13002-2355 I  1225     Measures uncertain, too close. Needs speckle.                                   
13003+3047 BU 1081     AB. 37 Com.                                                                     
           HDS1823     Aa,Ab. 1996.4274: Very weak detection, possibly an artifact.            Msn1999b
13003-6413 RST5372     Spectrum: F3/6IV/V+A.                                                           
13004+3545 HU 1141     Variability has been reported.                                                  
13005-0604 HJ 1224     Motion of pair represented by relative proper motion 0.104" in                  
                       81.8deg.  Footnote in ADS should be deleted; measure of 1922 is by              
                       Gauchet, from his own plate, but that of 1893 was taken by him from             
                       the San Fernando Astrographic Catalogue.                                B__1951a
13006+5904 FAR  15     GRV1201.  Primary is white dwarf WD 1258+593 = GD 322.                  Far2005b
13006-0322 AGC   5     46 Vir.                                                                         
13007+5622 BU 1082     78 UMa.                                                                 Baz1939b
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.69 +/- 0.73, 2.38, and 1.35 Msun, respectively.             Mlk2012 
13008+1423 STF1705     HJL 180.                                                                HJL1986 
13008+1223 GDM   1     AC: GJ 494 + ULAS J130041.72+122114.7. Primary is flare star DT Vir.            
                       Goldman et al. (2010 derive a spectral type T8.9 +0.2/-0.2 for this             
                       distant companion to Ross 458.                                          Gdm2010 
                       Based on colors and absolute magnitudes, Scholz et al. (2010) derive a          
                       spectral type T7.0 +/- 1.0 for the C component.                         Soz2010b
13014-2722 TOK 154     HIP 63559. A is SB without orbit, N04: dRV=17.0.                        Tok2011a
13015-5808 COO 146     Spectrum: A5/7+A1/2V.                                                           
13018+6337 LDS2662     M3.5 companion, distance just over 2' from F6 dwarf HD 113337 = HIP             
                       63584 = 2MASS J13014695+6336368. The pm for the M dwarf is -151+016,            
                       consistent with the brighter star pm of -171+025.  The spectroscopic            
                       distance for the fainter star is 36pc, compatible with the Hipparcos            
                       distance of 26.72 pc for HD 113337.                                     Red2007a
           JNN  83     Ba,Bb: 13015+6338 JNN  83 was found to be the B component of                    
                       13018+6337 LDS2662AB; systems merged.                                           
13020+4241 JNN  84     The companion to 2MASS J13015919+4241160 is clearly inconsistent with           
                       a background contaminant, but the astrometry is also inconsistent with          
                       a simple orbital motion of B around A - for instance, the separation            
                       decreases from June 2008 to February 2009, but then increases again to          
                       June 2009. This could for instance imply that either A or B is a close          
                       unresolved binary, where the photo-center shifts on a shorter                   
                       timescale than that of the AB orbit.                                    Jnn2012 
13020-0205 OSO  49     G014-024. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
13021+0717 STF1708     HJL 181.                                                                HJL1986 
13022+1058 BUP 147     eps Vir = 47 Vir = Vindemiatrix.                                                
13023-7133 del Mus     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13024-5201 JNN  85     Due to the very compact arrangement of the three components of 2MASS            
                       J13022691-5200507, it is highly probable that this is a physically              
                       bound triple system. Futhermore, the system is conspicuously close to           
                       the close binary J13025257-5201384 both on the sky and in distance (52          
                       versus 59 pc), hence this is a candidate quintuple system. Only one             
                       epoch of imaging exists, so common proper motion has not yet been               
                       demonstrated.                                                           Jnn2012 
13027-0159 HJ 1225     BAL 548.  Angular distance decrease 1.6" per century. Angular position          
                       decrease 1.8 degree per century. Minimal angular distance calculated,           
                       7.6" between 2600-2630 years.                                           FMR1999c
13029-6328 NZO  35     LDS 430.                                                                        
13030+0018 GRV1083     Aka SLW 816.                                                                    
13031+2358 LDS2896     LDS5220.                                                                        
13031-7129 CHR 228     As was the case with CHR 227, this star falls within the declination            
                       band missed in the surveys of Rossiter (1955) and van den Bos (1957).   Rst1955 
                       If physical, this 0".56 pair would presumably have an extremely long    B__1957a
                       period, given the spectral type and large calculated distance of its            
                       primary.  The small change in theta seen over 2.75 years is consistent          
                       with this, implying a period of order 500 - 600 years.                          
                       The star is noted in Abt & Biggs (1972) as having variable radial       AbH1972 
                       velocity; Hoffleit & Warren (1991) also note photometric variability    Hof1991 
                       of amplitude ~0.2 mag, as well as variability in the line width of              
                       H-alpha emission.                                                       Hrt1996b
13033-5936 COO 147     Spectrum: F5IV/V+A/F.                                                           
13038+2135 LDS2897     NLTT 32753/32754                                                        Chm2004 
13038-0510 GC 17714    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
           EVT   3     Primary is BY Dra type variable PX Vir.                                 EvT2012 
13038-2035 BU  341     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.39 +/- 0.67, 2.41, and 1.10 Msun, respectively.             Mlk2012 
13039-0340 BU  929     48 Vir.                                                                         
13040+2414 ITF  18     Aka ITF  96.                                                                    
13040-1738 BU  798     Closing. Earlier negative resuts are probably due to Burnham's                  
                       misidentification.                                                      B__1963b
13046+1028 OSO  50     G060-060. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
13047+1736 BPM 600     [PM2000] 1047714 + [PM2000] 1047703.                                    Gvr2010 
13050-4634 COO 148     SWR 137. CPM pair                                                       Skf2004 
13054-5735 I   914     Spectrum of secondary: A/F.                                                     
13055+0911 LDS 944     Wolf 472,3.  Also known as GEL   1.                                             
13057-2541 LIM   1     Kelu 1. Estimated orbital period >40 yrs, inclination >81deg.                   
                       Spectral types L2 +/- 1 and L3.5 +/- 1                                  Gno2006 
13058-3111 BRT2997     CD-30@10320?                                                                    
13062+2902 BU 1083     BC: Only two attempts since 1901, in 1958, with negative results.       B__1960b
13064+7618 HJ 2644     B is BD+77@501.                                                                 
13064+2109 CHR 150     Aa,Ab: 39 Com.                                                                  
13065-6505 HD 113659   LS 2919.  The classification is from Houk & Cowley (1975 Michigan               
                       Spectral Catalogue, vol. 1).                                            Msn1998a
13066+2226 LDS2899     LDS4315.                                                                        
13066-6434 I   916     Includes V948 Cen, an Algol type eclipsing binary, P = 0.97508d.        Zas2012 
13067-2111 HJ 2637     B is BD-20@3775.                                                                
13069-3407 HIP  64006  Astrometric binary. Elongated? Separation ~0.025", period ~1yr?                 
                       Accelerated pm.                                                         Tok2012b
13069-4954 DUN 128     xi 2 Cen. A is a spectroscopic binary.                                          
13072-5420 FIN  54     Includes V949 Cen, an Algol type eclipsing binary, P = 3.78697d.        Zas2012 
13073+0035 STF1719     HIP 64030. HIP 63810 at 2551" is CPM, possibly forming a wide triple            
                       system with AB = STF 1719 at 7".                                        Tok2011a
                       AB: A is SB1, P=445.8d                                                  Tok2014d
13074-5952 R   213     Spectrum composite; B9IV+F8-G2.                                                 
13075-6207 HJ 4568     B is CPD-61@3460.                                                               
13076+2629 BUP 148     B is BD+27@2217.                                                                
13077+2401 STT 259     B is BD+24@2540.                                                                
                       HJL 182.                                                                HJL1986 
                       SHY 245. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13081+2657 STT 260     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.47 +/- 0.91, 2.41, and 1.07 Msun, respectively.             Mlk2012 
13081-6518 RMK  16     the Mus. Wolf-Rayet binary, second brightest in the sky.                        
                       The classification is from Houk & Cowley (1975 Michigan Spectral                
                       Catalogue, vol. 1). Moffat & Seggewiss (1977 A&A 54, 607) found                 
                       evidence of orbital motion in the WR star, but the O star appeared              
                       stationary. We found a possible binary companion at a separation of             
                       0".04 which needs confirmation, but if correct, this suggests that the          
                       system is triple, consisting of a WR SB1 plus a distant O star.  The            
                       visual B component was observed and appeared to be single.              Msn1998a
                       The primary is the WR+O spectroscopic binary theta Mus = WR 48. B is            
                       reported as SB by both Chini et al. (2012) and Sota et al.              Cii2012 
                       (2014, ApJS 211, 10).                                                   Sna2014 
13084+6236 MLB 412     Heintz corrects the declination.                                        Hei1983a
13084+3019 JNN  88     Aside from the binary companion detected in the AstraLux images, the            
                       star has a possible wide companion at 101", as noted in the WDS.        Jnn2012 
13084+1529 STF1722     STF1726.                                                                        
13085+2249 POU3133     LDS2902.                                                                        
13085-0241 S   647     Primary is HY Vir, eclipsing binary of Algol-type, period 2.7323 d.     Zas2012 
13085-8243 HJ 4565     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
13086+1710 BPMA 45     [PM2000] 1049381 + [PM2000] 1049350.                                    Gvr2010 
13089+0512 CRJ   5     White-dwarf companion to G5IV-V star HD 114714 found via Keck NIRC2             
                       imaging and RV monitoring. Multi-epoch observations indicate companion          
                       is physical. Absolute magnitude of companion Mj = 13.97 +/- 0.11 and            
                       colors are consistent with a T3 dwarf, but dynamical considerations             
                       preclude interfpretation of a substellar companion. Minimum mass of             
                       companion 0.260 +/- 0.010 Msun.                                         CrJ2013b
13090+3353 LDS4321     NLTT 33051/33036                                                        Chm2004 
13093+4649 COU2105     Appears to be a 10' error in the original 1855 BD declination -                 
                       nothing  at purported coordinates.                                              
13095-1313 BRT2732     13 04.3 -12 47 (Mason) may be same star.                                        
13097+2900 LDS1365     A: Also known as GJ 1167 A, this star has a wide companion at about             
                       190" according to the WDS.                                              Jnn2012 
13097-2212 TOK  28     Primary is 20d SB1; estimated period of AO pair is 23y. G-solution in           
                       HIPPARCOS.                                                              Tok2006 
                       Triple: the inner SB1 of 20.4 day period has tertiary companion TOK 28          
                       at 0".31 with mass ratio of 0.2 which produces the acceleration and             
                       dmu. This tertiary is too faint to be resolved in the optical.          Tok2012a
13098+6214 STTA121     Pair appears in an appendix list, not part of discoverer's regular              
                       numbering sequence.                                                             
13099+5504 GRV1155     Common proper motion white dwarf pair found in SDSS data.                       
13099+3122 STF1727     HJL 183.                                                                HJL1986 
13099-0532 MCA  38     Aa,Ab: the Vir = 51 Vir. Also a long-period spectroscopic binary.               
                       1976.3669: Epoch incorrectly given as 1976.3699 in McAlister (1982)     McA1982b
                       Spectral types of primary and secondary assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       Individual J,H,K magnitudes are calculated from 2MASS combined                  
                       magnitudes and AO-derived magnitude differences                         Rbr2005 
           STF1724     AB: H 3  50.                                                                    
           H 6  43     AC: Incorrectly identified as H 3  50. Error noted by MacEvoy.          McE2010 
13100+1732 STF1728     42 Com = alp Com.                                                       Baz1964 
                       AB: Additional notes may be found in Madler (1844).                     Mad1844 
                       AB.  A preliminary orbit for this edge-on pair indicates that one of            
                       the F5 V stars may partially eclipse the other in early 1990.                   
                       Components reversed rel std sol's, e.g. in Hartkopf et al.              Hrt1989 
                       (1989). Their preliminary orbit for this edge-on pair indicated that            
                       one F5V star may have partially eclipsed the other in early 1990.               
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       1997.1179: The magnitude difference of the system is listed in the WDS          
                       as 0.0. Our reduction does not give the quadrant unambiguously, so we           
                       adopt the quadrant that gives a position angle consistent with                  
                       previous measures in the WDS.                                           Hor1997 
                       Spectral types amd masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       Calculated mass sum is 2.45 +/- 0.18 Msun, reasonable for two F5                
                       dwarfs. Closest approach of about 0.32 mas is predicted around 2015             
                       Jan 24 (to within about a week), eclipse duration ~1.5 days.            Mut2010b
                       Muterspaugh et al. (2015) revised their orbit, following discovery of   Mut2015 
                       three old measures whose theta measures had incorrect quadrants, which          
                       had led to an incorrect prediction of the eclipse timing.                       
13101+3830 STFA 24     17 CVn.                                                                         
           BU  608     BC: 15 CVn.                                                                     
13102+7358 STT 262     B is BD+74@524.                                                                 
13103+2423 LDS2904     LDS4322.                                                                        
13103-3447 B  2015     Rapid direct motion.                                                            
13106-3128 RST1706     Hipparcos parallax 19.27 +/- 1.23 mas. Dynamical parallax 19.6 mas,             
                       masses 0.90 and 0.71 Msun. RST 1706 is an example of a neglected                
                       binary, discovered by R.A. Rossiter in 1934 but observed so rarely      Rst1955 
                       that only now, after a nearly full revolution, the first orbit could            
                       be proposed.                                                            Tok2012b
13111+1220 OSO  51     G061-036. Neither is a common proper motion pair, based on astrometry           
                       and color                                                               Oso2004 
13112+3050 A  1359     The B component of this multiple is itself a close binary with a very   Grf2017a
                       short period of 3.34d.                                                          
13112-5739 JSP 573     Sinachopoulos (1988) apparently misidentified the Jessup pair; a                
                       nearby pair matching his measure has been given the component                   
                       designations EF.                                                                
13112-4717 COO 151     Beta Lyr (EB) type eclipsing binary, P = 0.88693 d.                     Zas2011 
13114+0938 LDS5771     LDS6272. HIP 64345. See Allen et al. (2000) for information on          AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
13115+2930 LDS1368     NLTT 33193/33185                                                        Chm2004 
13115-3508 HJ 4571     B is CD-34@8707.                                                                
13117-2633 FIN 305     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 6.21 +/- 2.03, 3.60, and 1.82 Msun, respectively.             Mlk2012 
                       Docobo & Andrade (2013) derive a dynamical parallax of 9.71 +/- 0.45            
                       mas and component masses 1.76 +/- 0.32 and 1.67 +/- 0.30 Msun. See              
                       paper for extensive notes on this system.                               Doc2013d
13119+2753 STT 578     bet Com = 43 Com. Possibly a long-period spectroscopic binary.                  
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
13119+1823 LDS 947     LDS6412, also at this location, has been removed. It had one measure,           
                       which was the same as the 1936 measure of LDS 947 with a quadrant flip          
                       G061-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
13119-1816 LDS4324     NLTT 33206/33173                                                        Chm2004 
13119-2038 DON 588     CPD-19@5377.                                                                    
13120+3205 STT 261     Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                       value of 159.2; this does not agree with other determinations of                
                       magnitude difference, however.                                                  
13121+2415 HDS1848     1997.4597  Very weak detection, possibly an artifact.                   Msn1999b
13121-1612 HJ 2645     53 Vir. AC: Not found in 1908.                                          Bu_1913 
13122+3214 JNN  90     Aa,Ab: 2MASS J13120525+3213332 and J13120689+3213179 constitute a               
                       known 26" binary pair in the Reid et al. (2007) sample, and in          Red2007a
                       addition, each of the components are discovered as close binaries in            
                       the AstraLux data. Hence, the system is a very likely quadruple                 
                       system, although the close pair of J13120689+3213179 has yet to be              
                       formally confirmed as physically bound.                                 Jnn2012 
13123+1731 GC 17881    Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from Marcy        CPS1999a
                       et al. (1999).                                                          HaI2001 
           PAT  47     Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                       candidate within separation/magnitude range listed. However,                    
                       further observations are required for verification                              
                       A is SB1, P=83.9d. "Exoplanet" with P=84d is actually a late-M dwarf?           
                       No transits.                                                            Tok2014d
13123-5803 JSP 918     Aka TDS8721.                                                            Dam2016b
13123-5955 SEE 170     The RV's of 1916 are quite uncertain. There may be a variation, and             
                       it may be related to the visual motion. The A component is also a               
                       Beta Lyrae-type system.                                                         
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       One component is V831 Cen, a beta Lyr system and also an SB with                
                       orbital period ~0.64d.                                                  Zas2009 
13124-4937 CPO 364     LDS 434. B is CD-48@8008.                                                       
13125-3445 LDS 436     B is CD-34@8719.                                                                
                       SHY 615. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13126+5827 STF1732     AB: SHY 616. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
13126-3207 SWR 138     CPM pair                                                                Skf2004 
13126-6034 WSI  75     Primary is V1266 Cen, eclipsing binary of Beta Lyr -type, period                
                       10.1572 d.                                                              Zas2012 
13127-1619 ALD  50     RST 3826.                                                                       
13127-3152 MUG   3     AB are CPM. Followup spectroscopy confirmed the B component is a                
                       dwarf; estimated mass is 0.253 +- 0.011 Msun.                           Mug2005 
                       HIP 64459. B at 8" is MUG 3, physical. Confirmed by ANDICAM images.     Tok2011a
                       Exoplanet host, P=1135d                                                 Tok2014d
13129-5949 COO 152     LDS 435.                                                                        
           HDS1850     Aa,Ab: Hipparcos parallax 23.72 +/- 0.60 mas. Dynamical parallax 23.6           
                       mas, masses 1.56 and 0.79 Msun. This is a chromospherically active G0V          
                       dwarf and a ROSAT X-ray source. There are at least four components in           
                       the system: Aa1,Aa2 is a double-lined spectroscopic and eclipsing               
                       binary with 4.2 d period, Aa,Ab is the pair considered here, and the            
                       visual companion B at 25.5" is physical. The orbits of Aa1,Aa2 and              
                       Aa,Ab may be co-planar.                                                 Tok2012b
                       Aa,Ab: GJ 2099. Aa is SB2E, P=4.233d                                    Tok2014d
13130-1223 LDS6274     NLTT 33271/33270                                                        Chm2004 
13131+1801 S   648     B is BD+18@2703.                                                                
                       This cannot be the close 401.5-d spectroscopic binary.                  Grf2014a
13132-0233 STF1731     AB: HJL 184.                                                            HJL1986 
           TOK  69     Aa,Ab: Estimated masses 1.09 and 0.71 Msun; sep 20.6 au, period 70 y.   Tok2010c
13132-0501 TOK 402     HIP 64499 has a variable RV, with a preliminary spectroscopic orbit             
                       of 17yr period (Latham 2012, private communication). It is resolved at          
                       0".1 and shows no motion in one month.                                  Tok2015c
13132-0742 LDS4326     NLTT 33282/33283                                                        Chm2004 
13133+3709 LDS4327     NLTT 33310/33311                                                        Chm2004 
13134-1850 SHJ 161     54 Vir. Both components are spectroscopic binaries. Primary is LM Vir,          
                       a W UMa eclipsing binary (period 0.9876 day). Aka H 2  45.              Zas2011 
                       Erroneously called SHJ 151 in BDS (#6422) and ADS (#8824).              MEv2010 
13134-5042 I  1227     Fairly rapid retrograde motion.                                                 
13135+6717 STFA 25     AB: Spectrum K2III+K2III.                                                       
                       Position of C: 13 13.0 +67 19.                                                  
                       AB: HJL1076.                                                            HJL1986 
13136+5643 SHY 246     AE: HIP  64532 + HIP  65327.  E component = F component of 13239+5456           
                       and A component of 13234+5754.                                                  
           SHY 246     AF: HIP  64532 + HIP  61100.  F component = G component of 13239+5456.          
13137+2949 HO   55     Frequent failure to see the companion is probably due to the large              
                       magnitude difference.                                                           
13139+1125 BPMA 46     [PM2000] 1051722 + [PM2000] 1051735.                                    Gvr2010 
13140+1409 BPM 601     [PM2000] 1051749 + [PM2000] 1051799.                                    Gvr2010 
13141+0619 LDS6275     GIC 104 = G062-019/G062-020. A typographical error led to this pair             
                       being originally entered in the WDS as 12141+0617GIC 104.                       
13142+5841 LDS2672     NLTT 33377/33378                                                        Chm2004 
13143+1320 LAW   2     Distance 9.8 +/- 2.0 pc                                                 Law2006 
                       NLTT 3370. Schlieder et al. (2014) derive the following properties for          
                       the A and B components:                                                         
                          log (L/Lsun)         -2.64 +/- 0.06        -2.68 +/- 0.06                    
                          Teff (K)             3200 +/- 500          3100 +/- 500                      
                          Mass (Mjup)          97 +41/-48            91 +41/-44                SJE2014 
                       Recently, Schlieder et al. (2014) reported NLTT 33370 as a binary. In   SJE2014 
                       NACO images approximately coincident with the AstraLux images, the              
                       projected separation of the binary is ∼75 mas, which is consistent      .     
                       with the fact that the binary is unresolved in the AstraLux images.     Jnn2014 
                       Dupuy et al. (2016) derive an orbit for LSPM J1314+1320AB using                 
                       astrometry from Keck/NIRC2 and the VLBA. Derived parameters for A and           
                       B are as follows:                                                               
                          Mass (Mjup)          92.8  +/- 0.6         91.7  +/- 1.0              .      
                          Age (Myr)            79.9  -2.7/+2.5       81.7  -3.3/+2.9            .      
                          Teff (K)             2954  +/- 3           2947  +/- 4                .      
                          Radius (Rjup)        1.831 +/- 0.018       1.808 +/- 0.018            .      
                          log(g) (cm/s^2)      4.836 +/- 0.010       4.842 +/- 0.011            .      
                          Li/Li_init           0.12  -0.05/+0.03     0.17  +/- 0.07             .      
                          Mbol (mag)           11.290 +/- 0.025      11.328 +/- 0.025           .      
                          log (Lbol/Lsun)      -2.616 +/- 0.010      -2.631 +/- 0.010           .      
                       Parallax is 57.975 +/- 0.045 mas, distance 17.249 +/- 0.013 pc, the             
                       integrated spectral type M7.0 +/- 0.2 (optical), M6 +/- 1 (near-IR).    Dup2016 
13143-5906 FIN 205     Unresolved at SOAR on 2013.13 (but in small field), remains                     
                       unconfirmed.  A is possible SB.                                         Tok2014d
13144+2358 POU3134     LDS2907.                                                                        
13145-2417 FIN 297     Inclination corrected from 65.6 to 66.6 by Ruymaekers & Nys (1995)      Ruy1995 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 0.94 +/- 0.48, 3.32, and 1.45 Msun, respectively.  Mlk2012 
13147-6335 MLO   3     Spectroscopic binary.                                                           
           WSI  58     Aa,Ab: One component of the 0.24" pair is a 13.6d SB1 (Sota et al.              
                       2014, ApJS 211, 10).                                                    Sna2014 
13149-1122 SHJ 162     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
13151+2725 B     1     LDS2908.                                                                        
13151+2621 GIC 112     LDS1373.  G149-062/G149-061.                                                    
13152-6754 DUN 131     eta Mus. The primary is a spectroscopic binary and a possible                   
                       eclipsing system.                                                               
13153-0250 JNN  91     LP 617-21.                                                                      
                       Due to the small separation of companion to 2MASS J13151846-0249516 it          
                       is very likely a physical binary, but common proper motion has not yet          
                       been tested for.                                                        Jnn2012 
13155-2650 BUG  14     Estimated spectral types are L3.5 +/- 2.5 and T7 +/- 0.6.  System age           
                       > 0.8-1.0 Gyr, estimated distance 19 +/- 3 pc.  Effective temperatures          
                       are 1760 +/- 70 and 790 +/- 70 K. For an age of 1 Gyr, masses are               
                       60 +/- 6 and 16 +/- 3 Mjup.                                             Bug2011b
13157+1154 AG  435     Single.                                                                 IDS1963A
13161-6235 HD 115071   V961 Cen. Hipparcos has shown this star to be an eclipsing binary with  HIP1997a
                       a period of 1.37d.  Both Penny (1996) and Howarth et al. (1997 MNRAS    Pny1996b
                       284, 265) found evidence of line-doubling.  Turner (1985 ApJ 292, 148)          
                       shows that this star appears close to and has a similar distance to             
                       the cluster Stock 16.                                                   Msn1998a
13163+1715 STF1733     BDS 6440, H 2  46.                                                              
13164+4202 HJ 1230     HJ observes HJ 1230: 1828 290@ 12" 11-11.                                       
13164+2906 LDS6276     HZ 43.                                                                  McA1996b
                       The 1977.10 observation of this system published by McAlister in 1996           
                       was a re-reduction of archival USNO-NOFS data by V.V. Kallarakal.               
                       Evidently, the 1974.345 and 1975.415 data were also from this source,           
                       and were reduced and added by Worley.                                   Wor9999 
13166+1948 HDS1862     1988.1655: Unresolved upon initial inspection (McAlister 1993), a very  McA1993 
                       weak peak was later found which agreed well with the Hipparcos                  
                       measurement.                                                            Msn1999b
           BGH  46     AB: HJL1077.                                                            HJL1986 
                       AB: SHY 617. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
13168+0925 KUI  62     59 Vir.                                                                         
           GJ  504     Aa,Ab: Kuzuhara et al. (2013) image a cold Jovian exoplanet orbiting            
                       the solar-type star GJ 504. Distance to the system is 17.56 +/- 0.08            
                       pc. They derive masses 1.22 +/- 0.08 Msun and 4.0 +4.5/-1.0 Mjup for            
                       the star and planet. The effective temperatures are 6234 +/- 25 and             
                       510 +30/-20K, spectral types are G0V and late-T/early-Y.                Kuz2013 
13169+1701 BU  800     Hyperbolic orbit by Hopmann (1960).                                     Hop1960b
                       sigma = areal constant in the true orbit = 0.2700 arcsec^2/yr                   
                       q = periastron distance in the true orbit = 5".0334                             
                       All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                       HIP 64797. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: H 2  46.                                                            MEv2010 
                       AB: Additional notes may be found in Worley (1956).                     Wor1956b
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
13169-3436 I  1567     Also known as SEE 171.                                                          
                       Hipparcos parallax 23.18 +/- 1.10 mas. Dynamical parallax 22.7 mas,             
                       masses 0.96 and 0.84 Msun.  I 1567 has a well-established orbit by              
                       Heintz (1986) which is corrected here to better match the new speckle   Hei1986a
                       data. Heintz notes that this pair is a "puzzling case" because of some          
                       very discordant historical measures; these deviant points were ignored          
                       in the calculation.                                                     Tok2012b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.20 +/- 0.36, 1.81, and 0.95 Msun, respectively.             Mlk2012 
13170+3949 OSO  52     G164-061. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
13174-2132 BU  222     HDO 136                                                                         
13175-0041 FIN 350     This binary is comprised of a pair of F0V stars of near-zero magnitude          
                       difference, so there is considerable uncertainty as to whether the              
                       orbit is of short-period/high-eccentricity (P~9yr, e~0.6) or long-              
                       period/low-eccentricity (P~18yr, e~0.0). The rms residuals to the               
                       speckle observations are slightly smaller for the long-period orbit,            
                       but mass sums (a^3/P^2) for the two orbits differ by just 2%,                   
                       insufficient to rule out either solution on the basis of plausibility.  Hrt1994 
                       (Later speckle observations near periastron appeared to favor a short-          
                       period solution, but this is still uncertain.)                                  
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.39 +/- 0.31, 3.27, and 1.45 Msun, respectively.             Mlk2012 
13178+4535 LDS4340     NLTT 33606/33599                                                        Chm2004 
13184-1819 H 6  90     61 Vir. H VI 90. Proper motion of A -1070 -1065.                                
                       B is BD-17@3815, proper motion -037 -010.                                       
                       Smyth's quoted separation is difference in RA only.                     Smy1844 
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
13186-6229 SNA  33     This new pair cannot be the 15.1d binary reported by Sota et al.                
                       (2014, ApJS 211, 10); HD 115455 is therefore at least a hierarchical            
                       triple system.                                                          Sna2014 
13189-2310 SMY   3     gam Hya = 46 Hya                                                                
13190-1514 LDS4343     NLTT 33649/33646                                                        Chm2004 
13193+1759 LDS4345     NLTT 33677/33673                                                        Chm2004 
13196+3507 HJ  529     AB: NLTT 33705/33706                                                    Chm2004 
13196+2422 LDS2913     NLTT 33701/33702                                                        Chm2004 
13198+4747 HU  644     Beuzit et al. (2004) AO observations confirm speckle third component    Beu2004 
                       of Hartkopf et al. (1994). Mass sum and mass ratio (Heintz, 1969)       Hrt1994 
                       clearly requires the primary to be a closer binary.                     Hei1969c
                       Masses and bolometric magnitudes are derived for the two components     Msn1999a
                       of this system by Mason et al. (1999), based on assumed spectral types          
                       and available  parallaxes. The Hipparcos parallax appears suspect.              
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
           HU  644     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.76 +/- 0.13, 1.11, and 0.85 Msun, respectively.  Mlk2012 
                       Aa,Ab: 1992.3126: This appears to be a new component to the 1".5 49-yr          
                       period pair of K/M dwarfs HU 644. This is the only one of the current           
                       crop of new interferometric binaries which has not yet been confirmed.          
13199-2748 B   247     Spectrum: Fm delta Del.                                                         
13199-6831 JNN  92     2MASS J13195689-6831142 has companion detected in the AstraLux images.          
                       Since the companion is relatively close (~0.88") and has a brightness           
                       and color that is consistent with expectation, it is probably a                 
                       physical pair. Only one epoch of images exists so far.                  Jnn2012 
13203+1746 A  2166     Elongations doubtful, quadrant indeterminate.                           B__1963b
                       Primary is eclipsing binary KR Com (period 0.40796 day).                Zas2010 
                       Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995)            Ruy1995 
                       Zasche et al. (2010) derived a combined solution orbit, based on        Zas2010b
                       published astrometry plus minima timings of the close-contact                   
                       binary KR Com, which comprises the primary of the Aitken pair.                  
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 7.10 +/- 3.80, 2.75, and 1.10 Msun, respectively.             Mlk2012 
13203-0140 LDS 437     AB: NLTT 33750/33731                                                    Chm2004 
13203-0224 LDS4347     NLTT 33739/33741                                                        Chm2004 
13207+0408 BDK   6     G 62-33 + 2MASS J13204427+0409045. Distance 30.5 +/0 1.0 pc for                 
                       primary, 33 +/- 3 pc for secondary. Estimated age of system 3.3-5.1             
                       Gyr. Mass of secondary estimated at 0.079-0.081 Msun.                   Fah2010 
13208+3158 ES  308     SEI 535.                                                                Nsn2017b
13208+0956 BDK   7     G 63-23 + 2MASS J13204159+0957506. Distance 38.1 +2.6/-2.3 pc for               
                       primary, 36 +/- 3 pc for secondary. Estimated age of system 1.0-3 Gyr.          
                       Mass of secondary estimated at 0.083-0.093 Msun.                        Fah2010 
                       NLTT 33793 + 2MASS J13204159+0957506. Baron et al. (2015) estimate              
                       spectral types K5 and M8, distances 38.1 +2.6/-2.3 and 36 +/-3 pc,              
                       masses 0.724-0.782 and 0.087-0.096 Msun.                                BFr2015 
13209+4359 GC 18063    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13216-0926 BRT 447     It appears that a possible 0.3s error in the RA of the primary may be           
                       the cause of the incorrect 1895 measure.                                        
13217+1542 FOX 177     HJL 185.                                                                HJL1986 
13218+1746 STF1737     BDS 6463, H IV 57.                                                              
                       H 4  57.                                                                MEv2010 
13218-1845 GC 18075    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13220+6748 GRV1087     SLW 862.                                                                        
13224+7011 LDS1767     NLTT 33937/33932                                                        Chm2004 
13224+1603 BPM 602     [PM2000] 1055415 + [PM2000] 1055437.                                    Gvr2010 
13225-2257 ARG  26     B is BD-22@3573, spectrum G1/2V.                                                
           SHY 618     AC: HIP  65266 + HIP  64670.                                                    
13226+2607 HO  259     AB: A is astrometric binary.                                            Tok2014d
13226-6059 FIN 208     Too close, measures uncertain. One component is the variable V790 Cen.          
13228+6442 LDS2674     NLTT 33948/33949                                                        Chm2004 
13228+4459 KZA  58     16' error in WDS designation.                                                   
13228-1311 H 4 119     H IV 119. B is BD-12@3801. Also known as STF1736. A is a spectroscopic          
                       binary, called "mild Am" by Bidelman.                                           
13229+8932 HJ 3154     2000 position deduced from 1830: 22 47.4 +89 28.                                
13229-7209 B  1736     Spectroscopic binary.                                                           
13230+3141 LDS1386     NLTT 33927/33931                                                        Chm2004 
13233+0344 HDS1878     This is the pair BAL2857 only noted on a 1910 AC-plate.                 Dam2016c
13234+5754 SHY  67     AB: HIP  65327 + HIP  59496.                                                    
13235+2914 HO  260     Undetermined (long) period in nearby K-dwarf pair.                              
                       Baize (1968) elements are provisory. Third body (P of order 30 yr)              
                       is suspected.                                                           Baz1968 
13235+1401 HJ  226     AB is galaxy NGC 5129.                                                          
13237+0243 STF1740     B is BD+03@2766.                                                                
                       HJL 186.                                                                HJL1986 
13237-0043 A  2489     A premature orbit has been computed.                                            
                       T has been revised to comply with recent quadrant determinations.       Zul1972a
13239+5456 STF1744     zet UMa or Mizar. Split by Benedetto Castelli. After resolving AD in    C__1616 
                       1617 he wrote to his friend, Galileo, to observe the pair, "It's one of C__1617 
                       the beautiful things in the sky and I don't believe that in our pursuit         
                       one could desire better." Galileo measured it in early 1617. See the    G__1617 
                       excellent discussion of its discovery in Leos Ondra's July 2004 Sky &           
                       Telescope article, from which Galileo's measure was extracted. It was           
                       independently found double in 1650 by Jean Baptiste Riccioli in         Ric1651 
                       Bologna: "There appears to be one star in the middle of the Great               
                       Bear's tail, where there are actually two, as the telescope reveals."           
                       This was also the first to be observed photographically, by John A.             
                       Whipple with the Harvard 15inch on 27 April 1857. According to Aitken,          
                       this was the first observed photographically (G.P. Bond at Harvard      A__1935f
                       College Observatory in 1857 using an 8 second exposure on a collodion   BdG1858 
                       plate), and the first spectroscopic binary discovered (E.C. Pickering   Pck1890 
                       in 1889). A is a spectroscopic binary, P = 20.54d (first orbit 1901).   Vog1901 
                       B is also a spectroscopic binary (first orbits 1908), P  = 175.6d,      FEB1908 
                       spectrum A1m or A1/A2/A7. Also, common proper motion with 80 UMa        LH_1908 
                       80 UMa (Alcor) and other members of the Ursa Major stream.                      
                       AC: SHY 247. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
           PEA   1     Mistakenly given the discoverer designation 'MKT   8' in the WDS,       Pea1925 
                       but actually first resolved by Pease in 1925, six decades before the            
                       Mark III interferometer measures. This system has completed some 1,350          
                       revolutions since its first resolution, probably a record for any               
                       "visual" binary.                                                                
                       The orbit of Aa,Ab by Russell (1927) is combined interferometric/       Rus1927 
                       spectroscopic (double-lined spectrum). A small magnitude difference             
                       (which would probably place the ascending node in the second quadrant)          
                       is uncertain.                                                                   
                       Star B (mag. 3.96, 15") is physical, and is itself a 175.55d SB1.               
                       Visual orbit by Hummel et al. (1995) is based on astrometry from the    MkT1995 
                       Mark III interferometer. Additional spectroscopic data yield component          
                       masses, luminosities, radii, effective temperatures, and distance.              
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
           SMR  4      AD: This was the first component of Mizar split by Benedetto Castelli   C__1616 
                       in late 1616. It was called "Sidus Ludoviciana" (Ludwig's Star) by      Ond2004 
                       Johann Georg Liebnecht for the Landgrave Ludwig of Hessen-Darmstadt             
                       who thought he has discovered a planet. He was wrong.                           
           SHY 247     AE: HIP  65378 + HIP  64532.  E component = A component of 13136+5643           
                       = C component of 12487+6019.                                                    
           SHY 247     AF: HIP  65378 + HIP  65327.  F component = D component of 12417+5543.          
           SHY 248     CE: HIP  65477 + HIP  64532.                                                    
           SHY 248     CF: HIP  65477 + HIP  65327.                                                    
           SHY 248     CG: HIP  65477 + HIP  61100.  G component = G component of 13136+5643.          
           SHY 248     CH: HIP  65477 + HIP  61481.                                                    
           STF1744     AB: H 3   2.                                                            MEv2010 
13240-2055 BU  610     HDO 137. Spectrum: K1/2III/IV.                                                  
13242-0159 GLP   9     B is BD-01@2813.                                                                
13245+1226 GC 18139    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1986).                                                         Grf1986c
13245-2837 BRT3000     Not found by Heintz at IDS position.                                    Hei1990b
13246-0510 66 Vir      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13246-5130 I  1231     Too close after 1927. Needs speckle.                                            
13246-5557 JNN 155     Secondary appears to be a brown dwarf; masses are estimated at 1.3              
                       Msun and 65 +35/-30 (based on intrinsic brightness) or 45 +/- 10 Mjup           
                       (based on temperature).                                                 Jnn2012b
13247+1755 BPM 603     [PM2000] 1056418 + [PM2000] 1056405.                                    Gvr2010 
13250+0146 GRV1088     SLW 868.                                                                        
13251+2351 SHY 620     HIP  65466 + HIP  65508.                                                        
13252-1110 BUP 150     alp Vir = 67 Vir = Spica. A is an Alpha CVn-type variable and                   
                       spectroscopic binary, spectrum B1III-IV+B2V. According to R.G. Aitken,  A__1935f
                       this is the fourth binary recognized by spectroscopic methods. It was           
                       identified as such based on photographic spectra obtained by Prof.              
                       H.C. Vogel at Potsdam in early 1890. It has been resolved by intensity          
                       interferometry.                                                                 
                       AC. Smyth's quoted separation is difference in RA only.                 Smy1844 
13252-6429 HJ 4583     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
13253+7559 STT 267     Position angles scattered, mostly near 150@. Quadrant uncertain.                
                       Probably in rapid motion.                                               B__1963b
13253+4028 HJ 1231     This is a measure of A and BD+41@2392.                                          
13254-5947 WSI  76     A = V379 Cen, eclipsing binary of Algol type, period 1.874696 days.     Zas2015 
13258+4430 A  1609     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.47 +/- 0.63, 1.91, and 0.85 Msun, respectively.  Mlk2012 
13258-4815 JNN 156     V966 Cen. Secondary appears to be a brown dwarf; masses are estimated           
                       at 1.3 Msun and 55 +30/-20 (based on intrinsic brightness) or                   
                       70 +35/-15 Mjup (based on temperature).                                 Jnn2012b
13258-7038 67 Mus      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Dworetsky (1982).                                                       Dwo1982 
13264+2334 LDS5779     NLTT 34105/34116                                                        Chm2004 
13264-4303 HJ 4587     SWR 140. CPM pair                                                       Skf2004 
13265+4233 ES 2645     B is BD+43@2334.                                                                
13267-2418 BGH   6     SHY 249. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13270-7710 GLI 291AB,C #190 in the original list of Gilliss.                                           
13271+6444 STTA123     LDS2675.                                                                        
                       AB: HJL 188.                                                            HJL1986 
                       AB: SHY 622. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
13273-3111 DAE   4     GJ 3786 = LHS 2739                                                              
                       Daemgen et al. (2007) derive a distance of 30.2 +/- 7.7 pc, separation  Dae2007 
                       of 16.4 +/- 4.2 au, and a predicted orbital period of 108 +/- 43 yr.            
                       Spectral types for both stars are M3.5 +/- 0.5; masses are 0.33                 
                       +0.10/-0.09 and 0.30 +0.11/-0.09 Msun.                                          
13274-2138 LDS6278     NLTT 34137/34150                                                        Chm2004 
13274-6152 B  2752     A is an Algol-type system, V380 Cen.                                            
13276+0655 HJ 1232     HJL 187.                                                                HJL1986 
13283-0222 B  2753     LDS5781.                                                                        
                       NLTT 34200/34203                                                        Chm2004 
13284+1543 STT 266     Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                       value of 178.1; this does not agree with other determinations of                
                       magnitude difference, however.                                                  
13284+1347 STT 579     AB: 70 Vir. B is BD+14@2622.                                                    
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           RBR  18     2001.0994: PA is measured in zenith mode. If data collected in                  
                       equatorial mode, PA = 241.2. Confirmation of the pair should establish          
                       the correct theta value.                                                Rbr2011d
           70 Vir      A: Combined solution, based on reduction of Hipparcos intermediate              
                       astrometric data together with spectroscopic elements from Marcy &      CPS1996a
                       Butler (1996).                                                          HaI2001 
13285-4829 SWR 141     CPM pair                                                                Skf2004 
13288+5956 S   649     CA: HJL1079.                                                            HJL1986 
                       CA: SHY 623. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       CA: H 6  22.                                                            MEv2010 
13289+2131 LDS 948     GIC 113. G149-090/G149-089 = NLTT 34235/34234.                          Chm2004 
13291-6441 GC 18206    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13291-6604 LDS 444     B is CPD-65@2344.                                                               
                       SHY 624. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13293+6452 LDS2321     NLTT 34300/34302                                                        Chm2004 
13295+5142 JNN  93     The B component seen in the AstraLux images appears to be a very close          
                       binary itself due to a PSF extension visible in five separate epochs.           
                       However, we count the system as a regular binary here since we do not           
                       get a converging fit for the closer pair.                               Jnn2012 
13297-2317 HO  381     A is a Mira-type variable, R Hya.                                               
                       A has a magnitude range of 3 to 11 with a period of 388.0 days.                 
                       B has a B-V (U-B) color of 1.04 (0.97)                                  Egg1971 
13298+0106 J  2091     A is FO Vir, an eclipsing Beta Lyrae-type binary, period 0.77557d.      Zas2011 
13300-7634 RSS  18     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
13303-0834 LDS 448     Proper motion -1093 -419.                                                       
                       Primary is white dwarf WD 1327-083.                                     Far2005b
13304+4010 LDS5782     LDS6279.                                                                        
                       NLTT 34325/34326                                                        Chm2004 
13304-0628 STF1750     72 Vir. A is a spectroscopic binary.                                            
                       H N  27.                                                                MEv2010 
13304-7851 HD 116852   The classification is from Morgan et al. (1955 ApJS 2, 41). Sembach &           
                       Savage (1994 ApJ 431, 201) suggest that the star lies at 1.3 kpc from           
                       the Galactic plane, so we have assigned it to the "runaway" category.   Msn1998a
13305+2231 SHY 626     HIP  65899 + HIP  65884.                                                        
13305-2339 HO  540     A is an Algol-type system, SS Hya.                                              
13306-4311 CPO 371     Nothing at this position, according to Heintz.                          Hei1987a
13309+2414 STT 268     AB: A is possible SB, no orbit.                                         Tok2014d
           H 5  70     AC: STTA124.                                                                    
                       AC: H V 70. C is the variable FK Com.                                           
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
13310+3626 HLM   5     Also known as STF1753.                                                          
13310-3924 SEE 179     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                       15.46 +/- 7.56 and 8.91 Msun, respectively.                             Mlk2012 
13316+5857 TOK 290     We count 2MASS J13313493+5857171 as single close in, although its PSF           
                       appears somewhat extended in the 2009.13 epoch. However, it is a                
                       likely companion to the nearby G2-star HD 117845 at 11" separation.             
                       HD 117845 has been included in the AstraLux field and appears to be             
                       itself a close binary with a ~0.5" separation.                          Jnn2012 
                       AB: A is SB, no SB orbit. X-ray source.                                 Tok2014d
13316-6135 HDS1894     Primary is Cepheid V659 Cen.                                                    
                       Masses are 5.2 and 4.4 Msun. Estimated period = 3400y,                          
                       a = 500au = 0.67".                                                      Evs2013 
13317-0219 HDS1895     Horch et al (2012) generate two possible orbits, one based on only      Hor2012a
                       astrometry, the second "constrained" solution fixes P, T, e, and Omega          
                       to values determined in a spectroscopic orbit by Torres et al. (2002).  Trr2002 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.27 +/- 0.49, 1.75, and 0.88 Msun, respectively.             Mlk2012 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Latham et al. (2002). They derived component masses 0.93 and 0.42 Msun  Lat2002 
                       and an estimated semimajor axis of 95.29 mas.                           Ren2013 
13320+3108 WOR  24     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.37 +/- 0.39, 1.20, and 0.55 Msun, respectively.             Mlk2012 
13320-1844 B  2542     73 Vir.                                                                         
13320-6519 FIN 369     In rapid direct motion.                                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.13 +/- 0.94, 2.57, and 1.70 Msun, respectively.             Mlk2012 
                       Docobo & Andrade (2013) derive a dynamical parallax of 15.87 +/- 1.35           
                       mas and component masses 1.14 +/- 0.37 and 1.08 +/- 0.36 Msun. See              
                       paper for extensive notes on this system.                               Doc2013d
13321-1115 TOK 291     No previous indication of binarity was available for HIP 66018, apart           
                       from the CPM companion B at 84". We discovered another faint component          
                       Ab at 0".89, dI=4.6, likely to be physical (low background density).            
                       The B component  (V=14.8) was targeted, but its speckle signal was              
                       weak and no obvious close companions to B were found.                   Tok2015c
13321-2258 HJ 4593     B is BD-22@3617, spectrum F2IV.                                                 
13322+0744 LDS3074     SLW 887.                                                                        
13324+3649 STF1755     Spectroscopic binary. Spectral type of B: F5IV.                                 
13324-1240 SHJ 165     B is BD-11@3537.                                                                
                       H 5 128.                                                                MEv2010 
13327+3100 LDS1392     NLTT 34410/34417                                                        Chm2004 
13328+1649 VYS   6     LDS4374. Both components are flare stars, VW Com.                               
13328-1746 HU  469     Includes LV Vir, a W UMa type eclipsing binary, P = 0.40943d.           Zas2012 
13329+4143 LDS4375     NLTT 34434/34433                                                        Chm2004 
13329+3454 STT 269     1986.397: The separation of this partially resolved pair was                    
                       calculated under the assumption of zero or otherwise known magnitude            
                       difference.                                                             Tok1985 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 5.23 +/- 1.58, 3.13, and 2.06 Msun, respectively.  Mlk2012 
13329-1522 HJ 2658     75 Vir.                                                                         
13332-7734 HJ 4590     LDS 447. A is a variable, S Cha. B is CPD-76@769.                               
13333+2301 STF1756     HJL 189.                                                                HJL1986 
13337+4801 ODE  11     HJL1080.                                                                HJL1986 
13341+6746 STF1767     LDS1393.                                                                        
                       NLTT 34535/34534                                                        Chm2004 
13343-0019 STF1757     AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
13344+3847 HJ 1234     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
13344-5931 TOK 403     HIP 66230 has a variable RV in GCS and an astrometric acceleration. We          
                       resolved it at 0".1, dI=2.5, estimated period ~10yr. The pair moved by          
                       4deg in one month.                                                      Tok2015c
13345-1326 S   650     B is BD-12@3842.                                                                
13346+1726 BPM 604     [PM2000] 1060833 + [PM2000] 1060846.                                    Gvr2010 
13347-0036 HNK   1     zet Vir = GJ 3792. Observations over 4.75 years indicate pair has               
                       common proper motion and shows clear evidence of orbital motion.                
                       Hinkley et al. (2010) constrain elements a > 24.9au, P > 124yr, and     Hnk2010 
                       e >0.16. Mass of the companion is estimated at 0.168 +0.012/-0.016              
                       Msun, suggesting a spectral type of M4V-M7V.                                    
13347-1313 BU  932     Variable?                                                               Mlr1956a
                       Only elements P, T, and a have been amended by Starikova (1980) from    Sta1980a
                       the orbit of Heintz (1969).                                             Hei1969a
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Measures hard to reconcile. There has been practically no change in             
                       the last 10-12 years, yet the present position differs by some 290deg           
                       from Burnham's discovery position in 1879. Some of the measures are             
                       evidently spurious.                                                     VBs1954 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 13.50 +/- 8.22, 5.27, and 2.24 Msun, respectively. Mlk2012 
13347-6320 HDS1907     The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
13348+3711 BH CVn      Close binary comprised of F2IV primary and K2IV secondary. Orbital              
                       elements are from Eker & Doherty (1987 MNRAS 228, 869) except for the           
                       ascending node. The Eker & Doherty inclination was corrected for CW             
                       rotation determined by Abbuhl et al. (2015)                             Abb2015 
13349+7430 LDS1775     B component is NLTT 34606.                                                      
                       Possible common proper motion with BD+75@510, about 1900" distant.              
                       G255-038.  Besides the known companion at 14.275", Gliese & Jahreiss    GJ_1988 
                       list this star as a wide companion to G255-034, separated by 33'.               
                       However, the different Hipparcos distances to G255-038 and G255-034,            
                       and the different measurements of mu_delta, suggest that the two stars          
                       are not related.                                                        Oso2004 
           PRB   4     C, D, and E components are NLTT 34503, NLTT 33451, and WD 1337+70 =             
                       NLTT 34829, respectively. E is also the primary of 13388+7017 KUI 122.          
                       All are possible CPM pairs, according to Probst (1983).                 Prb1983 
13349+3746 DAE   5     CLS 73 = 2M1334                                                                 
                       Daemgen et al. (2007) derive a distance of 35.8 +/- 9.4 pc, separation  Dae2007 
                       of 2.9 +/- 0.9 au, and predicted orbital period of 8 +/- 4 yr.                  
                       Spectral types for both stars are M3.5 +/- 0.5; masses are 0.34                 
                       +0.11/-0.10 and 0.30 0.10/-0.08 Msun.                                           
                       Although the close binarity of 2MASS J13345147+3746195 was reported in          
                       Daemgen et al (2007) and our AstraLux data have a similar sensitivity,  Dae2007 
                       the star appears single in our images. Since the separation was only            
                       82 mas in 2006, it has presumably moved inward since then.              Jnn2012 
13356+1012 HJ  228     B is BD+10@2566.                                                                
                       HJL 190.                                                                HJL1986 
13358-2807 TDS8890     Galaxy 6dFGS gJ133548.0-280642.                                                 
13360+4829 FAR  38     GJ 2103. SKF 319.  Primary is white dwarf WD 1333+487.                  Far2006 
13360+0112 OSO  54     G062-052. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
13363+3514 KZA  71     WDS garbled (dec copied from KZA 70)                                            
13364+2156 LDS4381     NLTT 34611/34612                                                        Chm2004 
13367+3555 KZA  72     15' error in WDS designation                                                    
13368-2630 H N  69     Spectral type of B: A7IV-V.                                                     
13370+0751 VBS  23     LDS3082 = LDS4382.                                                              
13371-1627 RST3845     Spectrum: F2/3III/IV.                                                           
13372+3005 STF1766     LDS1394.                                                                        
                       HJL 191.                                                                HJL1986 
13372-6142 I   365     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.39 +/- 1.84, 2.57, and 1.17 Msun, respectively.  Mlk2012 
13372-8427 HJ 4585     B is CPD-83@531.                                                                
13374-1204 LDS4384     NLTT 34648/34647                                                        Chm2004 
13375+3618 STF1768     25 CVn. AB: Malkov et al. (2012) derive dynamical, photometric, and             
                       spectroscopic masses 4.61 +/- 2.52, 3.03, and 1.82 Msun, respectively.  Mlk2012 
13376-0752 STF1763     AB: H 1  80.                                                            MEv2010 
13377+5043 STF1770     Composite spectrum; M2II-III+F3III.                                             
13377+0223 STF1764     C and D components are A and B of STF 1765 rej. WAL  64CD measures              
                       moved, but systems not merged, as optical/physical nature of STF1764AC          
                       and WAL  64AD are unknown.                                                      
13377-2337 RST2856     In rapid motion, but quadrant ambiguity makes interpretation uncertain          
                       Two orbit solutions bu Heintz (1967); neither is clearly preferable.    Hei1997 
13378+2819 HJ 3341     AC: Possible error in original reduction?                                       
13379+4808 ES  608     At least one component is variable.                                             
13379+0221 STF1765     WAL  64CD. Systems not merged, as optical/physical nature of STF1764AC          
                       and WAL  64AD are unknown.                                                      
13381+3910 STF1769     AB: A is SB1, P=11.589d                                                 Tok2014d
                       C is BD+39@2662.                                                                
                       AC: HJL 192.                                                            HJL1986 
                       AC: Additional notes may be found in Baize (1936).                      Baz1936c
           TOK  29     AE is CPM. Primary is 11.6d SB1. C component is known CPM; D component          
                       found in 2MASS, confirmed CPM by POSS (approximate 1950 measure: 9.3",          
                       230deg). A is triple, the whole system is quintuple. Metal-poor, high           
                       proper motion.                                                          Tok2006 
                       AE: A,C are on the MS, E below. E is optical or WD?                     Tok2014d
13382-2341 LDS4385     AB + TOK 404Aa,Ab:  HIP 66530 has a variable RV according to the GCS.           
                       It is resolved at 0".16 in the I band only, estimated period ~20yr.             
                       This is a triple system, considering the CPM companion B at 28".        Tok2015c
           TOK 404     Aa,Ab: SB, no orbit                                                     Tok2014d
13383-6416 HRG  88     Aka WFC 138.                                                                    
13385-1042 J  3001     Galaxy PGC 48213 = MCG-02-35-011.                                               
13387+3823 COU1429     The KZA pairs are probably wider companions.                                    
13388+1913 LDS4386     NLTT 34761/34772                                                        Chm2004 
13389+1807 BPM 605     [PM2000] 1062803 + [PM2000] 1062804.                                    Gvr2010 
13390-1052 LDS6280     Ross 479                                                                        
13392-4900 HJ 4600     B is CD-48@8376.                                                                
13395+5255 VIG  16     Optical/physical nature of the faint companion is undefined.            Vig2012 
13396+1045 BU  612     Masses and bolometric magnitudes are derived for the two components     Msn1999a
                       of this system by Mason et al. (1999), based on assumed spectral types          
                       and available parallaxes.                                                       
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.41 +/- 0.36, 3.27, and 1.40 Msun, respectively.  Mlk2012 
13399-5328 RST5376     eps Cen                                                                         
13400+3759 KZA  76     AC: Error in RA caused resulting incorrect measure by Kazeza.           KZA1984 
13404+5031 STF1774     GJ 521.2. A is X-ray source. Debris disk? In Duquennoy & Mayor (1991).  Duq1991 
13407+7651 HJ 2682     C is BD+77@518.                                                                 
13407+5944 HJ 2673     B is BD+60@1481.                                                                
13407+1957 STF1772     1 Boo. B is a metallic-line star.                                               
13408-1748 SHY 630     HIP  66749 + HIP  66717.                                                        
13401-6033 TOK 292     HIP 66676 (A) and HD 118735 (B, G6V, V=9.17) at 77" share common PM             
                       (although it is small, 58mas/y) which, together with photometry,                
                       indicates with high probability that it is a  physical pair AB                  
                       (Tokovinin & Lepine 2012). We targeted the secondary component B and    Tok2015c
                       found it to be a resolved triple. The faint star C, at 0".92 from B,            
                       is itself a close 0".16 pair Ca,Cb.  Note that this is a region of the          
                       sky with very high stellar density, raising suspicion that the Ca,Cb            
                       pair might be a random background object. Re-observation of the triple          
                       in 2015  (to be published) shows, however, that it is physical because          
                       the center of C=(Ca,Cb) moves relative to B with a speed of 11mas/y             
                       (or 3km/s), compatible with the expected orbital motion of BC and much          
                       less than the system's PM of 58mas/y. The estimated period of Ca,Cb is          
                       ~30 years, the period of BC is ~300 years.                              Tok2015c
13412-3053 BGG   1     2MASS J13411160-30525049. Bardalez Gagliuffi et al. (2015) resolved             
                       this very low -mass binary, and derived spectral types L2.5 +/- 1.0             
                       and T6.0 +/- 1.0. Depending on age, this pair has a projected                   
                       separation of 8.1 +/- 0.5 au and estimated orbital period of 63-85y.            
                       Mass estimates range from 0.052-0.075 Msun for the primary,                     
                       0.022-0.061 for the secondary.                                          BGg2015 
13413+3422 SKF  41     AB: FAR  65.                                                                    
13414-6152 JSP 591     Spectrum composite: K2/3III+B8/A0V.                                             
13417-7507 HJ 4598     Spectrum composite: A0V+G8/K0III.                                               
13427+3459 HR 5161     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Beavers & Griffin (1979).                                               Bvr1979c
13430-3011 DAW 166     Possibly variable?                                                      B__1931b
13431+0332 STF1777     84 Vir. A is a spectroscopic binary.                                            
                       H 2  44.                                                                MEv2010 
13433-2458 HJ 2671     B is CD-24@11047.                                                               
13434+1341 BPM 606     [PM2000] 1064873 + [PM2000] 1064881.                                    Gvr2010 
13434-0556 LDS6281     NLTT 35007/35006                                                        Chm2004 
13435-0416 STF1775     A is a spectroscopic binary.                                                    
13440-5914 DUN 142     B is CPD-58@5094.                                                               
13441+1701 BPM 607     [PM2000] 1065196 + [PM2000] 1065149.                                    Gvr2010 
13444+2536 LDS5791     LDS6283.                                                                        
                       AB: NLTT 35070/35071                                                    Chm2004 
13446+5142 KUI  64     Ross 492.                                                                       
13446-1652 LDS6284     NLTT 35064/35065                                                        Chm2004 
13451+2512 BRT3300     Originally published as BRT 164.                                        Brt1928 
13451+1747 BUP 153     AB: Proper motion of A = +455.7 -1832.9 (Tycho).                                
                       Proper motion of B +012-014.                                                    
                       AC: Bu_1912 measures from 1875-1911 are Delta declination                       
                       (i.e., north-south vector separations).                                         
                       Proper motion of C -001-001.                                                    
13453+0903 BU  115     AB: B=SB? AC optical, shows reflex PM.                                  Tok2014d
13453-1031 S   652     AB: B is BD-09@3768.                                                            
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AC: C is BD-09@3766.                                                            
13454-4234 TOK 157     HIP 67121. A is SB without orbit (dRV=14.8).                            Nrd2004 
13456-1546 HJ 2677     85 Vir. A is a spectroscopic binary and occultation triple.                     
13459-1226 BU  935     86 Vir.                                                                         
           STF1780     AC: Additional notes may be found in Burnham (1894).                    Bu_1894 
13461+3131 LDS5222     LDS5792 = LDS6285.                                                              
                       NLTT 35170/35180                                                        Chm2004 
13461+0507 STF1781     One of the stars is probably variable.                                  Baz1972 
                       One component is a W UMa-type eclipsing binary.                         Wor1956b
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       One component is a W UMa-type eclipsing binary. A is the variable HT            
                       Vir. Errors for orbit of Alzner (2007) provided by author (private      Alz2007 
                       comm.) With the Hipparcos parallax of 15.39 +/- 2.72 mas, the Alzner            
                       solution yields a mass sum of 3.98Msun.                                         
13462+3054 PIN   8     Primary is a spectroscopic binary.                                      Pin2006 
13466+2826 KOP   1     Djurkovitz suspected the primary of being a close double. It looked             
                       single to me.                                                           B__1963b
                       Pair is +1m28s, +10' from BD+28 2257. Kopal (1939) believes motion is   Kop1939 
                       orbital, with period ~700y.                                             Cou1956 
13467-3636 POL   8     POL 2 1/2.                                                                      
13467-5126 HDO 225     A is a long-period spectroscopic binary.                                        
           M Cen       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Jones (1928).                                                           Jon1928d
13470+3833 S   654     AB: STTA125. B is BD+39@2679.                                                   
                       HJL 194.                                                                HJL1986 
           SHY 633     AC: HIP  67250 + HIP  67041.                                                    
13470+0621 LDS3101     B is BD+07@2692.                                                                
                       HIP 67246. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       SHY 253. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13472-4640 HRG  91     Aka SKF 468.                                                                    
13472-6235 COO 157     A semiregular variable, V766 Cen.                                               
13473+1727 STT 270     tau Boo = 4 Boo. A is a Delta Scuti-type variable.                              
                       AB: Tau Boo. A hosts exolanet, P=3.31d                                  Tok2014d
13477-3226 COO 159     SWR 145. CPM pair                                                       Skf2004 
13478+0639 GIC 115     G065-004/G065-005.  The B component corresponds to the primary of               
                       LDS6286; systems merged, with LDS pair labelled BC pair. However, no            
                       obvious C component is found, so the BC pair is X-coded.                        
13478+0112 BAL1459     RST 5529.                                                                       
13479-6352 COO 158     Includes V979 Cen, a Beta Lyr type eclipsing binary, P = 2.56835d.      Zas2012 
13481-1345 DEA   1     LHS 2803. Deacon et al. (2012) derive Teff 2940 +/- 60 and 1100-120K            
                       for the primary and secondary, respectively. The primary is M4.5 +/-            
                       0.5, the seconary T5.5 +/- 0.5. Distance estimates are consistent with          
                       the pair being physical: 21 +/- 3pc for the primary, 24 +5/-4 pc for            
                       the secondary.                                                          Dea2012 
                       Wide M/T binary. Spectral types M4.5 +/- 0.5 and T5.5 +/- 1, masses             
                       0.18 +/- 0.02 and 0.04 +/- 0.01 Msun, age > 4.0 Gyr. Distances for the          
                       two components are consistent, at 21.5 +/- 2.1 and 20.0 +/- 2.0 pc.     Muz2012 
13482+2248 COU 401     Docobo et al. (2010) derive a dynamic parallax of 16.28 +/- 0.20 mas    Doc2010h
                       and a total mass of 1.53 +/- 0.07 Msun.  The dynamical and Hipparcos            
                       parallaxes are discrepant.                                                      
13482-7739 NZO  42     Hipparcos acceleration double solution.                                         
13483-3653 RSS  19     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
13484+2337 LDS4410     GJ 1179A+B = NLTT 35290 + 35281. Secondary is white dwarf WD 1345+238.  Far2005b
13489-3542 HWE  94     HIP 67408. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
13490-2822 BU  413     A is a long-period variable, W Hya. B is CD-27@9430.                            
13490-6417 RST 659     13490-6417RST 659 Also knows as TDS8978. The identity of these two              
                       pairs determined by Skiff.                                              Skf2006 
13491+2659 STF1785     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.43 +/- 0.39, 1.49, and 1.34 Msun, respectively.             Mlk2012 
13492+0746 LDS3107     No companion is seen on Aladin at Luyten's original theta value. It     Luy1975 
                       appears likely that his theta value was due to a trigonometry error,            
                       however, and that the correct value was 270-28 = 242deg rather than             
                       270+28 = 298deg. A star seen at that position angle and Luyten's                
                       separation agrees with his magnitude and has a proper motion in                 
                       reasonable agreement, as well. Theta has been changed accordingly.              
13492-6206 DUN 143     Spectral types B2(II), K2/3II/III.                                              
13493-2135 LDS 459     NLTT 35336/35335                                                        Chm2004 
13495-2621 TOK 405     HIP 67458 is a double-lined chromospherically active binary with                
                       orbital period of 7.2d (Latham, 2012, private communication). We found          
                       a faint tertiary companion at 0".73 with an estimated orbital period            
                       on the order of 100yr. The speckle survey of chromospherically active           
                       stars by Mason et al. (1998) did not detect this tertiary, lacking the  Msn1998b
                       dynamic range of HRCam.                                                 Tok2015c
13496+3459 STF1786     AB: Identical with BDS 6644, HJ 852.                                            
           SHY 634     BC: HIP  67476 + HIP  67446.                                                    
13496+1302 SHY 635     HIP  67470 + HIP  67673.                                                        
13496-4228 HDO 226     mu Cen. A is an irregular variable.                                             
13496-4722 DUN 144     SWR 146. CPM pair                                                       Skf2004 
13496-6818 JNN  95     Due to the compact configuration of the three components resolved by            
                       AstraLux, the probability is very high for this to constitute a                 
                       physical triple system. Common proper motion has not yet been tested.   Jnn2012 
13498+3638 GC 18691    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
13499-2811 RSS  20     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
13501+4749 HIP  67526  Candidate brown dwarf companion found in MARVELS RV survey; period              
                       90.27d. Teff 6004K, minimum mass 65.0 +/- 2.9 Mjup.  Lucky imaging and          
                       AO find no tertiary companion, ruling out any stars with mass greater           
                       than 0.2 Msun at separations larger than 40au.                          Jia2013 
13501-4451 UC 2623     AC: CPM candidate confirmed physical by photometry (2MASS and V mags).  Tok2013c
13503-2742 UC 2624     SKF1493.                                                                        
13504+2117 S   656     STTA126 = H 6  89.  B is BD+21@2579.                                            
                       BDS 6648, H VI 15 probably same star. Called a spectroscopic binary in          
                       the BSC Supplement.                                                             
13505-5925 R   225     A variable?                                                                     
13507-2140 LDS 461     NLTT 35412/35392                                                        Chm2004 
13510+6819 STTA127     LDS2329.                                                                        
13513+2442 HIP  67615  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Griffin (1982).                                                         Grf1982e
13513-2423 WSI  77     The 10.3 yr SB1 orbit by Abt & Willmarth (2006) matches the speckle     AbH2006 
                       pair WSI 77 and explains the large dmu.                                 Tok2012a
                       Astrometric binary. Hipparcos parallax 51.35 +/- 0.45 mas. Dynamical            
                       parallax 50.3 mas, masses 0.99 and 0.63 Msun. WSI 77 is a                       
                       chromospherically active G5 dwarf within 20 pc from the Sun. According          
                       to Abt & Willmarth (2006), it is also a single-lined spectroscopic      AbH2006 
                       binary with 10.3 yr period. We used RVs from that work and the average          
                       RV from Nidever et al. (2002) together with four speckle points for     Nid2002 
                       the combined orbital solution presented. The spectroscopic elements             
                       are K1 = 6.06 +/- 0.25 km/s and V0 = 5.38 +/- 0.10 km/s, the rms                
                       residual in RV is 0.11 km/s. The node listed in Table 3 corresponds to          
                       the primary component, therefore Omega was chosen to describe the               
                       secondary’s relative motion. The pair was "caught" at close separation  .     
                       in 2012.                                                                Tok2012b
                       Omega for Tokovinin et al. (2012) orbit flipped by 180deg, at request           
                       of author.                                                              Tok2012b
13513-2734 LDS 855     NLTT 35441/35442                                                        Chm2004 
13514+6443 HJ 3342     10 Dra. A is an irregular variable, CU Dra.                                     
13514+3441 BU  613     C is BD+35@2495.                                                                
13515-4818 CPO  61     LDS 462. B is CD-47@8664.                                                       
                       SHY 636. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
13516-2945 LDS5797     Assuming the current identification is correct, it appears that the             
                       pair was originally tabulated at the position of the B component, but           
                       with magnitutes switched. Luyten's theta value has been flipped by 180          
                       deg and precise coordinates of the primary have been corrected. The             
                       11th magnitude component appears to be comprised of a ~4" pair.                 
                       (WIH, May 2008)                                                                 
13518+3143 LDS4415     NLTT 35491/35500                                                        Chm2004 
13518-3300 H 3 101     H III 101. 3 Cen.                                                               
13520-4752 HJ 4619     B is CD-47@8669.                                                                
13521-6653 DON 625     TDS9009.                                                                        
13529-6243 HD 120678   Hen 3-939.                                                                      
                       The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
13531+1251 HEI 524     The Durchmusterung identification is uncertain.                                 
13532-3156 H N  51     4 Cen. A is a spectroscopic binary. B is CD-31@10727.                           
13535-3540 I  1618     AD: WDS has 1 measure in 1927. 2MASS: AD at 28.3" 152d. AD optical?     Tok2014d
           H 5 124     AE: H V 124.                                                                    
13538+5210 JNN  96     The secondary detected in the AstraLux images is perhaps itself a               
                       close binary, as it appears extended in epochs 2008.64 and 2009.42.             
                       However, we count it as a single component of the system here.          Jnn2012 
13539+1008 BU  614     Same as STT 271.                                                                
                       Easier to see in 1964 than in 1962. Companion perhaps variable.         Cou1964 
13539-1440 RST3852     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.88 +/- 1.13, 3.17, and 1.40 Msun, respectively.             Mlk2012 
13540-4708 HJ 4624     A is the variable V767 Cen.                                                     
13540-7400 NZO  43     Spectrum composite: A3V+F8/G2III.                                               
13546+2429 BRT3302     Originally published as BRT 165.                                        Brt1928 
13546-5041 BSO   9     B is CD-50@8112.                                                                
                       SWR 148. CPM pair                                                       Skf2004 
13546-6654 DUN 145     B is CPD-66@2371.                                                               
13547+1824 eta Boo     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Bertiau (1957).                                                         BFC1957 
                       Daniel & Burns orbit rejected from Fourth Orbit Catalog                 Dni1939 
                       ("amplitude below noise level")                                         Wor1983 
           SHJ 169     eta Boo = 8 Boo = Muphrid. A is a long-period spectroscopic binary.             
                       B is BD+19@2726.                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
                       H 6  95.                                                                MEv2010 
13550+8724 STF1887     Doolittle (1901) 1897 measure corrected by the author for refraction            
                       and precession. Epoch=1900.  Probably rectilinear motion.               Doo1901 
13550-0804 STF1788     AB: A is SB, no orbit. A is X-ray source.                               Tok2014d
                       Hopmann's (1970) B and F are interchanged, and his orientational        Hop1970 
                       elements contain additional computing errors.                                   
           TOK 570     AE: AE can be optical (Pphys=0.24), but accepted because it is bright.  Tok2014d
13550-4235 I   401     Measures rather discordant.                                                     
13557-0925 RAP  19     Aa,Ab: EPIC 212651213. The primary of J 1609 consists of two eclipsing          
                       binaries, resolved at a separation of ~90mas:                                   
                       Aa1,Aa2: P =  5.08d, M = 0.94 +/- 0.06 and 0.89 +/- 0.05 Msun                   
                       Ab1,Ab2: P = 13.19d, M = 1.09 +/- 0.07 and 0.64 +/- 0.03 Msun.                  
                       Resolved pair has estimated period ~65y and separation of ~25au.        Rap2016 
           J  1609     AB: EPIC 212651213 + 212651234. The B component is single.              Rap2016 
13559-0945 TOK 158     HIP 68038.                                                              Tok2011a
13560-2532 H N  59     B is CD-24@11171.                                                               
13562+3627 SHY 641     AC: HIP  68069 + HIP  68576.                                                    
13563+2409 LDS5799     LDS6287.                                                                        
13563+0517 BU 1438     AB,C: The C "component" is the galaxy NGC 5363.                                 
13564+1654 BPM 608     [PM2000] 1071043 + [PM2000] 1071058.                                    Gvr2010 
13569-7349 HJ 4621     B is CPD-73@1217.                                                               
13571-2731 I   234     A premature orbit has been computed.                                            
13573-5602 DUN 151     A is an irregular variable. B is CPD-55@5793.                                   
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
                       Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                       candidate within separation/magnitude range listed. However,                    
                       further observations are required for verification                              
                       Additional notes may be found in van den Bos (1926).                    B__1928d
13574-6229 FIN 370     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.48 +/- 0.38, 2.34, and 1.12 Msun, respectively.             Mlk2012 
13575-5743 DUN 150     A is variable.                                                                  
13576-3139 SKF1963     Primary is the RS CVn-type binary V988 Cen.                                     
13577+1744 LDS 951     LDS1400.                                                                        
13577-1717 WHC  12     Wilson's 1882 distance for AC should read 31".42 (+ 1/2 rev.)           B__1950c
13579-5624 R   228     B is CPD-55@5797.                                                               
13583+0213 A  2167     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.24 +/- 1.47, 2.57, and 1.05 Msun, respectively.             Mlk2012 
13583-7158 TRR  15     AC: Also known as SIN  84AC.                                                    
13588+3140 JNN  97     LP 324-42.                                                                      
13588+1434 BPM 609     [PM2000] 1072223 + [PM2000] 1072207.                                    Gvr2010 
13593-6228 JSP 603     V1202 Cen, Algol (EA) type eclipsing binary, P = 15.5543 d.             Zas2011 
13594+2515 LDS6288     NLTT 35918/35919                                                        Chm2004 
13597-5056 SWR 149     CPM pair                                                                Skf2004 
13598+5144 LDS1401     NLTT 35954/35953                                                        Chm2004 
13599+2810 HDS1964     CX CVn, Algol (EA) type eclipsing binary, P = 6.563197 d.               Zas2011 
13599+2520 BUP 156     Distances 1033.9" and 1035.6". B is BD+26@2517.                                 
                       Secondary of BUP 156 is 14012+2522 A   569.