04005+1935 KOH   1     Metchev & Hillenbrand say pair probably physical, based on proximity.   Met2004b
                       Member of Taurus-Auriga molecular cloud.                                Dae2015 
04005-4145 DON  58     B is above the MS in (V,V-K). Tuc-Hor moving group? (Kiss et al., 2011          
                       MNRAS 411, 117)                                                         Tok2014d
04005-5120 TOK  83     HIP 18713. NOMAD: PM(B)=(+44,+43). PM(A)=(+162,-39).                    Tok2011a
04007+2023 BD+19  641  Hyades vB 9                                                                     
                       SB with P > 7 yr according to Griffin et al. (1988).                    Grf1988 
04008+1812 BUP  49     A is a spectroscopic binary. B is BD+17@664.                                    
04008+0505 A  1937     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.32 +/- 1.76, 2.84, and 2.00 Msun, respectively.             Mlk2012 
04009+2312 STF 479     H N 93.                                                                         
04009-1027 STF 487     B is BD-10@814.                                                                 
04021-3429 BU 1004     HIP 18824. See Allen et al. (2000) for information on metallicity,      AlC2000 
           LDS3551     age, galactic orbital parameters, etc.                                          
           BU 1004     AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           LDS3551     AD: Holberg et al. (2013): D at 64" is CPM, WD(DA9.9)                   Hbg2013 
04022+2808 STF 481     AD: Declination difference 11.18".                                              
                       AD: Component D is 04039+2808VBS   9.                                           
04024-2832 DAW  79     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.29 +/- 0.72, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04025+0638 HDS 510     Cvetkovic et al. (2016) estimate spectral types K2 and K3, masses 0.81          
                       and 0.79 Msun. Dynamical parallax is 13.24 +/- 0.28 mas.                Cve2016b
04025-6121 LDS 109     Jenkins et al. (2010 A&A 515, 17): RV(A) var with P>6.5yr, M2min=66     CPS2002b
                       Mjup. However, Jones et al. (2002) do not detect RV variation.          Tok2014d
04027+3210 HJ  670     SEI  34.                                                                Nsn2017a
04029+1228 BPM  88     [PM2000]  152895 + [PM2000]  152883.                                    Gvr2010 
04031-1149 GAL 362     Object #113a in Gallo's original list.                                  Gal1912b
04032+2553 DCH  45     HBC 356/357 = V1067 Tau.                                                        
                       Member of Taurus-Auriga molecular cloud.                                Dae2015 
04033+3516 OSO  16     Not a common proper motion pair, based on comparison with POSS2 red             
                       plates. PM of A = +1732 -1356.                                          Oso2004 
04033+1820 BPM  89     [PM2000]  153212 + [PM2000]  153228.                                    Gvr2010 
04036-3611 WHI   5     Listed as possibly resolved by White et al. (1991).                     Whi1991 
04037-1545 A  2913     1989.9413: This system closed steadily from its discovery at 0".45 in           
                       1915 to 0".22 in 1959; this is the first observation in 30 years so it          
                       is unknown whether the pair has passed through periastron.              Hrt1993 
04038+3758 ES 2085     A is V380 Per.                                                                  
04038-4429 LCL 120     AB: B is CD-44@1388.                                                            
                       AB: Additional notes may be found in Herschel (1847).                   HJ_1847a
           SHY 458     AC: HIP  18958 + HIP  18888.                                                    
04039+2808 VBS   9     An Algol-type binary, RW Tau.                                                   
                       This is the D component of 04022+2808.                                          
04040+3932 L    51     Not found in Heintz at IDS position.                                    Hei1987a
04042+2324 OSO  17     Not a common proper motion pair, based on comparison with POSS2 red             
                       plates                                                                  Oso2004 
04043-1231 GAL 363     Object #116 in Gallo's original list.                                   Gal1912b
04044+2406 MCA  13     36 Tau. A is an occultation binary, first detected by Dunham et al.     Dnh1973 
                       Now resolved by speckle interferometry.                                         
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 16.02 +/- 8.21, 11.83, 2.92 Msun, respectively.    Mlk2012 
04044+2025 RED   1     1996.0656: RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al. (1981)                                         Luy1981 
                       Candidate Hyades member; Reid considers definite binary.                Red1997 
04045+1512 BPM  90     [PM2000]  154069 + [PM2000]  154068.                                    Gvr2010 
04046+5504 HO  221     Both A and B are above the MS. AC: reflex PM(A), likely optical.        Tok2014d
04047+2205 STT 558     AB: 37 Tau.                                                                     
04047-0303 LDS3555     NLTT 12486/12488                                                        Chm2004 
04049-3527 CHR 224     AC. Surprisingly, no record of this wide companion to the 0".8 pair             
                       I 152 is listed in the WDS, despite 17 observations spanning 90+ years          
                       since Innes' discovery in 1896.  Misidentification appears ruled out,   I__1897b
                       since both the Innes pair and the new component are seen on two                 
                       separate occasions.                                                     Hrt1996b
04050+3705 KU   83     AB: HJL  55.                                                            HJL1986 
04050-0600 BFR   4     BD-06 813 + 2MASS J04050209-0600409. Baron et al. (2015) estimate               
                       spectral types K0 and M6.5 +/- 1, distances 68 +/-10 and 86 +2/-37 pc,          
                       masses 0.925-1.014 and 0.096-0.114 Msun.                                BFr2015 
04053+2201 CHR 158     Aa,Ab: 39 Tau. Variable?                                                        
                       Aa,Ab: Observed 7 times 1985-1998, then resolved at 0.22" in 1988       McA1993 
                       (note: "uncertain"), unresolved in 2002 (3.6m AO), and finally          Rbr2005 
                       resolved at 0".41 in late 2003                                          Hrt2009 
04056+1255 BPM  91     [PM2000]  154891 + [PM2000]  154924.                                    Gvr2010 
04057+2248 COU 151     Metchev & Hillenbrand say the AB pair is probably physical, based on            
                       proximity.                                                              Met2004b
04058+7117 LDS1589     NLTT 12426/12424                                                        Chm2004 
04059+3438 ES  238     A measure in 1946 gives distance as 7.2".                                       
04063+3548 BRT3241     ALI 57.                                                                         
04063+1952 BAG   4     A preliminary circular orbit is determined                              Bag2001 
04064+4325 A  1710     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.72 +/- 0.73, 2.49, and 0.95 Msun, respectively.             Mlk2012 
04065+1422 S   443     B is BD+13@643.                                                                 
04066+2018 BNV   2     V1300 Tau. DAE 17. Member of Taurus-Auriga molecular cloud.             Dae2015 
                       Primary is F8-G1, mass = 1.14 +/- 0.05 Msun, age = 25 +25/-10 Myr,              
                       Teff = 5970-6100K. Secondary is M8-L1, mass = 32 +18/-14 Mjup,                  
                       Teff = 2537 +95/-182K.                                                  Bnv2014 
04066-6019 R    40     B is CPD-60@292. Spectral type of B may be G8.                                  
04067+1309 BPM  92     [PM2000]  155660 + [PM2000]  155680.                                    Gvr2010 
04067+0324 HJ 2221     A component: V = 11.8; B-V = +0.9; Spectral type: K-M.                          
                       B component: V = 13.5; B-V = +0.8; Spectral type: M                     FMR2000a
04068+5035 HU  547     Variable of unknown type.                                                       
04069+3327 STT  71     A is an Algol-type eclipsing binary, AG Per, P = 2.03d.                         
04070-1000 SHY 165     AB: HIP  19206 + HIP  21489.                                                    
           HDS 521     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.68 +/- 0.48, 2.13, and 1.96 Msun, respectively.  Mlk2012 
04070-2200 HU 1363     1994.8069: Quadrant determined by speckle imaging analysis.             Hor1996 
04072+2731 TOK 241     Makarov & Kaplan (2005) note as astrometric companion to A, but there   Mkr2005 
                       is RV data for A to support this astrometric sub-system.                Tok2014d
04075-5234 TOK  15     Astrometric binary in Hipparcos catalog. Estimated period of visual             
                       pair 6y. Primary is 2.5d SB1. G-solution in HIPPARCOS.                  Tok2006 
                       Triple system, consisting of 2.5d SB and 0".1 tertiary companion                
                       discovered by Tokovinin (2006) and previously revealed by Hipparcos     Tok2006 
                       acceleration and RV trend. It is not resolved here; apparently it               
                       closed in.                                                              Tok2013b
04076+3804 STT 531     A: V491 Per. CPM with BD+37@882 (50 Per), 12' distant.                  Cou1955c
                       Premature orbits have been calculated. Motion retrograde.                       
                       G039-001. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
           ALC   1     AE: Also known as BU  545CA.                                                    
                       AE: SHY  19. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       E: 50 Per = V582 Per.                                                           
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04077+1510 STF 495     A is a Delta Scuti-type variable. A = Hyades vB 11, B = Hyades vB 12.           
                       AB pair, with rho = 3".8 is outside our detection window.               Msn1993a
04077+1413 LDS5187     old LDS6164.                                                                    
04078+6220 ES 2603     SZ Cam                                                                          
           STF 485     The classification is from Chocol (1980 Bull. Astron. Inst. Czech. 31,          
           CHR 209     321).  The discovery of speckle companion CHR 209 Ea,Eb with a period           
           WSI  20     of some 60 y confirms the third body model advocated by  Mayer et al.           
           HZG   2     (1994 A&A 288, L13) based on the appearance of the spectrum and                 
           HLM   3     variations in the time of light curve minimum (they suggest a third             
                       body period of 50.7 y).  Another light curve solution is given by               
                       Harries et al. (1998 MNRAS 295, 386).  The B component was also                 
                       observed and appeared to be single. Classification of the B component           
                       is from the WDS.                                                        Msn1998a
                       This complex multiple system has had numerous identification errors             
                       due to various difficulties. The diagram of Lewis in his catalog of     L__1906b
                       the Struve pairs, which seemed a good first step, was hampered by the           
                       quadrant error of the pair he designated Ca. This quadrant error was            
                       repeated in the ADS, IDS, and in earlier editions of the WDS. In the            
                       ADS (where this pair is listed as #2984, but note that #2989 is part            
                       of this system, too) the errors multiplied. The pair Holmes AF (WDS             
                       designation HLM   3AF) is apparently the same as STF 485Ac. Inspection          
                       of scanned images of this region of the sky have allowed the                    
                       Hertzsprung pairs (HZG   2) whose components are given within                   
                       quotation marks in the ADS to be identified. Of the HZG pairs, the              
                       "CD" pairing is the same as STF 484AC and the "CE" pairing is the               
                       same as STF 484AB. The ADS note to the "AJ" pairing of HZG   2 is a             
                       typographical error. The correct position angle is 77 degrees, which            
                       corresponds to the AD (now AO) pair. Below outlines the changes from            
                       the WDS 2001.0 to the current version.                                          
                                                                                                       
                       ES 2603Aa ---> ES 2603AB                                                        
                       STF 485Ab ---> STF 485AC                                                        
                       STF 485Ac ---> STF 485AD                                                        
                       STF 485AB ---> STF 485AE                                                        
                       STF 485BE ---> STF 485EF                                                        
                       STF 485   ---> STF 485EG (formerly STF 485B to STF 484A)                        
                       STF 484AB ---> STF 484GH                                                        
                       STF 484AC ---> STF 484GI                                                        
                       STF 485Bb ---> STF 485EC                                                        
                       HLM   3AF ---> STF 485AD                                                        
                       STF 485AD ---> STF 485AO                                                        
                       STF 485   ---> STF 485AL (formerly STF 485A to HLM   3A)                        
                       HLM   3AB ---> HLM   3LM                                                        
                       HZG   2AC ---> STF 484AI                                                        
                       HZG   2AD ---> STF 484AG                                                        
                       HZG   2AE ---> STF 484AH                                                        
                       HZG   2AG ---> HZG   2AN                                                        
                       HZG   2BC ---> STF 484EI                                                        
                       HZG   2BE ---> STF 484EH                                                        
                       HZG   2CD ---> STF 484GI                                                        
                       HZG   2CE ---> STF 484HI                                                        
                       HZG   2JK ---> HZG   2OP                                                        
                       HZG   2   ---> HZG   2JK                                                        
                       SLV   3   ---> STF 485AF                                                        
                       CHR 209Ba ---> CHR 209Ea,Eb                                                     
           CHR 209     Ea,Eb: The primary of this pair is the Beta Lyrae-type O9/B0 eclipsing          
                       system SZ Cam, with a period of 2.698d. The Gorda et al. (2007) orbit   Grd2007a
                       is based on changes in the period of SZ Cam to determine P, omega, e,   Grd2007b
                       and T, and speckle measures to derive i, Omega, and a. They derive a            
                       distance of 1125 +/- 135 pc, which exceeds by 30% the 800pc distance            
                       to the open cluster NGC 1502; they conclude that SZ Cam is not a                
                       member of the cluster. The mass of the eclipsing pair (Ea) is 28.5              
                       +/- 0.5 Msun, that of the third body (Eb) 23.4 +/- 2.4 Msun.                    
                       Eb is also a close binary.                                                      
           STF 484     GH: STI 492.                                                                    
04079+1750 DAE  18     V1302 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04080+4311 AG  308     B is BD+42@897.                                                                 
04080+0119 HJ 2223     BAL 1262.                                                                       
04082+1957 DAE  19     V1196 Tau.                                                              Dae2015 
04083+1327 BPM  93     [PM2000]  156773 + [PM2000]  156823.                                    Gvr2010 
04087+2553 OCC 777     Griffin (2013) notes that the magnitude and parallax of this pair               
                       suggest a star of luminosity class III, rather than the published               
                       spectral type of G8II. He derived a spectroscopic orbit of P=2224.4             
                       +/- 2.3 days, e=0.477 +/- 0.009.                                        Grf2013g
04088+1126 LDS5188     LDS5508.                                                                        
04089+2911 BU 1232     Only elements P, T, and a in the Starikova (1980) orbit have been       Sta1980b
                       amended from the orbit of Muller (1978).                                Mlr1978a
                       Griffin et al. (1988) find this to be a SB but doubt its                Grf1988 
                       membership in the Hyades in spite of its inclusion by                   Sym1965 
                       Wayman et al. (1965).                                                   Msn1993a
                       Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       However, this is a Hyades non-member                                    Grf1988 
                                                                                               Grf2013c
04089+2306 STF 494     H N  17.                                                                MEv2010 
04090-5153 HJ 3625     B is CPD-52@499.                                                                
04091+2901 KOH   3     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04091+2839 HO  326     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 9.61 +/- 4.45, 2.43, and 1.10 Msun, respectively.             Mlk2012 
04091-1624 SKF 950     GWP 556.                                                                Tob2012b
04092+2105 ALP  11     2MASSI J0409095+210439                                                          
                       Physical companionship of B component to this ultracool dwarf ruled             
                       out based on I-J color, using I-band photometry taken at WIYN in                
                       August 2002. C component seen as elongated; its physical companionship          
                       also ruled out.                                                         AlP2007 
04093+1835 LDS1154     NLTT 12637/12636                                                        Chm2004 
04093-0756 A   469     Only elements P and T in the Starikova (1984) orbit have been amended   Sta1984 
                       from the orbit of Baize (1981).                                         Baz1981b
                       Typographical error in semimajor axis for Brendley & Mason (2007)       USN2007b
                       orbit corrected from 2".435 to 0".2986.                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 8.49 +/- 6.33, 3.80, and 2.09 Msun, respectively.             Mlk2012 
04094+2328 POU 412     LDS5509.                                                                        
04094+0546 LAW  12     LSPM J0409+0546 = NLTT 12648. Law et al (2008) derive a distance of     Law2008 
                       19.9 +9.1/-3.8 pc and a projected separation of 4.9 +2.7/-0.7 au.               
                       Estimated spectral types are M4.5 and 04094-0125 BAL 290     J  3334.                                                                Nsn2016 
04095-0742 BRT 533     Not found by Heintz at IDS position.                                    Hei1990b
04095-1729 ENG  17     B is BD-17@806.                                                                 
04096+3139 HO  327     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       SEI  36.                                                                Nsn2017a
04096-6023 R    41     B is CPD-60@297.                                                                
04096-8151 RST2345     A semi-regular variable, U Men. Hipparcos suspected non-single.                 
04097+1154 BPM  94     [PM2000]  157774 + [PM2000]  157781.                                    Gvr2010 
04097+0006 GRV 207     HJL  56.                                                                HJL1986 
04099+2446 ITO  16     V1306 Tau. Young member of Taurus-Auriga molecular cloud.               Dae2015 
04100+8042 STF 460     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 7.24 +/- 2.42, 5.27, and 4.54 Msun, respectively.             Mlk2012 
04100+0944 LDS1155     LIT  10.                                                                        
04102-0217 FIL  10     BAL  27.                                                                        
04105+5751 HDS 529     Pair originally X coded due to lack of resolution, however, elsewhere   Msn1999b
                       it is noted as a "very close double" so uncertain. Ambiguity from old   MCK1956 
                       reference recently found.                                               Dam2015 
04107+3808 WNT   2     IRAS 04073+3800 = Parsamian 13. Weintraub (1992) suggests that both     Wnt1992 
                       the northern and southern components are double, with separations of            
                       about 5" and 8", respectively.                                                  
04107-0452 A  2801     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.83 +/- 0.33, 2.34, and 1.05 Msun, respectively.             Mlk2012 
                       Docobo et al. (2017) derive an orbital parallax of 16.18 +/- 0.23 mas           
                       and component masses 1.203 +/- 0.059 and 1.114 +/- 0.054 Msun. Age of           
                       of the system is estimated at 5 Gyr.                                    Doc2017d
04108-1252 PHB   1     LP 714-37                                                                       
                       Phan-Bao et al. (2005) derive distance 18.1 +/- 2.2 pc, spectral types  PhB2005 
                       M5.5 and M7.5, masses 0.11 +/- 0.01 and 0.09 +/- 0.005 Msun.                    
                       Phan-Bao et al. (2006) derive spectral types, absolute K-band mags,     PhB2006 
                       masses of components as follows:                                                
                       A   M5.5 +/- 0.5    9.11 +/- 0.25   0.11 +/- 0.01 Msun                          
                       B   M8.0 +/- 0.5   10.05 +/- 0.30   0.09 +/- 0.01 Msun                          
                       C   M8.5 +/- 0.5   10.35 +/- 0.30   0.08 +/- 0.01 Msun                          
04111-1826 UPT   1     No change in angle; distance decreased 2" in 70 years.                  B__1951a
04112+2630 STF 502     LDS5514 (both AB and BC).                                                       
04112+1538 CHR 202     First detected as an occultation binary by Radick & Lien.               Rad1982a
04113+0531 ENG  18     45 Tau.  Hyades vB 14.  CPM companion with rho = 124".1 is outside              
                       detection window. An additional component was noted as spectroscopic    Grf1988 
                       by Griffin et al. (1988).                                               Msn1993a
04119+2338 CHR  14     Observed under poor seeing conditions. Griffin & Gunn (1981) found a    Grf1981d
                       2.4-day SB.                                                             Msn1993a
04120-0916 A   471     Motion increasing, but only three measures since 1933.                          
04123+6908 HJ 1141     A 13.3 magnitude star is 20" preceding.                                         
04125+3538 HJ  341     ALI 59. BU gives 1880 position +35 25.                                          
04125-3609 HJ 3628     B is CD-36@1632.                                                                
04128+1937 KOH   4     V1307 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04130+5237 PRV   1     GJ 164. Discovered by Palomar 5m/STEPS astrometry and confirmed                 
                       using HST/NICMOS, the combined solution by Pravdo et al. (2004)                 
                       yielded an absolute parallax of 0".0820 +/- 0".008, spectral types of           
                       M4.5V and M6-8V and masses 0.170 +/- 0.015 and 0.095 +/- 0.015 Msun.            
                       Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                      Prv2004 
                       Combined AO+STEPS analysis of this M dwarf binary yields a total mass           
                       0.343 +/- 0.026 Msun, individual masses 0.257 +/- 0.020 and 0.086 +/-           
                       0.007 Msun. Metallicity is at least solar.                              Mtc2008 
                       Inclination = 57 +13/-17, omega = 133 +45/-20 deg.                              
                       GJ 164 = LHS 1642. A known close binary system with a well-determined           
                       orbit (Pravdo et al. 2004; Martinache et al. 2009). Its separation is   Prv2004 
                       smaller than 100 mas at all times, and it therefore remains unresolved  Mtc2009 
                       by AstraLux. We do detect one other point source in the field of view,          
                       but it is a suspected background contaminant based on its blue color,           
                       with dz'= 5.8 +/- 0.1 mag and di' = 5.3 +/- 0.1 mag.                    Jnn2014 
04132+5032 CHR  15     Ross 29.  Van Maanen (1941) suspected this star to be a binary, but     Maa1941 
                       these are the first measurements of a companion.                        McA1987b
04132+2258 HU  302     A premature orbit has been computed.                                            
04135+2816 KSA 102     Primary is variable star V1096 Tau.                                             
04135+1813 BPM  95     [PM2000]  160209 + [PM2000]  160214.                                    Gvr2010 
04135-2554 LDS3564     NLTT 12805/12807                                                        Chm2004 
04136+0743 A  1938     46 Tau. Hipparcos astrometric solution adopted some elements from the   HIP1997d
                       orbit of Heintz.                                                        Hei1984b
                       Combined spectroscopic/astrometric solution of SB1. Calculated masses           
                       1.38 +/- 0.26 and 0.82 +/- 0.21 Msun.                                   Mut2010b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.17 +/- 0.14, 2.77, and 2.55 Msun, respectively.             Mlk2012 
04139+0916 BU  547     47 Tau.                                                                         
                       Spectral types of primary and secondary assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
04140+8216 LUH   7     LHS 1643 + WISE J041328.73+821854.7. Companion is likely not physical,          
                       based on proper motion.                                                 Luh2012b
04140-1222 GAL 364     Object #120 in Gallo's original list.                                   Gal1914 
04142+2813 GHE   1     Aa,Ab: V773 Tau.  Orbital elements and dynamical mass determinations            
                       were published by Tamazian et al. (2002).                               Tam2002 
                       Aa,Ab: The combined solution by Boden et al. (2012) yields a mass and   Bod2012 
                       luminosity for the Ab component of 2.35 +/- 0.67 Msun and 2.6 +/- 0.6           
                       Lsun. This mass is higher than expected, and suggests the Aa,Ab pair            
                       may instead be a multiple system.                                               
                       Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04142-4608 RST2338     Half-period solution equally good, but gives large mass-sum.                    
                       More speckle obs needed (the only existing one erroneous?).                     
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.72 +/- 0.26, 2.26, and 1.07 Msun, respectively.             Mlk2012 
                       Gomez et al. (2016) derive dynamical parallax and component masses:             
                       20.75 +/- 0.42 mas, 1.245 +/- 0.012 Msun, 0.954 +/- 0.009 Msun.         Doc2016i
04143-2742 SWR   7     CPM pair                                                                Skf2004 
04144+1523 BPM  96     [PM2000]  160726 + [PM2000]  160650.                                    Gvr2010 
04144-1015 STF 516     39 Eri.                                                                         
                       AB: H N  24.                                                            MEv2010 
04144-6228 HJ 3638     alp Ret. Possible spectroscopic binary.                                         
04145+2851 GRV 208     2MASS J04143060+2851298 and J04143109+2851518, both from the Riaz et            
                       al (2006) sample, are separated by only 23" and although the estimated  Ria2006 
                       spectroscopic distances of 55 and 72 pc are not fully equal, they are           
                       consistent to within the 37% error. In addition, they have very                 
                       similar proper motions (e.g. Roser et al. 2010) and thus probably form  Rsr2010 
                       a physical pair.                                                        Jnn2012 
04148+2813 GHE   2     FO Tau.  Orbital elements and dynamical mass determinations were                
                       published by Tamazian et al. (2002).                                    Tam2002 
04148+2753 GHE   3     HBC 368 = V1098 Tau = LkCa 3. Torres et al. (2013) find that both               
                       components of this 0".5 pre-MS pair are spectroscopic binaries, with            
                       periods for Aa,Ab and Ba,Bb of 12.942 and 4.068d, respectively.         Trr2013 
04148+2648 DAE  21     CX Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148+2646 DAE  20     FP Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04148-6212 HJ 3641     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
04149+5824 LDS9165     Old LDS6165.                                                                    
04149+4825 STT  73     mu Per = 51 Per. A is a Beta Lyrae-type system.                                 
                       The elements P, T, and e of Alden (1925) were adopted from the          Ald1925 
                       spectroscopic orbit of Cannon (Pub. DAO Ottawa 2, 365, 1915).                   
           H 6  20     H VI 20. SHJ 364.                                                               
04152+5052 AG  309     B is BD+50@944.                                                                 
04153+2044 KOH   6     Metchev & Hillenbrand say the pair is probably physical, based on               
                       proximity.                                                              Met2004b
                       V1199 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04153-0739 STF 518     A: omi 2 Eri = 40 Eri = Keid                                                    
                       LDS 114 = STFB 1. Proper motion of A -2224 -3423.                               
                       C is a flare star, DY Eri, and a strong X-ray source.                           
                       AE: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       BC: NLTT 12868/12869                                                    Chm2004 
                       BC at 83" is physical, and is a Delta Scuti star showing coronal X-ray          
                       emission.                                                                       
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       HIP 19849. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       BC: Additional notes may be found in Worley (1956).                     Wor1956b
04155+0611 STTA 45     AB: H VI 98. A is V774 Tau. B is BD+05@613, and a suspected variable.           
                       AB: SHY  21. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       AB: H 6  98.                                                            MEv2010 
                       Toyota et al. (2009) monitored the RV of both the A and B components            
                       every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion           
                       echelle (precision ~10 m/s). Standard deviations of the RVs of both             
                       components are <40 m/s and velocities show no periodic variation.               
                       These results rejects the association of a planet of mass > 1.8 Mjup            
                       with either star.                                                       Toy2009 
04157+2049 TOK 659     Hyades, vB162.  primary is SB2, P=55.130d                               Tok2014d
                       The 55.1-day SB of Griffin & Gunn (1981) is outside our detection       Grf1981d
                       window.                                                                 Msn1993a
           RED   2     1996.1230: RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al. (1981).                                        Luy1981 
                       Candidate Hyades member; Reid considers definite binary.                Red1997 
04158+4524 STF 512     HJL  58.                                                                HJL1986 
04158+3100 KOH   7     V952 Per. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04158+1524 BUP  51     A: 48 Tau = V1099 Tau                                                           
04159+3142 STT  77     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.90 +/- 3.64, 2.97, and 1.10 Msun, respectively.  Mlk2012 
           STTA 43     AB,C: HJL  59.                                                          HJL1986 
04162+1648 RED   3     1995.8821: RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al. (1981).                                        Luy1981 
                       Candidate Hyades member; Reid considers possible binary.                Red1997 
04163+0710 WSI 97      This is a single-lined nearby binary. Using the radial velocities               
                       measured by D. Latham (2012, private communication), we computed a              
                       combined orbit (the previous visual orbit reported by Riddle et al.     RAO2015 
                       (2015) had a wrong period). The inclination is close to 180deg and had          
                       to be fixed in order to match the RV amplitude.                         Tok2015c
04163-6057 GLE   1     Variable: TT Ret. A premature orbit has been computed.                          
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
04164+0710 WSI  97     Provisionally designated WSI9102.                                       Tok2010 
04165+0041 J  1458     BAL 971.                                                                        
04165-5918 JSP  56     eps Ret                                                                         
                       The companion is a possible white dwarf.                                Cvn2006 
                       Companion confirmed as DA white dwarf.                                  Cvn2007 
                       Optical spectroscopy suggests the companion is a mid- to late-B                 
                       (B3-B9) dwarf.                                                          Mug2007b
04166+2447 LDS1158     NLTT 12896/12897                                                        Chm2004 
04170+1941 HO  328     Only elements P and T in the Starikova (1980) orbit were amended from   Sta1980b
                       the orbit of Heintz (1978).                                             Hei1978a
                       Additional notes may be found in Van Biesbroeck (1954) and              VBs1954 
                       Couteau (1963).                                                         Cou1963a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 6.92 +/- 2.37, 2.74, and 1.20 Msun, respectively.             Mlk2012 
04171+6408 STF 503     BD is +63  489a.                                                                
04171+0409 BAL2119     J 1814.                                                                         
04173+4613 STTA 44     B is BD+45@904.                                                                 
04173+2035 LDS5535     HJL1032.                                                                HJL1986 
04176+2833 SAR   2     HBC 371 = LkCa 5.                                                               
04176+1658 LDS3568     This cannot be the close 3079-d or 5.609-d spectroscopic binaries of    Grf2012b
                       Griffin. The 3079-d pair has an estimated separation of 0.06", but              
                       delta-mag may be considerable.                                                  
04176+1657 HD  27130   Hyades vB 22.  The 5.6-day SB of Griffin et al. (1985) is outside our   Grf1985b
                       detection window.                                                       Msn1993a
04177-6315 RMK   3     the Ret                                                                         
04179+5847 STF 511     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.60 +/- 1.54, 3.37, and 2.09 Msun, respectively.             Mlk2012 
04179-3348 I   270     ups 4 Eri = 41 Eri. Duplicity of AB doubtful.                                   
                       A is a spectroscopic binary, and possible variable.                             
           HMM   2     Aa1,Aa2: close SB resolved by VLTI. A combined spectroscopic/                   
                       interferometric orbit by Hummel et al. (2017) yields component masses           
                       3.17 +/- 0.07 and 3.07 +/- 0.07 Msun, luminosities 100.6 +/- 4.3 and            
                       87.4 +/- 3.3 Lsun, and an orbital parallax of 18.05 +/- 0.17 mas.       Hmm2017 
04180+1815 HD  27149   Hyades vB 23. The 75.6-day SB of Batten & Wallerstein (1973) is         Bte1973 
                       outside our detection window.                                           Msn1993a
04180-0031 SKF 848     Pair originally published as BVD 45, but with incorrect sign given to   Bvd2010b
                       declination. Pair later "rediscovered" and published with correct               
                       declination; this latter discoverer designation has been maintained.            
04181+0446 TOB9003     Measured as BAZ   3 = STF1063 but with an error of -3h in RA!           Tob2010 
                                                                                               Dam2012 
04181-1448 LDS9166     Old LDS6166.                                                                    
                       NLTT 12975/12973                                                        Chm2004 
04182+5018 b Per       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hill et al. (1976).                                                     HlG1976 
04182+2248 STF 520     Measured separation too large, estimated at probably 0.30".             Cou1955c
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 14.33 +/- 9.16, 3.42, and 1.20 Msun, respectively.            Mlk2012 
04183-3000 LDS3571     NLTT 12992/12990                                                        Chm2004 
04184+2135 MCA  14     51 Tau. Hyad (vB 24). B is BD+21@619. A is a long-period spectroscopic          
                       binary, resolved by speckle interferometry. Analysis of the                     
                       spectroscopic/interferometric orbit is given by McAlister (1977).       McA1977 
                       1978.1490:  Theta was incorrectly given as 325.5 degrees                McA1980b
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       A new orbit with a period of 11.3 years was determined by Dombrowski    Dmb1991 
                       (1991).                                                                 Msn1993a
                       Torres et al. (1997) derive a combined spectroscopic/astrometric        Trr1997a
                       solution, yielding an orbital parallax 0.01792 /- 0.00058 and masses            
                       1.80 +/= 0.13 and 1.46 +/- 0.18 Msun.                                           
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Deutsch & Lowen (1971).                                                 Deu1971 
                       Aa,Ab: Martin et al. (1998) derive component masses 1.756 +/- 0.343             
                       and 0.953 +/- 0.247 Msun.                                               Mig1998 
                       Pourbaix (2000) gives a combined solution for this resolved SB2,        Pbx2000b
                       yielding orbital parallaxes and component masses.                               
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 2.96 +/- 0.47, 2.99, and 1.45 Msun, respectively.  Mlk2012 
04184-2347 RST2344     BRT2832.                                                                Brt1947 
04185+2817 HAT   4     AB: Additional notes may be found in Herbig (1962).                     Her1962 
04186+1606 BPM  97     [PM2000]  163490 + [PM2000]  163456.                                    Gvr2010 
04187+2819 SKN   1     Measure of 1990.725 made by the VLA at radio wavelengths.               Skn1993 
04187-5252 SHY 462     AB: HIP  20109 + HIP  20074.                                                    
04188+2820 KSA 104     Primary is variable star V1023 Tau.                                             
04189+0146 STTA 49     B is BD+01@734.                                                                 
04190-0725 STF 527     H 2  80.                                                                MEv2010 
04192+6135 STF 513     Same as STF 507.                                                                
04192+1100 BPM  98     [PM2000]  163846 + [PM2000]  163809.                                    Gvr2010 
04193-4416 HJ 3643     B is CD-44@1505.                                                                
04195+3800 HDS 552     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.74 +/- 0.86, 2.77, and 1.45 Msun, respectively.             Mlk2012 
04195+2808 DAE  23     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04196+3355 HJ  674     The discovery observation of 220 deg may be in error. The AC2000                
                       catalog include one measurement for 1924.381: 22.3 deg and 16.1".               
                       Proper motion of B is mu(AR) = +0.004+-0.007, mu(DEC) = -0.022+-0.002   FMR2000b
04196-2847 SHY 463     HIP  20184 + HIP  19926.                                                        
04197+1416 GIC  45     G008-027/G008-026 = Melotte 25 VA 174 + 170.                                    
04198+1538 BLM   1     gam Tau = 54 Tau. SB resolved by speckle interferometry.                        
                       This object was misidentified as HR 1349 by McAlister (1978).           McA1978c
                       Observed under rather poor seeing conditions. Morgan et al. (1982)      BLM1982 
                       also report a large magnitude difference.                               Msn1993a
04199+3145 J   934     Jonckheere gives the 1950 position: 04 17.0 +31 43.                     J__1958 
                       Couteau corrects the position.                                          Cou1953a
04199+1631 STT  79     Hyad (vB 29). SB according to Griffin et al. (1988).                    Grf1988 
                       1978.6183: The date of this observation was given incorrectly as                
                       1977.6183 by McAlister & Fekel (1980).                                  McA1980b
                       Observed under poor seeing conditions.                                  Msn1993a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.57 +/- 1.41, 2.25, and 1.07 Msun, respectively.             Mlk2012 
04200+1402 BUP  53     57 Tau. A is a Delta Scuti-type variable, V483 Tau.                             
04201+1953 LDS1164     LDS9167 (old LDS6167).  NLTT 13024 = LP 414-169                         Chm2004 
                       NLTT 13024/13026                                                        Chm2004 
04202+3336 FAR   4     Primary is white dwarf WD 0416+334 = GD 60. Aka SKF 316.                Far2005b
04203+3150 HJ 5460     SEI  40.                                                                Nsn2017a
04203+1833 LDS5540     Companion at 264" agrees with Luyten's astrometry, but star at 307" is  Luy1984 
                       in much better magnitude and proper motion agreement. This pair added           
                       as AC pair, until proper identification can be determined.                      
04204+3434 BU 1382     54 Per.                                                                         
04204+2721 SHJ  40     phi Tau = 52 Tau. STTA 48 = H 5  13. B is BD+26@712.                            
04205-0119 RST4769     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.54 +/- 0.98, 3.17, and 2.00 Msun, respectively.             Mlk2012 
04206+2429 COU 704     Probably the A component of POU 442.                                            
04207+1514 JNN 261     LP 475-7. Estimated age 1000-10000 Myr; masses 0.45 +/- 0.04 and 0.21           
                       +/- 0.03 Msun; a ~7.4 au.                                               Jnn2014 
04208+3009 KOH   8     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04209+1352 BAS   3     Hyad - Melotte 25 VA 201 = vB 34.                                               
                       The combined spectroscopic/interferometric solution by Konacki et al.   Knc2004 
                       (2004) uses data from the Palomar Testbed Interferometer and assumes            
                       the eccentricity = 0.0 and the K-band brightness ratio = 1.0. Results           
                       include P = 3.0591080 +/- 0.000011 d, T = 44497.185696 +/- 0.0026 MJD,          
                       derived masses 1.38 +/- 0.13 and 1.39 +/- 0.13 Msun, spectral types             
                       F6V, and diameters 0.25 mas.                                                    
                       Aa,Ab is resolved with PTI, orbit (Konacki & Lane 2004). The B          Knc2004 
                       component is a white dwarf (Barstow et al. 2001), DA3.1; mass 0.98      Bas2001 
                       Msun.  Shaya & Olling (2011): co-moving HIP 1996 at 0.75pc, prob.       Shy2011 
                       0.96: another Hyades star?                                              Tok2014d
           HD  27483   Mel 25 VA 201: Malkov et al. (2012) derive dynamical, photometric, and          
                       spectroscopic masses 3.04 +/- 6.10, 2.70, and 3.17 Msun, respectively.  Mlk2012 
04209-1156 GAL 365     Object #125 in Gallo's original list.                                   Gal1914 
04210+5015 S   445     STTA 47. B is BD+49@1161.                                                       
04211+5532 STTA 46     B is BD+55@869.                                                                 
04215+1704 BPM  99     [PM2000]  165579 + [PM2000]  165489.                                    Gvr2010 
04215-2055 LDS9168     Old LDS6168.                                                                    
                       AC: NLTT 13102/13095                                                    Chm2004 
                       AC: SHY 167. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
04215-2544 BU  744     Star A is SB1, P = 4.0 d, tho this may be spurious,                     Wor1983 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.42 +/- 1.00, 2.96, and 1.35 Msun, respectively.  Mlk2012 
04216-1559 LDS9169     Old LDS6169.                                                                    
                       NLTT 13109/13110                                                        Chm2004 
04217+1046 TOK  84     HIP 20366. Small PM(A)=(-31,-12). NOMAD: PM(B)=(+39,-63), V=13.95.      Tok2011a
04218+1949 KNT   2     LDS2228. The variable U Tau.                                                    
04218+1929 SIG   1     LP 415-20 = Bryja 262.  Spectral types M7.0, M9.5. Probable Hyades              
                       member. Estimated orbital period 23 +7/-6 yrs.                          Sig2003 
                       Konopacky et al. (2010) derive a distance of 21. +/- 5. pc and a                
                       system mass of 0.09 +/- 0.06 Msun.                                      Kon2010 
04219+5749 BRG  34     XO-3. Bergfors et al. (2013) estimate spectral types F5V and G0-M2.5V.  Brg2013 
04219+1530 CHX   1     IRAM 04191+1522. Primary is a Class 0 protostar, resolved into 7.8"             
                       pair in 1.3mm continuum observations at Submillimeter Array (SMA).      ChX2012 
                       Chen et al. quote position angle as "SE/NW"; followup check on Aladin           
                       by cataloguer suggests angle approximately 290deg.                              
04220+2826 ISM   1     RY Tau, a T-Tauri star.                                                         
04220+2818 ITO  21     V987 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04220+2658 SMN   9     FS Tau.                                                                         
                       Measure of 1989.5 made by triangulation of multiple measures and was            
                       in a red filter.                                                                
                       Tamazian et al. (2002) solution includes a mass determination based on  Tam2002 
                       an estimated distance.                                                          
                       AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
04220+1932 GHE   6     Components A, Ba, and Bb of this system are also commonly designated            
                       as N, Sa, and Sb, respectively, due to the north-south orientation of           
                       the wider pair.                                                                 
                       AB: Measure of 1982.5 made by the VLA at radio wavelengths.             Scw1984 
                       Measure of 1983.75 made by the VLA at radio wavelengths.                Scw1986 
                       Measures of Johnston et al. and Loinard et al. made by the VLA at       Jnt2003 
                       radio wavelengths.                                                      Loi2003 
                       AB: Rho and theta errors for Ghez et al. (1995), Furlan et al. (2003),  Ghe1995 
                       and Roddier et al. (2000) measures have been added/updated as noted by  Fun2003 
                       Koehler et al. (2008). Koehler et al. derive a preliminary orbit for    Rod2000 
                       the AB pair, yielding a system mass of 5.57 +0.11/-0.29 Msun.           Koh2008b
                       A,Ba: The 2000.886 Duchene et al. (2002) theta value was corrected by   Dch2002 
                       Duchene et al (2006). Also, the Duchene et al. (2006) theta value for   Dch2006 
                       2005.801 was changed by 90deg to correct for the orientation of the             
                       camera (Schaefer, priv. comm. cited by Koehler et al. 2008)             Koh2008b
           KRS   2     Ba,Bb: Tamazian derives a total system mass of 2.82 +/- 0.74 Msun,      Tam2005 
                       consistent with the IRC model of Koresko et al. (1997).                 Krs1997 
                       T Tau Sa-Sb orbit gives range 1991-2001 for T, 0.09-0.87 for e,                 
                       11-60 for i. Values for P and a are lower limits.                       Sfr2006 
                       Duchene et al. (2006) derive masses for the Ba and Bb components of     Dch2006 
                       2.73 +/- 0.31 and 0.61 +/- 0.17 Msun, respectively.                             
                       Ba,Bb: The 2000.886 Duchene et al. (2002) theta value was corrected by  Dch2002 
                       Duchene et al (2006)                                                    Dch2006 
                       The 2002.829 Schaefer et al. (2006) measure is a reanalysis of data     Sfr2006 
                       from Beck et al. (2004).                                                Bck2004 
                       Koehler et al. (2008) derive a system mass of 2.96 +0.15/-0.24 Msun     Koh2008b
                       and individual masses of 2.13 +0.14/-0.20 and 0.83 +0.10/-0.11 Msun             
                       for the Ba and Bb components, respectively.                                     
                       Ba,Bb: The Schaefer et al. (2014) orbit, combined with a VLBA parallax          
                       of 6.90 +/- 0.09 mas (147.6 +/- 0.6pc; Loinard et al. 2007, ApJ 671,            
                       546) yields a total mass for Ba+Bb of 2.70 +/- 0.22 Msun.               Sfr2014 
                       Ba,Bb: Csepany et al. (2015) generated new orbital parameters for T             
                       Tau N-S (KRS   2Ba,Bb), but their grid search yields a wide range of            
                       possible solutions (P 475-27000y, a 0.57-16.8", etc.)                   Cse2015b
04220+1405 HD  27628   Hyades vB 38 = V775 Tau. The 2.14-day SB of Abt (1961) is outside our   AbH1961 
                       detection window.                                                       Msn1993a
           BUP  54     60 Tau. A is a specroscopic binary and variable, V775 Tau.                      
04221+2826 KSA 105     V1071 Tau = LkCa 21. Young member of Taurus-Auriga molecular cloud.     Dae2015 
04221-2849 BWL  15     Pair is a 0".7 equal-flux K7V2 binary. Torres et al. (2006 A&A 460,             
                       695) found strong Halpha emission and lithium absorption. Age is                
                       consistent with that of the Pleiades, so an age range of 50-200 Myr             
                       is adopted for this system.                                             Bwl2015 
04221+1934 KOH   9     Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04224+1118 PAT   5     The 3-year SB of Griffin et al. (1988) is outside our detection         Grf1988 
                       window.                                                                 Msn1993a
                       The double-lined spectroscopic solution of this 1043.5-d pair           Grf2012b
                       determined by Griffin.                                                          
04226+2538 STF 528     chi Tau = 59 Tau                                                                
                       H 4  10.                                                                MEv2010 
                       The secondary is SB2 (F8+G6), with period 17.6 days for Ba,Bb; RV               
                       residuals indicate the presence of a more distant Bc companion. Based           
                       on spectroscopic observations obtained at CfA 1988-2004, Torres (2006)          
                       derived an orbit for Bab,Bc with period 9.447 +/- 0.017 yr. Mass for            
                       the A component is determined to be 2.60 +/- 0.5 Msun. Inclination              
                       angle for the Ba,Bb orbit is 53.5 +/- 0.5deg, yielding masses 1.19 and          
                       1.02 Msun for Ba and Bb. Bc appears to be over-massive; based on                
                       infrared excess this could be well explained as an equal-mass binary            
                       composed of late-type stars of masses ~0.70 Msun (spectral type ~K4).           
                       Total mass of B is 3.6 Msun.  Torres estimates the Bab,Bc semi-major            
                       axis at about 83.6 mas and the magnitude difference dV~3.3mag                   
                       (dK~1.5mag), making the pair potentially resolvable by speckle                  
                       interferometry.                                                         Trr2006b
04227+1503 STT  82     Hyades vB 40A. The primary is SB1, P = 4.00 d (Sanford 1921).           San1921 
                       Primary is SB2, P=4.0002d (Griffin 2012)                                Grf2012b
                       Also a wider companion (LDS 1166 AC, rho = 62", M = 17.8).                      
                       The 255.5-year binary, ADS 3169 = STT 82 AB is outside our detection            
                       window, although part of a peak is seen at the edge of the window at            
                       the expected position angle, according to the orbit in the Worley &             
                       Heintz (1983) orbit catalog. A wider companion (LDS 1166AC, rho = 62",  Wor1983 
                       M = 17.8) and the 4d SB are also outside our detection window.          Msn1993a
                       A component of pair determined to be a 4.0-d spectroscopic binary.      Grf2012b
04228+1647 HD  27685   Hyades vB 39. Spectroscopic binary with P > 7 yr, according to Griffin  Grf1988 
                       et al. (1988).                                                          Msn1993a
04230+1732 CHR 262     del 1 Tau = 61 Tau. The primary is a long-period spectroscopic and              
           BUP  55     occultation binary.                                                             
                       This system, first announced in Mason et al. but considered of          Msn1993a
                       uncertain veracity, has been included. While its status is not                  
                       definitive, subsequent confirmation or suspected duplicity (by another          
                       technique) makes the discovery measurement somewhat more probable.              
                       1991.8995: This is a particularly unexpected result, given the four             
                       previous epochs at which our observations have shown no indications of          
                       duplicity.  All four of the earlier observations were reanalyzed using          
                       the same procedures employed here, but no additional supporting                 
                       evidence of duplicity was found.  If this additional component is               
                       confirmed,  vB 41 will be the second K0 giant binary that has been              
                       resolved in the Hyades (HR 1411 being the other).  The common proper            
                       motion companion at a separation of 195".5 is far outside our window            
                       of observation, and the 530-day spectroscopic component of Griffin &            
                       Gunn (1977) would have an angular separation below the diffraction      Grf1977d
                       limit of the KPNO 4-m telescope.                                        Msn1993a
                       Aa,Ab : If real, this pair could be the 530.1-d spectroscopic binary    Grf2012b
                       of Griffin.                                                                     
04231-0117 BU  402     Aka OL  201.                                                                    
04232+7510 MLR 459     Also known as TDS 138.                                                          
04232-1135 GAL 366     Object #127 in Gallo's original list.                                   Gal1914 
04233+1123 STF 535     A premature orbit has been computed.                                            
                       Ruymaekers & Nys (1995) noted discrepancies in the orbit of Popovic     Ruy1995 
                       (1982), and calculated elements from their Thiele-Innes elements.       Pop1982a
04233-0500 HJ  342     Same as STF 539 and H IV 117.                                                   
                       AB: H 4 117.                                                            MEv2010 
04233-2138 B  2571     CPD-21@545.                                                                     
04234+1940 V988 Tau    Hyades vB 43. Hipparcos astrometric solution adopted some elements      HIP1997d
                       from the orbit of Griffin et al. (1985).                                Grf1985b
                       The 1.6-year SB of Griffin et al. is outside our detection window.      Msn1993a
04234+1647 HD  27749   Hyades vB 45.  The 8.418-day SB of Abt & Levy (1985) is outside our     AbH1985 
                       detection window.                                                       Msn1993a
04235+2059 CHR  16     An occultation binary, now resolved.                                            
04236+4226 STT  80     1977.7420: The date of this observation was given incorrectly as                
                       1978.7420 by McAlister & Fekel (1980).                                  McA1980b
04237+1538 MET   3     Metchev & Hillenbrand say the pair is probably optical, based on                
                       proximity.                                                              Met2004b
04238-0414 BUG   7     SDSS J042348.57-041403.5                                                        
                       Estimated spectral types are L6.5 + T2, effective temperatures 1490             
                       +/- 100 and 1250 +/- 80 K. Masses are estimated at 0.039-0.062 and              
                       0.029-0.051 Msun, and the orbital period (assuming the semi-major axis          
                       = 1.26 * rho) is ~19yr.                                                 Bug2006a
04239+0928 HU  304     66 Tau.                                                                         
                       Spectral types and masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.81 +/- 1.40, 6.11, and 4.43 Msun, respectively.             Mlk2012 
04239-1102 GAL 367     Object #128 in Gallo's original list.                                   Gal1914 
04240+2418 STF 534     62 Tau.                                                                         
                       AB: H 4 109.                                                            MEv2010 
04241+1727 BUP  56     del 2 Tau = 64 Tau. Hyades vB 47. A is spectroscopic binary.                    
04242+1445 HDS 564     1991.8992: Noted as a possible spectroscopic binary by Griffin et al.   Grf1988 
                       (1988), it is uncertain whether the system we detect here is also               
                       producing the radial velocity variation.                                Msn1993a
                       Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       The spectroscopic solution of this ~42000-d pair determined by Griffin, Grf2012b
                       its gamma velocity "removing any remaining doubt about the systems      Grf2013c
                       credentials as a Hyades member."                                                
04244+3419 STF 533     AB: H 4  72.                                                            MEv2010 
                       Primary is V590 Per, a Beta Lyr type eclipsing binary, P = 5.6866d.     Zas2012 
04245+5051 TOK 245     AC: The physical nature of C is not certain: CPM, but the PM is small.  Tok2014d
04245+2244 BU 1235     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.22 +/- 2.00, 2.88, and 1.35 Msun, respectively.             Mlk2012 
04245+1653 PAT   6     Noted as a possible spectroscopic binary by Griffin et al.              Grf1988 
                       (1988).                                                                 Msn1993a
                       Hyades vB 52. Mass of B 0.49 Msun (Metchev & Hillenbrand 2009).         Met2009 
04246+3358 STT  81     AB: 56 Per.                                                                     
04247+0442 HJL1115     Hyades vB 140. The 156.4-day SB of Griffin et al. (1985) is outside     Grf1985b
                       our detection window.                                                   Msn1993a
                       A combined interferometric/spectroscopic solution by Halbwachs et al.           
                       (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
04247-0845 STF 544     Primary is SB1, P=1248d = 3.41y. RV(B)=var?                             Tok2014d
04247+0442 HJL1115     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                       (2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun.      HJL2016 
04248+1552 PAT   7     SB with P > 7 yr according to                                           Grf1988 
                       Griffin et al. (1988).                                                  Msn1993a
                       The spectroscopic solution of this 5688-d pair determined by Griffin.   Grf2012b
04248-5037 RST1273     HIP 20606. Both components A,B are above the MS, young? B is too red in         
                       the (Kabs,V-K) CMD, infrared companion? Planetary companion to A = HD           
                       28254 is detected with RV. No relevant references in SIMBAD.            Tok2011a
                       A is exoplanet host, P=1116d.  Roell et al. (2012 A&A 542, A92) list B          
                       as physical, confirmed by Naef et al. (2010 A&A 532, A15).              Tok2014d
04249-3445 I    59     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
04251+8603 WFC  23     HJL  57.                                                                HJL1986 
04252+2545 TOK 247     Not Hyades member: different PM and RV. (Griffin 2013).                 Grf2013c
04252-6415 HJ 3656     B is CPD-64@333.                                                                
04253-0932 GAL 368     Object #129 in Gallo's original list.                                   Gal1914 
04254+2218 STF 541     A: kap 1 Tau = 65 Tau = K Tau                                                   
                       A,CD: H 6   8.                                                          MEv2010 
                       AB: HJL1034.                                                            HJL1986 
           STF 541     04253+2215STF 541CD and 04254+2218STFA  9AB were found to                       
           STFA  9     be the same wide pair, so designations for these two                            
                       multiple systems were combined, as follows:                                     
                       04253+2215STF 541AB   --> 04254+2218STF 541CD                                   
                       04253+2215STF 541AB,C --> 04254+2218STF 541A,CD                                 
                       04253+2215STF 541AB,D --> 04254+2218STF 541B,CD                                 
                       04254+2218STFA  9AB   --> 04254+2218STF 541AB                                   
                       04254+2218STFA  9Aa   --> 04254+2218STF 541AE                                   
                       04254+2218STFA  9Bb   --> 04254+2218STF 541BF                                   
                       A : kap 1 Tau = 65 Tau = K Tau. Occult. binary, Hyades member (vB 54)           
                       B : kap 2 Tau = 67 Tau. Delta Scuti variable, Hyades cluster member.            
                       CD : J 2722. This faint pair is between kap 1 and kap 2 Tau.                    
                       Pairs STFA  9AB (rho = 339"), STFA  9Aa (rho = 141") and STFA  9Bb              
                       (rho = 107") are all far outside our detection window.                  Msn1993a
04255+1756 KUI  17     del 3 Tau = 68 Tau. A is spectroscopic binary and variable, V776 Tau.           
           H 6 101     H VI 101. There is a wide faint pair noticed by John Herschel, 320@             
                       Class VI.                                                               H__1867 
                       The B, C, D, and E components all fall outside our detection window.    Msn1993a
04256+1556 FIN 342     Aa,Ab: Hyad (vB 57). HR 1391 = 70 Tau.                                          
                       Combined spectroscopic/astrometric solution. Orbital parallax 0.02144   Trr1997b
                       +/- 0.00067, masses 1.363 +/= 0.073 and 1.253 +/- 0.075 Msun.                   
                       Quadrant determinations made at several epochs by McAlister et al.      McA1988 
                       (1988) have shown that this system is best represented by an eccentric          
                       orbit of period 6.3 years, rather than a circular 13-year orbit.                
                       1977.7421  Theta was incorrectly given as 6.0 degrees by McAlister &            
                       Fekel 1980).                                                            McA1980b
                       This resolved spectroscopic binary (with P = 6.28 yr) is discussed by   McA1988 
                       McAlister et al. (1988) and by Dombrowski (1991).                       Dmb1991 
                       The published measure for 1988.6582 (McAlister et al. 1990) is          McA1990 
                       is spurious. The data leading to this measure are actually the same as          
                       those for HR 1331 (= McA 14) for the same epoch. These two stars were           
                       observed in immediate sequence but with different microscope                    
                       objectives, and the final reductions calculated two results from the            
                       same data set, but with different scale factors; the HR 1331 measure            
                       for 1988.6582 is the correct one.  Reanalysis of the correct data for           
                       FIN 342 gives the 25 mas result shown here. Peterson (1992, private             
                       communication) pointed out the inconsistency of our originally                  
                       published measure with respect to our previous orbital analysis of              
                       this Hyades binary (McAlister et al. 1988).                             Hrt1992b
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Aa,Ab : New spectroscopic solution determined by Griffin.               Grf2012b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 2.50 +/- 0.47, 2.48, and 1.13 Msun, respectively.  Mlk2012 
04257+6340 HJL1033     SHY 464. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
04257-0214 BU  403     Linear elements fit nicely at present, but this is a physical pair and          
                       an orbit can be computed at some future date.                                   
04258+1800 COU2682     Spectroscopic binary with P > 15 yr, according to Griffin et al.        Grf1988 
                       (1988).                                                                 Msn1993a
                       The spectroscopic solution of this 15650-d pair determined by Griffin.  Grf2012b
04258+1733 RED   4     1996.1449: RHy ID and coordinates from Reid (1992).                     Red1992 
                       Candidate Hyades member; Reid considers definite binary.                Red1997 
04259+1852 BU 1185     Hyad (vB 58).                                                                   
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       1982.7579: This autocorrelogram was remeasured; the new results are     McA1987b
                       listed here.                                                                    
                       The 27.67-year binary (see Dombrowski 1991) ADS 3210  was observed at   Dmb1991 
                       a time when atmospheric seeing was rated as poor.  Also noted as a SB   Grf1988 
                       in Griffin et al. (1988).                                               Msn1993a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.01 +/- 0.36, 2.00, and 0.98 Msun, respectively.             Mlk2012 
04260+4515 ES  567     B is BD+44@946.                                                                 
                       Measures attributed to BC are all AC. Component designation changed.            
04261-1059 GAL 369     Object #130 in Gallo's original list.                                   Gal1914 
04262+3313 HJ  676     AC: SEI  44.                                                            Nsn2017a
04263+3443 HU  609     Only elements P and T have been amended from the orbit of               Sta1978c
                       Heintz (1967).                                                          Hei1967d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 12.01 +/- 10.65, 3.16, and 1.20 Msun, respectively.           Mlk2012 
04263+2249 BUP  58     ups Tau = 69 Tau. A is an occultation binary.                                   
04263+2128 TOK  16     Hyades vB 62. Primary is 8.55d SB1 (Griffin & Gunn 1978); estimated     Grf1978b
                       period of visual pair 9300y. Unresolved by Patience et al.              Tok2006 
                       The SB  is outside our detection window.                                Msn1993a
04263+1538 HD  28052   Hyades vB 141. A CPM companion with rho = 134".4 is outside our         Msn1993a
                       detection window.  Also, noted as a 14.24-year SB by Abt (1965).        AbH1965 
04263+1537 BUP  59     71 Tau. A is a long-period spectroscopic binary,                                
                       P = 5200d, and occultation pair. V777 Tau.                                      
                       Peirce noted a close companion to A component (1868.13, 70deg) which            
                       he said was "much closer than 80 Tau". His 1868.13 separation                   
                       measure for 80 Tau (= 04301+1538 STF 554) was 0".75.                    Pei1882 
04263+1400 HJ 3256     LDS5558.                                                                        
04264+2249 HD  28024   Hyades vB 60. A CPM companion with rho = 110".2 is outside our                  
                       detection window.                                                       Msn1993a
04264+1651 HD  28068   Hyades vB 63. A spectroscopic binary B with P ~ 7 yr, according to      Grf1985b
                       Griffin et al. (1985).                                                  Msn1993a
04268+1525 LDS2236     LDS5559.                                                                        
04268+1052 PAT   8     1991.8990: This K dwarf is noted as a binary with a period in excess            
                       of 16 years in Griffin et al. (1988), and it is likely that we have     Grf1988 
                       detected the spectroscopic companion.                                   Msn1993a
                       The spectroscopic solution of this 6950-d pair determined by Griffin.   Grf2012b
04268+0843 HJ  678     This is not BD+08  690, according to Heintz.                            Hei1992a
04268-0143 UC 1168     Candidate on Tokovinin list, now reconfirmed as CPM.                    Tok2013c
                       AB is CPM according to Hartkopf et al. (2013).  A is on Keck RV         UC_2013b
                       program, RV trend.                                                      Tok2014d
04269+2607 LEI   2     Measure of 1987.8 made by triangulation of multiple measures and was            
                       in a red filter.                                                                
           SMN  10     Ca,Cb: Called FV Tau-c by Simon, therefore given component designation          
                       of Ca,Cb. Relationship to LEI  02 uncertain.                            Smn1992 
                       Measure of 1987.8 made by triangulation of multiple measures and was            
                       in a red filter.                                                                
                       aka COR   3Ca,Cb                                                                
                       FV Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04270+1907 STF 546     HJL  60.                                                                HJL1986 
                       H 2  54.                                                                MEv2010 
04270-7238 B  2091     Composite spectrum: G8III+(A/F).                                                
04271+2542 THB   1     Preliminary orbital elements give total mass 2.8 +/- 1.5 Msun.          Thb1995b
                       Tamazian et al. (2002) solution includes mass determination based on    Tam2002 
                       estimated distance.                                                             
                       DF Tau orbit by Schaefer et al. (2006) gives range 1974-2022 for T,     Sfr2006 
                       0.05-0.76 for e. Values for P and a are lower limits.                           
                       Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                       mass 1.17 +/- 0.13 Msun. The orbital period of 43.7y closely matches            
                       the 44yr timescale of photometric variations; this is consistent with           
                       a suggestion by Lamzin et al. (2001 A&A 372, 922) that the variability          
                       is caused by the circumstellar accretion rate onto the primary being            
                       modulated by the orbital motion of the companion.                       Sfr2014 
04271+1812 STF 545     AB: H 4  74.                                                            MEv2010 
04275+1113 BU 1186     A is variable.                                                                  
04275-1707 HU  440     Primary is HH Eri, eclipsing binary (Algol), P=8.5d.                    Tok2014d
04275-2427 I   413     Baize (1993) value of omega incorrectly listed as 96.0, same as Omega.  Baz1993b
04276+1927 RED   5     1995.6986: RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al.(1981).                                         Luy1981 
                       Candidate Hyades member; Reid considers definite binary.                Red1997 
04277+2631 GIC  47     LDS1171.  G008-035/G039-014.                                                    
                       NLTT 13302/13303                                                        Chm2004 
04278+1001 STF 549     AB: H 4  75.                                                            MEv2010 
04280+2137 BUP  60     A is a spectroscopic and occultation binary.                                    
04281-1033 GAL 370     Object #131 in Gallo's original list.                                   Gal1914 
04282+5303 RUC   3     AO Cam. Spectral type of resolved companion later than M5V.             Ruc2007 
04282+0600 LDS9170     Old LDS6170.                                                                    
04283-1400 GAL 371     Object #132 in Gallo's original list.                                   Gal1914 
04284+1622 RCH   2     Measure of 1998.921 made by triangulation of multiple measures.         Rch2002 
04284-6543 HJ 3662     B is CPD-65@@345.                                                               
04285+1742 GUE   5     The spectroscopic solution of this 7022-d pair determined by Griffin.   Grf2012b
04285+1458 BPM 100     [PM2000]  170962 + [PM2000]  171001.                                    Gvr2010 
04285+0505 HJ 2233     BAL 2614.                                                                       
04286+1944 HD  28291   Hyades vB 69.  The 41.66-day SB of Griffin et al. (1985) is outside     Grf1985b
                       our detection window.                                                   Msn1993a
04286+1911 BUP  61     eps Tau = 74 Tau = Ain                                                          
04287+2714 KON   2     Estimated masses 0.15 and 0.06 Msun. Primary spectral type M5.25        Kon2007b
04287+2613 HDS 576     Cvetkovic et al. (2014) derive spectral types M0 and  M0, masses 0.46           
                       and 0.46 Msun. Dynamical parallax is 25.86 +/- 0.27 mas.                Cve2014 
04287+1552 STFA 10     AB: the 2 Tau = 78 Tau. Hyades vB 72 = HR 1412.                                 
                       Pair appears in an appendix list, not part of discoverer's regular              
                       numbering sequence. B is BD+15@631.                                             
                       Also variable, probably of  Delta Scuti type.                                   
                       The 140.7-day SB of Ebbighausen (1959 Pub. DAO, 11, 235) is outside             
                       our detection window.                                                   Msn1993a
           MKT  13     Aa,Ab: Data from lunar occultation, spectroscopy, and Mark III                  
                       astrometry are combined by Torres et al. to generate orbital elements.  Trr1997c
                       Distance and component masses and absolute magnitudes are derived from          
                       these elements.                                                                 
                       Period is fixed for the Armstrong et al. (2006) orbit. The resulting    MkT2006 
                       component masses are 2.15 +/- 0.12 Msun and 1.87 +/- 0.11 Msun.                 
                       Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                       astrometric data. Derived component masses are 2.03 +/- 0.87 and                
                       1.78 +/- 0.76 Msun.                                                     Ren2010 
                       Aa,Ab: Combined spectroscopic/astrometric solution, using data from             
                       Mark III interferometer plus high-resolution spectroscopy from ELODIE,          
                       HERMES, and CfA. Torres et al. (2011) determine an orbital parallax of  Lmp2011 
                       20.90 +/- 0.14 mas and component masses 2.86 +/- 0.06 and 2.16 +/-              
                       0.02 Msun. Effective temperatures for both components are 7800 +/-              
                       170K, absolute magnitues are 0.33 +/- 0.03 and 1.44 +/- 0.03 mag.               
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 4.46 +/- 0.29, 3.81, and 2.00 Msun, respectively.  Mlk2012 
           MCA  15     Ba,Bb:The primary of 04286+1558 was found to be the B component of              
                       physical pair 04287+1552; systems were merged.                                  
                       the 1 Tau = 77 Tau. Hyad (vB 71). Physical companion to the 2 Tau.              
                       A spectroscopic, occultation, and interferometric binary.                       
                       First detected as an occultation binary by White.                       Wit1979 
                       1979.698, 1979.857:  possible third component                           Heg1983 
                       This is a long period interferometric companion in addition to the              
                       spectroscopic component suggested by Griffin & Gunn (1977) to have a    Grf1977d
                       period of about 16 years.  An estimate of Delta m = 0.76 was made by    Dmb1991 
                       Dombrowski (1991).                                                      Msn1993a
                       Masses and distance of the 2 Tau are derived from spectroscopic                 
                       elements, adopting astrometric elements from Pan et al. (1992)          MkT1992e
                       Combined spectroscopic/astrometric solution by Torres et al. (1997).    Trr1997c
                       Distance (from relative proper motions and orbital parallax of the 2            
                       Tau) 47.6 +/- 1.9 pc, masses 2.91 +/= 0.88 and 1.31 +/- 0.14 Msun.              
                       Ba,Bb : New spectroscopic solution determined by Griffin.               Grf2012b
                       Ba,Bb: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                       4.14 +/- 0.35 and 2.88 Msun, respectively.                              Mlk2012 
           BPMA  7     BC: [PM2000]  171052 + [PM2000]  171309.                                Gvr2010 
04288+1617 BPMA  8     [PM2000]  171281 + [PM2000]  171421.                                    Gvr2010 
04289+3022 STF 548     AB: B=HIP 20907 is bluer than A, below the MS. A is 1.7mag above. But           
                       they are physical: CPM, parallax, same RV! Primary is SB1, P=460.7d.    Tok2001 
                       A,B have same RV (Tokovinin & Gornya 2001), both rotate fast            Tok2014d
04290+1610 HU 1080     Hyad (VB 75); RV possibly variable, as noted by Wilson (1948).          WOC1948 
                       The spectroscopic solution of this 14697-d pair determined by Griffin.  Grf2012b
                       B is also a close 21.3-d pair.                                                  
04290+1338 SIG   2     LP 475-855. Spectral types M7.5, M9.5. Probable Hyades member.                  
                       Estimated orbital period 86 +20/-19 yrs.                                Sig2003 
04292-1206 LDS3591     NLTT 13376/13372                                                        Chm2004 
04293+1733 HD  28394   Hyades vB 77.  The 238.9-day SB of Griffin et al. (1985) lies outside   Grf1985b
                       our detection window.                                                   Msn1993a
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin et al. (1985).                                                  Grf1985b
04294+2701 KON   3     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M6.0          Kon2007b
04294-3335 HJ 3652     Primary is CT Eri, a Beta Lyr type eclipsing binary, P = 0.63420d.      Zas2012 
04295+2617 SMN  11     Measure of 1990.25 made by triangulation of multiple measures and was           
                       in a red filter.                                                                
                       AB: Additional notes may be found in Simon et al. (1992).               Smn1992 
           WHT   2     AC: Primary is the Orion-type variable FW Tau. Multi-epoch astrometry           
                       by Kraus et al. (2014) confirm the AC pair is co-moving, and estimate           
                       mass of the companion at 10 +/- 4 Mjup for a system age of 1-5 Myr.     KsA2014 
           HER   8     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04295+1752 BGH   2     LDS 2244. Variable, V921 Tau. B is +17@  734.                                   
                       HJL1035.                                                                HJL1986 
04295+0025 BAL 972     RST 5206.                                                                       
04296+0350 BAL2121     J 2725.                                                                         
04297+2633 HAT   6     AB: Additional notes may be found in Herbig (1962).                     Her1962 
                       DI Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
           ITO  13     BC: B component is the Orion-type variable DH Tau = HBC 38. Colors of           
                       both B and C are consistent with T Tauri stars. The B component has a           
                       lower effective temperature than A (2700-2800K, vs 3580K), and is               
                       redder. The stars are probably early and late M stars; mass of the              
                       companion is estimated at 30-50 Mjup.                                   Ito2005 
                       Kraus et al. (2014) estimate mass of the companion at 18 +/- 4 Mjup.    KsA2014 
04298-0949 LDS3592     NLTT 13393/13392                                                        Chm2004 
04299+2607 HER   9     Aka IQ Tau. Additional notes may be found in Herbig (1962).             Her1962 
04300+8320 HR 1304     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Prieur et al. (2006).                                                   Pru2006 
04300-6955 OGL 193     LMC157.7.150   + LMC157.7.333                                           Pli2012 
04301+1814 JOY   2     A RW Aur-type variable, UX Tau.                                         Her1962 
04301+1538 STF 554     80 Tau. Hyad. Star A is SB1, P = 30.5d                                  Hei1981e
                       Spectral types and masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
04302+3516 TTH   1     HBC 40 = LkHA 101. Herbig Ae/Be star imaged at multiple wavelengths             
                       shows evidence of a companion at ~180 mas to the East-Northeast of the          
                       primary. Derived physical parameters for A and B for three possible             
                       distances are:                                                                  
                          160pc: L/Lsun =  1300 and  340   R/Rsun = 1.9 and 1.0                        
                          340pc: L/Lsun =  5900 and 1500   R/Rsun = 4.1 and 2.1                        
                          800pc: L/Lsun = 30000 and 8500   R/Rsun = 9.7 and 5.0                Tth2002 
04302-0303 PRB   2     Primary is WD 0427-03 = NLTT 13402, secondary is LP 655-33. Possible            
                       CPM pair, according to Probst (1983).                                   Prb1983 
04302-6753 TOK  85     HIP 20998. Not observed, but J-K=2.92 for B in the 2MASS PSC, hence             
                       optical.                                                                Tok2011a
04303+1950 PAT  10     Noted as a probable SB in                                               Grf1988 
                       Griffin et al. (1988).                                                  Msn1993a
                       Member of the Hyades (vB 81) and "probable SB" according to Griffin et  Grf1988 
                       al. (1988). This WDS pair PAT 10 was resolved by speckle.               Tok2012a
                       The spectroscopic solution of this 4023-d pair determined by Griffin.   Grf2012b
04306+1612 LDS2246     Hyades vB 82. A is possibly variable. B is BD+15@640.                           
                       The primary was noted as a possible occultation binary by Peterson      Pts1981a
                       et al. (1981).                                                          Msn1993a
                       HJL1036.                                                                HJL1986 
04306+1545 HD  28545   Hyades vB 182.  The 358.4-day SB of Griffin & Gunn (1981) is outside    Grf1981d
                       our detection window.                                                   Msn1993a
04306+1542 BUP  62     81 Tau = LDS2247. Hyades vB 83.  B is BD+15@638.                                
                       AB: HJL1037.                                                            HJL1986 
           ARN  36     The CPM B companion with rho = 161".8 is outside our detection window,          
                       as are C and D.                                                         Msn1993a
                       D component is primary of 04309+1547 TDS2876. Pair does not appear to    .      
                       be physical, so systems not merged.                                             
04306+1344 HD  28556   Hyades vB 84. A CPM companion with rho = 111".9 lies far outside our            
                       detection window with a large Delta m of 5.8.                           Msn1993a
04306+1343 BUP  63     83 Tau.                                                                         
04307+2601 SMN  12     Measure of 1990.77 made by triangulation of multiple measures and was           
                       in a red filter.                                                        Smn1992 
04307-1627 HJ 3653     B is BD-16@879.                                                                 
04308+1609 PAT  11     Hyades. The 0".3 binary PAT 11 was not resolved by speckle. The GCS did         
                       not detect RV variability despite large scatter of 4.8 km s-1 in their          
                       three measures.                                                         Tok2012a
04309+2442 SMN  13     ZZ Tau. Sfr2003 astrometry for 1995.081 and 1996.124 was based on               
                       interpolation of one-dimensional data by Simon.                         Smn1996a
                       The first ZZ Tau orbit by Schaefer et al. (2006) gives range 1994-1999  Sfr2006 
                       for T, 0.35-0.88 for e, 115-134 for i, 111-129 for Omega, 268-336 for           
                       omega.  Values of P and a are lower limits.  The second orbital                 
                       solution includes a lunar occultation measure by Simon et al. (1995).   Smn1995 
                       Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total            
                       mass of 0.83 +/- 0.16 Msun.                                             Sfr2014 
04309+1547 TDS2876     D component of 04306+1542. ARN  36AD does not appear to be physical,            
                       so systems not merged.                                                          
04309-0849 KO    2     CPM pair; A = LP 655-23 (spec early M), B = 2MASS J0430516-084901               
                       (M8.0V). Mean separation (1953-2000) 0.328 +/- 0.004 arcmin. Data               
                       sources: Palomar Sky Survey red (1953.2), UK Schmidt blue (1982.8), UK          
                       Schmidt red (1985.9), 2MASS (1998.7), DENIS I (1998.9), UK Schmidt              
                       near-IR (2000.0). Masses of components estimated at 0.26 +/- 0.04 and           
                       0.086 +/- 0.004 Msun.                                                   Cab2007b
                       A known component of the wide binary Konigstuhl 2AB with a separation           
                       of 20" (Caballero 2007), 2MASS J04305203-0849193 is single closer in,   Cab2007b
                       in the AstraLux images.                                                 Jnn2012 
04310+7724 MLR 461     Also known as TDS 142.                                                          
04310-6911 OGL 194     LMC156.6.7     + LMC156.6.6                                             Pli2012 
04311+0647 STT  84     HJL  61.                                                                HJL1986 
04311-4522 TOK 208     Possibly triple. The new companion at 1".6 should not produce RV                
                       variability by 3.8 km s-1.                                              Tok2012a
04312+5858 STI2051     A is an astrometric binary. B (mag. 12.44, 8", DC) is a white dwarf,            
                       in slow retrograde motion about the mass-center. A very large proper            
                       proper motion brought this pair close to a 13th magnitude star which            
                       was measured as the C component by Pauwels & Lampens.                   Pws1993 
                       Also known as HDS 584.                                                          
04312+0621 LDS9171     Old LDS6171.                                                                    
04313-6959 OGL 195     LMC157.7.2247  + LMC157.7.2249                                          Pli2012 
04314+4001 STF 552     H N  44.                                                                MEv2010 
04314-0934 GAL 372     Object #136 in Gallo's original list.                                   Gal1914 
04314-1339 STF 560     B is BD-13@905.                                                                 
04315+1706 SAR   3     HBC 392 = V1074 Tau. SB2.                                               Sar1998 
                       Member of Taurus-Auriga molecular cloud.                                Dae2015 
04316+1743 HD  28634   This is a 2.31-year spectroscopic binary, according to Griffin et al.   Grf1985b
                       (1985).                                                                 Msn1993a
           vA 627      VVO 394. Hipparcos astrometric solution adopted some elements from the  HIP1997d
                       orbit of Griffin et al. (1985). Hyad.                                   Grf1985b
                       Perturbation orbit by McArthur et al. (2011) is based on HST FGS        AST2011 
                       astrometry, plus radial velocities from Griffin et al. (1985). Derived  Grf1985b
                       masses are 0.83 +/- 0.05 and 0.42 +/- 0.05 Msun.                                
04316-7037 OGL 196     LMC158.1.29    + LMC158.1.122                                           Pli2012 
04317+2330 POU 458     LDS 886 = LDS1173.                                                              
04317+1814 HER  10     AB: Additional notes may be found in Herbig (1962).                     Her1962 
           GHE   9     Aa,Ab: Dodin et al. (2016) generated the following preliminary orbital          
                       elements: P = 155-256y, a = 27.2-37.2au, i <47deg, e = 0.29-0.64.       Dod2016 
                       Carrasco-Gonzalez et al. (2006) found a close companion to the Aa       CGo2006 
                       component at 7mm wavelength (~6deg, 0.09", dm 0.4 +/- 0.3 mag).                 
                       However, subsequent observations by Forgan et al. (2014) and the ALMA   Fgn2014 
                       Partnership (2015) found no evidence of this additional component and   ALM2015 
                       concluded it was a false detection.                                             
04317+1538 WOR  16     The A component is a known Hyad.                                                
           LDS1174     The C component may or may not be a physical companion, possibly                
                       sharing CPM only as a member of the cluster.                                    
04318+2424 CHN   3     Formerly known as LEI  15.                                                      
04319-0851 HJ 2234     B is BD-09@917.                                                                 
04320+5355 STF 550     1 Cam. A spectroscopic binary.                                                  
                       AB: H N  67.                                                            MEv2010 
04320+1822 CHN   4     Formerly known as LEI  16.                                                      
                       AB: Additional notes may be found in Herbig (1962).                     Her1962 
           HER  11     AD: Additional notes may be found in Herbig (1962).                     Her1962 
04320-6939 OGL 197     LMC157.5.2454  + LMC157.5.2477                                          Pli2012 
04322+3630 AG   80     ALI 293.                                                                        
04322+1820 KSA 107     Primary is variable star V827 Tau.                                              
04322+1757 MSR   1     HBC 397 = V1075 Tau.                                                    Msr2005 
04323+2422 KON   4     Estimated masses 0.07 and 0.06 Msun. Primary spectral type M6.5         Kon2007b
04323-6918 OGL 198     LMC156.7.3411  + LMC156.7.3620                                          Pli2012 
04324+0128 HDO 307     Aka BAL 1273.                                                           Hei1983a
04325+2420 HAT   7     Additional notes may be found in Herbig (1962).                         Her1962 
04325+2044 RED   6     1996.0902  RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al. (1981).                                        Luy1981 
                       Candidate Hyades member; Reid considers possible binary.                Red1997 
04325+1732 LEI   3     Aa,Ab: GG Tau.                                                                  
                       Tamazian (2002) solution includes mass determination based on an        Tam2002 
                       estimated distance.                                                             
                       Aa,Ab: Kohler (2011) derives orbits both coplanar and not coplanar              
                       with the disk; only his "most plausible" orbit is tabulated in the              
                       orbit catalog. Elements are as follows: P = 403 +67/-32 y, a = 0".429,          
                       i = 132.5 +1.0/-2.5 deg, Omega = 131 +13/-8 deg, e = 0.44 +0.02/-0.03,          
                       T = 2463400 +1470/-5420, omega = 19 +9/-10.                             Koh2011 
           CHN   5     AB: formerly known as LEI   3.                                                  
           DIF   1     Ab1,Ab2: Di Folco et al. estimate spectral types for Ab1 and Ab2 of M2V         
                       and M3.5V, respectively. Assuming the close pair is coplanar with the           
                       outer diskof the system, the stars were separated by 5.1au in Dec 2012. DiF2014 
04326+2628 GIC  48     LDS1176 = G008-040/G039-021.                                                    
                       NLTT 13455/13456                                                        Chm2004 
                       HD 283702. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
04326-0313 H 6  64     H VI 64. Probably a variable of Delta Scuti type,                               
                       DZ Eri. B is BD-03@810.                                                         
04327+2553 GHE  11     Aa,Ab: Measure of 1990.77 made by triangulation of multiple measures            
                       and was in a red filter.                                                Smn1992 
           JOY   3     AB: A RW Aur-type variable, UZ Tau.                                             
                       Measure of 1990.77 made by triangulation of multiple measures and was           
                       in a red filter.                                                        Smn1992 
                       AB: Additional notes may be found in Herbig (1962).                     Her1962 
04327+1855 DAE  26     V1203 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04327+1803 SAR   4     HBC 403 = V1076 Tau.                                                            
04328+1600 CHR 152     This is probably the spectroscopic system found by Griffin et al.       Grf1988 
                       (1988) to have a period in excess of 15 years.                          Msn1993a
                       The spectroscopic solution of this 9377-d pair determined by Griffin.   Grf2012b
04329+0007 LDS 121     BC: NLTT 13492/13491 = LSPM J0432+0006. Law et al (2008) derive a       Law2008 
                       distance of 16.5 +8.2/-2.7 pc and a projected separation of                     
                       76.2 +38.7/-11.8 au. Estimated spectral types are M4.5 and M5.5.                
04330-3817 BU  747     RZ Cae, Algol (EA) type eclipsing binary, P = 2.486955 d.               Zas2011 
04331+2410 GHE  13     Ab1,Ab2: Second and third Schaefer et al. (2006) orbits for Elias 12    Sfr2006 
                       Na-Nb include a lunar occultation measure by Simon et al. (1995)        Smn1995 
                       Schaefer et al. (2012) derive spectral types, Teff, luminosities, and           
                       masses for the Aa, Ab1, and Ab2 components (assuming a distance of              
                       140pc for M and L) as follows:                                                  
                          Aa:  K7       4060K  1.05 +/-0.20 Lsun  1.040+/-0.016 Msun (Mtotal)          
                          Ab1: M2       3560   0.447+/-0.058      0.564+/-0.018                        
                          Ab2: M2-M2.5  3560   0.356+/-0.038      0.476+/-0.017                Sfr2012 
                       Aa,Ab: V807 Tau. Young member of Taurus-Auriga molecular cloud.         Dae2015 
           HAT   9     AB: Additional notes may be found in Herbig (1962).                     Her1962 
           GHE  12     Ba,Bb: GH Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04331-1208 STF 564     The pair GAL 145 is identical                                           Hei1983a
04331-4646 SKF1205     The pair also show matching radial velocities, but primary is a SB1.    TrC2006 
04332+2434 SAR   5     HBC 405 = V830 Tau.                                                             
04332-6829 OGL 199     LMC155.5.3403  + LMC155.6.576                                           Pli2012 
04333+6847 LDS9172     Old LDS6172.                                                                    
04333+5921 TOR   7     Formerly known as PAN   4.                                                      
04333+5248 MLR 695     Aa,Ab: Also known as HDS 591.                                                   
           ES 2607     B is BD+52@844.                                                                 
04333+2505 LDS5190     old LDS6173.                                                                    
04334+4304 SHJ  44     57 Per. STTA 50 = H 6  99.                                                      
04335+7232 HJ 2228     AB: A is a spectroscopic binary.                                                
                       Also an unresolved 4.194d spectroscopic binary.                         XXX2017a
           LDS1595     AC: Initially merged with AB under mistaken belief was same pair.               
04335+1801 STF 559     H N 132.                                                                MEv2010 
04336+2610 GHE  14     Aa,Ab: IS Tau. Young member of Taurus-Auriga molecular cloud.           Dae2015 
04336+2421 POU 460     AB: Haro 6-22. Both components variable (A: 13.9-15.5, B: 14.1-16.1)            
                       according to Wenzel (1957 Nach. astr. Zentralst. 11,28)                 Her1962 
                       A is GK Tau. B is GI Tau.                                                       
04336-6249 HJ 3670     B is CPD-63@343.                                                                
04337+1824 DAE  27     V1323 Tau.                                                              Dae2015 
04337+1752 CHN   7     Formerly known as LEI  17.                                                      
                       HN Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04338+1451 rho Tau     Hipparcos astrometric solution assumes circular orbit (e = omega = 0);  HIP1997d
                       Hyades VA 725 = vB 95.  1.337-year SB according to Abt (1965).          AbH1965 
04339-0644 BU  881     46 Eri. A is variable EH Eri, P = 3.8d, small amplitude.                        
04340+1510 CHR  17     This rapidly moving system within the wide binary ADS 3317 is probably  Grf1988 
                       the spectroscopic system with P ~13 yr found by Griffin et al. (1988).  Msn1993a
                       New spectroscopic solution determined by Griffin.                       Grf2012b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.27 +/- 0.34, 1.66, and 0.95 Msun, respectively.             Mlk2012 
04340-5503 B  2092     alp Dor. Hyad (vB 96).                                                          
                       High mass-sum, illustrative solution only, speckle/spectroscopic orbit          
                       needed, cf. Griffin et al. (1988).                                      Grf1988 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 5.51 +/- 1.51, 4.25, and 2.69 Msun, respectively.  Mlk2012 
           HJ 3668     AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
04342+2612 SMN  14     Measure of 1990.77 made by triangulation of multiple measures and is            
                       in a red filter.                                                        Smn1992 
04343+1830 SAR   6     HBC 407 = V1077 Tau.                                                            
04344+6928 HJ 1145     Aka TDS2898.                                                            Skf2016a
04344+1630 OL  107     The ES pair formerly listed at 04350+1631 (= ADS 3313)                          
                       is identical to this pair.                                              Hei1980a
04345-6859 OGL 200     LMC156.4.9     + LMC156.4.130   + LMC155.1.775                          Pli2012 
04345-6958 OGL 201     LMC157.2.3089  + LMC157.2.3113                                          Pli2012 
04346-6948 OGL 202     LMC157.3.2891  + LMC157.3.2890                                          Pli2012 
04346-7015 OGL 203     LMC151.5.4     + LMC151.5.38    + LMC151.6.4891                         Pli2012 
04348+3206 SEI  49     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
04349-7651 HJ 3691     B is CPD-77@176.                                                                
04350-1246 GAL 373     Object #143 in Gallo's original list.                                   Gal1914 
04352+1822 SAR   7     TAP 51  = V1078 Tau.                                                            
04352-0944 STF 570     B is BD-10@958.                                                                 
                       H 3 100.                                                                MEv2010 
04353+2254 KSA 108     Primary is variable star FF Tau.                                                
04353+2232 HER  23     HAT  11.                                                                        
04354+1045 RED   7     Identification with GCS2 uncertain.                                             
                       1996.8130  RHy ID and coordinates from Reid (1992).                     Red1992 
                       LP ID from Luyten et al. (1981).                                        Luy1981 
                       Candidate Hyades member; Reid considers definite binary.                Red1997 
04356+2408 HRM   1     AB = DCH  56. IRAS 04325+2402.                                                  
04356+1206 TOK  17     Hyades vA 771.                                                                  
                       Primary is 1.9d SB2. Estimated period of visual pair 400y.              Tok2006 
04357+2411 CHN   8     Formerly known as LEI  19.                                                      
04357+1953 L     4     First resolved by Lewis in 1902, this system was unconfirmed for        GrO1932A
                       several decades despite numerous attempts, notably those of Aitken              
                       with the 36inch between 1910 and 1922. In the ADS, Aitken concluded     A__1932b
                       "It is very doubtful whether the star is double". The system was                
                       subsequently removed from the WDS, until its resolution by Prieur et            
                       al. over 90 years after its discovery.                                  Pru2002b
04357+1010 CHR  18     Aa,Ab: 88 Tau. A is an Alpha CVn-type variable, and spectroscopic               
                       binary, now resolved by speckle interferometry.                                 
                       B is BD+09@606.                                                                 
                       1997.071: Absolute quadrant determined by triple-correlation                    
                       techniques                                                              Pru2002b
           88 Tau      Lane et al. (2007) combine PHASES astrometry with speckle and radial    Lne2007 
                       velocity data to derive an orbit for the Aa,Ab components of the                
                       nearby sextuple 88 Tau, as well as the Aa1,Aa2 and Ab1,Ab2 subsystems.          
                       The parallax of the system is determined at 0".01973 +/- 0".00034,              
                       with semimajor axes for Aa,Ab; Aa1,Aa2; and Ab1,Ab2 of 12.17 +/- 0.17,          
                       0.0689 +/- 0.0012, and 0.0997 +/- 0.0021 au, respectively. Other                
                       derived quantities for the four components are as follows:                      
                              Star     Mass (Msun)        M_K (mag)      Spec Type                     
                              Aa1    2.06  +/- 0.11     0.69 +/- 0.26      A6m                         
                              Aa2    1.361 +/- 0.073    2.20 +/- 0.28      F5V                         
                              Ab1    1.069 +/- 0.069    2.31 +/- 0.27      G2-3:V                      
                              Ab2    1.057 +/- 0.068    2.00 +/- 0.27      G2-3:V                      
           SHJ  45     STTA 52.                                                                        
                       AB: H 6  31.                                                            MEv2010 
04358-6655 OGL 204     LMC152.7.209   + LMC152.7.891                                           Pli2012 
04359+2352 KOH  15     V1324 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04359+2254 LEI  21     Primary is variable star HP Tau.                                                
04359+1631 BU  550     alp Tau = 87 Tau = Aldebaran. A is an unclassified variable.                    
           STFB  2     AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       Incorrectly listed as STFA  2.                                                  
           STFA  2     AC: H 6  66.                                                            MEv2010 
04359-0332 LDS9174     Old LDS6174.                                                                    
04360-0337 STF 571     AB: H 3  95.                                                            MEv2010 
04361+5525 HIP  21433  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Tokovinin et al. (1994). They derived component masses 0.88 and 0.24    Tok1994c
                       Msun and an estimated semimajor axis of 28.68 mas.                      Ren2013 
04362+0814 A  1840     Observations suggest eccentricity >0.80 and period 150-200y.            Mlr1956a
                       Star C (mag. 9, 6") is probably physical.                                       
04363+5502 RAO  35     Triple, consisting of a 2.6 day spectroscopic binary (Gorynya &                 
                       Tokovinin 2014 MNRAS 441, 2316) and the Robo-AO and 2MASS companion at          
                       5".7. The field is crowded and PM(A) is small. Our photometry places B          
                       slightly above the MS. The star is young and active according to                
                       Guillout et al (2009 A&A 504, 829) and we retain B as likely physical.  Rbr2015d
04363+4722 S   451     STTA 51. B is BD+47@1012.                                                       
04363-0321 BUP  64     nu Eri = 48 Eri. A is a Beta CMa-type variable.                                 
04363-6655 OGL 205     LMC152.7.23    + LMC152.7.88                                            Pli2012 
04364+3413 HU  610     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                       the orbit of Baize (1961).                                              Baz1961b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.70 +/- 1.07, 2.11, and 0.95 Msun, respectively.             Mlk2012 
04365-0559 LDS9175     Old LDS6175.                                                                    
04365-0611 LDS 843     Aka LDS9175.                                                                    
04366+1930 LDS3597     The primary is a BY Draconis-type variable.                                     
04366+1845 RUC   4     RZ Tau. Spectral type of resolved companion M3-5V or possibly later.    Ruc2007 
04367+4116 58 Per      Wyller orbit rejected from Fourth Orbit Catalog                         Wye1957 
                       ("not confirmed by subsequent observations")                            Wor1983 
04367+4105 STF 563     H 3  65.                                                                MEv2010 
04367+1155 LDS1181     Hyades vB 210.                                                                  
                       NLTT 13608/13606                                                        Chm2004 
04367-6733 OGL 206     LMC153.7.3072  + LMC153.7.3092                                          Pli2012 
04368+2708 GIC  49     LDS1180 = G008-044/G039-027 = GJ 171.2AB. A component is the variable           
                       V833 Tau = Melotte 25 301.                                                      
                       NLTT 13601/13599                                                        Chm2004 
                       Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
04368-6205 HJ 3679     A is a long-period variable, R Dor.                                             
04372+3108 KOH  16     V961 Tau. Member of Taurus-Auriga molecular cloud.                      Dae2015 
04372+1108 GIC  50     LDS1182 = G083-024/G083-023.                                                    
04372-6658 OGL 207     LMC152.7.3126  + LMC152.7.3127                                          Pli2012 
04373+1748 BPM 101     [PM2000]  178584 + [PM2000]  178531.                                    Gvr2010 
04373-6853 OGL 208     LMC155.1.4867  + LMC155.1.5999                                          Pli2012 
04373-6905 OGL 209     LMC149.7.8     + LMC149.7.35    + LMC149.5.668                          Pli2012 
04374+0034 STTA 53     B is BD+00@801.                                                                 
                       Pair appears in an appendix list, not part of the discoverer's                  
                       regular numbering sequence.                                                     
                       SHY 465. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
04375+1509 CHR 153     1991.9021: Reprocessing of archival speckle data have confirmed this            
                       already strong detection and have shown a change in theta of 15 deg in          
                       2.7 yr.  CHR 153 cannot be the 2-yr  spectroscopic system of Griffin    Grf1988 
                       et al. (1988). In the Hyades.                                           Msn1993a
                       The preliminary orbital solution is clearly in error as the visual      Ole2003b
                       companion shows only linear motion. It can be another member of the     Hrt2012a
                       Hyades or a wide pair in projection. The acceleration could be          Hrt2012a
                       produced by the 1.8 yr SB companion.                                    Tok2012a
                       This is not the 734.2-d spectroscopic binary of Griffin but a more      Grf2012b
                       distant companion.                                                              
04376-0228 WAL  32     After analysis of proper motions, radial velocities, etc. conclude              
                       that A (= 51 Eri) and C (= GJ 330) comprise a wide physical binary and          
                       are members of the young bet Pic moving group. Distance is ~30pc and            
                       estimated orbital period is ~60,000y; pair form a very fragile system.  Fgl2006 
                       C component is GJ 3305; A and C are members of bet Pic moving group.    Zuc2001b
           BU   88     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           KAS   1     Ca,Cb: Better known as GJ 3305, this binary is part of the beta Pic             
                       moving group (Zuckerman et al. 2001), and is also bound to 51 Eri in a  Zuc2001b
                       wide orbit (Feigelson et al. 2006) with a projected separation of 66".  Fgl2006 
                       The binarity of GJ 3305 was first reported by Kasper et al. (2007),     Kas2007b
                       and has been observed with AstraLux on several occasions.               Jnn2012 
                       Ca,Cb: Montet et al (2015) derive a combined spectroscopic/astrometric          
                       orbital solution, yielding masses 0.67 +/- 0.05 and 0.44 +/- 0.05               
                       Msun, luminosities 0.112 +/- 0.007 and 0.043 +/- 0.005 Lsun, and an             
                       age of 37 +/- 9 Gyr.                                                    Mtt2015 
04379-6701 OGL 210     LMC152.2.1     + LMC152.2.31                                            Pli2012 
04379-6915 OGL 211     LMC149.7.39    + LMC149.7.80                                            Pli2012 
04380-1302 STF 576     B is BD-13@938.                                                                 
04381+1457 LDS5582     LDS6138.                                                                        
04382+2813 BEU   6     GJ 3304 = G039-029.  Daemgen et al. (2007) derive a distance of 14.5    Dae2007 
                       +/- 3.8 pc, a separation of 11.4 +/- 3.4 au, and a predicted orbital            
                       period of 76 +36/-35 yr. Spectral types are M4.0 +/- 0.5  and M4.5 +/-          
                       0.5; masses are 0.23 +0.10/-0.07 and 0.20 +0.07/-0.05 Msun.                     
                       Estimated age 60-300 Myr; masses 0.28 +/- 0.06 and 0.19 +/- 0.05 Msun;          
                       a ~13.4 au.                                                             Jnn2014 
04382+1603 PAT  12     Aa,An. CPM companion (rho = 140".5) is outside our detection window.    Msn1993a
04382+1602 BUP  65     89 Tau.                                                                         
04382+1231 BUP  66     Hyades vB 104. 90 Tau. A is a spectroscopic binary.                             
                       Two CPM companions (rho = 44" and 120") fall outside detection window.  Msn1993a
           MRN   2     Aa,Ab: Marion et al. (2014) estimate the companion to this Hyades               
                       member as K4V.  Assuming a face-on, circular orbit with a semi-major            
                       axis of 11.1 mas (0.52 au), the minimum period would be ~84d.           Mrn2014 
04382-1315 TOK 660     Resolved using ANDICAM2. PM(A) is small, B is considered physical from          
                       photometry and low crowding                                             Tok2014d
04382-1418 KUI  18     53 Eri.                                                                         
04384+2611 ITO   6     AC: Itoh et al. (2008) estimate that if the AC pair is physical, the            
                       H-band magnitude of C suggests a mass of order 1 Mjup. Followup                 
                       astrometry and spectroscopy is needed to confirm its companionship.     Ito2008b
04385+2656 STF 572     AB: One component is a spectroscopic binary.                                    
04385+2611 SMN  15     Measure of 1990.77 made by triangulation of multiple measures                   
                       and is in a red filter.                                                 Smn1992 
04385+1752 BPM 102     [PM2000]  179567 + [PM2000]  179474.                                    Gvr2010 
04386-0921 TOK 387     HIP 21265 is an X-ray source and an SB2 according to GCS (only one              
                       observation). It is resolved here at 56mas, which corresponds to a              
                       period of ~5yr.                                                         Tok2015c
04387-6822 OGL 212     LMC148.5.112   + LMC148.5.706                                           Pli2012 
04388+2147 JNN 262     G 8-48. Estimated age 300-1000 Myr; masses 0.12 +/- 0.04 and 0.10 +/-           
                       0.03 Msun; a ~21.9 au.                                                  Jnn2014 
04388-2702 TOK 661     CA: Resolved using ANDICAM2. Tuc-Hor moving group. PM(C) is small,              
                       physical from ptm only.                                                 Tok2014d
04388-7015 OGL 213     LMC151.4.44    + LMC151.4.45                                            Pli2012 
04389+1406 HD  29461   Hyades vB 106.  This is SB with P ~ 10 yr according to Griffin et al.   Grf1988 
                       (1988).                                                                 Msn1993a
04389+1406 MET  41     This optical companion cannot be 3760d spectroscopic binary of Griffin  Grf2012b
04389-1207 HDS 599     Cvetkovic et al. (2014) derive spectral types A1 and  F2, masses 2.28           
                       and 1.56 Msun. Dynamical parallax is 15.50 +/- 0.75 mas.                Cve2014 
04390+2149 LDS1183     NLTT 13673/13674                                                        Chm2004 
04391+0752 BUP  67     B is BD+07@680.                                                                 
04392+2553 TER   1     IRAS 04361+2547.                                                                
04393+3331 JNN 263     Estimated age 1000-10000 Myr; masses 0.32 +/- 0.16 and 0.20 +/- 0.10            
                       Msun; a ~2.6 au.                                                        Jnn2014 
04393+2221 LKCA 15     Sallum et al. (2015) resolve three planetary companions to LkCa 15.             
                       Companion b has a best-fit orbital semi-major axis 14.7 +/- 2.1 au,             
                       that of companion c is 18.6 +2.5/-2.7 au. Companion d is only seen in           
                       the L' band, so less information can be gleaned.                        Sll2015b
04393+1555 STFA 11     A: sig 2 Tau = 92 Tau. A is a spectroscopic binary.                             
                       B: sig 1 Tau = 91 Tau. B is BD+15@665, SB and occultation binary.               
04394-6938 OGL 214     LMC150.4.33    + LMC150.4.139                                           Pli2012 
04395-1141 GAL 374     Object #147 in Gallo's original list.                                   Gal1914 
04395-4507 I  1489     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.49 +/- 0.82, 1.60, and 0.79 Msun, respectively.             Mlk2012 
04396-2115 BU 1236     AC: SHY 467. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
04397+0952 GIC  51     LDS1184.  AB = G083-028/G083-029 = GJ 9162AB.                                   
04397-6722 OGL 215     LMC153.3.3746  + LMC153.3.4025                                          Pli2012 
04399+5305 BU 1043     3 Cam. A is an eclipsing binary of the W UMa-type.                              
04399+1940 RED   8     1996.0929  RHy ID and coordinates from Reid (1992). Candidate Hyades    Red1992 
                       member; Reid considers possible binary.                                 Red1997 
04399+1631 BU 1044     Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 of               
                       04404+1631 = CHR 154 were actually of this pair. Those measures have            
                       been included here.                                                             
04400+5328 BU 1295     2 Cam.                                                                          
                       The high-eccentricity solution for AB by Valbousquet (1980) is          Val1980b
                       questioned by Heintz (1962) on grounds of a mass discrepancy.           Hei1962 
                       The equinox-1900 position was incorrectly given as 04320+5310 in                
                       McAlister & Hendry (1982).                                              McA1982d
           STF 566     A is the D component of 04404+5328.                                             
04400+3534 HJ  681     ALI 64.                                                                         
04400+2556 KON   5     Estimated masses 0.1 and 0.06 Msun. Primary spectral type M5.75         Kon2007b
04403-6924 OGL 216     LMC149.2.6     + LMC149.2.26                                            Pli2012 
04404+5328 D     4     AD: D component is primary of 04400+5328BU 1295AB. AD not physical, so          
                       systems not merged.                                                             
04404+1631 CHR 154     Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 were             
                       actually of 04399+1631 = BU 1044. Measures X coded here but retained            
                       to maintain original catalog pedigree.                                          
04404-1940 STN   9     54 Eri. A semiregular variable, DM Eri. No very positive observations           
                       as a visual double. Needs speckle.                                              
04406-4152 HDO 190     AB: alp Cae. A is a Delta Scuti-type variable.                                  
                       AB: Physical/optical nature undefined.                                  Ehr2010 
04407+2519 KON   6     Estimated masses 0.15 and 0.08 Msun. Primary spectral type M5.5         Kon2007b
04407-2812 TOK 209     Resolved with NICI, uncertain measure. Not resolved with speckle.       Tok2012a
                       Direct motion by 16deg since first resolution at Gemini on 2011.80;             
                       estimated period is 15 yr.                                              Tok2013b
04408-3951 RSS   5     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
04408-6741 OGL 217     LMC146.8.31    + LMC146.8.30                                            Pli2012 
04409+0058 STF 583     AB: H 2  81.                                                            MEv2010 
04410-6935 OGL 218     LMC150.4.7439  + LMC150.4.8170                                          Pli2012 
04413+3242 JNN 264     Estimated age 300-1000 Myr; masses 0.54 +/- 0.04 and 0.40 +/- 0.06              
                       Msun; a ~58.9 au.                                                       Jnn2014 
04414+2715 KOH  20     V1328 Tau.                                                              Dae2015 
04413+2054 LWR   5     V834 Tau                                                                        
04415-4328 Anon        EQ 0439-4333. ID as EQ 0439-4333 is uncertain, as it was based on a             
                       Simbad search using epoch-1950 coordinates 043955-433318 from White et  Whi1991 
                       al. (1991).                                                                     
04416-4302 WHI   6     Possibly resolved.                                                      Whi1991 
04417+2302 KSA  29     Primary is of spectral type M8.5 and shows evidence of a circumstellar          
                       disk and active accretion. The Ab companion is estimated as type                
                       M9.5-L0, mass 5-10 Mjup. Todorov et al. (2010) also resolved the B              
                       component into a 0.23" pair.                                            Tod2010 
04418+2658 KOH  21     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04419-6714 OGL 219     LMC146.5.3639  + LMC146.5.3827                                          Pli2012 
04421+2523 LEI  24     The measures and component designations of the Ba and Ca pair were              
           GHE  15     assigned incorrectly and were correctly re-assigned 5/22/02. The                
                       designations LEI  24Ba <---> GHE  15Ca were flipped and the                     
                       designation LEI  25Aa became LEI  24Aa.                                         
04422+3731 STF 577     CfA: SB? Not clear if it is A or B.                                     Tok2014d
04422+2257 MCA  16     Aa,Ab: tau Tau = 94 Tau. Occultation binary and short-period SB.                
                       Hough suspected duplicity due to a slow occultation. Finally resolved           
                       by McAlister in 1980.                                                   McA1983 
                       1983.9337, 1983.9391: Interferometric observations are incompatible     Jef1963 
                       with the large delta m reported by Jeffers et al. (1963).               Bnu1984 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 12.44 +/- 4.14, 7.48, and 6.92 Msun, respectively. Mlk2012 
           S   455     STTA 54 = H 6   7.                                                              
04422+0259 A  2424     Position angles uncertain.                                                      
04423+8103 LDS1596     NLTT 13589/13587                                                        Chm2004 
04423+0932 TOB 369     Aka GWP 610.                                                                    
04423-2943 LDS 126     NLTT 13802/13804                                                        Chm2004 
04423-6657 OGL 220     LMC145.7.3953  + LMC145.7.4003                                          Pli2012 
04426+2516 KSA 111     Primary is variable star DP Tau.                                                
04427-2147 LDS3608     NLTT 13805/13809                                                        Chm2004 
04428-7030 OGL 221     LMC144.7.6     + LMC144.7.441                                           Pli2012 
04429+1843 LDS2266     BC: HJL1038.                                                            HJL1986 
                       RV(A)=+14.5, not Hyades member! On Lick RV program.  B is SB2,          HJL2012b
                       P=56.445d (Halbwachs et al. 2012)                                       Tok2014d
04430+5712 A  1014     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                       the orbit of Baize (1958).                                              Baz1958 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.27 +/- 0.48, 2.37, and 1.10 Msun, respectively.             Mlk2012 
04431+3356 HJ  348     Also known as STF 580.                                                          
04431-0725 A   476     KP Eri, Algol (EA) type eclipsing binary, P = 7.447126 d.               Zas2011 
04431-6844 OGL 222     LMC148.2.7773  + LMC148.2.7774  + LMC148.2.7791                         Pli2012 
04432-5436 TOK  87     HIP 21960.                                                                      
04432-6723 OGL 223     LMC146.3.22    + LMC146.3.117                                           Pli2012 
04433+5931 A  1013     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 5.20 +/- 2.40, 3.42, and 1.82 Msun, respectively.             Mlk2012 
04434+1558 BPM 103     [PM2000]  183754 + [PM2000]  183745.                                    Gvr2010 
04436-0848 STF 590     55 Eri. B is a Delta Scuti-type variable, DW Eri., BD-09@969. Spectral          
                       type F4IIIpSr. Both components are spectroscopic binaries.                      
                       H 3  99.                                                                MEv2010 
04441+1739 LDS2268     NLTT 13828/13829.                                                               
04441+0205 HL    1     This is a measure of HL 04441+0204 and A 3006 04440+0204                        
04442-6959 OGL 224     LMC143.8.7618  + LMC143.8.8368                                          Pli2012 
04443+2017 KOH  22     V1205 Tau.                                                              Dae2015 
04444+1952 KOH  23     V1333 Tau.                                                              Dae2015 
04444+1109 BUP  68     Hyades vB 111.  A may be variable. Two CPM companions with rho = 74".7          
                       and rho = 10".0, both outside our detection window.                     Msn1993a
04445+3953 COU1524     Primary is eclipsing binary V592 Per (period 0.71572 day).              Zas2010 
04448-6946 OGL 225     LMC143.6.9637  + LMC143.6.10050                                         Pli2012 
04449+2717 KOH  24     Member of Taurus-Auriga molecular cloud.                                Dae2015 
04449+1757 LDS2271     LDS5590.                                                                        
04450+1605 BPM 104     [PM2000]  185037 + [PM2000]  185149.                                    Gvr2010 
04453-6943 OGL 226     LMC143.6.9561  + LMC143.6.9815                                          Pli2012 
04454+2955 NI   12     BVD  47.                                                                        
04454+2421 POU 477     Also known as GRV 215.                                                          
04454-5949 FIN  89     A is the Mira-type variable, T Dor.                                             
04454-7006 OGL 227     LMC143.8.7703  + LMC143.8.7822                                          Pli2012 
04455-0512 HJ   27     B is BD-05@1021.                                                                
04455-2226 DON  77     CD-22@1801.                                                                     
04455-7018 OGL 228     LMC144.3.38    + LMC144.3.177                                           Pli2012 
04458+3515 ES 2410     ALI 65.                                                                         
04459+1911 AG  311     B is BD+18@714.                                                                 
04460+1616 BPM 105     [PM2000]  185978 + [PM2000]  185928.                                    Gvr2010 
04460+1142 BUP  69     A is possibly a spectroscopic binary.                                           
04464+4221 COU2031     1985.740:  The separation of this partially resolved pair was                   
                       calculated under the assumption of zero or otherwise known magnitude            
                       difference.                                                             Tok1985 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.53 +/- 0.35, 2.85, and 1.05 Msun, respectively.             Mlk2012 
                       Combined spectroscopic/interferometric orbit. Resulting masses are              
                       1.75 +/- 0.08 and 1.32 +/- 0.08 Msun. Spectral types are estimated as           
                       G3IV and F6V.                                                           Doc2014i
04465+1528 HD  30246   Hyades vB 142.                                                          Grf1988 
                       Noted as a SB in Griffin et al. (1988).                                 Msn1993a
04465+1528 MET  42     This optical companion cannot be 989.8-d SB of Griffin.                 Grf2012b
04466+4002 BRT2206     ALI 1040.                                                                       
04468+1745 PAT  15     This pair is noted as a slow spectroscopic binary in Griffin et al.     Grf1988 
                       (1988).                                                                 Msn1993a
04468+1744 LDS1187     LDS5601.                                                                        
04468+0901 PAT  16     This pair is a spectroscopic binary with P ~ 7 yr according to Griffin  Grf1988 
                       et al. (1988).                                                          Msn1993a
                       Hyades. The 0".1 pair PAT 16 was not resolved with speckle; its                 
                       estimated period is 7 yr.                                               Tok2012a
                       The spectroscopic solution of this 2446-d pair determined by Griffin.   Grf2012b
04468-2618 VIG   6     The B component appears to be a faint background star.                  Vig2012 
04469+1700 DAE  35     DQ Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04469-1117 JNN  28     2MASS J04465175-1116476 has a companion that has not yet been tested            
                       for common proper motion. Since the brightness and color match                  
                       expectations, the system counts as an unconfirmed binary.               Jnn2012 
04469-4630 LDS9177     Old LDS6177.                                                                    
04469-6036 TOK 388     First resolution of HIP 22229 at 0".043, dI=1.2. The measure is                 
                       uncertain, but the elongation is confirmed with 2-ms exposure and is            
                       not seen in other observed stars, so it is not caused by vibration.             
                       This is a triple system containing an eclipsing binary AL Dor (Algol)           
                       with an eccentric orbit (Bulut & Demirkan, 2007 MNRAS, 378, 179). The           
                       separation implies an orbital period of the outer system ~5yr.          Tok2015c
04470-6954 OGL 229     LMC143.2.264   + LMC143.2.1526                                          Pli2012 
04472+2027 KU   85     Also known as STF 593.                                                          
04472+1332 LDS1188     LDS5603.                                                                        
04472-1715 ARG  11     B is BD-17@951, spectrum G2/3V.                                                 
04476+1816 PAT  17     This pair is a spectroscopic binary with P >5 yr according to Griffin   Grf1988 
                       et al. (1988).                                                          Msn1993a
                       The spectroscopic solution of this 4822-d pair determined by Griffin.   Grf2012b
04476-0534 GRE   1     IRAS 04451-0539 = PDS 11.                                               Gre1992 
04477+4014 A  1545     Primary is V593 Per, a Beta Lyr type eclipsing binary, P = 3.2437d.     Zas2012 
04477-6945 OGL 230     LMC143.3.10488 + LMC143.3.11560                                         Pli2012 
04478+3643 GAA   2     AW Per. This Cepheid is an SB with an orbital period of ~40 yr. First           
                       discovered by Miller & Preston (1964 PASP 76, 47), it took several              
                       years to derive the first orbit from radial velocity data (Evans 1989           
                       AJ 97, 1737). It is likely that this companion is itself a binary, as           
                       argued by Evans and by Evans et al. (2000 AJ 120, 407), because the             
                       magnitude difference between the Cepheid and its companion is not               
                       consistent with equal masses and predictions from evolutionary tracks.          
                       Unfortunately, Gallenne et al. (2015) note they did not have enough             
                       angular resolution and sensitivity to detect this third companion. The          
                       properties of the brightest companion were studied based on IUE                 
                       spectra by Evans (1994 ApJ 436, 273; 1995 ApJ 445, 393), who found its          
                       spectral type to be B8.3V. This is in agreement with their detection            
                       with a flux ratio f = 1.22 +/- 0.30%, i.e., a spectral type in the              
                       range B6-B9V (using d = 853 pc from a P-L relation and K = 4.63 mag     .   
                       for the Cepheid). They estimate the companion mH = 9.6 +/- 0.3 mag      .     
                       (using for the Cepheid at theirgiven phase mH = 4.84 +/- 0.01 mag from  .     
                       Monson & Pierce (2011 ApJS 193, 12). Massa & Evans (2008 MNRAS 383,             
                       139) also determined the angular separation of the component for                
                       another epoch, which will allow an estimate all the orbital elements,           
                       (see also Gallenne et al. 2013 EAS Pub. Ser. 64, 197). Gallenne et al.          
                       (2015) derived a maximum sensitivity limit at 3sigma of 0.62%, i.e.,            
                       dmH> 5.5 mag, so can therefore exclude any additional components with   .     
                       a spectral type earlier than B9V.                                       GaA2015 
                       Spectroscopic binary orbit with P = 13954d determined.                  Grf2016c
04478+2925 CHN  10     Additional notes may be found in Herbig (1962).                         Her1962 
                       DS Tau. Young member of Taurus-Auriga molecular cloud.                  Dae2015 
04478-3043 LDS3620     NLTT 13968/13970                                                        Chm2004 
04479+2755 KOH  26     V1337 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04479+1902 LDS3619     LDS5604.                                                                        
04480+5645 BU 1387     4 Cam.                                                                          
04480+5307 STF 587     H 4  73.                                                                MEv2010 
04480-4154 TOK 490     AD: D component is the primary of 04490-4128 RST1285.                           
04481+7810 MLR 464     Also known as TDS 148.                                                          
04483-7036 OGL 231     LMC137.8.142   + LMC137.8.140                                           Pli2012 
04485+1056 HJ  684     CD: Also known as STF 601.                                                      
04486+1748 STF 598     HJL  62.                                                                HJL1986 
04486-6648 OGL 232     LMC138.6.5554  + LMC138.6.5870                                          Pli2012 
04487+2106 HD 284787   Hyades vB 115.  This pair is a spectroscopic binary SB with P ~ 4 yr    Grf1988 
                       according to Griffin et al. (1988).                                     Msn1993a
04487-6830 OGL 233     LMC141.4.9     + LMC141.4.22                                            Pli2012 
04488+5308 STF 586     Same position, and in field of, STF 587.                                        
04488-6124 JSP  60     AC, 180deg, 8" 14th mag noted.                                          Hln1966 
04488-6902 OGL 234     LMC142.4.13828 + LMC142.4.14777                                         Pli2012 
04489-6951 OGL 235     LMC136.7.1220  + LMC136.7.2869                                          Pli2012 
04491+1408 BPM 106     [PM2000]  189268 + [PM2000]  189301.                                    Gvr2010 
04491+0513 STTA 55     B is BD+04@755.                                                                 
04492+2448 HD 283882   Hyades vB 117.  The 11.93-day SB of Griffin & Gunn (1978) is outside    Grf1978b
                       our detection window.                                                   Msn1993a
04492-3505 TOK 210     The companion is close to the detection limit, but it is considered to          
                       be real. The measurement is uncertain.                                  Tok2012a
                       Retrograde motion by 5deg since resolution on 2011.78; period is about          
                       20y. Measurements are uncertain because of large dm. The "blue" color           
                       of the companion is caused by measurement error.                        Tok2013b
04492-6736 OGL 236     LMC139.2.2     + LMC139.2.1                                             Pli2012 
04492-6901 OGL 237     LMC142.4.13837 + LMC142.4.14005                                         Pli2012 
04493+3235 CHR  19     A spectroscopic binary with P = 7.05d.                                          
                       Fekel et al. (2013) derive a new spectrosopic orbit with P=7.051d and           
                       e (adopted) = 0.0. Estimated masses are 1.95 and 1.2 Msun. Differences          
                       between early DAO and more recent data suggest the possibility of a             
                       3rd component in the system. It in uncertain whether this corresponds           
                       to the never-confirmed speckle companion, however.                      Fek2013a
04493+2934 RAS  18     Magnetic star; primary is A0 silicon star. Companions A8-F0.            Ras2014 
                       LSC  31. V473 Tau.                                                              
04494+4828 JNN 265     G 81-34. Estimated age 30-300 Myr; masses 0.27 +/- 0.14 and 0.18 +/-            
                       0.09 Msun; a ~13.5 au.                                                  Jnn2014 
04497+1554 HJ 3261     96 Tau. BU  551A,BC.                                                            
04498+0658 STT 560     pi 3 Ori = 1 Ori. Obviously an optical pair. A spectroscopic binary             
                       and possibly a variable of Delta Scuti type.                                    
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
04499+2230 LDS9178     Old LDS6178. G085-017. See Allen et al. (2000) for information on       AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
                       NLTT 14005/13996                                                        Chm2004 
04500+2230 KOH  27     V1341 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04501+6632 STF 584     May be H 2  92.                                                         Bu_1906 
04501-6635 OGL 238     LMC138.4.30    + LMC138.4.63                                            Pli2012 
04502-0413 SLW 172     GWP 619.                                                                Tob2012b
04502-3113 B  1474     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.59 +/- 1.09, 1.93, and 0.91 Msun, respectively.             Mlk2012 
04503+0657 H 6  83     H VI 83.                                                                        
04503-4119 HJ 3697     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
04503-6649 OGL 239     LMC138.3.160   + LMC138.3.161   + LMC138.3.468                          Pli2012 
04504+1712 HD  30676   Hyades vB 119                                                           Grf1988 
                       This pair is noted as a SB in Griffin et al. (1988).                    Msn1993a
04505+0103 A  2622     A premature orbit has been computed.                                            
04505-3834 GC 5916     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
04506+1505 CHR  20     Hyad (vB 120). Preliminary circular orbit, speckle/spectroscopic                
                       orbit needed, cf. Griffin et al. (1988).                                Grf1988 
                       1991.9023: This may be the spectroscopic system found by Griffin et             
                       al., but more observations are needed to determine the orbital motion.  Msn1993a
                       New spectroscopic solution determined by Griffin.                       Grf2012b
                       This is a Hyades binary for which Griffin (2012) published an SB2       Grf2012b
                       orbit. We combined his RVs with the speckle data, resulting in a very           
                       accurate period. The combined orbit corresponds to a mass sum of 2.1            
                       Msun and an orbital parallax of 22mas, in good agreement with the HIP2          
                       parallax of 23.69 +/- 0.87mas.                                          Tok2015c
04506-6711 OGL 240     LMC139.4.89    + LMC139.4.1334                                          Pli2012 
04507-4540 HJ 3699     old LDS6179.                                                                    
04508+1613 HD  30738   Hyades vB 121                                                                   
                       The 5.751-day SB of Griffin & Gunn (1978) is outside our detection      Grf1978b
                       window.                                                                 Msn1993a
04508-4013 I  1492     Variable, Y Cae.                                                                
04509+3746 TOK 249     Cmp? Crowded field (N*=81), small PM, hence B can be optical.           Tok2014d
04509-5328 DUN  18     iot Pic                                                                         
           SHY 172     AC: HIP  22531 + HIP  22562.                                                    
           SHY 173     BC: HIP  22534 + HIP  22562.                                                    
04511-2731 TOK  88     HIP 22538. The original Hipparcos gives parallax 13.9 mas. A is X-ray           
                       source 1RXS J045103.5-273115.                                           Tok2011a
04512+1104 BU  883     Hyad (vB 122).                                                                  
                       Mass-sum calls for sp subsystem, but RV-ampl <1km/s according to                
                       Griffin et al. (1988).                                                  Grf1988 
                       AO photometric analysis by ten Brummelaar et al. (2000) includes mass           
                       determination.                                                          TtB2000 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.58 +/- 0.49, 2.36, and 2.24 Msun, respectively.  Mlk2012 
                       AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
04512-2213 BRT1378     CD-22@1851.                                                                     
04512-6843 OGL 241     LMC134.7.16981 + LMC134.7.17012                                         Pli2012 
04513-6804 FIN 362     Only one observation, with many negative results. Duplicity                     
                       questionable. Needs speckle.                                                    
04514+1850 BUP  70     97 Tau = LDS1190. A is a Delta Scuti-type variable, V480 Tau.                   
                       B is BD+18@742.                                                                 
04515+5550 LDS5615     relative motion of AB is 0.1"/yr, too fast. optical?                    Tok2014d
04515-3454 FIN 320     Appears to have completed a revolution if the quadrants are correct.            
                       Period about 40y.                                                               
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.50 +/- 1.29, 3.59, and 2.19 Msun, respectively.             Mlk2012 
                       Docobo & Andrade (2013) derive a dynamical parallax of 13.78 +/- 0.41           
                       mas and component masses 1.85 +/- 0.21 and 1.58 +/- 0.18 Msun. See              
                       paper for extensive notes on this system.                               Doc2013d
04515-6653 OGL 242     LMC138.3.7274  + LMC138.3.7555                                          Pli2012 
04515-6933 OGL 243     LMC136.5.13108 + LMC136.5.13830                                         Pli2012 
04516-6841 OGL 244     LMC134.7.20843 + LMC134.7.21738                                         Pli2012 
04518+3047 JOY   4     A is the RW Aur-type variable, UY Aur.                                  Her1962 
                       Hioki et al. (2007) calculate a period of 1640 +/- 90 yr and a total    Hio2007 
                       mass of 1.73 +/- 0.29 Msun.                                                     
04518+1339 BU  552     Hyad (vB 124).                                                          Wor1963a
                       The primary is 143d SB (Griffin et al. 1985).                           Grf1985b
                       The spectroscopic system of Griffin et al. would be too close for us            
                       to resolve by speckle interferometry.                                   Msn1993a
                       A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Turner et al. (1986). They derived component masses 1.42 and 0.55 Msun  TrD1986 
                       and an estimated semimajor axis of 15.67 mas.                           Ren2013 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.67 +/- 1.47, 2.30, and 1.00 Msun, respectively.  Mlk2012 
                       A faint component (about mag. 13, 45") is unobserved since 1906; its            
                       physical nature is unknown.                                                     
04519-3414 BVD  48     AC: SHY 470. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
04519-6058 JSP  62     CD-61@974.                                                                      
04519-6635 OGL 245     LMC138.4.6967  + LMC138.4.6968                                          Pli2012 
04521-6706 OGL 246     LMC138.1.8041  + LMC138.1.8261                                          Pli2012 
04525-3631 LDS9180     Old LDS6180.                                                                    
04526+4302 ES 1526     BC: BRT 111                                                                     
04526-2646 LDS3625     NLTT 14126/14125                                                        Chm2004 
04527-2546 TOK 662     With plx(A), B is on the MS, likely physical.                           Tok2014d
04527-6936 OGL 247     LMC136.4.307   + LMC136.4.140                                           Pli2012 
04527-7043 OGL 248     LMC137.1.262   + LMC137.1.650                                           Pli2012 
04531-0117 S   457     B is BD-01@743.                                                                 
04533+1401 BPM 107     [PM2000]  194282 + [PM2000]  194455.                                    Gvr2010 
04534-0925 RST4256     BRT 2834.                                                                       
04535-5551 LDS 131     See note to 05287-6527 SHY  27AD.                                               
04538-6831 OGL 249     LMC134.3.20577 + LMC134.3.20575                                         Pli2012 
04540-6943 OGL 250     LMC136.3.223   + LMC136.3.524                                           Pli2012 
04540-7022 OGL 251     LMC137.3.14145 + LMC137.3.18362                                         Pli2012 
04541+8125 MLR 490     Also known as TDS 152.                                                          
04541+6621 alp Cam     Fullerton (1990) presents high quality profiles that indicate the       Ful1990 
                       presence of line profile variations; his associated radial velocity             
                       measurements do not confirm any of the periods suggested by Zeinalov &          
                       Musaev (1986 SvAL 12, 125) and Musaev & Snezhko (1988 SvAL 14, 68).     Msn1998a
04542+4935 STF 603     AB: H N  77.                                                            MEv2010 
04543+0722 STF 612     HD 31208. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: HJL  64.                                                            HJL1986 
04544-6720 OGL 252     LMC132.6.11391 + LMC132.6.12002                                         Pli2012 
04545-0314 RST5501     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.79 +/- 1.45, 3.77, and 1.20 Msun, respectively.             Mlk2012 
04547+1221 TOK 251     A is exoplanet host, P=466d. RV(A)=+12.1, not Hyades                    Tok2014d
04547-0257 J  1348     GCB 7. BRT 370.                                                                 
04548+1126 MCA  17     6 Ori.                                                                          
04549+1009 ENG  19     7 Ori = pi 1 Ori. B is BD+09@682.                                               
04549+0836 STT  90     V1834 Ori, Algol (EA) type eclipsing binary, P = 1.51058 d.             Zas2011 
04549-6934 OGL 253     LMC136.4.18656 + LMC136.4.18660                                         Pli2012 
04551+5516 BU 1187     5 Cam.                                                                          
04551+3535 MLB 923     Not found by Heintz at IDS position.                                    Hei1985a
04551-6718 OGL 254     LMC132.4.88    + LMC132.4.1271                                          Pli2012 
04552+1827 DAE  39     V1349 Tau.                                                              Dae2015 
04552-6656 OGL 255     LMC131.7.14509 + LMC131.7.14673                                         Pli2012 
04552-6908 OGL 256     LMC135.3.30074 + LMC135.3.30071                                         Pli2012 
04552-7923 HJ 3733     B is CPD-79@163.                                                                
04554-7109 OGL 257     LMC130.7.31    + LMC130.7.349   + LMC130.7.1118                         Pli2012 
04555+1711 BPM 108     [PM2000]  197155 + [PM2000]  197180.                                    Gvr2010 
04556+3018 MSR   3     HBC 426 = V396 Aur.                                                     Msr2005 
04557+1742 DAE  40     V1350 Tau. Member of Taurus-Auriga molecular cloud.                     Dae2015 
04557-6637 OGL 258     LMC131.4.8     + LMC131.4.7                                             Pli2012 
04558+3033 BNS   1     HBC 78 = MWC 93 = AB Aur                                                        
04558-3100 LDS3628     NLTT 14212/14213                                                        Chm2004 
04558-6741 OGL 259     LMC132.1.137   + LMC132.1.297                                           Pli2012 
04558-7056 OGL 260     LMC130.6.29    + LMC130.6.186                                           Pli2012 
04559+0440 LDS9181     Old LDS6181.                                                                    
           EGN   4     Aa,Ab pair bound. Ab component is likely an early M dwarf with mass             
                       0.43 +/- 0.02 Msun                                                      Egn2007 
                       Aa,Ab: A is on Keck program, RV var.                                    Tok2014d
04560+3021 SFN   1     Aa,Ab: Steffen (2000, 2001) combined solutions each yield values for    Sfn2000 
                       the masses, as well as an orbital parallax.                             Sfn2001 
                       Simon et al. (2013) derive masses 0.86 +/- 0.11 and 0.55 +/- 0.05 Msun          
                       and distance 187.7 +/- 3.9 pc for this pre-MS binary.                   Smn2013 
           KSA  31     HBC 427 = V397 Aur.                                                     Msr2005 
04560-6938 OGL 261     LMC128.5.315   + LMC128.5.772                                           Pli2012 
04560-7040 OGL 262     LMC129.8.308   + LMC129.8.309                                           Pli2012 
04561-7116 OGL 263     LMC130.8.10926 + LMC130.8.11364                                         Pli2012 
04562+2554 GIC  52     G039-042/G039-041.                                                              
                       NLTT 14180/14179                                                        Chm2004 
04563+5206 STF 608     AB,C: HJL  65.                                                          HJL1986 
04563+2415 LDS6148     Also known as GRV 220.                                                          
04564+1331 BU  553     omi 2 Ori = 9 Ori                                                               
04564-0510 SHJ  48     62 Eri. B is BD-05@1093.                                                        
                       AB: H 6 106.                                                            MEv2010 
04566+0422 TOB9004     Measured as BAL2622 but actually an anonymous pair added here.          Tob2010 
                                                                                               Dam2012 
04566-6629 DON  89     Variable.                                                                       
04566-7027 OGL 264     LMC129.7.22    + LMC129.7.188                                           Pli2012 
04567+3917 HU 1091     V560 Aur, Algol (EA) type eclipsing binary, P = 1.528311 d.             Zas2011 
04567-7106 OGL 265     LMC130.7.12419 + LMC130.7.12474                                         Pli2012 
04568+1825 BPM 109     [PM2000]  199012 + [PM2000]  199066.                                    Gvr2010 
04569-6721 OGL 266     LMC132.3.14233 + LMC132.3.14300                                         Pli2012 
04570+1716 BPMA  9     [PM2000]  199271 + [PM2000]  199591.                                    Gvr2010 
04570+1517 MET   4     Metchev & Hillenbrand say the C component is probably optical, based            
                       on proximity.                                                           Met2004b
04572+3838 ES 2338     ALI 780.                                                                        
04573+5345 D     5     7 Cam. A premature orbit has been computed for AB. The primary is SB1,          
                       P = 3.884 d (Lucy & Sweeney).                                           Lcy1971 
                       Drummond linear elements have been modified.                            Dru2014 
           STF 610     AB,C: Star C (mag. about 11.3, 26") may be physical.                            
04573+1524 HEI  38     KOH  36.                                                                        
                       Young member of Taurus-Auriga molecular cloud.                          Dae2015 
04573-7055 OGL 267     LMC130.6.14234 + LMC130.6.16118                                         Pli2012 
04574+0100 A  2624     Aa,Ab : Hipparcos identified the pair as a candidate for Hyades         HIP1998 
                       membership. However, it is not.                                         Grf1988 
                                                                                               Grf2013c
04574+0100 SHY 471     AB: HIP  23044 + HIP  23266. B component = A component of 05003+0100.           
04575-2358 LDS3630     NLTT 14263/14262                                                        Chm2004 
04576+1356 BPM 110     [PM2000]  200066 + [PM2000]  200068.                                    Gvr2010 
04576-0545 STF 624     B is BD-05@1103.                                                                
04576-6950 OGL 268     LMC128.6.11701 + LMC128.6.11986                                         Pli2012 
04578+2357 BU 1045     99 Tau.                                                                         
04580-2248 I   473     CD-22@1917.                                                                     
04580-6735 OGL 269     LMC124.7.79    + LMC132.2.17928                                         Pli2012 
04581+0141 STF 622     A,BC: H 1  68.                                                          MEv2010 
04582+8015 OSO  18     GD 288. Not a common proper motion pair, based on comparison with               
                       POSS2 red plates                                                        Oso2004 
04582+2503 BU 1390     98 Tau. A is a spectroscopic binary.                                            
04582+1423 BPM 111     [PM2000]  201029 + [PM2000]  201109.                                    Gvr2010 
04584-6739 OGL 270     LMC124.8.20199 + LMC124.8.20752                                         Pli2012 
04585-2749 RST 117     CPD-28@715.                                                                     
04585-6834 OGL 271     LMC126.6.46772 + LMC126.6.46857                                         Pli2012 
04587-7053 OGL 272     LMC130.3.25    + LMC130.3.4226                                          Pli2012 
04588-7027 OGL 273     LMC129.2.10    + LMC129.7.17168                                         Pli2012 
04589+6435 GNO   1     Distance is estimated at about 10.5 +/- 1.4 pc, giving a projected              
                       component separation of ~5 au. Estimated orbital period ~70 yr, for an          
                       assumed age of 1 Gyr.  Spectral types are estimates at T8.5 and T9;             
                       total system mass ~25 Mjup.                                             Gno2011 
04590+1433 SHJ  49     STTA 58 = H 5 113. B is BD+14@795. Probably same as BDS 2461, H V 57.           
                       AB: H 5  57.                                                            MEv2010 
04590-1623 BU  314     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.87 +/- 0.28, 2.66, and 2.36 Msun, respectively.  Mlk2012 
                       AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
04591+6322 HU 1090     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 12.31 +/- 4.18, 2.27, and 1.10 Msun, respectively.            Mlk2012 
04591+1123 BPM 112     [PM2000]  202364 + [PM2000]  202525.                                    Gvr2010 
04593+3753 STF 616     ome Aur = 4 Aur                                                                 
                       AB: H 2  14.                                                            MEv2010 
04595-4927 HJ 3715     Primary is VW Pic, a W UMa type eclipsing binary, P = 0.42576d.         Zas2012 
04595-6802 OGL 274     LMC125.6.10758 + LMC125.6.10639                                         Pli2012 
04595-6958 OGL 275     LMC128.2.17    + LMC128.2.402                                           Pli2012 
04596+3135 HO  222     Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       However, radial velocity classifies this as not a Hyades member.        Grf2013c
                       The colors from Tycho photometry are also not consistent with a         Fab2000a
                       physical pair.                                                                  
04597+1555 BUP  73     Hyades vB 128                                                                   
                       A CPM companion with rho = 106".4 is outside our detection window.      Msn1993a
04597-6940 OGL 276     LMC128.4.12    + LMC128.4.92                                            Pli2012 
04598-1016 63 Eri      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Vennes et al. (1998).                                                   Ven1998 
04599+5327 A  1303     A premature orbit has been computed.                                            
                       T corrected from 200.74 to 2000.74 by Ruymaekers & Nys (1995)           Ruy1995