d
03402-1936 GC 4392     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03403-0805 STF 433     B is BD-08@698.                                                                 
03404-1502 GWP 497     ABL 156.                                                                Tob2012b
03405-1925 GWP 498     ABL 157.                                                                Tob2012b
03406+2846 STF 427     H N  23.                                                                MEv2010 
                       V1268 Tau, Algol (EA) type eclipsing binary, P = 8.161235 d.            Zas2011 
03407+0643 A  1934     Companion not seen in 1934.                                                     
03409+1435 BPM  79     [PM2000]  137052 + [PM2000]  137046.                                    Gvr2010 
03409-1237 STF 436     B is BD-13@712.                                                                 
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
03413+4554 BU 1181     Motion in separation. The period may be fairly short. Needs speckle.            
                       Additional notes may be found in van den Bos (1963).                    B__1963b
                       Known triple system. Inner binary has been known for over a century     Bu_1894d
                       (Burnham 1894); its first orbit was computed by Riddle et al. (2015).   RAO2015 
                       They also detected a third component C which was confirmed by                   
                       examination of 2MASS images. The close binary is detectable in our Ks           
                       images, but the PSFs of the stars are overlapping and we are unable to          
                       make a consistent measurement with fitstars. We are able to extract             
                       the astrometry of the AC pair and consider it as likely physical.       Rbr2015d
03414-0934 GWP 501     ABL 159.                                                                Tob2012b
03414-1421 GWP 499     ABL 158.                                                                Tob2012b
03416+2655 LDS6095     Also known as GRV 187.                                                          
03418+6239 BLL  12     A is a semi-regular variable, U Cam. B is BD+62@594.                            
03418+5317 A   985     Primary is the eclipsing binary CV Cam, P = 0.97326 day.                Zas2010 
03419-5542 JNN  25     2MASS J03415581-5542287 and J03415608-5542408 are separated by only             
                       12" and have similar estimated spectroscopic distances (14 and 20 pc,           
                       respectively) in Riaz et al. (2006), hence it is likely that they form  Ria2006 
                       a physical pair. 2MASS J03415581-5542287 is a close (~0.61") binary in          
                       our data, so the system is likely triple in reality, although common            
                       proper motion of all components has yet to be proven.                   Jnn2012 
03422+6313 BD Cam      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1984).                                                         Grf1984c
03422+5436 HJ 2198     B is BD+54@704.                                                                 
03423+3141 COU 691     A premature orbit has been computed.                                            
03424+3358 STF 431     40 Per = o Per. A spectroscopic binary. Spectrum of B: A1Vn.                    
                       H 3  39.                                                                MEv2010 
03424-1200 GWP 503     ABL 160.                                                                Tob2012b
03424-8001 HJ 3612     Spectrum: G0/2III/IV. B is CPD-80@94.                                           
03425+3256 HJ  336     Also known as STF 432.                                                          
03425+1416 BPM  80     [PM2000]  138169 + [PM2000]  138144.                                    Gvr2010 
03425+1216 JNN  26     Since the two epochs of observation were acquired over a baseline of            
                       only a few months, there is not yet sufficient motion to confirm                
                       common proper motion of the companion that was detected with AstraLux.          
                       However, the separation between components is rather small (~0.86"),            
                       and the fact that the companion is clearly detected in z' but too               
                       faint in i' implies that it must be very red, as expected for a real            
                       companion. Hence, we count it as a binary system for statistical                
                       purposes.                                                               Jnn2012 
                       Primary is an active M4.0Ve star, age 60-300 Myr. Bowler et al (2015)           
                       confirm B is physically bound and detect slight orbital motion. The             
                       projected separation is 19.8 +/- 0.9 au. Spectral type of B is                  
                       L0 +/- 1, mass 35 +/- 8 Mjup.                                           Bwl2015 
03425+0202 BAL1260     HJL  52.                                                                HJL1986 
03426+1718 GC 4435     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03426-2445 RST2317     TDS2636.                                                                        
03427+1448 BPM  81     [PM2000]  138368 + [PM2000]  138396.                                    Gvr2010 
03427-2428 LDS3527     NLTT 11680/11682                                                        Chm2004 
03429+4747 BUP  46     del Per = 39 Per. A possible variable of the Alpha CVn type.                    
03430+4554 JNN 259     NLTT 11633. Estimated age 1000-10000 Myr; masses 0.28 +/- 0.03 and              
                       0.20 +/- 0.04 Msun; a ~21.8 au.                                         Jnn2014 
03430+2515 LDS1148     NLTT 11651/11648.                                                               
03431+2541 STF 435     H 3  88.                                                                MEv2010 
03435-4549 PRB   1     Primary is WD 0341-45 = VY Hor, secondary (not found in Aladin) is              
                       BPM 31492. Possible CPM pair, according to Probst (1983).               Prb1983 
03438+4236 ENG  14     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
03439+1640 GIC  44     AB = G006-029/G006-028 = GJ 9122AB.                                             
                       AB: NLTT 11693/11688                                                    Chm2004 
                       AB: SHY  17. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
03439-7100 HJ 3603     B is CPD-71@@218.                                                               
03440+3822 STF 434     B is BD+37@@821.                                                                
03440-1836 GWP 505     ABL 161.                                                                Tob2012b
03441+3207 DCH   3     HMW 72. Monitored for photometric variability 1998-2003 by Cohen et             
                       al. (2004). Range of variability dI = 0.527 mag, no periodicity found.  CHW2004 
03442+3207 STF 437     H 3  37.                                                                MEv2010 
                       SEI  31.                                                                Nsn2017a
03442-6448 LDS 104     bet Ret. A is a spectroscopic binary. B has separation of 1480". B is           
                       CPD-65@272.                                                                     
           bet Ret     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Jones (1928).                                                           Jon1928a
03443+3217 BU  535     38 Per = omi Per = Atik. Ellipsoidal and spectroscopic binary.                  
03443+3208 DCH   4     HMW 73. Monitored for photometric variability 1998-2003 by Cohen et             
                       al. (2004). Range of variability dI = 1.271 mag; multiple periods,              
                       average = 7.582d. Photometry may be contaminated by nearby star.        CHW2004 
03444+3210 DCH   5     HMW 10/78 = LLRL 10/45. Monitored for photometric variability                   
                       1998-2003  by Cohen et al. (2004). Range of variability dI = 0.030 mag          
                       for A component, 4.816 mag for B. No periodicity found for either               
                       component. Photometry of B may be contaminated by nearby companion.     CHW2004 
03444+3207 DCH   7     HMW 136. Monitored for photometric variability 1998-2003 by Cohen et            
                       al. (2004). Range of variability dI = 0.789 mag, no periodicity found.  CHW2004 
03444+3206 DCH   6     HMW 39. Monitored for photometric variability 1998-2003 by Cohen et             
                       al. (2004). Range of variability dI = 0.251 mag; multiple periods,              
                       average = 9.667d.                                                       CHW2004 
03444+2812 A  1826     Not seen on three nights 1964-1982.                                             
03444+1637 BPM  82     [PM2000]  139475 + [PM2000]  139465.                                    Gvr2010 
03445+3212 DCH   8     HMW 13 = LLRL 12. Monitored for photometric variability 1998-2003 by            
                       Cohen et al. (2004). Range of variability dI = 0.048 mag, no                    
                       periodicity found.                                                      CHW2004 
03445+3211 DCH  10     HMW 86. Monitored for photometric variability 1998-2003 by Cohen et             
                       al. (2004). Range of variability dI = 0.318 mag, no periodicity found.  CHW2004 
03445+3210 DCH   9     HMW 75 = LRLL 40. Monitored for photometric variability 1998-2003 by            
                       Cohen et al. (2004). Range of variability dI = 0.337 mag, nonperiodic.  CHW2004 
03445+3209 DCH  12     HMW 12 = LLRL 29. Monitored for photometric variability 1998-2003 by            
                       Cohen et al. (2004). Range of variability dI = 0.181 mag; multiple              
                       periods, average = 2.237d.                                              CHW2004 
03445+3208 DCH  13     HMW 42 = LRLL 86. Monitored for photometric variability 1998-2003 by            
                       Cohen et al. (2004). Range of variability dI = 0.097 mag; multiple              
                       periods, average = 6.532d.                                              CHW2004 
03445-1322 GAL 354     Object #99 in Gallo's original list.                                    Gal1912b
03446+3210 BU  880     AB: HMW 1 = LRLL 1. Monitored for photometric variability 1998-2003 by          
                       Cohen et al. (2004). Range of variability dI = 0.455 mag, no                    
                       periodicity found.                                                      CHW2004 
                       SEI  32.                                                                Nsn2017a
           STF 439     AB,C: H 3  38.                                                          MEv2010 
03446+3209 DCH  11     AB: HMW 27/28 = LLRL 16/33. Monitored for photometric variability               
                       1998-2003 by Cohen et al. (2004). Range of variability dI = 0.097 mag           
                       for A, 1.462 mag for B. Multiple periods seen for A, average = 2.656d.          
                       Photometry of B may be contaminated by nearby companion.                CHW2004 
03446+3209 HER  20     CD: HM 107 = LLRL 165. Monitored for photometric variability 1998-2003          
                       by Cohen et al. (2004). Range of variability dI = 0.328 mag, no                 
                       periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03446+3208 HER   7     Additional notes may be found in Herbig (1962).                         Her1962 
03446+3207 DCH  14     HMW 11 = LRLL 6. Monitored for photometric variability 1998-2003 by             
                       Cohen et al. (2004). Range of variability dI = 0.094 mag; multiple              
                       periods, average = 1.687d.                                              CHW2004 
03446+2754 STTA 38     Optical with BU 1041BC, which is BD+27@558, at 03 44.7 +27 55.                  
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           BU 1041BC   The B component has both an astrometric and a spectroscopic orbit       Gln2007 
                       which are not associated with the optical BC pair.                      Grf2015c
03446-5416 HJ 3592     See claimed A was a close pair in 1897, but no trace of it was seen     See1898c
                       subsequently by van den Bos, Dawson, and Innes.                         Daw1918a
03447+3211 HER  21     HM 98 = LRLL 166. Monitored for photometric variability 1998-2003 by            
                       Cohen et al. (2004). Range of variability dI = 0.960 mag, no                    
                       periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+3210 DCH  15     HMW 99 = LRLL 221. Monitored for photometric variability 1998-2003 by           
                       Cohen et al. (2004). Range of variability dI = 2.136 mag, no                    
                       periodicity found.                                                      CHW2004 
03447+3209 DCH  16     HMW 14 = LRLL 9. Monitored for photometric variability 1998-2003 by             
                       Cohen et al. (2004). Range of variability dI = 0.109 mag; multiple              
                       periods, average = 2.539d.                                              CHW2004 
03447+3208 DCH  17     HMW 111 = LLRL 52. Monitored for photometric variability 1998-2003 by           
                       Cohen et al. (2004). Range of variability dI = 0.187 mag, no                    
                       periodicity found. Photometry may be contaminated by nearby star.       CHW2004 
03447+2449 ITO   7     Pleiades HII 405.                                                               
03447+2414 LDS6103     A component is Pleiades star Melotte 22 HII 430.                                
03448+4602 BAG   8     Combined astrometric/spectroscopic solution by Balega et al. (2002),    Bag2002b
                       including determination of component masses.                                    
                       The Balega (2002) orbit predicts a separation of 0.055" in mid-2006,    Bag2002b
                       opening rapidly to 0".197 in late 2007. Perhaps T0 is not quite                 
                       correct?                                                                Hrt2009 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.54 +/- 0.13, 1.54, and 0.79 Msun, respectively.             Mlk2012 
03448+2417 HL    6     Primary is Pleiades star Celaeno = 16 Tau.                                      
03448-7002 LFR   1     SHY 450. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
03449+2407 HL    7     Primary is Pleiades star Electra = 17 Tau.                                      
03452+4235 ES 2601     nu Per = 41 Per                                                                 
03452+2450 HL    8     Primary is Pleiades star 18 Tau.                                                
03452+2428 HJ 3251     Primary is Pleiades star Taygeta = 19 Tau = 19 Pleiadum.                        
                       A is a spectroscopic and occultation binary.                                    
03454+2402 HL   10     Primary is Pleiades star.                                                       
03454-2752 BU 1003     A premature orbit has been computed. Motion direct and increasing as            
                       the pair closes in. However, there are no measures in the last twenty           
                       years.                                                                          
03457+2438 YAM   1     Pleiades cluster member. Primary is the BY Dra type variable V855 Tau.  Yam2013 
03457+0603 HJ 2204     29 Tau. A is a spectroscopic binary.                                            
03458+2422 HL   11     Primary is Pleiades star Maia = 20 Tau.                                         
03458+2309 STF 444     Spectroscopic binary, P = 7.15d.                                                
03459+2433 HL   12     Primary is Pleiades star Asterope = 21 Tau.                                     
03459+2402 HL   13     Primary is Pleiades star.                                                       
03460+7302 MLR 457     Same as HDS 476.                                                                
03460+2432 HL   14     Primary is Pleiades star 22 Tau.                                                
03460+1721 BPM  83     [PM2000]  140561 + [PM2000]  140577.                                    Gvr2010 
03461-1522 GWP 508     ABL 163.                                                                Tob2012b
03461-1708 GWP 507     ABL 162.                                                                Tob2012b
03461-6405 HJ 3600     B is CPD-64@271.                                                                
03462+2434 POU 309     LDS6108.                                                                        
                       Both components are Pleiades variables. A = Melotte 22 HII 879 = V813           
                       Tau, while B = Melotte 22 HII 883 = V789 Tau.                                   
03462+1710 HJ 3252     This star has a possible wide companion at about 8" as noted in the             
                       WDS. It is however single in the separation range covered by the                
                       AstraLux data.                                                          Jnn2012 
03463+2411 BU  536     In the Pleiades. The motion so far is retrograde and rectilinear.       Hzg1958 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Both elliptical orbit and rectilinear trajectory were calculated by             
                       Popovic & Pavlovic (1995). See also rectilinear catalog.                Pop1995d
03463+2357 HL   15     Primary is Pleiades star 23 Tau = Merope.                                       
03463-1235 GAL 355     Object #103 in Gallo's original list.                                   Gal1912b
03464+7523 STF 418     Same as PRZ   4. Coordinates of PRZ   4 correct and retained.                   
03464+2435 ITO   8     AB: Pleiades HII 996.  Primary is the BY Dra-type variable V1045 Tau.   Ito2011 
           LDS6110     AC: Possibly common with LDS6108.                                               
03464+1143 LEP 119     LHS 1589 = NLTT 11793. Lepine et al. determine a photometric distance   Lep2007b
                       of 81 +/- 18 pc; masses are estimated at 0.25 and 0.20 Msun.                    
03465+2508 ITO   9     Pleiades HII 1015.                                                              
03465+2426 ITO  10     Pleiades HII 1032.  Primary is V1171 Tau. Both companions are                   
                       background stars.                                                       Yam2013 
03465+2415 CHR  12     Pleiades cluster member.                                                        
                       1985.8488: This measure is from reanalysis of archival data.  Not               
                       listed as an SB by Abt et al. (1965), but it may show measurable        AbH1965b
                       velocity variation at some phases of a possibly eccentric orbit.        Msn1993b
                       Aa,Ab: Observed 20 times 1982-1998 and resolved 4 times 1983-1989,              
                       with separations decreasing from 0.236" to 0.160". Motion indicates a           
                       ~40-year period orbit.                                                  Hrt2009 
03466+2950 BRT 233     MLB 683.                                                                        
03466+2458 MET  34     Pleiades cluster member. The companion is a background star.            Yam2013 
03466+2255 RDR   2     Primary is an F6 Pleiades member (HII 1132). Based on common motion             
                       over 4 years, Rodriguez et al. (2012) conclude the B component is               
                       either a companion to the primary or (less likely) a nearby comoving            
                       Pleiades member. Assuming they comprise a physical pair, the companion          
                       is a brown dwarf, with mass estimated at 0.06 +/- 0.01 Msun,                    
                       temperature 2600 +/- 100K.                                              Rdr2012b
03467+2402 LDS6111     A component is a Pleiades variable = Melotte 22 HII 1124 = V814 Tau.            
03467-1231 GAL 356     Object #104 in Gallo's original list.                                   Gal1912b
03470+4126 STF 443     HIP 17666. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: NLTT 11792/11791                                                    Chm2004 
                       Proper motion of A +596 -1249. Proper motion of B +594-1259. B is a             
                       single-lined spectroscopic binary, P = 48.65d. A common proper motion           
                       companion, G095-059, mag. 13.4, lies more than 2 degrees away.                  
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AB: HJL  53.                                                            HJL1986 
03470+2431 CHR 124     Occultation binary. Has variable radial velocity. Pleiad.                       
03471+2449 BU  537     Variable, V534 Tau.                                                             
03473+2424 BOV  18     Geissler et al (2012) conclude companion is an M8 brown dwarf, the              
                       first substellar companion discovered around a Pleiades star.  Mass             
                       estimates range from 0.052 to 0.063 Msun, depending on distance, etc.   Gei2012 
                       Pleiades cluster member. The companion shares common proper motion.     Yam2013 
03473+2348 HL   18     Primary is Pleiades star.                                                       
03473+2344 HL   19     Primary is Pleiades star.                                                       
           BOV  17     CF: 03471+2343BOV  17 = HL  19C, system merged.                                 
03474+2435 HL   20     Primary is Pleiades star.                                                       
03474+2355 STF 450     POU 311. Primary is Pleiades star.                                              
03474+2255 HD 23610    Hipparcos astrometric solution assumed circular orbit (e = omega = 0);  HIP1997d
                       Cluster Melotte 22 #1407.                                                       
03475+2417 HL   22     Primary is Pleiades star.                                                       
03475+2406 STFA  8     Primary is Pleiades star Alcyone = 25 Tau = eta Tau = V647 Tau.                 
                       STTA 42.                                                                        
                       A is an occultation and spectroscopic binary.                                   
                       B, at 03 47.4 +24 07, is an occultation binary.                                 
                       C is V647 Tau.                                                                  
                       BC: HJL1029.                                                            HJL1986 
                       BD: HJL1028.                                                            HJL1986 
                       CD: HJL1027.                                                            HJL1986 
03476+2337 HL   24     Primary is Pleiades star.                                                       
03478+3501 ES  235     Primary is eclipsing binary of Algol type, period 1.92873d.             Zas2014 
03478+3212 HR 1164     Orbit determined by fitting revised Hipparcos intermediate astrometric          
                       data. Derived component masses 1.44 +/- 0.09 and 1.15 +/- 0.08 Msun.    Ren2010 
03479+3336 STF 448     HJ 5457. A is a spectroscopic binary. Also, one component is variable.          
03479+2555 BRT2520     Heintz finds no pair in the field, and believes identity with J 27      Hei1985a
                       (03470+2855) is possible.                                                       
03479+2407 BU  538     AB. Identification of a 2000.8 measure by Lampens et al. (2007)         Lmp2007 
                       originally attributed to 03481+2409 COU  80 was corrected by the                
                       author; it actually was of this pair.                                           
03480+6840 KUI  13     See discussion by van de Kamp & Chao-Yuan Yang.                         Kam1967 
           WNO  16     AD: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
03480+4032 TOK 240     Primary is an exoplanet host, P=1565d                                   Tok2014d
03480-7048 HJ 3606     B is CPD-71@223.                                                                
03481+2409 COU  80     Pleiad.                                                                         
                       Identification of a 2000.8 measure by Lampens et al. (2007) originally  Lmp2007 
                       attributed to this pair was corrected by the author; it actually was            
                       of 03479+2407 BU  538AB.                                                        
03482+2419 CHR 155     Included in the Pleiades cluster survey of Abt et al. (1965), who did   AbH1965b
                       not detect variable RV. Pearce & Hill (1975 Pub DAO, 14, 319) did               
                       notice velocity variation at the 1% level, and Liu et al. (1997) found  Liu1997 
                       the system to be a SB2, although large velocity difference may imply a          
                       closer companion than this.                                             Msn1993b
03482+2219 EQ Tau      Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                       estimate the mass of the contact pair at 1.752 Msun and the minimum             
                       mass of the wider component at 0.49 Msun.                                       
03483+2325 HL   25     Pleiades H 722. Primary was misidentified as SAO 76125 in the first             
                       speckle catalogue.                                                      McA1984b
03483+1109 STF 452     30 Tau.                                                                         
                       H 3  66.                                                                MEv2010 
03483-0943 GWP 517     ABL 164.                                                                Tob2012b
03484+5202 HU  546     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.17 +/- 0.43, 1.53, and 1.20 Msun, respectively.             Mlk2012 
03486+3039 SHY 453     HIP  17796 + HIP  18204.                                                        
03486-3737 DUN  16     f Eri. One component is a possible Beta Lyrae-type system.                      
03489+6445 STT  62     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.82 +/- 0.52, 2.75, and 1.20 Msun, respectively.             Mlk2012 
03489+2351 HL   27     Primary is Pleiades star 26 Tau.                                                
03490+5120 LDS9160     Old LDS6160. NLTT 11871/11873.                                                  
03491+4358 V376 Per    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
03492+3651 J  2721     BRT 2586. ALI 288.                                                              
03492+2408 CHR 125     Aa,Ab: Pleione, 28 Tau = BU Tau. Shell star and suspected long-period           
                       spectroscopic binary (Hoffleit 1982) . Pleiades cluster member.         Hof1982 
                       Frequently unresolved, probably due to large Delta m.                   Msn1993b
                       For their measure, Roberts et al. reports that the "The close                   
                       proximity of the two star's PSFs prevented accurate measurement of the          
                       astrometry and photometry."                                             Rbr2007 
                       Aa,Ab: Observed 3 times 1987-1991 (all observations noted as weak),     Rbr2007 
                       then unresolved until a 2002 (0.24") measure at 900nm                   Hrt2009 
           RBR   4     AF: 2002.0924: PA is measured in zenith mode. If data collected in              
                       equatorial mode, PA = 119. Confirmation of the pair should establish            
                       the correct value for theta.                                            Rbr2007 
03492+2403 STF 453     Primary is Pleiades star Atlas = 27 Tau = Melotte 22 #2168                      
                       Position angles scattered. Distances range from "single" to 0.6". Some          
                       question duplicity. A is a long-period spectroscopic binary.                    
           MKT  12     Aa1,Aa2: Hipparcos astrometric solution assumed circular orbit (e =             
                       omega = 0).                                                             HIP1997d
                       Pan et al. (2004) orbit is based on Mark III and PTI measures. A        PTI2004 
                       distance to the Pleiades of 135 +/- 2 pc is determined. Masses for the          
                       components are calculated as 4.90 +/- 0.28 and 3.65 +/- 0.08 Msun.              
                       Zwahlen et al. (2004) orbit is based on published Mark III and PTI      Zwa2004 
                       measures, plus additional Mark III and NPOI astrometric data and                
                       ELODIE echelle spectra. This combined spectroscopic/interferometric             
                       solution yields masses of 4.74 +/- 0.25 and 3.42 +/- 0.25 Msun; the             
                       distance 132 +/- 4 pc found agrees with "traditional" Pleiades                  
                       distances obtained through MS fitting techniques.                               
                       Aa1,Aa2: Malkov et al. (2012) derive dynamical, photometric, and                
                       spectroscopic masses 5.68 +/- 0.79, 6.68, and 3.31 Msun, respectively.  Mlk2012 
03493+5707 S   436     STTA 39. B is BD+56@847.                                                        
                       HJL1030.                                                                HJL1986 
03493-1656 GWP 519     ABL 165.                                                                Tob2012b
03494+5214 ES  770     B is BD+51@781.                                                                 
03494+2423 STTA 40     AB: LDS6116. B is BD+23@560. A is Pleiades star and occultation double          
           HL   30     BC: Primary is Pleiades star.  Also known as STU   2BC.                         
           HL   30     BD: Also known as STU   2BD.                                                    
03495+5239 STF 446     Also known as STF 454. Another classification: B0Ib. The primary is             
                       slightly variable; the system is a member of the cluster NGC 1444.1             
03495+1255 AG   74     Primary is V1128 Tau, a 10th magnitude W UMa type eclipsing binary,             
                       with period 0.3053725d.                                                 Zas2011 
03496+6318 CAR   1     Also known as MOAI 1.                                                           
                       1995.948: Theta corrected from published value of 213 deg (Aristidi,            
                       private communication)                                                          
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.76 +/- 0.61, 3.36, and 1.82 Msun, respectively.             Mlk2012 
03496+3859 HU 1067     A RW Aur-type variable, XY Per. Both components may vary.                       
                       dm estimates on a number of nights. quadrant reversed on 1936 Jan 17,           
                       indicating primary is responsible for variation. Beyer (AN 263, 71,             
                       1937) established the irregular character of the variation.             VBs1954 
03496-0220 YR   23     Triple. The RV amplitude of 9.5 km s-1 and double lines seen in GCS             
                       cannot be caused by the visual system YR 23 with estimated period of            
                       ~50 yr which could however be responsible for dmu.                      Tok2012a
03497+2343 HL   32     Primary is Pleiades star.                                                       
03497+2320 YAM   2     BC: Pleiades cluster member. The companion is a background star.        Yam2013 
                       Pair initially 03495+2323 YAM 2; merged with 03497+2320 LDS6118.                
03498+2421 HL   33     Primary is Pleiades star.                                                       
03498+2342 ITO  11     Pleiades HII 2462.                                                              
03499+2313 ITO  12     Pleiades HII 2506.                                                              
           YAM   3     Pleiades cluster member. The companion is probably a background star.   Yam2013 
03500+2351 STT  64     A is a spectroscopic binary, P = 16.72d, spectrum B9.5VpSiSrCr. Pleiad          
03501+4458 CHR 126     A spectroscopic binary.                                                         
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       P'edoussaut et al. (1987).                                              Ped1987 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Pedoussaut et al. (1987).                                               Ped1987 
03501+0637 TOK  80     HIP 17936. The magnitude difference in the 2MASS PSC dK=1.8 is                  
                       suspect (5" separation), dK=3.4 is measured with ANDICAM.               Tok2011a
03502-1335 FAR  32     NLTT 11972. Primary is white dwarf WD 0347-137.                         Far2006 
03503+2535 STT  65     One star variable?                                                      Wor1967b
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.15 +/- 0.39, 3.39, and 3.91 Msun, respectively.             Mlk2012 
03503-0131 SHY 164     AE: HIP  17950 + HIP  16933. E component = A component of 03379-0231.           
                       AB: Hipparcos identified the pair as a candidate for Hyades membership. HIP1998 
                       However, radial velocity classifies this as not a Hyades member.        Grf2013c
03504+7120 HJ 2200     gam Cam                                                                         
03505-1219 GAL 357     Object #105 in Gallo's original list.                                   Gal1912b
03506+2431 YAM   4     Pleiades cluster member. Primary is V1174 Tau.                          Yam2013 
03506-4234 EGN   3     Pair bound, with projected separation 73au. Mass of secondary                   
                       0.15 +/- 0.01 Msun; spectral type M4-M6.                                Egn2007 
03507-1206 GAL 358     Object #106 in Gallo's original list.                                   Gal1912b
03508+4546 FMR  63     Typographical error in initial WDS designation (03508+4946)                     
03510+1414 JLM   1     Erroneously labelled as JML 1; changed upon request of discoverer.              
03511+3548 BRT3238     ALI 51.                                                                         
03511+1551 BPM  84     [PM2000]  144054 + [PM2000]  144088.                                    Gvr2010 
03513+2621 A  1830     The few observations do not define the nature of the motion.                    
03514+2538 HEI   9     Primary is eclipsing binary of Algol-type, period 1.26292 d.            Zas2012 
03514-1610 GWP 523     ABL 166.                                                                Tob2012b
03517+7030 HJ 1139     B is BD+70@263.                                                                 
03517+2433 LDS5437     A component is a Pleiades variable = Melotte 22 HII 3096 = V1054 Tau.           
                       B component is flare star V383 Tau.                                             
03518+3453 ARN  58     Also known as GRV 196.                                                          
03518-0306 GWP 524     ABL 167.                                                                Tob2012b
03520+2440 BOV  27     AB: Assuming a Pleiades parallax of 7.43 +/- 0.17 mas (distance 134.6           
                       pc; Soderblom et al. 2005, AJ 129, 161), Schaefer et al. (2014) find a          
                       total mass of 1.42 +/- 0.10 Msun. The revised Hipparcos parallax of             
                       8.32 +/- 0.13 (120.2 pc; van Leeuwen 2009, A&A 497, 209) gives a total          
                       mass of 1.01 +/- 0.05 Msun, which is not consistent with the                    
                       corresponding photometric masses of the components.                     Sfr2014 
03520+0632 KUI  15     31 Tau.                                                                         
                       AB: Additional notes may be found in Van Biesbroeck (1954) and          VBs1954 
                       Couteau (1955).                                                         Cou1955c
03525+3546 ES 2334     BRT 3239. ALI 52.                                                               
03525-0403 GWP 525     ABL 168.                                                                Tob2012b
03526-0829 RST4762     The few measures do not define the motion.                                      
03527-0522 HJ  338     30 Eri.                                                                         
03529+3532 ES 2459     BRT 3240.                                                                       
03529-0633 GWP 528     ABL 169.                                                                Tob2012b
03530+1158 BPM  85     [PM2000]  145369 + [PM2000]  145423.                                    Gvr2010 
03530-1332 GWP 529     ABL 170.                                                                Tob2012b
03534+1743 BPM  86     [PM2000]  145657 + [PM2000]  145663.                                    Gvr2010 
03535+3538 ES 2460     Identical to ALI 54 and BRT 3237                                        Hei1983a
03535-1229 GAL 359     Object #107 in Gallo's original list.                                   Gal1912b
03535-1440 GWP 531     ABL 171.                                                                Tob2012b
03536+2718 OCC9003     The OCC2010 solution is ambiguous and one is arbitrarily "T" coded              
                       until the true solution is determined.                                          
03536+2146 OL  184     TDS2678. Appears to be the same as 03549+2148 OL  200. IDS notes that           
                       OL  200 is possibly identical to 03559+2146 HU  815, but they appear            
                       to be different pairs.                                                          
03537+5316 A  1293     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.00 +/- 0.24, 1.94, and 1.05 Msun, respectively.             Mlk2012 
03539-1751 GWP 532     ABL 172.                                                                Tob2012b
03541+3153 STF 464     zet Per = 44 Per. A is a spectroscopic binary.                                  
                       AD: H 6  96.                                                            MEv2010 
03543-0257 STF 470     32 Eri. A is a spectroscopic binary.                                            
                       AB: H 2  36.                                                            MEv2010 
03544+0116 TOK  81     RoboAO finds a companion to B (233deg, 3.05", dI=5.88mag), but it is            
                       thought to be optical.                                                  Tok2014d
03544-0649 A   461     Less than 0.1" in 1954 - 1961. It appears that a revolution has been            
                       completed.                                                                      
03544-4021 FIN 344     Spectroscopic binary.                                                           
                       1989.9438: This is the first observation of this system since those of          
                       Finsen in the 1960's, and is considerably closer than any of his                
                       results.  It is known that in some instances Finsen's rho values                
                       appeared systematically larger than those of speckle; further                   
                       observations of this system will determine whether such is again the            
                       case.                                                                   Hrt1993 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.24 +/- 0.59, 4.58, and 4.88 Msun, respectively.  Mlk2012 
03545+3203 LEI   6     Member of Taurus-Auriga molecular cloud.                                Dae2015 
03545+0510 STTA 41     A is a Delta Scuti-type variable, V479 Tau. B is BD+04@@600.                    
                       A,BC(60") is probably physical.                                                 
           A  1831     BC: Less than 0.1" in 1954 - 1955 with 82-inch.                                 
                       A premature orbit has been computed. Motion direct.                             
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
03546+2507 HAT   1     30' error in WDS designation.                                                   
                       Member of Taurus-Auriga molecular cloud.                                Dae2015 
03546+2131 LDS1149     Old LDS6161. LDS9161.                                                           
03547+5200 TOR   5     Formerly known as PAN   2.                                                      
03547+1529 BPM  87     [PM2000]  146665 + [PM2000]  146678.                                    Gvr2010 
03547-1811 GWP 533     ABL 173.                                                                Tob2012b
03548-3542 TOK  82     HIP 18305. NOMAD: PM(B)=(-89,+19), V=11.48(??).                                 
                       PM(A)=(+108,+218).                                                      Tok2011a
03549-1426 GAL 360     Object #109 in Gallo's original list.                                   Gal1912b
03553-0237 BRT1928     BAL 25.                                                                         
03553-1921 GWP 534     ABL 174.                                                                Tob2012b
03554+3103 HO  325     A is a RW Aur-type variable, X Per, and also a long-period                      
                       spectroscopic binary.                                                           
03557-2236 I   722     CD-22@1398.                                                                     
03558+5225 TOR   6     Formerly known as PAN   3.                                                      
03558+5224 STF 462     HJ 2206.                                                                        
03561-4509 CPO 121     LDS 108.                                                                        
03561-4746 HU 1361     HIP 18402. B is definitely physical, but it is too red in the                   
                       (Kabs,V-K) CMD. Infrared companion? Nothing on B in SIMBAD.             Tok2011a
03562+5939 ENG  16     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           HDS 497     AD: CfA: P=12625d=34.6y? Abt & Willmarth (2006): RV=-22.18 const.       AbH2006 
03563-1935 GWP 535     ABL 175.                                                                Tob2012b
03564+4404 LDS5186     NLTT 12174/12173                                                        Chm2004 
03565-3642 BAS   2     This is the X Ray source EUVE J0356-36.6.                                       
03566+5042 S   440     43 Per. A is a spectroscopic binary. B is BD+50@861.                            
                       AB: H 5  41.                                                            MEv2010 
03571-0828 RST4764     Rapid retrograde motion.                                                        
03572-0706 OSW   7     Typographical error in WDS - initially entered as 03572-0025, with dec          
                       portion copied from OSW 8.                                                      
03573-1054 GWP 536     ABL 176.                                                                Tob2012b
03575-0110 BU  543     A premature orbit has been computed. A is a flare suspect.                      
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       NLTT 12237/12236                                                        Chm2004 
03576+5712 ES 1820     Doubtful this system is physically bound, since relative motion is              
                       larger than pm of A.                                                    Kiy2012 
03578+4932 KU   82     B is BD+49@1068.                                                                
03579+5142 SCA 176     Scardia (2017) measured an 8" pair located near the close (0".4) pair   Sca2017b
           COU2358     COU2358. Proper motions for the COU pair and the primary of the SCA     Cou1988b
                       pair were similar, so they were merged into one multiple system, with           
                       an 18" pair added to link them. This wide pair was given the same SCA           
                       176 discoverer designation and assigned components AB. The components           
                       for the COU pair were changed to Aa,Ab, those of the 8" pair to BC.             
03579+4001 STF 471     eps Per = 45 Per. A is a Beta Lyrae-type binary.                                
                       AB: H 2  22.                                                            MEv2010 
03580-1331 HJ 3608     gam Eri = 34 Eri = Zaurak. Variable?                                            
                       The faint pair, presumeably the original system, was recovered in       Dal2009 
                       2009, which appears to have common proper motion. All subsequent                
                       measures of the HJ 3608 were of a more distant pair with linear                 
                       motion relative to the primary, presumeably optical.                            
03583+2757 ARG  58     AG 75.                                                                          
03583-1659 GWP 537     ABL 177.                                                                Tob2012b
03584+2538 LDS5459     Also known as LDS9162.                                                          
                       NLTT 12251/12250                                                        Chm2004 
03586-0239 BU 1042     B is BD-03@651.                                                                 
03587+1646 LDS5462     GWP 538. Luyten's original 1960 measure listed theta = 144deg, 90deg    Luy1984 
                       different from the angle found by Bernal. Agreement on coordinates,     ABl2012a
                       separation, and magnitude difference led to the conclusion Luyten made          
                       a trigonometry error in his reduction.                                          
03590+3547 TRN  16     = ksi Per = Menkib.                                                             
                       The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.7342 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
03590+0947 HU   27     The value of omega for Ling's (2001) orbit was incorrectly given as     Lin2001b
                       263.1 in IAU Inf. Circ. 144.                                                    
                       Ling (2004) derived an orbital parallax 0".01239 and a mass sum of      Lin2004a
                       1.94 +/- 0.82 Msun.                                                             
03590-0056 HEI 215     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       However, radial velocity classifies this as not a Hyades member.        Grf2013c
03591-0656 LDS3545     NLTT 12296/12294                                                        Chm2004 
03591-2312 FAR   3     FAR  33. Primary is white dwarf WD 0357-233.                            Far2005b
03592+8020 JNN  27     A companion to 2MASS J03591438+8020019 was detected on two separate             
                       occasions with AstraLux, in both cases the detection is rather                  
                       tentative, but since it is detected twice with consistent properties            
                       we count it as a genuine detection. However, due to the poor quality            
                       of the fit and the fact that the two epochs of observation are only             
                       separated by 3 months, we do not try to acquire two epochs of                   
                       astrometry, but merely quote the astrometry as the mean (and standard           
                       deviation) of the two epochs.                                           Jnn2012 
03596-1019 HU   29     Motion in a highly-inclined orbit.                                              
03597+4809 STT  68     A is an Algol-type binary, IQ Per. B is BD+47@921.                              
03597-1147 GWP 540     ABL 178.                                                                Tob2012b
03597-1301 GAL 361     Object #110 in Gallo's original list.                                   Gal1912b
03598+1133 STF 478     LDS5464.                                                                        
03599+1325 LDS1150     Aka LDS5465.