05001-6217 B  1942     Composite spectrum: G5/8III + F/G.                                              
05001-6953 OGL 277     LMC128.2.32346 + LMC128.2.32381                                         Pli2012 
05002+1811 GIC  53     LDS1198. G083-047/G083-048.                                                     
05003+3924 CHR 159     5 Aur.                                                                          
05004+6925 STF 606     B is BD+69@289.                                                                 
05005+0506 STT  93     Hyperbolic orbit by Janova (1966).                                      Jnv1966 
                       sigma = areal constant in the true orbit = 0.00576 arcsec^2/yr                  
                       q = periastron distance in the true orbit = 0".366                              
05006+0337 STF 627     B is BD+03@736.                                                                 
05007-0204 VIG   7     Optical/physical nature of the six faint companions (B-G) is undefined. Vig2012 
05007-6856 SKF1044     OGL 278. LMC126.1.9 + LMC126.1.100                                      Pli2012 
05008+3913 STF 621     Same as AG   83.                                                                
05008+3811 SEI  52     Secondary not seen on POSS plate; may be either variable star or flaw           
                       on AC Potsdam plate.                                                            
05009-7052 OGL 279     LMC130.4.19979 + LMC130.4.21083                                         Pli2012 
05010-6948 OGL 280     LMC128.3.14335 + LMC128.3.14552                                         Pli2012 
05012+3430 COU1229     Primary is V410 Aur, a W UMa type eclipsing binary, P = 0.36636d.       Zas2012 
05015+3733 BRT2207     ALI 523.                                                                        
05015-7107 OGL 281     LMC122.7.267   + LMC122.7.1784                                          Pli2012 
05016+6105 HU 1093     Primary is possible astrometric pair?                                   Tok2014d
05016-7056 OGL 282     LMC122.6.146   + LMC122.6.918                                           Pli2012 
05017+2640 A  1844     Masses and bolometric magnitudes are derived for the two components     Msn1999a
                       of this system by Maosn et al. (1999), based on assumed spectral types          
                       and available parallaxes.                                                       
                       Visual separations systematically too small.                                    
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.83 +/- 0.31, 2.12, and 1.00 Msun, respectively.  Mlk2012 
           S   461     STTA 59 = STFA 12.                                                              
           BAG  21     Ca,Cb: SB2, P=186.28d                                                   Tok2014d
05017+2050 HU  445     Quadrant uncertain, Delta m at least 0.3.                               B__1963b
                       Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                       orbit of Baize (1957).                                                  Baz1957a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 0.15 +/- 0.04, 1.78, and 1.05 Msun, respectively.             Mlk2012 
05020+4349 BU  554     AB: eps Aur = 7 Aur. Strand orbit rejected from Fourth Orbit Catalog    Str1959 
                       ("amplitude below noise level")                                         Wor1983 
           eps Aur     A is a enigmatic supergiant eclipsing system. Also a spectroscopic and          
                       eclipsing binary                                                        Fin1970b
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Heintz & Cantor (1994).                                                 Hei1994b
05020+0137 STF 630     A,BC: H 3  52.                                                          MEv2010 
05021+6910 BU  313     The AB component, BU 313 AB, originally in the BDS and IDS, was                 
                       removed by Worley following multiple unresolved observations. The new           
                       Hipparcos binary (AB), is almost certainly not the Burnham AB star,             
                       which was seen at 10", 250 deg, and had a Delta-M of 5.0.                       
                       AC: Burnham (BDS) notes 1874 observation made with 6-in telescope but           
                       says no 10" companion was found during subsequent searches with either          
                       the 36-inch or 40-inch.                                                 Bu_1906 
05022+3116 RUC   5     V402 Aur. Spectral type of resolved companion later than M5V.           Ruc2007 
05023-1932 LPM 201     NLTT 14407/14408                                                        Chm2004 
05023-5605 LDS 135     B is CPD-56@767.                                                                
                       Primary is SB1; Jenkins et al. (2010 A&A 515, 17) estimate P(Aa,Ab)             
                       ~6.5y, M2min=55 Mjup.                                                   Tok2014d
05023-6821 OGL 283     LMC125.1.12039 + LMC125.1.12040                                         Pli2012 
05024+1628 BPM 113     [PM2000]  207217 + [PM2000]  207230.                                    Gvr2010 
05024-6454 GLI  32     B is CPD-65@416.                                                                
05025+4105 MKT   6     zet Aur. Eclipsing binary (K4IB + B5V).                                         
                       This object was misidentified as rho Aur by McAlister (1978).           McA1978c
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Wright (1970).                                                          Wri1970 
                       Bennett et al. (1996) orbit is combined solution, using astrometry      MkT1996 
                       from the Mark III interferometer, spectroscopy from HST Goddard High            
                       Resolution Spectrograph, and published photometry to determine masses,          
                       radii, etc. Positions of component stars on theoretical H-R diagram             
                       are compared to current evolutionary models.                                    
                       Errors to individual measures are given as "error ellipses"; these              
                       values are tabulated below, together with filters used. The columns             
                       include date (BY), major and minor axes of the ellipse (in mas),                
                       ellipse orientation (deg), and filter effective wavelengths (nm):               
                            1989.7857   1.63    0.31    98.1   800,550,450                             
                            1989.7994   0.56    0.14    86.9   800,550,450                             
                            1989.8213   0.58    0.12    84.5   800,550,450                             
                            1989.8240   0.73    0.15    78.6   800,550,450                             
                            1989.8350   0.50    0.12    85.3   800,550,450                             
                            1989.9281   0.48    0.17    96.1   800,550,450                             
                            1989.9363   1.24    0.27    86.1   800,550,450                             
                            1990.7029   1.14    0.16   104.0   800,550,500                             
                            1990.8124   0.56    0.17    97.5   800,550,500                             
                            1990.8179   0.69    0.14    91.7   800,550,500                             
                            1991.7488   2.00    0.20   111.9   800,550,500                             
                            1991.7871   0.65    0.12    92.4   800,550,500                             
                            1991.8364   0.32    0.09    94.1   800,550,500                             
                            1991.9048   0.21    0.07    86.4   800,550,500                             
                            1992.0855   1.31    0.15    90.4   800,550,500                             
                            1992.0965   1.50    0.25    73.5   800,550,500                             
                            1992.7700   0.63    0.14    99.5   800,550,500                             
                            1992.7946   0.65    0.11    98.5   800,550,500                             
                            1992.7974   0.44    0.08   104.2   800,550,500                             
                            1992.8932   1.82    0.24   111.3   800,550,500                             
                            1992.9206   1.39    0.27    99.0   800,550,500                             
                            1992.9452   1.23   0.23    101.9   800,550,500                             
                       Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                       8.40 +/- 3.79 and 10.96 Msun, respectively.                             Mlk2012 
05025-2115 DON  91     Good period, indeterminate a/e/i, more obs needed!                      Hei1978c
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05027-3309 HJ 3718     B is CD-33@2076.                                                                
05028-4909 RST 120     AB: Physical/optical nature undefined.  Primary is eta 1 Pic.           Ehr2010 
           EHR   6     AC: Physical/optical nature undefined.                                  Ehr2010 
05028-7020 OGL 284     LMC121.6.34935 + LMC121.6.34941                                         Pli2012 
05029+1433 BPM 114     [PM2000]  208075 + [PM2000]  208110.                                    Gvr2010 
05031+4933 BU  315     ID uncertain. Listed as BD+49 1288 in ADS, but no obvious 10" pair at   A__1932a
                       those coordinates. X-coded measures of a 45" pair refer to a wide               
                       companion to BD+49 1288.                                                        
05031+2523 MSR   5     HBC 429 = V836 Tau.                                                     Msr2005 
                       Young member of Taurus-Auriga molecular cloud.                          Dae2015 
05031+2135 OCC 230     iot Tau.                                                                        
05031-6944 OGL 285     LMC120.6.45262 + LMC120.6.45347                                         Pli2012 
05033+2125 LAW  13     Ba,Bb: LSPM J0503+2122 = NLTT 14406. Law et al (2008) derive a          Law2008 
                       distance of 13.7 +6.5/-2.5 pc and a projected separation of                     
                       4.4 +2.3/-0.7 au. Estimated spectral types are M4.5 and M5.5.                   
                       Ba,Bb: LP 359-186. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.03           
                       and 0.16 +/- 0.01 Msun; a ~8.3 au.                                      Jnn2014 
05033-1722 B  2583     LPM 202. L 736-49.                                                              
05034+6027 S   459     bet Cam = 10 Cam. STTA 57 = H 6  36.                                            
05034-7104 OGL 286     LMC122.7.14740 + LMC122.7.14741                                         Pli2012 
05035+1449 BPM 115     [PM2000]  209034 + [PM2000]  208947.                                    Gvr2010 
05036+6305 STF 618     LDS 889. STTA 56. D is BD+62@721.                                               
                       AB: HJL  66.                                                            HJL1986 
05037-0232 J   307     Reality of BC is in doubt.                                                      
05037-6834 OGL 287     LMC118.6.42400 + LMC118.6.42472                                         Pli2012 
05038+1457 BPM 116     [PM2000]  209491 + [PM2000]  209477.                                    Gvr2010 
05039-6738 OGL 288     LMC124.1.32825 + LMC124.1.32850                                         Pli2012 
05042-6956 OGL 289     LMC120.7.16863 + LMC120.7.18028                                         Pli2012 
05043+4013 ES 1718     Espin incorrectly identified this pair as BD+40 1144 in 1919, but       Es_1919 
                       corrected this to +40 1158 in 1925. Error in transcribing to catalog;   Es_1925a
                       WDS designation originallyVIG   7 05041+4023, corrected when matched with      .
                       05043+4013TDS3056.                                                              
05043+2319 J  1816     POU 523.                                                                        
05043-6946 OGL 290     LMC120.6.17556 + LMC120.6.17583                                         Pli2012 
05044+6237 HU 1094     Stein measure 1901.3, 289@, 4.2", 9.5-9.9. For this position            A__1932a
                       Hussey finds no such pair.                                              Hu_1905b
05044-3529 JC    9     gam 1 Cae. The secondary is variable (IBVS 2736, 1985).                         
05044-6706 OGL 291     LMC115.8.111   + LMC115.8.177                                           Pli2012 
05045+1622 BPM 117     [PM2000]  210663 + [PM2000]  210510.                                    Gvr2010 
05045-2402 LDS3638     NLTT 14472/14466                                                        Chm2004 
05046+5852 STF 625     A,BC: H 2  53.                                                          MEv2010 
05047+7404 STT  89     Judged single by Hussey, Burnham, and Aitken, and not inserted in ADS.          
                       Rediscovered by Kuiper in 1935 (PASP 47, 230). Obvious in 1938.         Baz1942b
05047-0925 GAL 375     Object #161 in Gallo's original list.                                   Gal1914 
05047-2017 WHC   2     CPD-20@742.                                                                     
05049+1520 BPMA 10     [PM2000]  211239 + [PM2000]  211233.                                    Gvr2010 
05050-6740 OGL 292     LMC116.8.65    + LMC116.8.164                                           Pli2012 
05051+0608 HD 32662    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05053+6923 HJ 2244     B is BD+69@295.                                                                 
05054-6905 SKF1072     OGL 293. LMC119.5.40836 + LMC119.5.40603                                Pli2012 
05055-5728 SHY  22     HIP  23693 + HIP  23708.                                                        
05056+2304 STT  97     See long note in BDS. Single in 1889.                                   Bu_1906 
                       Recovered in 1976 by McAlister.                                         McA1978b
                       Primary is V1154 Tau, an Algol-type eclipsing binary, period 1.76788d.  Zas2011 
05056-7056 OGL 294     LMC122.3.16    + LMC122.3.89                                            Pli2012 
05057+0628 PAT  18     This pair is a spectroscopic binary with P ~ 2 yr, according to         Grf1988 
                       Griffin et al. (1988).                                                  Msn1993a
                       The spectroscopic solution of this 631.08-d pair determined by          Grf2012b
                       appears to be a closer pair.                                                    
                       Hipparcos identified the pair as a candidate for Hyades membership.     HIP1998 
                       It appears to match on grounds of proper motion and photometry but      Grf1988 
                       still appears slightly off based on radial velocities.                  Grf2013c
05061+5858 STFA 13     A: 11 Cam. B: 12 Cam =  BD+58@805. B is a spectroscopic binary,                 
                       P = 80.2d, spectrum K0III.                                                      
05062-6247 TOK  91     HIP 23742. ANDICAM confirms the 2MASS PSC photometry of B in K-band.            
                       B is well below the MS in the CMDs.                                     Tok2011a
05063+3738 ES 2339     Aka BRT2587 and ALI 528.                                                        
05063+3722 SEI  60     ALI 527.                                                                        
05064-1649 GAL 376     Object #164 in Gallo's original list. Aka POC9001.                      Gal1914 
05064-6700 OGL 295     LMC115.7.14821 + LMC115.7.14818                                         Pli2012 
05066-6830 OGL 296     LMC118.4.12    + LMC118.4.529                                           Pli2012 
05067+5136 BU 1046     9 Aur. A is a spectroscopic binary.                                             
           H 6  35     AC: H VI 35.                                                                    
05067+3748 SEI  61     ALI 529.                                                                        
05067+1427 GC 6239     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                       Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                       (2013). Periods match "tolerably well," other common elements less so.          
05067-6725 OGL 297     LMC116.6.12552 + LMC116.6.14377                                         Pli2012 
05068-0439 STF 642     66 Eri. A is a spectroscopic binary.                                            
05069-6718 OGL 298     LMC116.5.13203 + LMC116.5.16702                                         Pli2012 
05069-6728 OGL 299     LMC116.6.12514 + LMC116.6.14626                                         Pli2012 
05070+1650 HJ 3267     LDS1199. Possibly the same as STF 672.                                          
05070-3939 HJ 3725     B is CD-39@1789.                                                                
05071-7042 OGL 300     LMC121.1.12614 + LMC121.1.12789                                         Pli2012 
05074+2715 DOO  30     J 3259.                                                                         
05074+1839 A  3010     104 Tau.                                                                        
                       Two orbit solutions (Eggen 1956). Observations of this close pair       Egg1956 
                       are so scattered that both orbits are highly conjectural.                       
                       A measure on 1977.9196 was incorrectly attributed to ADS 3701 in                
                       McAlister & Hendry (1982); it actually belongs to ADS 4020.             McA1982b
                       Visual and speckle observations at 0".1 sep ruled out as spurious by            
                       constant RV (Duquennoy & Mayor 1991).                                   Duq1991 
                       Precise velocities are stable to better than 100 m/s over 388 days,     Nid2002 
                       so there are no "hot jupiters" and a 2-year period is excluded with     Tok2010b
                       high confidence.                                                                
                       104 Tau is a G4V dwarf at 16 pc resolved into equal components at 0.1"          
                       by R. Aitken in 1912. The WDS contains 16 resolutions of this pair.     A__1927a
                       Apart from Aitken himself, it has been resolved on multiple occasions           
                       by R.H. Wilson in 1934-1971, by W. Finsen (1953-1955) and by others,    WRH1941a
                       although in other instances those observers found it to be single.      Fin1953d
                       The measures suggest a near-circular orbit seen face-on with a semi-            
                       major axis on the order of 0.1" or 1.5 au. Assuming a mass sum of 2             
                       Msun, the orbital period should be around 1.3 yr; in fact, two orbits           
                       with periods 1.19 yr and 2.38 yr were published by Eggen (1956). This   Egg1956 
                       binary should be an easy target for speckle interferometry at 4-m               
                       telescopes. It was observed 10 times from 1976.9 to 1980.7 with                 
                       speckle and, surprisingly, found unresolved on all occasions,                   
                       excluding any short-period orbits. Later, however, two measures were            
                       made by the author at a 1-m telescope with a phase-grating                      
                       interferometer. The first resolution in 1984.8 at 0.04" was tentative   Tok1985 
                       (below the diffraction limit), but the second in 1985.7 was secure,     Tok1988 
                       being an average of two observations. It was followed by the speckle            
                       resolution at 4-m telescope in 1988.17, after which the pair            Mca1993 
                       disappeared again. It was found unresolved in 2012.                     Tok2012b
                       The star is well studied. Two statistical surveys of binaries within            
                       25 pc consider it to be single (Duquennoy & Mayor 1991; Raghavan et     Duq1991 
                       al. 2010). Heintz & Borgman (1984) state that measures cannot be        Rag2010 
                       fitted by any orbit and conclude: "Although this alleged visual binary  Hei1984i
                       (ADS 3701) has three published orbits, it is probably spurious".                
                       Several independent RV studies have shown that this star is not a               
                       spectroscopic binary. Precise RVs measured by Nidever et al. (2002)     Nid2002 
                       are stable to better than 100 m s-1 over 388 days, excluding orbital            
                       periods from one to two years with high confidence. Data with lower             
                       precision show a constant RV of +21 km/s over many years (Duquennoy &           
                       Mayor 1991; Abt & Willmarth 2006; Raghavan et al. 2010). The star is    AbH2006 
                       located about 1m above the main sequence, supporting the thesis of an           
                       equal-component binary. If the orbit is seen face-on, the RV variation          
                       would be small, especially if the components are of equal brightness            
                       (blended lines move in opposite directions, the centroid stays                  
                       constant). However, the lines in this star remain narrow and the                
                       speckle non-resolution during 3.8 yr firmly excludes a face-on orbit.           
                       Remember that 104 Tau is bright (no identification errors possible)             
                       and that the components are supposedly equally bright, hence easy to            
                       resolve by speckle. If this star is single (as everything seems to              
                       suggest), we cannot dismiss its multiple resolutions with micrometer,           
                       eyepiece interferometer, and speckle as spurious; occasional image              
                       doubling (or at least elongation) must be real.                         Tok2012b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 0.65 +/- 0.09, 2.12, and 1.02 Msun, respectively.             Mlk2012 
                       In the WDS summary line this carries an "X" code (non double), but              
                       still retains all the historical measures.                                      
05074-6641 OGL 301     LMC115.4.42    + LMC115.4.508                                           Pli2012 
05076+1631 BPM 118     [PM2000]  215983 + [PM2000]  215874.                                    Gvr2010 
05076+0928 STT 561     AB: 16 Ori. A is a spectroscopic binary.                                        
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
05076-7018 OGL 302     LMC121.3.45664 + LMC121.2.45533                                         Pli2012 
05076-8852 HJ 4047     1900: 06 56.4.                                                                  
05078+3024 JOY   5     RW Aur, prototype of its class.                                         Her1962 
05078+1622 BPM 119     [PM2000]  216289 + [PM2000]  216084.                                    Gvr2010 
05078-0505 BUP  74     bet Eri = 67 Eri = Cursa. STF 647.                                              
05079+6849 HJ 1152     BDS 2479 has an error of 30', making it identical with HJ 1152                  
                       (Van Biesbroeck).                                                       VBs1914 
05079+2142 S   466     105 Tau. B is BD+21@764. A is a spectroscopic and occultation binary.           
                       H 6 105.                                                                MEv2010 
05079+1519 BPM 120     [PM2000]  216579 + [PM2000]  216575.                                    Gvr2010 
05079+0830 STT  98     14 Ori. One component, probably the primary, is SB; the RV range in the         
                       combined light is 22 km/s.                                                      
                       According to Eggen, the system shares common proper motion with         Egg1963 
                       ADS 3712 = STF 643 (mags. 9.5-9.5, 3", K2), which is 6' distant.                
05080+3703 HJ 3265     AB: SEI  69.                                                            Nsn2017a
                       AC: SEI  70.                                                            Nsn2017a
05080-2648 MUG  13     Spectral type of comoving secondary estimated as M4-5, mass 0.17 Msun.  Mug2014 
05080-6934 OGL 303     LMC120.4.70309 + LMC120.4.70525                                         Pli2012 
05081+3701 COU1530     Also known as HDS 673.                                                          
05081+3658 HJ 3266     SEI  73.                                                                Nsn2017a
05081+3609 HJ  692     SEI  71.                                                                Nsn2017a
05081+2416 EDG   2     103 Tau. A is a spectroscopic and occultation binary.                           
           H 5 114     H V 114.                                                                        
05083+7538 JNN 266     G 248-32. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.15           
                       +/- 0.03 Msun; a ~3.1 au.                                               Jnn2014 
05080+2214 ARU   2     Mistakenly added to WDS as BD+22 0834; however, Argue et al. measure    Aru1984 
                       was of AGK3 +22 0834 = BD+22 1589 = 07085+2159 OCC 337.                         
05083-0840 STF 649     AB: H 4  43 = H N  46.                                                  MEv2010 
05084+5525 GC 6249     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05085+1418 LDS5662     LDS6166.                                                                        
05085-1036 GAL 377     Object #165 in Gallo's original list.                                   Gal1914 
05085-4113 HJ 3728     NLTT 14574/14573                                                        Chm2004 
                       HIP 23926. B = HIP 23923. A is above the MS, evolved (despite sp. type          
                       G3V). The pair was observed with NICI in 2010. Both A and B have large          
                       PM, PM(A)=(-77,+284). The original Hipparcos parallax of B is 8.5mas,           
                       obviously wrong. IRAS source.                                           Tok2011a
                       Moutou et al. (2011 A&A 527, A63): exoplanet around A, P~2800d +drift   Tok2014d
05085-7058 OGL 304     LMC114.6.224   + LMC114.6.480                                           Pli2012 
05087+3703 SEI  78     ALI 302.                                                                        
05087+1251 BPM 121     [PM2000]  218040 + [PM2000]  218004.                                    Gvr2010 
05087-6846 MLO  13     AC: Identification uncertain.                                                   
05088-6800 OGL 305     LMC117.3.18237 + LMC117.3.18886                                         Pli2012 
05090+1238 BPM 122     [PM2000]  218603 + [PM2000]  218372.                                    Gvr2010 
05092-6701 OGL 306     LMC115.2.14607 + LMC115.2.14813                                         Pli2012 
05093+0950 BUP  75     13 Ori. Hyades vB 130.                                                          
                       Two CPM companions with rho = 88".6 and rho = 168".0, both outside              
                       our detection window.                                                   Msn1993a
05094-6857 OGL 307     LMC111.5.43680 + LMC111.5.44857                                         Pli2012 
05096+2947 STTA 61     HJL1040.                                                                HJL1986 
                       SHY 474. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       AB: Primary is SB2, P=1469.4d (Halbwachs et al. 2012)                   HJL2012b
05097+1536 STT  99     15 Ori. Round (Hussey). May not be double.                                      
05097-7009 OGL 308     LMC113.5.47798 + LMC113.5.47799                                         Pli2012 
05098+2802 BU 1047     BC: Van Biesbroeck in 1953 noted "no evidence of change in 65 years."           
                       However, the pair is now apparently in rapid motion in a highly-                
                       inclined orbit.                                                         Wor1967b
                       BC. The star was noted as a spectroscopic binary by Griffin et          Grf1988 
                       al. (1988).                                                                     
                       Hipparcos identified the pair as a non-Hyades member, however, the      HIP1998 
                       results invesigating proper motion, photometry and radial velocity      Grf1988 
                       yield a more ambiguous finding. The jury is still out!                  Grf2013c
           STF 645     A,BC: HJL  67.                                                          HJL1986 
                       A,BC: H 3  90.                                                          MEv2010 
05099-6715 OGL 309     LMC116.4.13354 + LMC116.4.13836                                         Pli2012 
05100+4009 ES  169     Aka BRT 112.                                                                    
05100+3754 SEI  81     ADS 3729a.                                                                      
05100+1054 J   323     A is probably variable.                                                 J__1952 
05100-0704 STF 651     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
05100-6722 OGL 310     LMC108.6.14    + LMC116.3.15651                                         Pli2012 
05101+2733 BGH  21     NLTT 14576/14572                                                        Chm2004 
                       HJL1041.                                                                HJL1986 
                       SHY 175. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       Secondary is SB1, P=2273.8d (Halbwachs et al. 2012)                     HJL2012b
05101-0204 BAL 296     1deg error in IDS led to similar error in WDS designation.                      
05101-2341 WSI 121     Both 2MASS J05100427-2340407 and J05100488-2340148 are binaries in the          
                       AstraLux images, so since they are separated by only 27" on the sky             
                       and have very similar proper motions (e.g. Roser et al. 2010), this is  Rsr2010 
                       likely a quadruple system in reality. Common proper motion remains to           
                       be confirmed for both of the close components.                          Jnn2012 
05101-6929 OGL 311     LMC111.8.8839  + LMC119.8.34937                                         Pli2012 
05101-7008 OGL 312     LMC113.5.48001 + LMC113.5.48018                                         Pli2012 
05102+1400 S   468     Also known as STF 650.                                                          
05102+0439 GWP 650     This is also known as V1396 Ori (ZZ Cet type var).                              
05103+3718 STF 644     One component is a spectroscopic binary.                                        
                       AB: H 1  45.                                                            MEv2010 
                       AB: Additional notes may be found in van den Bos (1963).                B__1963b
05103-0736 A   484     Position angles uncertain but near 130@-310@.                                   
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.20 +/- 0.18, 2.28, and 1.10 Msun, respectively.             Mlk2012 
05104+3741 SEI  84     Also known as ALI 531.                                                          
05105-1854 HJ 3727     CPD-19@760.                                                                     
05108-6716 OGL 313     LMC108.5.27    + LMC108.5.171                                           Pli2012 
05108-6740 OGL 314     LMC108.8.34    + LMC108.8.462                                           Pli2012 
05111+3718 BLL  13     B is BD+37@1072.                                                                
05112-0833 RUC  18     Multiple system including contact binary ER Ori. Pribulla & Rucinski            
                       (2006) estimate the mass of the contact pair at 2.510 Msun and the      Pbl2006 
                       minimum mass of the wider component at 0.93 Msun.                               
05113-6707 OGL 315     LMC107.8.492   + LMC107.8.1389                                          Pli2012 
05114-0101 BAL 297     Duplicity suspected by Baillaud but no measure.                         Bal1943 
05115+5305 HJ 2251     HJ gives position angle as 319.9@.                                              
05115-5519 HJ 3738     B is CPD-55@759.                                                                
05115-6753 OGL 316     LMC109.5.9247  + LMC109.5.9566                                          Pli2012 
05117+0031 HU   33     One component is a spectroscopic binary. Variable, V1085 Ori.                   
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 5.26 +/- 4.75, 9.35, and 2.57 Msun, respectively.             Mlk2012 
05119+3544 HJ  358     SEI  92.                                                                Nsn2017a
05119-0907 BUP  76     B is BD-09@1093.                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
05119-4253 HJ 3734     LDS 137.                                                                        
05119-6830 OGL 317     LMC110.5.14459 + LMC110.5.14649                                         Pli2012 
05120+0650 STTA 62     B is BD+06@865.                                                                 
                       Pair appears in an appendix list, not part of the discoverer's regular          
                       numbering sequence.                                                             
05121-6511 TOK  92     HIP 24221.                                                              Tok2011a
                       A is SB without orbit, dRV=56.7                                         Nrd2004 
05123-1152 STF 655     iot Lep = 3 Lep                                                                 
                       AB: H 3  67.                                                            MEv2010 
05123-6708 LDS 140     Aka MLO  15.                                                                    
05126-1727 S   470     B is BD-17@1046.                                                                
05130+1242 BPM 123     [PM2000]  226150 + [PM2000]  226362.                                    Gvr2010 
05130-6941 OGL 318     LMC112.4.1006  + LMC112.4.1258                                          Pli2012 
05130-7028 JNN  32     There is a companion to 2MASS J05130132-7027418 in the AstraLux images          
                       which has a brightness and color that is consistent with a physical             
                       companion. It counts as an unconfirmed binary here, since it has not            
                       yet been tested for common proper motion.                               Jnn2012 
05131-5959 HJ 3743     Large parallax error in HIP! Primary is possible SB.                    Tok2014d
05133+0252 STF 654     rho Ori = 17 Ori. A is long-period spectroscopic binary, P = 1031.4d.           
                       A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Bertiau (1957).                                                         BFC1957 
                       AB: H N  21.                                                            MEv2010 
05134+3829 CHR 256     mu Aur = 11 Aur. Hipparcos stochastic double solution.                          
05134+2411 POU 586     POU 588.                                                                        
05134+0341 TOK 211     The 1".25 companion discovered with NICI is hardly the one that                 
                       produced the acceleration of 17 mas yr-2.                               Tok2012a
05135+1608 BPM 124     [PM2000]  227301 + [PM2000]  227493.                                    Gvr2010 
05135+0158 STT 517     Star C (mag. 13, 7") may be physical.                                           
                       Trajectory appears quasi-linear.                                        Mlr1956a
05135-5534 HJ 3742     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
05136-7025 OGL 319     LMC113.3.8348  + LMC113.3.9695                                          Pli2012 
05137-0856 MLL   2     Aka BRT3264.                                                                    
05138-1641 GAL 378     Object #171 in Gallo's original list.                                   Gal1914 
05139+3958 HU 1100     ES 280.                                                                         
                       J  3306.                                                                Nsn2016 
05139-5648 HJ 9001     Previously known as HJ 5450a.                                                   
05140+5126 HU  821     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
05140-6827 OGL 320     LMC110.4.6684  + LMC110.4.7756                                          Pli2012 
05142+2535 BRT3263     Originally published as BRT 136.                                        Brt1928 
05142-6701 OGL 321     LMC107.2.166   + LMC107.2.193                                           Pli2012 
05143+6949 STF 638     H 2  92.                                                                MEv2010 
05143+1953 KIR   1     AB. Using data from 2MASS and IRTF, Kirkpatrick et al (2001) derive     Kir2001b
                       spectral types K4V and M6V, conclude is probably a physical pair with           
                       separation 225 au.                                                              
05143-1550 GJ 193      The acceleration is due to the 2.2 yr SB with estimated axis of 55 mas          
                       and q > 0.14. The companion is too faint and close to be resolved with          
                       NICI or speckle. The system is triple with a faint common-proper-motion         
                       (CPM) companion at 14".6.                                               Tok2012a
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by Nidever            
                       et al. (2002). They derived component masses 0.98 and 0.22 Msun and     Nid2002 
                       an estimated semimajor axis of 57.81 mas.                               Ren2013 
05143-1723 FEN   3     Aka OL  127.                                                                    
05145+1707 BPM 125     [PM2000]  229086 + [PM2000]  229142.                                    Gvr2010 
05145-0812 STF 668     bet Ori = 19 Ori = Rigel. The companion is a spectroscopic binary and           
                       suspected visual double, although it remains unconfirmed. Magnitudes            
                       of B and C very uncertain. Changed from IDS values (10.4 for B, C, and          
                       BC). AD pair first mentioned by Mitchel in 1846 (Sidereal Messenger,            
                       May 1847) but no astrometry included.  See extensive notes by Burnham.  Bu_1906 
           bet Ori     1975.631: Possible binary (450 and 656 nm).                             Bla1977a
                       1975.636: Possible binary (400, 500, 600, and 750 nm).                  Bla1977a
           STF 668     A,BC: H 2  33.                                                          MEv2010 
05145-6957 HJ 3754     B is CPD-70@376.                                                                
05146+7628 HU 1097     B may be variable.                                                              
05147+3707 SEI 115     Primary not seen on POSS plate; may be flaw on AC Potsdam plate.                
05147-0704 STF 667     H 1  54.                                                                MEv2010 
05149+3309 HJ  694     Aka HJ  361.                                                                    
05150+3813 BRT2208     ALI 788.                                                                        
05150+0108 OL   95     The south following of two faint stars.                                 B__1963b
05151-3639 HJ 3740     B is CD-36@2133.                                                                
05152+0826 STF 664     Same as CHE  79. Verified by DAL04.                                             
05152-1404 LDS3648     Luyten gives a separation of 130", but this appears to be a             Luy1978 
                       typographical error; if identification is correct, rho ~13"; this               
                       secondary corresponds to a high proper motion CPM companion.                    
05153+4710 A  1031     A 1998.8317 measure by Mason et al. (2001) was actually of STT 98.      Msn2001b
05154+3241 STF 653     14 Aur. A is the Delta Scuti-type variable KW Aur, and is also a                
                       spectroscopic binary.                                                           
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AC: SEI 124.                                                            Nsn2017a
                       AC: H 4  19.                                                            MEv2010 
05154-6700 OGL 322     LMC107.2.14205 + LMC107.3.195                                           Pli2012 
05155+2217 COU 158     108 Tau.                                                                        
05155-7001 OGL 323     LMC112.1.64694 + LMC112.1.64780                                         Pli2012 
05156+7857 LDS1604     NLTT 14588/14589                                                        Chm2004 
05156-6139 JSP9002     Previously known as JSP  71a.                                                   
05156-7049 OGL 324     LMC105.5.15    + LMC105.5.761                                           Pli2012 
05157+3738 SEI 126     AC: WLY  18AC.                                                          Nsn2017a
05157-4927 GC 6457     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05159+3425 ES  170     AB: SEI 130.                                                            Nsn2017a
05160-7002 OGL 325     LMC103.8.32853 + LMC103.8.32837                                         Pli2012 
05160-7214 JAO   3     Also known as LHS1749. Parallax = 46.08 +/- 1.40 mas.                   Rdl2010 
05162-1121 CHR 225     It in uncertain whether the pair resolved here is the known G8III+A0V           
                       composite spectrum binary (Hoffleit & Warren 1991). The small apparent  Hof1991 
                       change in theta over the 4-year span between observations does not              
                       appear consistent with our estimated period of ~15 or so years;                 
                       however, the magnitude difference between the components is small, so           
                       we are unable to rule out a 180 deg quadrant flip or perhaps an                 
                       eccentric orbit.                                                        Hrt1996b
                       Docobo et al. (2014) use the spectroscopic elements of Carquillat &             
                       Prieur (2007), together with speckle data and the Hipparcos parallax,   Crq2007 
                       to derive the remaining orbital elements. The resulting masses are              
                       1.92 +/- 0.26 and 2.50 +/- 0.29 Msun.                                   Doc2014h
05163+3419 TRN  17     Aa,Ab is an AO artifact as per Turner and Roberts.                      Trn2010 
                       Aa,Ab: Additional notes may be found in Turner et al. (2008).           Trn2008 
           SEI 136     AB: AE Aur. Nova remnant, probably not double.                                  
                       The companion indicated by the Potsdam Astrographic catalogue is non            
                       existing. There's the remark: Very doubtful.                            VBs1960 
05164-1531 GAL 172     J  1468.                                                                J__1962a
05164-7124 OGL 326     LMC106.5.13    + LMC106.5.66                                            Pli2012 
05165+3635 SEI 137     SEI 138.                                                                        
05165-2106 DON  97     Variable dm?                                                            Hln1965 
05165-6947 OGL 327     LMC103.6.11600 + LMC103.6.11652                                         Pli2012 
05167+4600 ANJ   1     Aa,Ab: 13 Aur = alp Aur = Capella.  Composite spectrum; G5IIIe+G0III.           
                       AKA "The Interferometrist's Friend."                                            
                       Separations from Anderson (1920) have been modified as described in     AnJ1920 
                       Merrill (1922).                                                         Mrr1922 
                       Measures of Kulagin made by a transit interferometer; quadrants were            
                       flipped for all his measures.                                           Kul1970 
                       See discussion in Labeyrie et al. (1974).                               Lab1974 
                       Combined spectroscopic/interferometric orbit by Heintz (1974):          Hei1974a
                       P = 104.0237 d, a = 0.0547", eccentricity neligibly small. Ascending            
                       node revised according to Heintz's astrometry                                   
                       1969.1348: This position angle was incorrectly published as 303.0               
                       degrees in Balega & Tikhonov (1977).                                    Bag1977 
                       1978.915, 1978.929, 1979.082: Observations on these three dates                 
                       overlap in two papers by Koechlin et al. (1979, 1983), with only        Koe1979 
                       slight changes.  Values from the later paper are given in the catalog.  Koe1983 
                       1984.9309, 1985.1062, 1985.1994: Estimates of the position angle and            
                       angular separation are deduced from the elongation of the central               
                       speckle peak in the autocorrelation.                                    Bnu1986 
                       Colors and spectral types determined by speckle photometry are                  
                       given by Bagnuolo & Sowell (1988).                                      Bgn1988 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Observations by Hummel et al. (1994) were made through narrow band      MkT1994 
                       filters centered at 800, 550, and 450 nm. Colors were derived from all          
                       1988-1992 data, so are listed at the mean epoch of 1991.9.  This paper          
                       also includes a new orbit. Finally, errors are given as "error                  
                       ellipses"; these values are tabulated below.  Columns include date              
                       (BY), major and minor axes of the ellipse (in mas), and ellipse                 
                       orientation (in degrees).                                                       
                            1988.7973     0.95     0.11      96.                                       
                            1988.8000     0.42     0.03      93.3                                      
                            1988.8028     0.22     0.03      85.7                                      
                            1988.8055     0.15     0.02      88.2                                      
                            1990.9411     0.09     0.02      86.6                                      
                            1990.9548     0.13     0.05      88.6                                      
                            1991.7159     0.73     0.08     124.1                                      
                            1991.7214     0.37     0.06     179.6                                      
                            1991.7241     0.23     0.05     156.5                                      
                            1991.7871     0.07     0.01      93.7                                      
                            1991.8364     0.07     0.02      91.6                                      
                            1991.8665     0.04     0.01      94.5                                      
                            1991.8857     0.06     0.02      88.4                                      
                            1991.8939     0.10     0.05     149.3                                      
                            1991.9021     0.16     0.05      77.9                                      
                            1991.9733     0.10     0.03      87.6                                      
                            1991.9870     0.09     0.02      77.5                                      
                            1992.0006     0.50     0.07      83.0                                      
                            1992.0417     0.24     0.05      73.4                                      
                            1992.0445     0.09     0.02      83.8                                      
                            1992.0691     0.25     0.05      74.6                                      
                            1992.0855     0.22     0.02      93.5                                      
                            1992.0965     0.10     0.02      78.5                                      
                            1992.7399     0.33     0.05     111.1                                      
                            1992.7426     0.42     0.04     118.5                                      
                            1992.7454     0.21     0.06     110.6                                      
                            1992.7481     0.40     0.09     121.2                                      
                            1992.7508     0.62     0.08     121.3                                      
                            1992.7536     0.71     0.16     103.9                                      
                            1992.7563     0.76     0.12     121.9                                      
                            1992.7755     0.05     0.01     105.9                                      
                            1992.8357     0.19     0.02     118.1                                      
                            1992.8658     0.09     0.04      78.1                                      
                            1992.8658     0.14     0.04      91.8                                      
                            1992.8686     0.09     0.02      69.5                                      
                            1992.8686     0.14     0.07      92.9                                      
                            1992.8823     0.07     0.02      88.8                                      
                            1992.8932     0.11     0.02     116.4                                      
                            1992.9206     0.43     0.07      98.8                                      
                            1992.9452     0.15     0.03     113.0                                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1994).                                                   MkT1994 
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       Branham (2008) derives combined interferometric/spectroscopic orbit,    Bnh2008 
                       using a semidefinite programming technique. The resulting masses are            
                       3.049 +/- 0.513 and 2.569 +/- 0.432 Msun; he also determines a value            
                       for the parallax of 74.85 +/- 1.53 mas.                                         
                       Aa,Ab: Following an extensive review of historical spectroscopic and            
                       astrometric measurements of Capella, Torres et al. (2009) derived a     Trr2009 
                       new combined-solution orbit, assuming a circular orbit. They determined         
                       an orbital parallax of 76.67 +/- 0.17 mas (distance 13.042 +/-                  
                       0.028 pc), an age of 540-590 Myr, and the following physical                    
                       parameters for the two components:                                              
                       Mass (Msun):       2.466 +/- 0.018     2.443 +/- 0.013                          
                       Radius (Rsun):     11.87     0.56      8.75      0.32                           
                       Teff (K):          4920      70        5680      70                             
                       Luminosity (Lsun): 79.5      4.8       72.1      3.6                            
                       Mv (mag):          0.315     0.017     0.186     0.016                          
                       Aa,Ab: Weber & Strassmeier (2011) derived new spectroscopic elements,   WbS2011 
                       assuming the period determined by Torres et al. (2009). The new         Trr2009 
                       solution yielded masses of 2.573 +/- 0.009 and 2.488 +/- 0.008 Msun.            
                       Aa,Ab: A combined solution by Torres et al (2015) yields the following  Trr2015 
                       physical parameters for Aa and Ab:                                              
                           mass (Msun):       2.5687 +/- 0.0074     2.4828 +/- 0.0067                  
                           Teff (K):          4970       50         5730       60                      
                           Radius (Rsun):     11.98      0.57       8.83       0.33                    
                           log g (cgs):       2.691      0.041      2.941      0.032                   
                           Luminosity (Lsun): 78.7       4.2        72.7       3.6                     
                           a(AU):                      0.74272 +/- 0.00069                             
                           Distance (pc):              13.159      0.015                               
                           Age (Myr):                  590-650                                         
                           [Fe/H}:                     -0.04       0.06                                
           HJ 2256     AF: H VI 30.                                                                    
                       AF: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           SHY  23     AM: HIP  24608 + HIP  26779.                                                    
           SHY  23     AN: HIP  24608 + HIP  26801.                                                    
                       MN is 05413+5329AB.                                                     Dam2017i
           ST    3     Capella HL, the distant (723") double companion to Capella with                 
                       common proper motion. A premature orbit has been computed.                      
           HJ 2256     AF: H 6  30.                                                            MEv2010 
05171-7128 OGL 328     LMC106.6.13434 + LMC106.6.13435                                         Pli2012 
05172+3747 HJ 3271     SEI 149.                                                                Nsn2017a
05172+3320 STF 666     H 2  48.                                                                MEv2010 
05173+5335 ES 2610     A is R Aur, variable 6.5-13.8. B is BD+53@880, F8V.                             
05174+3500 SEI 155     J   184.                                                                Nsn2016 
05175+2008 STF 674     A is the Algol-type binary CD Tau, eclipsing SB2, P = 3.44d.                    
                       AB has estimated period of 11000y.  B has spectral type dK2.            Tok2006 
05175-3454 KIR  12     omi Col.                                                                        
05175-7031 OGL 329     LMC104.7.15822 + LMC104.7.16197                                         Pli2012 
05176-0651 H 5  25     tau Ori = 20 Ori. H V 25.                                                       
05176-1513 S   473     B is BD-15@1000.                                                                
05177-1809 SEE  49     See's 1897 angle should read 196.7.                                     B__1953a
05179+3724 SEI 162     The discrepant measure by Scheiner (1908) is apparently due to a        Sei1908 
                       typographical error in the AC Potsdam Astrographic Catalog, as the              
                       correct position of the secondary is off by exactly 24" in dec.                 
                       Matches to other AC plates from 1929 and 1930 agree well with the               
                       Aladin image, as well as more recent observations.                              
05181-3402 TOK  61     Aa,Ab: Estimated masses 1.04 and 0.15 Msun; sep 43.6 au, period 260 y.  Tok2010c
           HJ 3745     HIP 24711. B = HIP 24712.                                               Tok2011a
05181-7654 TOK 663     Resolved using ANDICAM2. B is not in PPMX.                              Tok2014d
05182+3739 BU 9002     Previously known as BU 885 1/2.                                                 
05182+3322 STT 103     16 Aur. A is a long-period spectroscopic binary. P = 434.8d.                    
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Christie (1936).                                                        Crs1936 
05182-6809 OGL 330     LMC102.7.16903 + LMC102.7.16902                                         Pli2012 
05183-7143 OGL 331     LMC106.7.13197 + LMC106.7.13239                                         Pli2012 
05184-3108 LDS3651     NLTT 14861/14860                                                        Chm2004 
05185+3800 SEI 171     ALI 536.                                                                        
05185-6933 OGL 332     LMC103.5.107911+ LMC103.5.110011                                        Pli2012 
05186+4020 SMA  50     IDS and old-WDS location in error. Nothing at 05194+4020 (Heintz),      Hei1987a
                       but probably identical to a pair at this location.                              
                       SLE  64.                                                                        
05187+3331 ES   59     A pair found many years ago with the 3in refractor. The distant double          
                       comes was found with the 13in reflector at the Oxford Univ. Obs. and            
                       the comes C with the 17 1/4. AB was measured by Burnham in 1882.        Es_1902a
05187+0359 STF 682     BAL 2143.                                                                       
                       HIP 24774. The B-companion could possibly be a semi-resolved binary.            
05187-7122 OGL 333     LMC106.5.14568 + LMC106.5.14749                                         Pli2012 
05188+5250 STF 657     Same as STF 660.                                                                
05188-1808 SEE  50     A is a spectroscopic binary.                                                    
05189-6810 OGL 334     LMC102.7.22886 + LMC102.7.22769                                         Pli2012 
05189-6948 OGL 335     LMC103.6.38675 + LMC103.3.2                                             Pli2012 
05189-6957 OGL 336     LMC103.7.31356 + LMC103.7.31945                                         Pli2012 
05190-2829 BUG   8     2MASS J05185995-2828372                                                         
                       Estimated spectral types are L6: + T4:, effective temperatures ~1600            
                       and ~1330 K. Masses are estimated at 0.042-0.077 and 0.031-0.074 Msun,          
                       and the orbital period (assuming the semi-major axis = 1.26 * rho) is           
                       ~10yr.                                                                  Bug2006a
05191+4006 STFB  3     lam Aur = 15 Aur                                                                
                       AC and AD: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
                       AD: H 5  22.                                                            MEv2010 
                       DE: H 5  88AC. = H V 88.                                                Dam2017i
05191-6803 OGL 337     LMC102.3.50    + LMC102.3.51                                            Pli2012 
05192+3548 SEI 179     A is an irregular variable, V348 Aur.                                           
05192+2008 STF 680     Spectrum composite; G8II-III+G1IV-V (BSC).                                      
05192+1212 BPM 126     [PM2000]  237882 + [PM2000]  238008.                                    Gvr2010 
05192-0304 A    53     HIP 24819. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: NLTT 14867/14868                                                    Chm2004 
05192-1800 FEN   4     Aka ARA 331.                                                                    
05193-1045 STF 688     BDS 2665, H III 94 same star. B is BD-10@1152.                                  
                       H 3  94.                                                                MEv2010 
05193-1831 S   476     AB: B is BD-18@1056.                                                            
05193-2845 LDS3653     NLTT 14889/14887                                                        Chm2004 
05194+3359 HO   18     18 Aur.                                                                         
05196-0107 BAL 303     RST 4779.                                                                       
05197+3614 WEI   8     AB: SEI 189.                                                            Nsn2017a
05197+3526 SEI 186     SEI 187.                                                                        
05197+2511 STF 679     HJL  68.                                                                HJL1986 
05199-0723 JNN  34     2MASS J05195412-0723359 and J05195513-0723399, both from the Riaz et            
                       al. (2006) sample, are separated by only 16" and have comparable        Ria2006 
                       estimated distances (59 and 70 pc), as well as quite similar proper     Rsr2010 
                       motions (e.g. Roser et al 2010), and thus likely form a physical pair.  Jnn2012 
05200+4546 GIC  54     G096-032/G096-031.                                                              
                       NLTT 14857/14855                                                        Chm2004 
05201+3236 SEI 194     J 1089.                                                                         
05201-7100 OGL 338     LMC105.3.5578  + LMC105.3.5594                                          Pli2012 
05202-6810 OGL 339     LMC102.2.30    + LMC102.2.37                                            Pli2012 
05203+2510 STF 683     Chevalier's measure was incorrectly identified as STF 694, so never     Che1910 
                       added to the WDS; correct ID was determined based on his coordinates.   Hrt2012b
05204-0802 STF 692     AB,C: H 4  87.                                                          MEv2010 
05206-1031 GAL 379     Object #176 in Gallo's original list.                                   Gal1914 
05206-7024 OGL 340     LMC104.3.8821  + LMC104.3.9924                                          Pli2012 
05207+5848 GIC  46     G191-030/G191-029 or GJ 3342A/3343B.  A 1hr typographical error in RA           
                       led to this pair being initially entered in the WDS as 04205+5852.              
                       LDS6183.                                                                        
05207+3726 SEI 201     Fullerton et al. (1991) describe profile and radial velocity            Ful1991 
                       variations that suggest that this star is a short-period, radial                
                       pulsator.  Underhill (1995 PASP 107, 513) also discusses radial                 
                       velocity measurements.                                                  Msn1998a
05209+2402 STF 686     POU 650.                                                                        
05210+7113 HJ 1154     The ADS incorrectly added the CD component of 05061+5858 (STFA 13) as   A__1932a
                       an additional component of this pair.                                           
05213-6835 OGL 341     LMC101.3.42767 + LMC101.3.42931                                         Pli2012 
05217+3322 LDS6184     NLTT 14919/14920                                                        Chm2004 
05217+1854 KU   87     B is BD+18@832.                                                                 
05217+1240 STT 105     Not seen since 1971. Needs speckle.                                             
                       Additional notes may be found in van den Bos (1963).                    B__1963b
05218+3231 HU  614     A is the Mira-type variable UV Aur.                                             
05218-2446 HJ 3752     Spectrum composite; G7II-III+A7IV-V.                                            
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
05219+4203 AG  314     B is BD+41@1166.                                                                
05222+2008 J   144     OL  204.                                                                        
05222+0524 STT 106     HJL  69.                                                                HJL1986 
05223-7109 OGL 342     LMC105.2.15955 + LMC105.2.16304                                         Pli2012 
05224-6934 OGL 343     LMC103.4.118812+ LMC103.4.118814                                        Pli2012 
05225-7044 OGL 344     LMC105.4.45008 + LMC105.4.45010                                         Pli2012 
05226+7914 STF 634     STTA 60.  B is BD+79@168.                                                       
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
05226+0236 A  2641     Only elements P and T have been amended by Starikova (1978) from the    Sta1978c
                       orbit of Baize (1957).                                                  Baz1957b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.27 +/- 0.35, 1.39, and 0.95 Msun, respectively.             Mlk2012 
05228+4755 GIC  55     G096-035/G096-034. See Allen et al. (2000) for information on           AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
                       NLTT 14943/14940                                                        Chm2004 
05228+3658 SEI 220     AB: SEI 221.                                                                    
05228+0333 STF 696     23 Ori. B is BD+03@872.                                                         
                       H 4  84.                                                                MEv2010 
05229-4219 TOK  93     HIP 25148. A is SB without orbit, dRV= 3.7                              Nrd2004 
                       and also an astrometric binary (Makarov & Kaplan 2005).                 Mkr2005 
                       The companion at 66 mas is at the diffraction limit, the NICI                   
                       measurement is not accurate. The pair can be resolved by speckle.       Tok2012a
                       Aa,Ab: The tentative resolution at Gemini om 2011.70 is confirmed here,         
                       with 25deg of direct motion.                                            Tok2013b
05229-7143 OGL 345     LMC165.7.83    + LMC165.7.149                                           Pli2012 
05230-0850 JNN  36     This star has been classified as a probable T Tau star in Alcala et             
                       al. (1996 A&AS 119, 7).                                                 Jnn2012 
05230-1613 GAL 380     Object #177 in Gallo's original list.                                   Gal1914 
05231+3110 STF 691     B is BD+31@947.                                                                 
                       SEI 227.                                                                Nsn2017a
05231+0103 STF 700     H 1  75.                                                                MEv2010 
                       V1804 Ori, Algol (EA) type eclipsing binary, P = 2.22878 d.             Zas2011 
05232-2642 HIP  25180  Large RV amplitude (31.7 km s-1) hints at short orbital period, but             
                       only small dmu = 3 mas yr-1 is detected by Hipparcos. Triple?           Tok2012a
05232-3145 HJ 3757     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
05232-7112 OGL 346     LMC164.8.18917 + LMC164.8.18916                                         Pli2012 
05233+3445 SEI 229     FOX 140.                                                                        
05233+3409 MLB1037     HJ  363.                                                                        
05233-0825 STF 701     H 2 102.                                                                MEv2010 
05234-7128 OGL 347     LMC165.6.20315 + LMC165.6.20368                                         Pli2012 
05235+5733 BU 1393     16 Cam. A is a spectroscopic binary.                                            
05235+1602 STF 697     B is BD+15@804.                                                                 
05237+6841 GIC  56     LDS5192. G248-038/G249-007.                                                     
05237+3606 SEI 233     SEI 234.                                                                        
05238-7018 OGL 348     LMC163.6.62323 + LMC163.6.62352                                         Pli2012 
05239+1743 BPM 127     [PM2000]  247544 + [PM2000]  247826.                                    Gvr2010 
05239-0052 WNC   2     A,BC: Primary is SB2, P=22.58d                                          Tok2014d
           A   847     BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.74 +/- 0.51, 2.47, and 1.13 Msun, respectively.  Mlk2012 
05239-6832 OGL 349     LMC160.6.38837 + LMC160.6.39333                                         Pli2012 
05240+3238 COU1090     Primary is V424 Aur, an Algol type eclipsing binary, P = 1.8368d.       Zas2012 
05240-0940 GAL 381     Object #178 in Gallo's original list.                                   Gal1914 
05243+0222 STF 702     BDS 2709, H I 75 same star.                                                     
05244+1723 S   478     111 Tau. A is a spectroscopic binary. B is BD+17@919.                           
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
           WNO  52     AC: HJL1043.                                                            HJL1986 
                       AC: GJ 202 + GJ 201. CPM pair.                                          Mkr2008 
                       AC: SHY  25. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
           S   478     AB: H 5 110.                                                            MEv2010 
05245-0224 MCA  18     eta Ori = 28 Ori. Quintuple; primary is a double-lined spectroscopic            
                       triple with periods 7.99 d (Aa1,Aa2) and 9.2 yr (Aa,Ab). The close              
                       pair eclipses, and shows an 8-hour pulsation in one of the components.          
                       Aa is also eclipsing binary (period 7.9904 day).                        Zas2010 
                       Aa,Ab.  McAlister (1976) orbit uses the elements P, T, e, and the       McA1976 
                       longitude of  periastron for the 9-year orbit, from a spectroscopic             
                       orbit by Ziska & Beardsley (1981), and assumes the orbit is edge-on;    Bey1981 
                       semi-major axis and node are based on a single speckle observation.             
                       The ascending node has been reversed.                                           
                       The visual companions are star B (mag. 4.8, 1.5") in slow retrograde            
                       motion, and C (mag. 9.4, 115").                                                 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       1985.8542: This measurement of the Aab,c component of eta Ori,                  
                       overlooked in the original analysis of this run, was discovered during          
                       preparation of a paper on absolute quadrant determinations by Bagnuolo  Bgn1992 
                       et al. (1992)                                                           Hrt1992b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 25.82 +/- 24.95, 24.50, 22.65 Msun, respectively.  Mlk2012 
05245-0224 MCA 18      Aa,Ab has an SB1 orbit with P=9.44yr. The orbit given here uses only            
                       the speckle data, however.                                              Tok2015c
           H 6  67     H VI 67.                                                                        
05246+0149 S   479     B is BD+01@1003.                                                                
05246-0535 SKF 248     There is a possible companion at 7.8" noted in the WDS, but inside the          
                       AstraLux field of view, the star appears single.                        Jnn2012 
05247+6323 STF 677     AB: CfA: RV var? Can be a sub-system in A or B.                         Tok2014d
                       Now a 3 tier quadruple system since we resolved the secondary                   
                       component of the binary STF 677AB into a new 0".18 pair Ba,Bb and               
                       confirmed that the Robo-AO tertiary C at 7" is physical. We find C to           
                       be slightly below the MS, within errors. Although the relative motion           
                       of AC is fast, it is not directed away from PM(A) as would be the case          
                       for a distant background star; it is produced by the orbital motion of          
                       the inner binary AB. The presence of an inner subsystem in the binary           
                       AB was suspected previously from its variable RV (Nordstrom et al.              
                       2004). The estimated masses of Ba and Bb, 0.98 and 0.65 Msun,           Nrd2004 
                       respectively, remove the discrepancy between the mass sum of 3.05 Msun          
                       calculated for the AB system from its grade 4 orbit by Hartkopf et al.  Hrt2008 
                       (2008) and the expected mass sum. Although such discrepancies are not           
                       uncommon for low-quality orbits, in this case it serves as an indirect          
                       confirmation of Ba,Bb. Estimated period of Ba,Bb is ~20 yr.             Rbr2015d
05247+3723 BU  888     sig Aur = 21 Aur                                                                
05247+2009 J   145     OL  185.                                                                        
05248-1642 GAL 382     Object #179 in Gallo's original list.                                   Gal1914 
05248-5219 I   345     the Pic. A is a spectroscopic binary.                                           
                       Quoted errors in P and a for the Argyle et al. (2002) solution are      Ary2002b
                       +259/-54y, +0".20/-0".01, respectively.                                         
                       1989.9388: This system has also decreased in separation steadily                
                       since the 1920's, and was last resolved visually in 1983.               Hrt1993 
05249+1658 BPM 128     [PM2000]  249674 + [PM2000]  249613.                                    Gvr2010 
05249-7105 OGL 350     LMC164.7.34239 + LMC164.7.34339                                         Pli2012 
05250-0249 H 6  68     H VI 68. B is BD-02@1238.                                                       
05251+1212 BPM 129     [PM2000]  250160 + [PM2000]  250278.                                    Gvr2010 
05251+0621 BUP  78     gam Ori = 24 Ori = Bellatrix                                                    
05251-6818 OGL 351     LMC159.8.17075 + LMC159.8.17418                                         Pli2012 
05251-6833 OGL 352     LMC160.6.45288 + LMC160.6.46200                                         Pli2012 
05252+3451 STF 698     Spectrum composite; K1pIII-IV+F6V. B is BD+34@1030.                             
                       Same as WZ    9. Verified by Daley.                                     Dal2001b
                       AB: H 4 101.                                                            MEv2010 
05252+3434 BU  191     AB: SEI 243.                                                            Nsn2017a
05252+0155 STF 708     H 1  52.                                                                MEv2010 
05252-1119 STF 710     B is BD-11@1168.                                                                
05255-0033 A   848     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       1977.9196: This measure was incorrectly attributed to ADS 3701 in               
                       McAlister & Hendry (1982), with an incorrect position angle.            McA1982b
05256+3803 STF 699     AB: SEI 244.                                                            Nsn2017a
05256+3652 SEI 246     Not found by Heintz at IDS position.                                    Hei1987a
                       Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
05256-6005 HJ 3764     CD-60@1161.                                                                     
05257-0909 DAE   2     NLTT 15049 = LP 717-36.  Daemgen et al. (2007) derive a distance of     Dae2007 
                       20.2 +/- 4.7 pc, a separation of 10.9 +/- 2.5 au, and a predicted               
                       orbital period of 58 +/- 21 yr. Spectral types are M3.5 +/- 0.5 and             
                       M4.0 +/- 0.5; masses are 0.36 +/- 0.09 and 0.28 +0.11/-0.08 Msun.               
05257-6931 OGL 353     LMC161.1.5     + LMC161.1.38                                            Pli2012 
                       Also known as SKF1046.                                                          
05257-7123 OGL 354     LMC165.5.38071 + LMC165.5.38133                                         Pli2012 
05258-7124 OGL 355     LMC165.5.16733 + LMC165.5.16837                                         Pli2012 
05258-7308 GLI  34     Incorrectly assigned precise coordinates of 04026-7109 GLI  25,                 
                       leading to incorrect matches against 2MASS, UCAC4, etc.                         
05259+5033 LDS3656     NLTT 15008/15009                                                        Chm2004 
05260-0938 GAL 383     Object #182 in Gallo's original list.                                   Gal1914 
05260-1942 HJ 3759     B is BD-19@1172. Spectrum F5/7V.                                                
05260-6846 OGL 356     LMC160.2.87    + LMC160.2.86                                            Pli2012 
05262+3808 SEI 250     ALI 798.                                                                        
05262-0223 TOB9005     Measured as DOO  33 but actually an anonymous pair added here.          Tob2010 
                                                                                               Dam2012 
05263+2836 BAR  26     bet Tau = 112 Tau = gam Aur = Elnath                                            
05263-6754 OGL 357     LMC159.4.67    + LMC159.4.1007                                          Pli2012 
05264+1324 BPM 130     [PM2000]  253244 + [PM2000]  253203.                                    Gvr2010 
05264-1210 GAL 384     Object #183 in Gallo's original list.                                   Gal1914 
05264-4323 HJ 3763     B is CD-43@1846.                                                                
05264-7121 OGL 358     LMC165.4.21895 + LMC164.1.435                                           Pli2012 
05265+0256 STF 712     AB: H 1  53.                                                            MEv2010 
05266+3524 STF 705     SEI 257.                                                                Nsn2017a
05266+3138 SEI 259     Secondary not seen on POSS plate; may be either variable star or flaw           
                       on AC Potsdam plate. Damm (2016) misidentified SEI 259; that pair has           
                       been given the designation DAM1282.                                     Dam2016c
05266+0652 SHY 478     HIP  25453 + HIP  25483.                                                        
05267+0045 LEO  57     BAL 981.                                                                        
05267-6827 OGL 359     LMC160.4.4940  + LMC160.4.5097                                          Pli2012 
05268+3557 SEI 258     Secondary not seen on POSS plate; may be either variable star or flaw           
                       on AC Potsdam plate.                                                            
05268+0306 KNT   3     psi 2 Ori = 30 Ori. A is a variable, P = 2.52d.                                 
                       a spectroscopic binary.                                                         
05268-6817 OGL 360     LMC159.1.14589 + LMC159.1.14662                                         Pli2012 
05269+3141 DAM1282     Misidentified by Damm (2016) as SEI 259.                                Dam2016c
05271+3410 BLL  14     A is a semiregular variable, S Aur.                                             
05271-6913 OGL 361     LMC161.3.12128 + LMC161.3.12137                                         Pli2012 
05272+1758 MCA  19     115 Tau. A is an occultation binary which has been resolved by                  
                       speckle interferometry.                                                         
                       First detected as an occultation binary by Africano.                    Afr1978 
                       1982.7551: All archival data for this system were reprocessed using             
                       more powerful algorithms than earlier available, resulting in four new          
                       unresolved measures as well as the new 1991 measurement. In addition,           
                       new rho and theta values have been determined for the observations      McA1989 
                       originally published from 1986.9-1988.3 (McAlister et al. 1989),        McA1990 
                       1988.7-1989.2 (McAlister et al. 1990), and 1990.3--1990.8 (Hartkopf     Hrt1992b
                       et al. 1992).  A preliminary orbit gives a period  of ~15.3 years and           
                       a semi-major axis of 0".080.                                            Hrt1994 
                       1988.2518: This date was incorrectly given as 1988.2490 in McAlister            
                       et al. (1989).                                                          McA1989 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 6.46 +/- 2.35, 8.01, and 4.79 Msun, respectively.  Mlk2012 
05273+3426 D     7     AB = 05275+3425 TOB  35                                                         
                       AB: SEI 263.                                                            Nsn2017a
                       CD: SEI 261.                                                            Nsn2017a
05274-6943 OGL 362     LMC162.3.103719+ LMC162.3.104199                                        Pli2012 
05275-6825 OGL 363     LMC160.4.32945 + LMC160.4.33386                                         Pli2012 
05275-6903 OGL 364     LMC161.4.20865 + LMC161.4.21143                                         Pli2012 
05275-6939 OGL 365     LMC162.4.41184 + LMC162.4.41229 + LMC161.2.25632                        Pli2012 
05276+3429 BUP  79     phi Aur = 24 Aur. D is BD+34@1049.                                              
05276+2156 HJ  365     114 Tau. A is an occultation binary.                                            
                       AC: H 5 115.                                                            MEv2010 
05276+1126 HER  12     Additional notes may be found in Herbig (1962).                         Her1962 
05276-2055 SEE  53     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.60 +/- 2.71, 3.13, and 1.35 Msun, respectively.             Mlk2012 
05276-6120 JSP  79     CD-61@1111.                                                                     
05276-6908 HJ 3771     Measure difficult because of nebula which involves principal star.      Daw1922 
05277-7022 OGL 366     LMC163.3.13645 + LMC163.3.27818                                         Pli2012 
05278+1707 BPM 131     [PM2000]  256139 + [PM2000]  255999.                                    Gvr2010 
05278-0400 A   319     Possible that two different pairs were measured in generating 1962.924          
                       mean, but pair faint for Washington, so scatter may result from that.   Wor1967b
05278-1447 GAL 385     Object #185 in Gallo's original list.                                   Gal1914 
05278-7109 OGL 367     LMC164.2.6335  + LMC164.2.5522                                          Pli2012 
05279+3447 HDS 721     The classification is from Mammano et al. (1977 A&A 59, 9), and                 
                       because the stars are are classified as B-type we have not included             
                       this system in our distributions for the O-stars.  Harries et al.               
                       (1998 MNRAS 295, 386) discuss the inner double-lined system and                 
                       evidence of a near tertiary in a 294-day orbit.  The distant, fourth            
                       star was detected both by us (on the suggestion of B. Schaeffer) and    HIP1997a
                       Hipparcos.                                                              Msn1998a
                       Primary is IU Aur, a Beta Lyr type eclipsing binary, P = 1.81147d.      Zas2012 
05280+3346 S   483     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
05281+4021 ES 2615     B is BD+40@1296.                                                                
05281+3425 STF 707     AE: SEI 270.                                                            Nsn2017a
05282+3349 ES  282     Not found by Heintz at old ES location (05296+3350).                    Hei1983a
                       Also known as TDS3205.                                                          
05282+0223 J    49     Too close 1951 with probable quadrant change (van Biesbroeck).          VBs1954 
05282-2046 BU  320     bet Lep = 9 Lep = Nihal                                                         
05283+0358 HJ 2266     BAL 2148.                                                                       
05284+8605 STF 573     B is BD+85@71.                                                                  
05284+3552 SEI 279     Primary not seen on POSS plate; may be flaw on AC Potsdam plate.                
05284+3549 SEI 273     B component spectral type A0:V:                                         AbH2000 
05284+3546 SEI 276     SEI 276AC incorrectly identified in WSI2008. This is actually the new           
                       pair WSI  40BD which is the same as ALI  74 with a quadrant flip.               
05284+3523 HJ 6999     SEI 271.                                                                Nsn2017a
05284+3447 SEI 272     MLB 1040.                                                                       
05285-1131 GAL 386     Object #186 in Gallo's original list.                                   Gal1914 
05285-7104 OGL 368     LMC164.2.33139 + LMC164.2.33650                                         Pli2012 
05287-0823 HJ 2268     Same as STF 722.                                                                
05287-6527 RST 137     The primary is AB Dor, a rapidly rotating, spotted star which shows             
                       both X-ray flares and microwave emission.                                       
           CLO  10     Aa,Ab: Close et al. discovered a companion to the A component at a      Clo2005 
                       separation of 0".156, which they refer to as the A and C components             
                       (the companion was labelled as C when detected as an astrometric                
                       reflex motion of AB Dor in observations by VLBI and Hipparcos).                 
                       Based on the astrometric orbit and the AO resolution, the mass of the           
                       Ab companion is estimated at 0.090 +/- 0.005 Msun, just above the mass          
                       of a brown dwarf. AO spectroscopy yields a spectral type of M8 +/- 1.           
           SHY  27     AC: HIP  25647 + HIP  31878. C component = C component of 06225-6013            
                       and 06380-6132.                                                                 
                       AD: HIP  25647 + HIP  22738. D component = A component of 04535-5551.           
                       AE: HIP  25647 + HIP  26373. E component = A component of 05369-4758            
                       = D component of 06225-6013.                                                    
           CLO  10     Ba,Bb: Close et al. also resolved the B component into a 66mas pair.    Clo2005 
                       Spectral types of Ba and Bb are estimated by Janson et al. at M5 and    Jnn2007 
                       M5-6, masses at 0.13-0.2 and 0.11-0.18 Msun.                                    
                       Aa is a rapidly-rotating spotted star (0.09 mag variability in V).      Boc2008 
                       Close et al. (2007) find spectral types for Aa, Ab, Ba, and Bb of K1,   Clo2007b
                       M5.5 +/- 1.0, M3.5 +/- 1.5, M4.5 +/- 1.5. Masses are 0.865 +/- 0.034,           
                       0.090 +/- 0.005, <0.25, <0.15 Msun; the system age is 75 +/- 25 Myr             
                       and the distance 14.9 +/- 0.1 pc.                                               
                       Ba,Bb: Wolter et al. (2014) made a multiwavelength study of AB Dor              
                       Ba,Bb. They derive effective temperatures 3260-3360 and 3200-3300K for          
                       Ba and Bb, respectively. Predicted system mass is 0.45-0.71 Msun,               
                       age 50-100 Myr.  (Ed note: Inclination for Wolter et al orbit (182deg)  WoU2014 
                       appears to be off by 90deg; changed to 92deg in orbit catalog)                  
                       Ba,Bb: Azulay et al. (2015) derive an orbit for AB Dor B, yielding a            
                       parallax of 66.4 +/- 0.5 mas, as well as component masses for Ba and            
                       Bb of 0.28 +/- 0.05 and 0.25 +/- 0.05 Msun.                             Azu2015 
05289+1233 LDS6186     NLTT 15139/15142                                                        Chm2004 
           TOK  94     HIP 25662. Mini-cluster. A is SB and astrometric pair (Vogt et al.)     CPS2002 
                       P = 1427d, M2 = 0.18 Msun. The system is thus a new quadruple.          Tok2011a
                       AB: Primary is SB1O, P=1426.7d (Katoh et al. 2013 AJ 145, 41)           Tok2014d
05290+3629 SEI 292     No star matching the position of the purported primary is seen on POSS          
                       plates, although another star is found at ~127deg, 15" from the SEI             
                       secondary. It is uncertain whether this pair is the SEI pair, although          
                       none of the stars in the vicinity appear to have large proper motion.           
05290+1707 BPM 132     [PM2000]  258672 + [PM2000]  258702.                                    Gvr2010 
05290-0442 WEB   4     A is the Mira-type variable S Ori. B is -04@1144.                               
05290-2237 HDO  69     HDO  71.                                                                        
05291+1152 BGR   1     GW Ori.                                                                         
05292-6749 OGL 369     LMC166.5.30    + LMC166.5.499                                           Pli2012 
05293+2509 STF 716     118 Tau.                                                                        
                       AB: H 2  75.                                                            MEv2010 
05293-2517 WHI   7     Listed as possibly resolved by White et al. (1991).                     Whi1991 
05294+3126 SHY 481     AC: HIP  25711 + HIP  25614.                                                    
05294+1152 HER   1     This is the T-Tauri variable V649 Ori = HBC 86.                                 
                       1980.95: Marginal evidence for additional component with separation             
                       0".47, pos. angle 36 or 216 deg.                                        Bai1985b
05294-0716 H 5 101     H V 101.                                                                        
05294-6849 OGL 370     LMC167.8.42748 + LMC167.8.42773                                         Pli2012 
05295+1257 JOY   8     Additional notes may be found in Herbig (1962).                         Her1962 
05296+3045 KU   88     B is BD+30@910.                                                                 
05296+1534 LDS6187     NLTT 15154/15153                                                        Chm2004 
05296+0309 STF 721     A,BC: H 4  45.                                                          MEv2010 
05297+6355 MLR 128     Also known as TDS 174.                                                          
05297+3523 HU  217     A is the Beta Lyrae-type system, LY Aur, P = 4.00d.                             
                       The classification is from Drechsel et al. (1989 A&A 221, 49). Howarth          
                       et al. (1997 MNRAS 284, 265) give Delta m for both spectroscopic and            
                       astrometric components.                                                 Msn1998a
05297+3327 S   484     B is BD+33@1063.                                                                
05297-0106 STF 725     31 Ori. A is the variable CI Ori.                                               
05298+1825 HJ 3275     STTA 64.                                                                        
05298-6904 OGL 371     LMC168.5.10887 + LMC168.5.10884                                         Pli2012 
05298-7154 OGL 372     LMC172.8.80    + LMC172.8.234                                           Pli2012 
05300+1214 HER  13     Additional notes may be found in Herbig (1962).                         Her1962 
05301+2933 STF 719     AC: H 4 110.                                                            MEv2010 
05301-3228 B  1946     Not seen for certain 1951-1967.                                                 
05302+4145 A  1720     A measure by A 1907.8, 259@, 1.9".                                              
05302-4705 HJ 3767     A,BC: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
05303-0247 J     7     Magnitude of A noted as 9.7 in 1909 and 8.7 in 1910. Other variations           
                       observed since then.                                                    J__1952 
05303-2331 B  2587     Spectrum: Fm delta Del.                                                         
05303-5359 JNN  38     The AstraLux images resolve this system into a likely triple, where             
                       all components have brightnesses and colors consistent with a                   
                       physically bound system. Since it has only been observed in one epoch,          
                       common proper motion has not yet been established.                      Jnn2012 
05303-6653 HJ 3779     AC: Whole in nebulous haze.                                             Hln1965 
05305+3239 ES  335     SEI 313.                                                                Nsn2017a
05307+5521 MLR 687     Also known as TDS 175.                                                          
05308+3950 STTA 63     B is BD+39@1321.                                                                
05308+0557 STF 728     32 Ori. The motion is still practically rectilinear, as represented     B__1956b
                       in formulae by van den Bos (1956) and Cester  (1964).                   Ces1964a
                       H 1  25.                                                                MEv2010 
                       Probably optical.                                                       B__1962d
05308-0022 A   852     Appears to be in rapid motion. This is the variable V1093 Ori.                  
05308-0034 CBL 228     GWP 684.                                                                Tob2012b
05308-1251 BRT2644     RST 3426. BRT identifies this as BD-12@1187.                                    
05311+4255 A  1721     Too close 1924-1931. This interval may mark a possible quadrant change          
05312+0318 STF 729     33 Ori = n 1 Ori. 1945.16 : Measure unpublished in orbit quotation.             
                       AB: H 1  22.                                                            MEv2010 
05312-7134 OGL 373     LMC172.6.6648  + LMC172.6.6645                                          Pli2012 
05314-0336 ENG  20     Proper motion of A +774 -2090. B is BD-03@1122, PM -013-041.                    
05314-0724 TUV   1     Primary is an F5V W UMa eclipsing binary, while B is redder and about           
                       1 mag fainter. At the derived distance of 600-800 pc, the physical              
                       separation of A and B would be more than 1000 au. The authors conclude          
                       it is unlikely the stars are bound.                                     Tuv2008 
05314-7110 OGL 374     LMC171.7.13103 + LMC171.7.13105                                         Pli2012 
05315+5439 STF 711     AB: HJL  70.                                                            HJL1986 
05315-6749 OGL 375     LMC166.4.145   + LMC166.4.337                                           Pli2012 
05316-0953 LDS 145     LDS 844 = LDS6188.                                                              
05316-1512 GAL 387     Object #188 in Gallo's original list.                                   Gal1914 
05317+1720 BPM 133     [PM2000]  263884 + [PM2000]  263996.                                    Gvr2010 
05317+0006 TOK  96     HIP 25905.  A is SB without orbit.                                      Nrd2004 
05318-7128 OGL 376     LMC172.5.13529 + LMC172.5.13581                                         Pli2012 
05319+7548 LDS1612     BVD 302.                                                                        
05319-7620 HJ 3795     gam Men                                                                         
05320+1118 V1410 Ori   Noted as possible binary (separation > 0".020) by Baines et al. (2006)  Bns2006 
05320-0018 HEI  42     del Ori = Mintaka. A is an Algol-type system, as well as a close                
                       visual binary.                                                                  
                       Aa,Ab: Orbital elements are also given by Levato et al. (1988). This    Lev1988 
                       close visual pair has increased in separation from 0".20 to 0".29               
                       between 1979 and 1994. The spectral classification for the C component  Lev1991b
                       is from Morrell & Levato (1991).                                        Msn1998a
           STFA 14     C is a spectroscopic binary.                                                    
                       AC: H 5  10.                                                            MEv2010 
05321-0305 JNN  39     V1311 Ori.                                                                      
                       2MASS J05320450-0305291 is identified as a beta Pic member in da Silva          
                       et al. (2009 A&A 508, 833). It is also known as V1311 Ori.              Jnn2012 
05321-0506 DOO  34     Doolittle identifies this as BDS 2801, but evidently it is a different          
                       pair.                                                                   Doo1923 
05321-1452 GAL 388     Object #190 in Gallo's original list.                                   Gal1914 
05322+1703 STF 730     A is a spectroscopic binary.                                                    
                       H N 124.                                                                MEv2010 
05322-0431 RAS  19     Includes the rotationally variable star V1101 Ori. Companion estimated          
                       as close to G5V; mass of system perhaps 7 Msun.                         Ras2014 
05323+0217 A  2509     Not seen 1913-1936, when about 100@ of orbital motion took place.               
05324+0132 SKF1047     These two T Tauri stars are V1884 Ori + V1883 Ori.                      Skf2012 
05324-0624 ENG  21     B is BD-06@1211.                                                                
05324-1458 GAL 389     Object #191 in Gallo's original list.                                   Gal1914 
05326+1700 BPM 134     [PM2000]  265797 + [PM2000]  266129.                                    Gvr2010 
05327-0136 BU 1048     A is variable.                                                                  
05327-1749 HJ 3766     alp Lep = 11 Lep = Arneb                                                        
05327-6758 OGL 377     LMC166.3.14    + LMC166.3.52                                            Pli2012 
05330-2415 DAW  85     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.69 +/- 0.65, 1.66, and 0.79 Msun, respectively.             Mlk2012 
05330-6414 28 Dor      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Lunt (1924).                                                            Lun1924 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Lunt (1924).                                                            Lun1924 
05331+2002 A  2434     HIP 26018. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc. Aka J  2606.                             
05331-0143 STF 734     H V 119.                                                                        
                       AC: H 5 119.                                                            MEv2010 
05332+1557 TOK  97     HIP 26027. Two companions are seen in the ANDICAM images.               Tok2011a
05332-6501 TOK  98     HIP 26030.                                                              Tok2011a
05333+4449 AST   3     G 96-45 = GJ 1081.                                                              
05334+1220 GIC  59     G097-049/G097-048 = Ross 43.                                                    
                       NLTT 15271/15272                                                        Chm2004 
05334-6847 OGL 378     LMC167.2.15319 + LMC167.2.15443                                         Pli2012 
05335-2420 HJ 3770     AB closed down from 12" in 1835 to 3.8" in 2MASS. Physical?             Tok2014d
05336-6956 OGL 379     LMC169.2.19326 + LMC169.2.19557                                         Pli2012 
05337+0157 LWR   6     V371 Ori                                                                        
05340-6814 OGL 380     LMC166.1.16552 + LMC166.1.16697                                         Pli2012 
05341-0102 H 5 118     H V 118. Wendell noted a possible companion to the south of A in                
                       1869.08, although "separation doubtful".                                Wen1882 
05341-1422 HLD  76     There must be some error in my single night's distance of AB in 1958.   B__1963b
05342+1019 LDS6189     This is the common proper motion pair Ross 45.                                  
05342-7120 OGL 381     LMC172.4.30962 + LMC172.4.31134                                         Pli2012 
05343+0346 STT 110     38 Ori                                                                          
05344+3549 AG   95     SEI 328.                                                                Nsn2017a
05344+0227 J  2002     BAL 1675.                                                                       
05345+3727 SEI 330     The 05345+3727SEI 330 system is actually 2 close doubles (33" apart).           
                       Most of the confirming measures were of the other, previously                   
                       uncataloged pair, 05345+3726SEI 332. Thanks to Ed Wiley for bringing            
                       this to our attention.                                                          
05346-0528 REP  51     V1438 Ori                                                                       
05346-0543 JNN  40     V1000 Ori.                                                                      
                       2MASS J05343767-0543044 has been classified as a likely member of the   Jnn2012 
                       ~1 Myr Orion OBIc/d association (Stassun et al. 1999 AJ 117, 2941).             
                       The companion that was detected with AstraLux has not yet been                  
                       confirmed to share a common proper motion, but its brightness and               
                       color are consistent with what would be expected for a physical                 
                       companion, hence it is counted as such in the statistical analysis.     Jnn2012 
05346-6836 OGL 382     LMC167.3.17320 + LMC167.3.18302                                         Pli2012 
05347-0520 REP  53     V1441 Ori = JW 63. Correia et al. (2014) derive the following                   
                       properties: spectral types M0.5 +/- 0.5 and M3.0 +/- 1.0, Teff 3777             
                       +/- 72 and 3415 +/- 145K, radii 2.2 +/- 0.3 and 1.7 +/- 0.2 Rsun.               
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05347-0534 REP  55     V1118 Ori                                                                       
05347-0545 SKF2420     MGM1241. IZ Ori.                                                        Kkl2016 
05347-6857 OGL 383     LMC167.1.20073 + LMC167.1.20205                                         Pli2012 
05348+0929 MCA  20     phi 1 Ori = 37 Ori. This speckle observation probably represents the            
                       known spectroscopic binary with P = 8.4y.                                       
05348-0524 GET   1     V1454 Ori                                                                       
05348-0525 REP  56     JW 81. Correia et al. (2014) derive the following properties:                   
                       spectral types M1.0 +/- 0.5 and M3.5 +/- 1.0, Teff 3705 +/- 72 and              
                       3442 +/- 72K, radii 2.0 +/- 0.3 and 1.1 +/- 0.1 Rsun.                           
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05348-0600 STF 745     H 3  13.                                                                Bu_1906 
05348-3240 JNN  41     All components of this triple system have colors and brightnesses               
                       consistent with expectation for physical companions. Common proper              
                       motion has however not yet been demonstrated.                           Jnn2012 
05349+0006 OL  178     Aka RST5217.                                                                    
05349-0007 STF 741     H 3  76.                                                                MEv2010 
05349-0523 REP  60     V1458 Ori = JW 128. Correia et al. (2014) derive the following                  
                       properties: spectral types M3.0 +/- 1.0 and M3.0 +/- 1.0, Teff 3415             
                       +/- 145 and 3415 +/- 145K, radii 2.4 +/- 0.2 and 2.2 +/- 0.2 Rsun.              
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05349-0530 REP  61     V1460 Ori                                                                       
05350+1544 HEI  43     Heintz reports a third star at 283 deg, 40".                            Hei1980a
05350-0524 GET   3     AB: JW 176. Correia et al. (2014) derive the following properties:              
                       spectral types M1.0 +/- 0.5 and M1.0 +/- 0.5, Teff 3705 +/- 72 and              
                       3705 +/- 72K, radii 2.9 +/- 0.2 and 3.2 +/- 0.5 Rsun.                           
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05350-0529 REP  66     V1320 Ori                                                                       
05350-0600 STF 747     STFA 15. B is BD-06@1233.                                                       
                       AB: H 3  14.                                                            MEv2010 
05351+2006 J  2606     Jonckheere unable to recover.                                           J__1962a
05351+0956 STF 738     lam Ori = Meissa                                                                
                       Both A and B components were observed and appeared to be single. The            
                       AB pair may not be physical (Lindroos). The photometry-based            Lnd1985 
                       classification of the C component is from Lindroos, who also gives a            
                       distance of 430 pc.                                                     Msn1998a
                       Classification of the B component is from Hoffleit & Warren (1991).     Hof1991 
                       AB: The image rotator was in an unknown state, so two possible theta            
                       values are listed for the 2001.7428 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
                       AB: H 2   9.                                                            MEv2010 
05351-0124 RAS  20     SrCrEu star; secondary probably early-K. System may belong to the               
                       Orion OB1 association.                                                  Ras2014 
05351-0508 JNN  42     V1321 Ori.                                                                      
                       This star has been classified as a probable T Tau star in Alcala et             
                       al. (1996 A&AS 119, 7). It is also known as V1321 Ori.                  Jnn2012 
05351-0523 GET   4     AB: V1274 Ori = JW 248. Correia et al. (2014) resolved a close (0".14)          
                       faint (dm=3mag) companion to the primary, and derive the following              
                       properties for Aa and B: spectral types M1.0 +/- 0.5 and M7.5 +/- 1.5,          
                       Teff 3705 +/- 72 and 2795 +/- 295K, radii 3.5 +/- 0.4 and 2.4 +/- 0.8           
                       Rsun. Masses and ages are determined for several published PMS tracks.  Cor2014 
05351-0532 MGM1501     LM Ori.                                                                 Kkl2016 
05351-0534 SKF2257     MGM1454. V982 Ori.                                                      Kkl2016 
05351-0551 MGM1171     V2134 Ori.                                                              Kkl2016 
05352+1014 STT 111     The primary is a single-lined spectroscopic binary, P = 1857d.                  
05352+0954 BYN   1     Separation and position angle calculated from tabulated RA and DEC of           
                       components. Quoted date and telescope aperture are rough means of all   ByN2007a
                       listed information in Barrado y Navascues et al. (2007).                ByN2007b
05352-0513 MGM2239     V2327 Ori.                                                              Kkl2016 
05352-0515 MGM2193     V2359 Ori.                                                              Kkl2016 
05352-0516 REP  72     Ba,Bb: V1492 Ori                                                                
05352-0517 REP  77     AB: V1329 Ori                                                                   
           KOH  98     DE: V1327 Ori                                                                   
05352-0521 REP  74     Ba,Bb: JW 391. Correia et al. (2014) derive the following properties:           
                       spectral types M0.0 +/- 0.5 and M7.0 +/- 1.0, Teff 3850 +/- 53 and              
                       2880 +/- 140K, radii 2.0 +/- 0.1 and 1.4 +/- 0.2 Rsun.                          
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05352-0522 GET  20     FG: V1496 Ori                                                                   
05352-0523 GET   9     DE: V1487 Ori                                                                   
           GET  25     NO: V1330 Ori                                                                   
           PRS   8     PQ:SMN   3Da,Db                                                                 
05352-0524 PRS   9     Aa,B:  Aka GET  28.                                                     Skf2016a
05352-0529 REP  76     V1495 Ori                                                                       
05352-0537 REP  79     V1500 Ori                                                                       
05352-0538 REP  80     V409 Ori                                                                        
05353-0515 REP  84     V1334 Ori                                                                       
05353-0520 HJ 1157EF   Aka POP 205.                                                                    
05353-0522 GET  45     NO: V1333 Ori                                                                   
           PRS  18     Ka,Kb: DAE  13Oa,Ob                                                             
05353-0523 STF 748     A: the 1 Ori A = 41 Ori A = V1016 Ori                                           
                       B: the 1 Ori B = 41 Ori B = BM Ori                                              
                       C: the 1 Ori C = 41 Ori C                                                       
                       D: the 1 Ori D = 41 Ori D                                                       
                       Trapezium. the Ori A, B, and C were first noted as a triple by          G__1617 
                       Galileo on 4 February 1617. It was independently found as a triple in           
                       by Christian Huygens, who is often given credit for recognizing this            
                       multiple system. the Ori D was found by Abbe Jean Picard, as            A__1935f
                       documented by a manuscript drawing of 20 March 1673. The D component            
                       was independently found by Huygens in 1684.                                     
                       A and B are both Algol-type systems, C is an RW Aur-type system.                
                       Common proper motion with the multiple system STF 16.                           
                       Stahl et al. (1996 A&A 312, 539) find that the H-alpha profiles of the          
                       C component vary with a 15.4-day cycle which they suggest is related            
                       to the star's rotational period; photospheric line radial velocity              
                       variations are small. All 4 of the Orion Trapezium stars were observed          
                       with the speckle camera (A = HD 37020; B =  HD 37021; C = HD 37022;             
                       D = HD 37023) and all appeared to be single. Classifications of the             
                       B and D components are from the WDS.  The spectral classification for   Lev1991b
                       the A component is from Morrell & Levato (1991).                        Msn1998a
                       AB: H 3   1.                                                            MEv2010 
                       AC: C component = D component of 05354-0525 STFA 17.                            
           WGT   1     Ca,Cb: The longer-period Kraus et al. (2007) solution gives a dynamic           
                       parallax 2.304 +/- 0.066 mas, the shorter-period solution gives 2.585           
                       +/- 0.074 mas. Mass sums are 47.8 +/- 4.2 and 44.8 +/- 3.9 Msun,                
                       respectively. Based on evolutionary models, spectral types for Ca and           
                       Cb are O5.5 and O9.5, masses are 34.0 and 15.5 Msun.                    Kss2007 
                       The Kraus et al. (2009) solution is based on VLTI data from 2007-2008,          
                       plus speckle (1997-2008) and radial valocity data. They derive a                
                       dynamic distance of 410 +/- 20pc and a system mass of 44 +/- 7 Msun.    Kss2009 
                       Ca,Cb: From their combined astrometric/spectroscopic solution, Balega           
                       et al. (2015) derive the following properties for the system:                   
                          total mass (Msun): 45.5 +/- 10.0                                             
                          mass ratio:        0.36     0.05                                             
                          distance (pc):     414      7                                                
                          flux ratio:        0.30     0.05                                             
                       Resulting properties for the two components are:                                
                          mass (Msun):       33.5 +/- 5.2      12.0 +/- 3.0                            
                          log L:             5.21     0.01     4.70     0.15                           
                          Spectral types:    O6Vp              B0V                                     
                          Teff               39000    1000     30000    1000                           
                          radii (Rsun):      8.91     0.50     8.24     0.50                   Bag2015 
           STF 748     CH: Additional notes may be found in Burnham (1894).                    Bu_1894 
           KSS   1     D component of ADS 4186 = the 1 Ori D                                           
05353-0523 DAE 130     Oa,Ob: The elongated shape of JW 519's primary suggests the primary to          
                       be binary itself. The photometry for JW 519, however, is based on the           
                       assumption of a single central object since separate components cannot          
                       be identified.                                                          Dae2012 
           GET  43     TU: the 1 Ori G                                                                 
           REP 110     Xa,Xb: AF Ori                                                                   
05353-0524 GET  38     FG: AC Ori                                                                      
05353-0533 REP  81     V1504 Ori                                                                       
05354-0450 DA    4     AB + TOK 430Aa,Ab: This is HIP 26237, HD 37018, HR 1892, 42 Ori, a              
                       young star in Orion which has not been observed at high angular                 
                       resolution so far, according to INT4 (Hartkopf et al. 2001). We         Hrt2001d
                       resolved the known binary DA 4AB and discovered the spectacular                 
                       subsystem Aa,Ab at 0".16.                                               Tok2015c
05354-0509 KOH 101     V1344 Ori                                                                       
05354-0510 MGM2300     V2377 Ori.                                                              Kkl2016 
05354-0524 PRS  34     AB: V1524 Ori                                                                   
           GET  56     CD: V494 Ori                                                                    
           GET  57     GH: V1231 Ori                                                                   
05354-0525 STFA 16     A: the 2 Ori A = 43 Ori. Spectroscopic binary, P = 21d.                         
                       B: the 2 Ori B = BD-05@ 1320.                                                   
                       C component is primary of 05355-0525 S   490.                                   
           STFA 17     AD: This is the the 1 / the 2 Ori system                                        
                       D component = C component of 05353-0523 STF 748.                                
           CHR 249     The A component (CHR 249 Aa,Ab) was resolved on 3 occasions, but the            
                       distant STFA 17B component was observed to be single.  Hipparcos        HIP1997b
                       results confirm the Aa,Ab pair.  The spectral classification for        Lev1991b
                       the B component is from Morrell & Levato (1991).                        Msn1998a
                       Classification of the C component is from Hoffleit et al. (1983).       Hof1983 
05354-0527 REP  89     JW 709. Correia et al. (2014) derive the following properties:                  
                       spectral types M0.5 +/- 0.5 and M0.5 +/- 0.5, Teff 3777 +/- 72 and              
                       3777 +/- 72K, radii 1.8 +/- 0.1 and 1.7 +/- 0.2 Rsun.                           
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05354-0532 REP  91     V1528 Ori                                                                       
05354-0535 CHN  14     Also known as AG Ori. The secondary = V2378 Ori.                                
05354-0555 STF 752     iot Ori = 44 Ori. A is a spectroscopic binary, P = 29.1d.                       
                       The classification is from Stickland et al. (1987).                     Stc1987 
           CHR 250     The A component was resolved (CHR 250 Aa,Ab); the B component was also          
                       observed but appeared to be single.                                     Msn1998a
                       Classification of the B component is from Hoffleit & Warren (1991).     Hof1991 
           STF 752     AB: H 3  12.                                                            MEv2010 
05355-0422 STF 750     H 2  26.                                                                MEv2010 
05355-0459 MGM2472     V2475 Ori.                                                              Kkl2016 
05355-0504 SKF2481     MGM2398.                                                                Kkl2016 
05355-0505 MGM2367     V2502 Ori.                                                              Kkl2016 
05355-0509 KOH 104     V360 Ori                                                                        
05355-0510 RBB   7     MGM2285. V419 Ori.                                                      Kkl2016 
05355-0516 PBS   2     NU Ori                                                                          
05355-0519 REP  96     JW 867. Correia et al. (2014) derive the following properties:                  
                       spectral types M0.5 +/- 0.5 and M1.5 +/- 0.5, Teff 3777 +/- 72 and              
                       3632 +/- 72K, radii 2.2 +/- 0.1 and 2.2 +/- 0.1 Rsun.                           
                       Masses and ages are determined for several published PMS tracks.        Cor2014 
05355-0524 GET  60     V1288 Ori                                                                       
05355-0525 S   490     Variable, V361 Ori. Primary is C component of 05354-0525 STFA 16AC              
05356+3801 AG   98     HDS 746.                                                                        
05357-0451 HLD 173     45 Ori.                                                                         
05357-0528 KOH 105     AN Ori                                                                          
05358-0059 STF 751     B is BD-01@966.                                                                 
05359+3530 SHY 483     AB: HIP  26290 + HIP  26322.                                                    
           SHY 476     BC: HIP  26322 + HIP  24934.                                                    
05359-0538 DA    3     A is a spectroscopic binary and light variable.                                 
05360+3614 SEI 349     Heintz equates this with ALI 308.                                       Hei1985a
05360-0616 JNN  43     V1178 Ori.                                                                      
                       Also known as V1178 Ori, this star has been classified as a probable T          
                       Tau star in Alcala et al. (1996 A&AS 119, 7). It has a companion that           
                       is as of yet unconfirmed with regards to common proper motion, but              
                       since the brightness and color are well consistent with expectations            
                       for a real companion, system is counted as binary in the statistics.    Jnn2012 
05360-7136 OGL 384     LMC172.3.13633 + LMC172.3.13778                                         Pli2012 
05361-1302 LDS3666     NLTT 15358/15357                                                        Chm2004 
05362-0112 BUP  81     eps Ori = 46 Ori = Alnilam. Possibly variable.                                  
05362-1349 WEI   9     B is BD-13@1193.                                                                
05362-2842 SHY 484     HIP  26309 + HIP  26453.                                                        
05363-0018 RAS  21     Triple includes the alpha2 CVn type variable star V1130 Ori.  Spectral          
                       types of B estimates as A7; uncertainty in magnitude does not allow             
                       estimate of specral type for C. Member of Orion OB1 association.        Ras2014 
05364+3408 STF 737     B is BD+34@1106.                                                                
                       SEI 353.                                                                Nsn2017a
05364+2200 STF 742     A premature orbit has been computed.                                            
                       The node and longitude of periastron have been corrected.                       
                       H 1  70.                                                                MEv2010 
05364-7056 OGL 385     LMC171.3.62055 + LMC171.3.62082                                         Pli2012 
05365+2556 CHR 203     First detected as an occultation binary by Schmidtke et al.             Smk1989 
05365-0643 J   798     Center of nebula H IV 33. Couteau did not find the Jonckheere AC        J__1912d
                       component. The two components may in fact be the same. The A component  Cou1960a
                       is the RW Aur-type variable V380 Ori.                                           
           COU2713     AC: Primary is in nebula NGC 1999. Did not see 13th mag companion at            
                       220deg seen by Jonckheere in 1912.  This observation confirms 15th mag          
                       companion seen at same time ~40deg, 5".                                 Cou1961a
05366-0604 STF 754     A is a spectroscopic binary.                                                    
                       H 3  13.                                                                MEv2010 
05366-1029 GAL 390     Object #193 in Gallo's original list.                                   Gal1914 
05367-0634 SKF2301     MGM 845. V846 Ori.                                                      Kkl2016 
05367-6904 OGL 386     LMC175.5.5552  + LMC175.5.5551                                          Pli2012 
05367-6930 I  1151     An S Doradus-type variable, R127, in the LMC.                                   
05368-1003 GAL 391     Object #194 in Gallo's original list.                                   Gal1914 
05369-4758 HDS 751     See notes to 05287-6527 SHY  27AE and 06225-6013 SHY  34AD.             Shy2011 
05370+2044 GJ 209      Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                       (2000).                                                                 HaI2001 
05370-0137 HDO  76     According to Burnham (1906) original measure is labelled "doubtful".    Bu_1906 
05370-6851 OGL 387     LMC174.8.25249 + LMC174.8.25968                                         Pli2012 
05371+2655 BOW   4CD   Aka ITF   4.                                                                    
05372+7928 MLR 492     Also known as TDS 187.                                                          
05372+1014 BPM 135     [PM2000]  278391 + [PM2000]  278458.                                    Gvr2010 
05372-2424 B    84     HIP 26404. AB = B 84 = ADS 4227, 3". The pair is optical according to           
                       the CMDs (B is too red, above the MS). Small PM(A)=(+13,-14). However,          
                       the field is not crowded, N*=14, an optical companion at 3.5" is                
                       unlikely. Is B an IR companion? No relevant references in SIMBAD.       Tok2011a
05373+6409 HU 1107     19 Cam.                                                                         
05373-6857 OGL 388     LMC174.8.25010 + LMC174.8.31202                                         Pli2012 
05375+3147 WZ   10     SEI 356.                                                                Nsn2017a
05375-7138 OGL 389     LMC179.7.17322 + LMC179.7.17360                                         Pli2012 
05376+2659 ITF   3     Aka ITF  35.                                                                    
05377+1618 BPM 136     [PM2000]  280129 + [PM2000]  280138.                                    Gvr2010 
05377-5330 HJ 3786     Spectrum of A is F/G.                                                           
05378-5434 HJ 3787     B is CPD-54@866.                                                                
05379+0058 STTA 65     Pair appears in an appendix list, not part of the discoverer's regular          
                       numbering sequence.                                                             
05380+1631 BPMA 11     [PM2000]  280939 + [PM2000]  280294.                                    Gvr2010 
05381-0011 STF 758     CD : Same as STF 765.                                                           
                       CD: H 3 111.                                                            MEv2010 
05382-4606 HJ 3784     HIP 26501. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
05383-7135 OGL 390     LMC179.6.5087  + LMC179.6.5328                                          Pli2012 
05384+4301 A  1563     Less than 0.1" with 82-inch 1953, 1954.                                         
                       A premature orbit has been computed.                                            
05384+3401 SMR  56     Pair initially designated SMR 55 in error, designation already in use.          
05384+1124 BPM 137     [PM2000]  282231 + [PM2000]  282180.                                    Gvr2010 
05384-6951 OGL 391     LMC176.7.81530 + LMC176.7.81923                                         Pli2012 
05386+3030 BU 1240     26 Aur. Composite spectrum; B9.5V+F9III. Light variability suspected.           
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                       orbit of Baize (1956).                                                  Baz1956 
                       Romero (2008) estimates masses of the A and B components as 2.1 +/-     FMR2008 
                       1.0 and 3.0 +/- 0.4 Msun, respectively; spectral types are G8III and            
                       A1IV or B9.5V.                                                                  
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 6.87 +/- 22.98, 5.45, and 4.82 Msun, respectively. Mlk2012 
           STF 753     Romero (2008) analyzes the optical/physical nature of the C component;  FMR2008 
                       the spectral is determined to be about A6V and it appears to be                 
                       gravitationally bound to the AB pair, with an estimated orbital period          
                       of ~46,000 years.                                                               
                       AB,C: H 3  64.                                                          MEv2010 
           BU   90     Romero (2008) derives a proper motion for D (+0.4 +/- 2.1 mas/yr in     FMR2008 
                       RA, -12.6 +/- 1.6 mas/yr in Dec) based on that of the AB pair plus the          
                       relative motion of AB,D between the years 1856 and 2002. He also                
                       concludes that D is optical, with a spectral type estimated at K1III            
                       and distance of ~870pc (both determinations corrected for reddening).           
05386-0233 STF 761     AB: B is BD-02@1323.                                                            
                       Primary = F component of 05387-0236 STF3135AB,F.                                
                       BC: H 2  10.                                                            MEv2010 
05386-0244 PLT   1     A is TX Ori, B is TY Ori.                                               Plt1934 
05386-1655 UC 1338     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
05387-0236 STF3135     Rabe measures principal stars STF 761 and STF 762.                      Rab1923 
                       1914, 324@, 209.79". This new WDS entry created 02/18/98.                       
                       Spectral types of primary and secondary assigned by ten Brummelaar et   TtB2000 
                       al., based on adaptive optics observations.                                     
           BU 1032     sig Ori = 48 Ori. A is the variable V1030 Ori. This is the brightest            
                       pair in a trapezium system with at least five components, including             
                       components C (mag. 8.79, 11", A2V), D (mag. 6.62, 13", B2V), and the            
                       helium-rich star E, BD-02@1327. A has also been reported to be a short          
                       period SB2.                                                                     
                       Heintz (1974) gives formulae for the motions AB,C and AB,D.             Hei1974b
                       The suspected small RV variation of AB was not confirmed in David               
                       Dunlap Obs. spectra.                                                            
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       The AB pair has decreased in position angle from 171 deg to 125 deg             
                       between 1975 and 1994.  Fullerton (1990) describes three spectral       Ful1990 
                       components in the He I 5876 A profile which suggests that one of the            
                       stars is a double-lined spectroscopic binary  (see Bolton, 1974 ApJ             
                       192, L7).  Classifications of the B, C, and D components are from       Hof1991 
                       Hoffleit & Warren (1991), while the classification for the E            Lev1991b
                       component is from Morrell & Levato (1991).                              Msn1998a
                       AB: Additional notes may be found in Worley (1956).                     Wor1956b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 27.34 +/- 40.70, 25.32, 21.87 Msun, respectively.  Mlk2012 
           sig Ori     Aa,Ab: Simon-Diaz et al. (2015) derive a new spectroscopic orbit for            
                       the primary (sig Ori Aa,Ab) as well as astrometry and photometry for            
                       the AB pair. New values for mass, log g, age, Teff, etc are derived             
                       for Aa, Ab, and B.                                                      SiD2015 
           NOI   6     Aa,Ab: Schaefer et al. (2016) resolved the primary of sig Ori A and             
                       derive a new combined solution, as well as a new orbit of the AB pair.          
                       Derived masses for Aa, Ab, and B are 16.99 +/- 0.20, 12.81 +/- 0.18,            
                       and 11.54 +/- 1.15 Msun, respectively. They also derive a parallax of           
                       2.5806 +/- 0.0088 mas, corresponding to distance 387.51 +/- 0.12 pc.    NOI2016b
           STF 762     AB,C: H 2  11.                                                          MEv2010 
                       Sigma Ori E (V1030 Ori) has a strong magnetic field and a magnetosphere IAU2014a
                       with two clouds of plasma constrained by magnetic and centrifugal               
                       forces which co-rotate with the 1.19d period of the star which results          
                       in eclipse features.                                                            
                       Note that the C component was first resolved by Dawes while D and E     Da_1835 
                       were first resolved by Mayer. However, the discovery designation is     MyC1784 
                       maintained due to the long standing historical designations.                    
           STF3135     AB,F: F component = primary of 05386-0233 STF 761.                              
           RAS  22     Ea,Eb: Helium star V1030 Ori, type B2; spectral type of Eb estimated            
                       as late-A.                                                              Ras2014 
           CAB  26     Ha,Hb: [W96] 4771-899 = Mayrit 528005                                           
           BOY  24     Ja,Jb: sig Ori IRS 1 = Mayrit 3020                                      Boy2009 
05387-6906 RMC 136     30 Dor cluster in Large Magellanic Cloud. Due to space limitations,             
                       component designations have been converted from the letter/number               
                       format (e.g., a1 or k10) adopted by Weigelt and collaborators to the    Wgt1985 
                       upper/lower case letter format (e.g., Aa or Kj) used in the WDS. The    Ner1988 
                       order of these components has not been changed, however. Of the 13      Peh1992 
                       companions discovered by Herschel, Dawes, and Innes, only the pair              
                       originally designated I  1152AB matches one of these close                      
                       interferometric pairs with any certainty; it has been merged with               
                       RMC 136Aa,Ac. Component designations for the others were adjusted.              
                       Results are tabulated from the combined data set only. RMS errors from          
                       comparing data sets are 0".011 in separation, 1.6 deg in position               
                       angle, 0.28 in magnitude difference.                                    Peh1992 
05388+1548 BPM 138     [PM2000]  283526 + [PM2000]  283334.                                    Gvr2010 
05389+1651 BPMA 12     [PM2000]  283738 + [PM2000]  283905.                                    Gvr2010 
05389-0713 49 Ori      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Abt (1965).                                                             AbH1965 
05389-1334 GAL 392     Hipparcos suspected non-single.                                                 
                       Object #196 in Gallo's original list.                                   Gal1914 
05391+1747 BPM 139     [PM2000]  284438 + [PM2000]  284293.                                    Gvr2010 
05391-5008 HJ 3789     B is CD-50@1871.                                                                
05391-7100 OGL 392     LMC178.6.14067 + LMC178.6.15179                                         Pli2012 
05391-7149 OGL 393     LMC179.8.23263 + LMC179.8.23619                                         Pli2012 
05391-7157 OGL 394     LMC180.5.22705 + LMC180.5.23355                                         Pli2012 
05392+2317 STF 755     124 Tau. C is a spectroscopic binary.                                           
05393-6750 OGL 395     LMC173.4.13898 + LMC173.4.14451                                         Pli2012 
05394+1658 BPMA 13     [PM2000]  285302 + [PM2000]  285761.                                    Gvr2010 
05394+1649 BPMA 14     [PM2000]  285537 + [PM2000]  286099.                                    Gvr2010 
05394+1618 BPM 140     [PM2000]  285398 + [PM2000]  285298.                                    Gvr2010 
05394-7001 SKF1049     OGL 396. LMC176.1.34431 + LMC176.1.34425                                Pli2012 
05395+1644 BPMA 15     [PM2000]  285719 + [PM2000]  285027.                                    Gvr2010 
05395-0334 VIG   8     Optical/physical nature of the two faint companions is undefined.       Vig2012 
05396+1531 BPM 141     [PM2000]  286142 + [PM2000]  286564.                                    Gvr2010 
05396-3404 HDO 193     alp Col = Phact                                                                 
05398+1537 BPM 142     [PM2000]  286537 + [PM2000]  286571.                                    Gvr2010 
05398-6859 OGL 397     LMC175.4.34483 + LMC175.4.34571                                         Pli2012 
05399+5145 ES  893     SMA  57.                                                                        
05399+1634 BPM 143     [PM2000]  286991 + [PM2000]  286795.                                    Gvr2010 
05400+1658 BPM 145     [PM2000]  287347 + [PM2000]  287190.                                    Gvr2010 
05400+1626 BPM 144     [PM2000]  287202 + [PM2000]  287554.                                    Gvr2010 
05401-7133 OGL 398     LMC179.6.15460 + LMC179.6.15507                                         Pli2012 
05402+1015 SHY 487     HIP  26680 + HIP  26646.                                                        
05402-6912 OGL 399     LMC175.3.9920  + LMC175.3.9955                                          Pli2012 
05403+3757 SEI 367     ALI 546.                                                                        
05403+1521 SHY  28     BC: HIP  26690 + HIP  26844.                                                    
05403-7112 OGL 400     LMC178.1.26335 + LMC178.1.115                                           Pli2012 
05404+2448 WNO  45     Identified as WNO  16 in USN1976. Discovered by B.Y. Riepe              USN1976 
                       and also known as Riepe's double.                                               
                       GJ 1083 = G 100-28 = V780 Tau. Estimated age 1000-10000 Myr; masses             
                       0.20 +/- 0.04 and 0.13 +/- 0.02 Msun; a ~4.9 au.                        Jnn2014 
05404+1643 BPM 146     AB: [PM2000]  288389 + [PM2000]  288781.                                Gvr2010 
           BPM 147     BC: [PM2000]  288781 + [PM2000]  288600.                                Gvr2010 
05405-7027 OGL 401     LMC177.2.57937 + LMC177.2.58437                                         Pli2012 
05406+1638 BPM 148     [PM2000]  289234 + [PM2000]  289578.                                    Gvr2010 
05406-7151 OGL 402     LMC179.8.11252 + LMC179.8.11284                                         Pli2012 
05407+1704 BPMA 16     [PM2000]  289597 + [PM2000]  289795.                                    Gvr2010 
05407-0157 STF 774     AB: zet Ori = 50 Ori = Alnitak. A premature orbit has been computed.            
                       Spectral types of AB: O9.5Ibe and B0III.                                        
                       Levato et al. (ApJS, 68, 319, 1988) and Fullerton (1990, PhD thesis,    Lev1988 
                       U. Toronto) report small RV variations (<35 km/sec), not confirmed.     Ful1990 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Both A and B components were observed and appeared to be single.        Msn1998a
                       Classification of the B component is from Hoffleit &  Warren (1991).    Hof1991 
                       AC: Star C (mag. about 9, 60") may be physical.                                 
           NOI   1     Aa,Ab: Combined spectroscopic/astrometric solution, using NPOI                  
                       interferometric measures with radial velocities from disentangled               
                       spectra to determine first dynamical mass for an O-type supergiant.             
                       Mass of the O9.5Ib primary is 24.8 +/- 5.6 Msun, that of the B0/1               
                       secondary is 16.4 +/- 4.9 Msun.                                         NOI2011 
                       Aa,Ab: Hummel et al. (2013) calculated a combined interferometric/              
                       spectroscopic orbit of zet Ori. Derived masses are 14.0 +/- 2.2 and             
                       7.4 +/- 1.1 Msun; orbital parallax is 3.4 +/- 0.2 mas, but as this is           
                       based on rather low velocity amplitudes, the photometric distance               
                       (2.6 +0.4/-0.3 mas) is considered more robust. Based on photometric             
                       distance, spectral types for Aa, Ab, and B are O9.5Iab, B1IV, and               
                       B0III, respectively. Masses for Aa and Ab are 33 +/- 10 and 14 +/- 3            
                       Msun, considerably larger than the dynamical values.                    Hmm2013 
           STF 774     AC: H 4  21.                                                            MEv2010 
05408+1657 BPMA 17     [PM2000]  289777 + [PM2000]  290265.                                    Gvr2010 
05408+1539 BPM 149     [PM2000]  289939 + [PM2000]  289977.                                    Gvr2010 
05408-0806 CON  14     AB: MGM 369.                                                            Kkl2016 
05409+1625 BPM 150     [PM2000]  290186 + [PM2000]  289998.                                    Gvr2010 
05410+3106 J   937     Aka MNG   1.                                                            Dam2016a
05410+1620 BPM 151     [PM2000]  290443 + [PM2000]  290760.                                    Gvr2010 
05411+3550 ALV   2     SH 2-235 IRS 1. Luminous YSO in SH 2-235 molecular cloud.               Alv2004 
05411-7023 OGL 403     LMC177.3.13891 + LMC177.3.13893                                         Pli2012 
05412+1632 BPM 152     AB: [PM2000]  290981 + [PM2000]  291008.                                Gvr2010 
           BPM 153     AC: [PM2000]  290981 + [PM2000]  290861.                                Gvr2010 
           BPM 154     BC: [PM2000]  291008 + [PM2000]  290861.                                Gvr2010 
05412+1631 BPM 155     [PM2000]  291034 + [PM2000]  290895.                                    Gvr2010 
05413+5329 ENG  22     LDS 890.                                                                        
                       AB: NLTT 15439/15446                                                    Chm2004 
                       AB: HJL  72.                                                            HJL1986 
                       AB: SHY  29. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       AB: This is MN of 05167+4600.                                           Dam2017i
05413+2929 STF 764     A is a spectroscopic binary. B is BD+29@954.                                    
                       Primary is eclipsing binary of Beta Lyr -type, period 0.674 d.          Zas2012 
                       H N  75.                                                                MEv2010 
05413+1706 BPMA 19     [PM2000]  291462 + [PM2000]  291073.                                    Gvr2010 
05413+1704 BPMA 18     [PM2000]  291452 + [PM2000]  291820.                                    Gvr2010 
05413+1632 BU 1007     126 Tau. The variable radial velocity indicates a spectroscopic                 
                       subsystem; the RV range of the blended light is about 50 km/s.                  
                       Single night's measure in 1960 apparently does not refer to this pair.          
                       Observed delta m definitely larger than given in ADS.                   Wor1967b
                       Spectral types of primary and secondary assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 17.71 +/- 23.89, 9.78, and 6.41 Msun, respectively.           Mlk2012 
05413-2621 HJ 3788     B is CD-26@2394.                                                                
05414+1527 BPM 156     [PM2000]  291745 + [PM2000]  292018.                                    Gvr2010 
05415-0840 CON  16     AB: MGM 222.                                                            Kkl2016 
05416+1629 BPM 157     [PM2000]  292234 + [PM2000]  292274.                                    Gvr2010 
05416-7024 OGL 404     LMC177.3.26963 + LMC177.3.26962                                         Pli2012 
05416-7111 OGL 405     LMC178.1.32870 + LMC178.1.33290                                         Pli2012 
05417+1644 BPM 158     [PM2000]  292535 + [PM2000]  292075.                                    Gvr2010 
05417-0254 BU 1052     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.67 +/- 2.70, 2.57, and 1.58 Msun, respectively.             Mlk2012 
05418+1541 BPM 159     [PM2000]  292945 + [PM2000]  292733.                                    Gvr2010 
05418-0155 ALV   3     NGC 2024 IRS 2.                                                         Alv2004 
05420+3401 SEI 374     Aka TOB  37.                                                                    
05420+1640 BPM 160     [PM2000]  293486 + [PM2000]  293135.                                    Gvr2010 
05421+3245 HJ  369     Measure does not agree with HJ, but so identified by Doolittle.         Doo1923 
05421+1522 BPM 162     [PM2000]  293889 + [PM2000]  293594.                                    Gvr2010 
05421+1519 BPM 161     [PM2000]  293806 + [PM2000]  293833.                                    Gvr2010 
05422-7119 OGL 406     LMC179.4.27320 + LMC179.4.30768                                         Pli2012 
05423+3247 HJ  370     SEI 376.                                                                Nsn2017a
05423+1704 BPM 164     AB: [PM2000]  294490 + [PM2000]  294334.                                Gvr2010 
           BPM 165     AC: [PM2000]  294490 + [PM2000]  294161.                                Gvr2010 
           BPM 166     BC: [PM2000]  294334 + [PM2000]  294161.                                Gvr2010 
05423+1646 BPM 163     [PM2000]  294407 + [PM2000]  294228.                                    Gvr2010 
05423+1557 BPM 167     [PM2000]  294597 + [PM2000]  294432.                                    Gvr2010 
05424+7920 STF 695     AB: HJL  71.                                                            HJL1986 
05424+1640 BPM 168     [PM2000]  294701 + [PM2000]  294561.                                    Gvr2010 
05425+4053 WEI  10     B is BD+40@1384.                                                                
05426-6810 OGL 407     LMC181.7.13965 + LMC181.7.14774 + LMC181.7.15836                        Pli2012 
05427+1705 BPMA 20     [PM2000]  295643 + [PM2000]  296373.                                    Gvr2010 
05427+1651 BPM 169     [PM2000]  295609 + [PM2000]  295407.                                    Gvr2010 
05427+1643 BPM 170     [PM2000]  295816 + [PM2000]  295876.                                    Gvr2010 
05427+0241 LDS6192     HIP 26907. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
05428+3322 STF 773     AC: DOO   8.                                                                    
05428+1806 CHR 213     First detected as an occultation binary by Edwards et al.               Evn1980 
05428-7222 OGL 408     LMC180.1.10    + LMC180.1.12050                                         Pli2012 
05429+1650 BPM 171     [PM2000]  296510 + [PM2000]  296883.                                    Gvr2010 
05429+0001 STF 782     B is BD-00@1060.                                                                
05429-0648 A   494     Suspected RV variation not confirmed (Heintz 1981). The faint pair      Hei1981a
                       CD (mag. 10-13, 1.0") is 100" distant from AB.                                  
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.77 +/- 0.28, 2.78, and 1.30 Msun, respectively.  Mlk2012 
05431+3933 BRT2210     ALI 1059.                                                                       
05431+1701 BPM 172     [PM2000]  296994 + [PM2000]  297084.                                    Gvr2010 
05431-3516 FAB  19     Originally inserted as a new solution to HDS 763, it now appears that           
                       both pairs are real.                                                            
05432+1559 BPM 173     [PM2000]  297486 + [PM2000]  297074.                                    Gvr2010 
05435+1526 BPM 174     AB: [PM2000]  298316 + [PM2000]  298293.                                Gvr2010 
           BPM 175     AC: [PM2000]  298316 + [PM2000]  298674.                                Gvr2010 
           BPM 176     BC: [PM2000]  298293 + [PM2000]  298674.                                Gvr2010 
05435-0753 A   495     Angle decreasing. No measures 1963-1988, during which period nearly             
                       two quadrants were described.                                                   
05436+6633 HU 1109     A is reported to be variable, type unknown.                                     
05436+1510 BPM 177     [PM2000]  298697 + [PM2000]  298487.                                    Gvr2010 
05436+1506 BPM 178     [PM2000]  298805 + [PM2000]  299090.                                    Gvr2010 
05436+1300 A   117     A 14.5 magnitude star is 26" from A in 191@.                            B__1963b
05438+1650 BPM 180     [PM2000]  299538 + [PM2000]  299218.                                    Gvr2010 
05438+1543 BPM 179     [PM2000]  299328 + [PM2000]  299117.                                    Gvr2010 
05438-6811 OGL 409     LMC181.2.42    + LMC181.2.240                                           Pli2012 
05439+1620 BPM 181     [PM2000]  299743 + [PM2000]  299422.                                    Gvr2010 
05439-6827 OGL 410     LMC182.5.20806 + LMC182.5.21242                                         Pli2012 
05440+1616 BPM 183     [PM2000]  300068 + [PM2000]  300159.                                    Gvr2010 
05440+1611 BPM 184     [PM2000]  300096 + [PM2000]  300502.                                    Gvr2010 
05440+1549 BPM 185     [PM2000]  300192 + [PM2000]  300353.                                    Gvr2010 
05440+1548 BPM 182     [PM2000]  300036 + [PM2000]  299690.                                    Gvr2010 
05441+1556 BPM 186     [PM2000]  300517 + [PM2000]  300475.                                    Gvr2010 
05441+0249 HJ 2277     BAL 1677.                                                                       
05441-0229 A  2918     B is BD-02@1354.                                                                
05441-7116 OGL 411     LMC186.8.7     + LMC178.1.20316                                         Pli2012 
05441-7121 OGL 412     LMC179.4.38816 + LMC179.4.40244                                         Pli2012 
05442+1644 BPM 187     [PM2000]  300711 + [PM2000]  300977.                                    Gvr2010 
05442+1544 BPM 188     [PM2000]  300888 + [PM2000]  300602.                                    Gvr2010 
05443+1546 BPM 189     [PM2000]  301137 + [PM2000]  300719.                                    Gvr2010 
05444+1551 BPM 190     [PM2000]  301700 + [PM2000]  301872.                                    Gvr2010 
05444-0528 SHY 489     HIP  27069 + HIP  26588.                                                        
05445-2227 H 6  40     AB: gam Lep = 13 Lep.H VI 40. LDS 148.                                          
                       AB: NLTT 15560/15558                                                    Chm2004 
                       AB: B = AK Lep.                                                         Tok2014d
           H 5  50     BC: H V 50. C is CPD-22@883.                                                    
05446+1607 BPM 195     [PM2000]  302614 + [PM2000]  302673.                                    Gvr2010 
05446+1545 BPM 191     [PM2000]  302270 + [PM2000]  302653.                                    Gvr2010 
05446+1536 BPM 192     [PM2000]  302289 + [PM2000]  302408.                                    Gvr2010 
05446+1532 BPM 193     [PM2000]  302321 + [PM2000]  302640.                                    Gvr2010 
05466+0110 RAG   1     Primary is exoplanet host, P=14.3d, 2135d. Benedict et al. (2010)       AST2010 
                       astrom. orbit for planet c, 1.05mas axis.                               Tok2014d
05447+1607 BPM 196     [PM2000]  302752 + [PM2000]  302935.                                    Gvr2010 
05447+1546 BPM 194     [PM2000]  302592 + [PM2000]  302169.                                    Gvr2010 
05447+1538 BPM 197     [PM2000]  302856 + [PM2000]  302664.                                    Gvr2010 
05447+0350 STF 788     AB: H 2  61.                                                            MEv2010 
05447-4618 HJ 3797     B is CD-46@1983.                                                                
05448+1617 BPM 198     [PM2000]  302916 + [PM2000]  302938.                                    Gvr2010 
05448+1539 BPM 199     [PM2000]  302951 + [PM2000]  303127.                                    Gvr2010 
05449+1645 BPM 200     [PM2000]  303487 + [PM2000]  303652.                                    Gvr2010 
05450+1604 BPM 201     [PM2000]  303785 + [PM2000]  303699.                                    Gvr2010 
05451+1605 BPM 206     [PM2000]  304191 + [PM2000]  304389.                                    Gvr2010 
05451+1556 BPM 204     AB: [PM2000]  304185 + [PM2000]  304317.                                Gvr2010 
           BPM 205     BC: [PM2000]  304317 + [PM2000]  304322.                                Gvr2010 
05451+1532 BPM 202     [PM2000]  303972 + [PM2000]  304218.                                    Gvr2010 
05451+1144 BPM 203     [PM2000]  304093 + [PM2000]  304082.                                    Gvr2010 
05454+1123 BPM 207     [PM2000]  305302 + [PM2000]  305441.                                    Gvr2010 
05454-0037 HER  14     Additional notes may be found in Herbig (1962).                         Her1962 
05456-1503 ENG  23     B is BD-15@1153.                                                                
05457+1636 BPM 208     [PM2000]  306501 + [PM2000]  306641.                                    Gvr2010 
05457-6833 OGL 413     LMC182.3.133   + LMC182.3.280                                           Pli2012 
05459+2555 STT 116     DE: Also known as TAR   1.                                                      
05460+1048 A  2711     May be a short period binary, but the few measures do not even permit           
                       certain determination of the direction of motion.                               
05460-0416 STF 790     Composite spectrum; K1III+G0IV.                                                 
05460-3218 mu Col      Additional radial velocity measurements by Fullerton (1990)             Ful1990 
                       and Penny et al. (1993) confirm the lack of                             Pny1993 
                       variability.                                                            Msn1998a
05461-6920 OGL 414     LMC183.2.41    + LMC183.2.263                                           Pli2012 
05462-2100 BRT 302     ARA1281.                                                                        
05462-7027 OGL 415     LMC185.7.75526 + LMC185.7.75527                                         Pli2012 
05463+3736 GCB  66     A is the short-period variable EU Tau.                                          
05464-6835 OGL 416     LMC182.3.18716 + LMC182.3.18717                                         Pli2012 
05465+7437 YSC 148     Docobo et al. (2014) use the spectroscopic elements of Latham et al.            
                       (2002), together with speckle data and the Hipparcos parallax, and      Lat2002 
                       derive possible solutions for both direct and retrograde motion. The            
                       resulting masses are 0.99 +/- 0.09 and 0.63 +/- 0.08 Msun.              Doc2014h
05465-6903 OGL 417     LMC183.4.105   + LMC183.4.1756                                          Pli2012 
05466+0110 GC 7226     Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from the Geneva           
                       Extrasolar Planet Search Programs home page.                            HaI2001 
05467+4322 ES 1530     BRT 90.                                                                         
05467+0005 BU  559     This system, listed in the ADS as #4374 was purged from an earlier              
                       edition of the WDS probably as it was buried in reflection nebulae              
                       NGC 2068.                                                                       
05468+3700 ALI 309     MLB 826.                                                                        
05469+0931 J   251     HJL  73.                                                                HJL1986 
05470+1600 BPM 209     [PM2000]  310850 + [PM2000]  310780.                                    Gvr2010 
05471+0023 PAD  24     MGM3385.                                                                Kkl2016 
05471+0022 PAD  25     MGM3374.                                                                Kkl2016 
05472+2153 HU   39     Measures scattering around 45 degrees, with variation in distance               
                       evident. Motion in a highly-inclined orbit?                                     
05472+1429 CHR 160     131 Tau.                                                                        
05472-2430 HJ 3798     B is CD-24@3430.                                                                
05473+3222 J   902     This pair is 1.36s f and +30.7" nf of BD+32@1087.                               
05473-5104 LGR   1     Primary is bet Pic, secondary is probably a giant planet. Estimated             
                       mass of companion 9 +3/-2 Mjup, assuming a distance of 19.3 +/- 0.2pc           
                       and an age 12 +8/-4 Myr.                                                Lgr2009a
                       Planetary companion later confirmed, with multiple measurements.                
                       Member of the bet Pic moving group.                                     Zuc2001b
                       Assuming an age of 12 +8/-4 Myr (Bonnefoy et al. 2013 A&A 555, A107),           
                       Absil et al. (2013) estimate the mass of bet Pic b at 8.0 +3.2/-2.1             
                       Mjup. Using the revised age of 21 +/- 4 Myr by Binks & Jeffries (2014           
                       MNRAS 438, L11) leads to a mass of 10.6 +1.2/-1.8 Mjup.                 Abs2013 
                       Nielsen et al. (2014) find a semi-major axis of 9.1 +5/-0.5 au and a            
                       period of 21 +21/-2 y; the planet appears to have reached maximum               
                       elongation and is moving back toward the star, with minimum angular             
                       separation expected ~2018. The primary mass is 1.76 +0.18/-0.17 Msun.   Nls2014 
05473-6832 OGL 418     LMC182.3.18737 + LMC182.3.18800                                         Pli2012 
05473-7119 OGL 419     LMC187.5.29667 + LMC187.5.29853                                         Pli2012 
05474+2858 HJ  709     First distance probably in error (Doolittle).                           Doo1923 
                       Two faint stars measured near the position given for HJ 709, BDS 2951.          
                       Neither fits the earlier descriptions by Herschel, Burnham, and                 
                       Doolittle, but these do not agree among themselves, either.             B__1962d
05474-1032 MCA  22     An eclipsing binary and spectroscopic triple, V1031 Ori, with the               
                       (presumably) wider pair now resolved by speckle interferometry.                 
                       Zasche et al. (2014) derive a combined solution, including                      
                       interferometry plus times-of-minimia variation in the eclipsing-binary          
                       primary.                                                                Zas2014b
05476+1736 BU 1401     Probably STF 767 rej.                                                           
05477+1354 HJ 3279     133 Tau.                                                                        
05479+3510 HO   19     SEI 385.                                                                Nsn2017a
05479+2441 STTA 66     B is BD+24@965.                                                                 
05479-6847 OGL 420     LMC189.7.12    + LMC189.7.52                                            Pli2012 
05480+0627 STF 795     52 Ori. One component is a spectroscopic binary.                                
                       H 1  20.                                                                MEv2010 
05482+0137 A  2657     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 3.86 +/- 2.35, 4.13, and 1.45 Msun, respectively.             Mlk2012 
05483-6948 OGL 421     LMC184.3.24360 + LMC184.3.24357                                         Pli2012 
05483-7002 OGL 422     LMC184.1.30453 + LMC184.1.30754                                         Pli2012 
05484+2052 STT 118     A is a spectroscopic binary. A premature visual orbit has been                  
                       computed.                                                                       
05485+2118 GIC  60     G100-037/G100-038.                                                              
05485-7127 OGL 423     LMC187.4.56    + LMC187.4.1142                                          Pli2012 
05486-7013 OGL 424     LMC185.4.18027 + LMC185.4.18356                                         Pli2012 
05487+1549 BPM 210     [PM2000]  317297 + [PM2000]  317306.                                    Gvr2010 
05488+1254 BPM 211     [PM2000]  317402 + [PM2000]  316980.                                    Gvr2010 
05488-6552 HJ 3815     B is CPD-65@506.                                                                
05489+2101 BU   93     B is BD+20@1112.                                                                
05489-7157 OGL 425     LMC188.4.9     + LMC188.4.10                                            Pli2012 
05490+3451 SEI 386     J 1114.                                                                         
05490+2434 MCA  23     132 Tau.                                                                        
05490+0108 GRE   2     IRAS 05464+0106 = PDS 17.                                               Gre1992 
05490-1105 GAL 393     Object #205 in Gallo's original list.                                   Gal1914 
05490-7150 OGL 426     LMC187.1.114   + LMC187.1.697                                           Pli2012 
05491-6108 HJ 3810     B is CPD-61@532.                                                                
05492+3911 BU  192     tau Aur = 29 Aur                                                                
           H 5  21     H V 21.                                                                         
05495+1239 BUP  84     134 Tau.                                                                        
05495-7047 OGL 427     LMC186.4.38205 + LMC186.4.38233                                         Pli2012 
05495-7100 OGL 428     LMC186.3.12362 + LMC186.3.12420                                         Pli2012 
05495-7123 OGL 429     LMC187.4.309   + LMC187.4.264                                           Pli2012 
05496+2244 CHR 205     First detected as an occultation binary by Africano.                    Afr1975 
05496-1429 BU   94     BDS 3207 probably same star.                                                    
05496-6836 OGL 430     LMC189.6.10983 + LMC189.6.10979                                         Pli2012 
05497-0427 SCJ   3     B is BD-04@1249.                                                                
05497-6843 OGL 431     LMC189.7.11539 + LMC189.7.11612                                         Pli2012 
05498+3258 S   500     B is BD+32@1099.                                                                
                       Although the field is crowded and the PM is small, it is CPM. With PM           
                       of 20 mas/yr it would move by 3.6" in 180yr since 1825.                 Tok2014d
05498-7225 TOK 431     First resolution, estimated period 12 yr.                               Tok2013b
05499+3147 STF 796     AB: H 1  67.                                                            MEv2010 
05499+2259 ARN  91     AC: Secondary of 05500+2258 ARN 91 found to be primary of 05499+2259            
                       POU 789. Pairs merged, with quadrant flip to ARN 91.                            
05500+2551 OL  165     Aka COU 765.                                                                    
05502+2658 RUC  19     Primary is V781 Tau.                                                            
05503-6854 OGL 432     LMC189.8.10709 + LMC189.8.12244                                         Pli2012 
05505-5246 B  1493     Spectrum composite; K0-1III+A4V+A.                                              
05506+5655 H 4 125     H IV 125. 29 Cam.                                                               
05507-6838 OGL 433     LMC189.3.372   + LMC189.3.990                                           Pli2012 
05507-7159 OGL 434     LMC188.4.11434 + LMC188.4.11429                                         Pli2012 
05510+2758 BU 1054     136 Tau. A possible occultation binary. Misidentified by Burnham,       Bu_1894 
                       corrected by van den Bos.                                               B__1960b
05510-3546 WFC  31     bet Col = Wazn                                                                  
05510-6954 HJ 3820     B is CPD-69@@535.                                                               
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
05514+3535 HJ  710     Points to a 14th magnitude star 30".                                            
05514+3207 ES  415     A is variable.                                                                  
05514-1108 GAL 394     Object #206 in Gallo's original list.                                   Gal1914 
05515+3909 H 5  90     nu Aur = 32 Aur. H V 90.                                                        
05515+1548 BPM 213     [PM2000]  328749 + [PM2000]  328867.                                    Gvr2010 
05515+1544 BPM 214     [PM2000]  328857 + [PM2000]  328714.                                    Gvr2010 
05515+1217 BPM 212     [PM2000]  328544 + [PM2000]  328831.                                    Gvr2010 
05516-6918 OGL 435     LMC190.2.201   + LMC190.2.474                                           Pli2012 
05517+3838 BRT2211     ALI 811.                                                                        
05518-4434 BLR   1     DENIS J055146.0-443412.2. NTT/SofI IR spectro-imager observations by            
                       Billeres et al. (2005) resolved the first wide ultracool binary dwarf;          
                       spectral types are M8.5 + L0.                                           Blr2005 
05520-0715 J  1913     Previously published coordinates corrected by +3'. Pair is +5s, +4'             
                       from BU 95.                                                             J__1949a
05521-6922 OGL 436     LMC190.2.13    + LMC190.2.123                                           Pli2012 
05522+1658 BPM 215     [PM2000]  331791 + [PM2000]  331753.                                    Gvr2010 
05522+1542 BPM 216     [PM2000]  332058 + [PM2000]  332011.                                    Gvr2010 
05522-6826 OGL 437     LMC189.4.9311  + LMC189.4.10038                                         Pli2012 
05523+3235 SEI 414     Identification of SEI 414 is uncertain,but is appears to correspond to          
                       the A and C components of 05523+3235.                                           
05523+1509 BPM 217     AB: [PM2000]  332310 + [PM2000]  332065.                                Gvr2010 
           BPM 218     BC: [PM2000]  332065 + [PM2000]  331572.                                Gvr2010 
05523+1431 BPM 219     AB: [PM2000]  332440 + [PM2000]  331988.                                Gvr2010 
           BPM 220     AC: [PM2000]  332440 + [PM2000]  332891.                                Gvr2010 
05523+1253 COU2704     BD: Couteau erroneously calls this AD.                                  Cou1958c
05524+3752 SEI 402     ALI 549.                                                                        
05524+3618 AG  101     SEI 409.                                                                Nsn2017b
05524+1711 BPM 221     [PM2000]  332860 + [PM2000]  332448.                                    Gvr2010 
05524+0151 BU 1404     56 Ori.                                                                         
05524-6940 OGL 438     LMC191.4.203   + LMC191.4.204                                           Pli2012 
05525+3235 SEI 424     AB: Appears to be the same pair as SEI 420.                                     
05525+3233 SEI 421     SEI 423.                                                                Nsn2017b
05525+1548 BID   1     A is a Mira-type variable, Z Tau.                                               
05525-0217 HDS 787     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.29 +/- 0.28, 2.19, and 1.20 Msun, respectively.             Mlk2012 
05526+1510 BPM 222     [PM2000]  333540 + [PM2000]  333628.                                    Gvr2010 
05526+1402 J   948     BRT 1185.                                                                       
05526-3738 I    64     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
05527+3731 ES 2341     ALI 550.                                                                        
05528+3233 SEI 428     Hipparcos suspected non-single.                                                 
05528+2946 STF 808     AC: HJL  74.                                                            HJL1986 
05529+3427 SHY 492     AC: HIP  27791 + HIP  28872.                                                    
05530+3624 HJ 5540     ALI 312. SEI 427.                                                               
05531+4127 ARG  61     B is BD+41@1290.                                                                
05531+1501 BPM 223     [PM2000]  335794 + [PM2000]  336159.                                    Gvr2010 
05531-6845 OGL 439     LMC189.2.9876  + LMC189.2.10434                                         Pli2012 
05531-7125 OGL 440     LMC194.5.537   + LMC194.5.1400                                          Pli2012 
05532+1424 J   656     OL 153 and GCB 13 are the same as this star                             Hei1985a
05533+1611 BPM 224     [PM2000]  336700 + [PM2000]  336469.                                    Gvr2010 
05534-0333 A  2919     Change in angle for AB doubtful, but separation certainly smaller.              
                       Error or misprint of 10deg in my angle for 1960 appears probable.       B__1960a
                       Probably optical.                                                       B__1962d
                       A faint pair 10s p 3' s.                                                        
                       The faint pair must be 10s following.                                   Dam2012 
05537+1245 BPM 225     [PM2000]  338633 + [PM2000]  339014.                                    Gvr2010 
05538-2218 BRT1382     CD-22@2561.                                                                     
05539+1653 BPM 226     [PM2000]  339901 + [PM2000]  340312.                                    Gvr2010 
05540+1552 BPM 228     [PM2000]  340363 + [PM2000]  340293.                                    Gvr2010 
05540+1225 LDS 891     NLTT 15772/15768                                                        Chm2004 
05540+1146 BPM 227     [PM2000]  340157 + [PM2000]  340110.                                    Gvr2010 
05541+0140 RST5219     Pre-main sequence star HBC 515, located in the Orion L1622 cometary             
           HBC 515     cloud. The primary appears to be comprised of two ~equal brightness             
                       weakline T Tauri stars of spectral type K2V. The B component dominates          
                       the system at mid-infrared wavelengths, suggesting that it is a                 
                       protostar still embedded in the nascent cloud of HBC 515.  The C and D          
                       components (L1622-6 and L1622-6N) are also T Tau stars and likely               
                       physically associated.                                                  Rep2010 
05542+1545 BPM 229     [PM2000]  341008 + [PM2000]  341038.                                    Gvr2010 
05542-2909 FIN 382     Angle decreasing.                                                               
05543+1555 BPM 230     [PM2000]  341566 + [PM2000]  342144.                                    Gvr2010 
05543+0143 CHN  19     HBC 190 = LkHa 336. Pre-main sequence stars in the Lynds 1622 star-             
                       forming cloud. Kun et al. (2008) derives effective temperatures, ages,  Kun2008 
                       and masses for both components based on model fitting and their                 
                       visible and IR data, assuming a distance of 400pc.                              
05543-2553 I  1614     B is CD-25@2770.                                                                
05543-7128 OGL 441     LMC194.5.8083  + LMC194.4.81                                            Pli2012 
05544+3836 WEI  11     B is BD+38@1326.                                                                
05544+2017 KNG   1     chi 1 Ori                                                                       
                       Combined astrometric/spectroscopic solution by Irwin et al. (1992)      Irw1992a
                       2002.161: This observation agrees with the orbit of Han & Gatewood      HaI2002 
                       (2002).                                                                         
                       Koenig et al. (2002) derive masses of 1.02+-0.08 and 0.15+-0.01 Msun.   Kng2002 
05544+0152 REP   6     L1622-10. Pre-main sequence stars in Lynds 1622 star-forming cloud.             
                       Kun et al. (2008) derives effective temperatures, ages, and masses for  Kun2008 
                       the A and B components based on model fitting and their visible and IR          
                       data, assuming a distance of 400pc.                                             
05544-7023 OGL 442     LMC192.3.122   + LMC192.3.1429                                          Pli2012 
05545-7044 OGL 443     LMC193.4.680   + LMC193.4.1614                                          Pli2012 
05546-7012 OGL 444     LMC192.4.133   + LMC192.4.1646                                          Pli2012 
05547+1351 S   502     STTA 68. B is BD+13@1027.                                                       
                       Both components were observed and appeared to be single.                Msn1998a
05548+3612 SEI 435     Duplicity not apparent on POSS plate; one component may be either a             
                       variable star or a flaw on AC Potsdam plate.                                    
05549+3836 COU2181     TDS3420.                                                                        
05549+1359 BPM 232     [PM2000]  344577 + [PM2000]  344421.                                    Gvr2010 
05549+1345 BPM 231     [PM2000]  344453 + [PM2000]  344387.                                    Gvr2010 
05549+0702 STF 817     H 4  98.                                                                MEv2010 
05549-7528 TOK 102     HIP 27957. Several other components are seen in the ANDICAM field,              
                       N*=35.                                                                  Tok2011a
05550+1616 BPMA 21     AB: [PM2000]  344770 + [PM2000]  344112.                                Gvr2010 
           BPMA 22     BC: [PM2000]  344112 + [PM2000]  344444.                                Gvr2010 
05551+1203 BPM 233     [PM2000]  345570 + [PM2000]  345715.                                    Gvr2010 
05552+0724 KAR   1     alp Ori = 58 Ori = Betelgeuse. Irregular variable, spectrum                     
                       M1-2Ia-Iab. Two close companions have been reported, detected by                
                       speckle interferometry.                                                         
           H 6  39     H VI 39.                                                                        
05553+1516 BPM 234     [PM2000]  346272 + [PM2000]  346598.                                    Gvr2010 
05553+1220 BPM 235     [PM2000]  346508 + [PM2000]  346532.                                    Gvr2010 
05556+5328 STT 120     B is BD+53@963.                                                                 
05557-3806 SHY 493     HIP  28036 + HIP  26990.                                                        
05558+4651 LDS3680     NLTT 15797/15796                                                        Chm2004 
05560+3949 ES 2153     ADS 4527a.                                                                      
                       Aka HDS 799.                                                            Dam2016a
05561+1356 S   503     AB: B is BD+13@1037.                                                            
                       AB, AC, and AD: Optical pair, based on study of relative motion of the          
                       components using the method of apparent motion parameters.              Kiy2008 
                       AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
05561+1302 BPM 236     [PM2000]  350375 + [PM2000]  351046.                                    Gvr2010 
05562+3143 HJ  714     SEI 444.                                                                Nsn2017b
05562+1755 BPM 237     [PM2000]  350997 + [PM2000]  351100.                                    Gvr2010 
05563+4353 ES 1531     AB: Barton identifies BRT 91 as same star.                              Brt1926b
05563+3140 HJ  715     SEI 445.                                                                Nsn2017b
05564+1634 BPM 238     [PM2000]  352134 + [PM2000]  351978.                                    Gvr2010 
05565-2631 B    94     1989.9362: This system was last resolved visually in 1978, and appears          
                       to be continuing to approach periastron.                                Hrt1993 
05566+1129 BPM 239     [PM2000]  353046 + [PM2000]  352711.                                    Gvr2010 
05566-7110 OGL 445     LMC193.2.5397  + LMC193.2.5487                                          Pli2012 
05567+1231 BPM 240     [PM2000]  353373 + [PM2000]  353196.                                    Gvr2010 
05567-7012 OGL 446     LMC199.5.36    + LMC199.5.193                                           Pli2012 
05568+1413 BPM 241     [PM2000]  354005 + [PM2000]  353928.                                    Gvr2010 
05569+3615 SEI 447     Secondary not seen on POSS plate; may be either variable star or flaw           
                       on AC Potsdam plate.                                                            
05569+2121 CHR 214     First detected as an occultation binary by Evans & Edwards.             Evn1983a
05569-1836 B  1953     J  1469. Identified by Jonckheere as BOS 1953 in his 1962 catalog.      J__1962a
05569-0700 HJ   33     AB: J  1915AC.                                                                  
           AOT  24     AC: J  1915AB.                                                                  
           AOT  24     BC: J  3228. J  1915BC.                                                 J__1962a
05570+1022 BPM 242     [PM2000]  355093 + [PM2000]  355331.                                    Gvr2010 
05570-7152 OGL 447     LMC194.1.135   + LMC194.1.687                                           Pli2012 
05571+1014 ARG  63     B is BD+10@939a.                                                                
05573+3601 HU 1235     Measure does not confirm apparent motion shown in IDS.                  Wor1967b
05573-2720 HJ 3818     Spectrum: G8/K0IIICNpv.                                                         
05574-6852 OGL 448     LMC196.1.80    + LMC196.1.833                                           Pli2012 
05575-3517 HJ 3819     gam Col.                                                                        
05576-6831 OGL 449     LMC196.3.15    + LMC196.3.93                                            Pli2012 
05576-7004 OGL 450     LMC198.8.6317  + LMC198.8.6316                                          Pli2012 
05578-1413 GAL 395     Object #208 in Gallo's original list.                                   Gal1914 
05578-7125 OGL 451     LMC194.4.4587  + LMC194.4.4769                                          Pli2012 
05580-6835 OGL 452     LMC196.3.66    + LMC196.3.65                                            Pli2012 
05581-3548 RSS  94     HIP 28241. No V-photometry for B in either WDS or SIMBAD.               Tok2011a
           TOK 212     A triple system consisting of the 0".54 inner pair resolved with NICI           
                       and the physical companion B at 11".                                    Tok2012a
05581-7000 OGL 453     LMC198.8.5791  + LMC198.8.5806                                          Pli2012 
05581-7108 OGL 454     LMC200.7.2     + LMC200.7.32                                            Pli2012 
05584+0150 H 5 100     H V 100. 59 Ori. A Delta Scuti-type variable, V1004 Ori, and also a             
                       spectroscopic binary.                                                           
05584-0439 LDS3684     AD: NLTT 15871/15867                                                    Chm2004 
           A   322     Pair bound. Primary is G0. B component estimated mass 0.50 +/- 0.02             
                       Msun, spectral type M0-M2.                                              Egn2007 
05586+2133 BRT2336     J 2588.                                                                         
05586-7147 OGL 455     LMC194.1.3678  + LMC194.1.3680                                          Pli2012 
05587-0110 LDS5668     LDS6194.                                                                        
05587-6856 OGL 456     LMC196.1.6419  + LMC196.1.6507                                          Pli2012 
05588+2121 JNN 267     LHS 6097. Estimated age 1000-10000 Myr; masses 0.20 +/- 0.04 and 0.10           
                       +/- 0.01 Msun; a ~8.1 au.                                               Jnn2014 
05588+0033 KUI  22     60 Ori. A is a spectroscopic binary.                                            
05589+1735 BPM 243     [PM2000]  364266 + [PM2000]  364720.                                    Gvr2010 
05589+1248 STT 124     1980.1560: This measure was incorrectly attributed to STF 784 in                
                       McAlister et al. (1983).                                                McA1983 
05589-3422 GC 7577     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
05590+1321 HJ 3280     Probably J  1916.                                                       Nsn2016 
05590-1729 LDS 150     LDS5193.                                                                        
05590-7040 OGL 457     LMC199.8.4949  + LMC199.8.4969                                          Pli2012 
05592+7749 MLR 470     Also known as HDS 811.                                                          
05594-0642 HDS 826     YSC 187.                                                                        
05595+5853 ES 9002     Previously known as ES   66a.                                                   
05595+5417 ENG  24     33 Aur = del Aur                                                                
05595+4457 H 6  88     AB: bet Aur = 34 Aur = Menkalinan.  H VI 88. An Algol-type system,              
                       P = 3.96d. According to R.G. Aitken, this is the third binary           A__1935f
                       recognized by spectroscopic methods. It was identified as such by Miss          
                       Maury at the Harvard College Observatory in early 1890.                         
           KOE   1     Aa,Ab: Visual orbit by Hummel et al. (1995) based on astrometry from    MkT1995 
                       Mark III interferometer. Additional spectroscopic data yield component          
                       masses, luminosities, radii, effective temperatures, and distance.              
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1995).                                                   MkT1995 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 4.70 +/- 9.41, 3.85, and 2.19 Msun, respectively.  Mlk2012 
05595+1522 HEI 112     BC: AB is 34 deg at 49", J 2735 is not AB and not in BD according to            
                       Heintz.                                                                 Hei1983a
05596+1130 BPM 244     [PM2000]  367567 + [PM2000]  367897.                                    Gvr2010 
05597+3713 STT 545     37 Aur = the Aur. A is a variable of the Alpha CVn type.                        
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AC: H 5  89.  AD: H 6  34.                                              MEv2010 
05599+5834 GIC  61     G192-011/G192-012 = GJ 3371A+3372B. The A component is the variable             
                       star EG Cam.                                                                    
05599+1234 BPM 245     [PM2000]  368722 + [PM2000]  369058.                                    Gvr2010 
05599-3703 B  1044     HIP 28403.                                                              Tok2011a