11001-5149 VIG  13     The C and D components appear to be faint background stars; the                 
                       optical/physical nature of the E component is undefined.                Vig2012 
11003+4255 KUI  53     A is also a spectroscopic binary with a period of 5244d which is not    Grf2014c
                       either of these visual pairs. With the proper motion similarity of              
                       the A and B components this could be a physical quadruple.                      
                       AB: A is SB1, P=10.812y. CfA: P(Aa,Ab)=5241d = 14.35y                   Tok2014d
           LEP  38     AC: SHY 219. Bayesian analysis by Shaya & Olling (2011) indicates only  Shy2011 
                       ~50% probability pair is physical.                                              
11005+1131 BPMA 43     [PM2000]  995938 + [PM2000]  995834.                                    Gvr2010 
11006+3832 ES  304     ALI 1090 is not present                                                 Hei1983a
11006+0337 CHR  33     58 Leo. Also an occultation binary.                                             
11006-1819 HJ 1181     A is the semiregular variable R Crt. B is BD-17@3279.                           
11007+0606 BU  598     59 Leo.                                                                         
11007-5835 BRT3160     Aka JSP 447.                                                                    
11009-4030 FIN 365     Hipparcos parallax 15.42 +/- 0.42 mas. Dynamical parallax 11.2 mas,             
                       masses 1.75 and 1.65 Msun. The latest measure contradicts the first             
                       orbit published in Hartkopf et al. (2012), which in fact predicts an    Hrt2012a
                       unrealistically small mass sum. We propose here an alternative orbit            
                       with retrograde motion which reproduces the non-resolutions by Finsen   Fin1966a
                       in 1963-1966 and corresponds to a reasonable mass sum. Double lines             
                       were noted by Nordstrom et al. (2004). The star appears to be evolved.  Nrd2004 
                       The Hipparcos parallax could be affected by the orbital motion                  
                       unaccounted for in its data reduction.                                  Tok2012b
11013-7627 BRR   1     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M1.5 +- 1        Teff = 3630 +- 150        L = 0.20  +- 0.03           
                          Age =  4.4 +5.1/-1.6   M =    0.41 +0.10/-0.06   R = 1.14  +- 0.05           
                       B: SpT = M2               Teff = 3560 +- 180        L = 0.22  +- 0.03           
                          Age =  3.3 +3.5/-1.0   M =    0.37 +0.13/-0.07   R = 1.24  +- 0.06   Dae2013 
11020+1437 STF1502     HJL 136.                                                                HJL1986 
11020-7131 Hen 3-554   Noted as possible binary (separation > 0".020) by Baines et al. (2006)  Bns2006 
11021+1659 BPM 579     [PM2000]  996665 + [PM2000]  996649.                                    Gvr2010 
11021-1542 H 1  77     H I  77.                                                                        
11022+0954 STF1503     A is the W UMa-type system AM Leo.                                              
11022+0945 HJ  172     HJL 137.                                                                HJL1986 
                       A small relative motion is obtained with uniform accuracy. There is no          
                       doubt the pair is physical.                                             Kiy2012 
11022-0335 BRT 548     J 2658.                                                                         
11024-2650 B   208     Too close, with few measures. Needs speckle.                                    
11026-2400 ALP  16     2MASSW J1102337-235945                                                          
                       Further observations are required to determine the physical/optical             
                       nature of this pair.                                                    AlP2007 
11026-7729 BRR   2     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M3               Teff = 3560 +- 270        L = 0.11  +- 0.03           
                          Age =  7.0 +8.0/-3.5   M =    0.37 +- 0.05       R = 0.90  +- 0.03           
                       B: SpT = M5               Teff = 3130 +- 270        L = 0.018 +- 0.003          
                          Age = 13.  +50/-7      M =    0.13 +0.08/-0.09   R = 0.44  +- 0.04   Dae2013 
11028-5944 JSP 455     The primary is variable.                                                        
11029+3541 HO   47     A,BC: SCH   1.                                                                  
11030-0323 LDS 330     NLTT 26095/26096                                                        Chm2004 
11031+3215 SEI 522     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
11033+3558 Lal 21185   GJ 411 = Ci 20,604                                                              
                       Lippincott (1960) orbit rejected from Fourth Orbit Catalog              Lip1960 
                       ("not confirmed by subsequent observations")                            Wor1983 
                       They investigated the entire 40y plate series on Lalande 21185 and      Hry1982b
                       suggested a companion of, at most, two Jupiter mass and a period of             
                       22 years. They state that the 8y period, seen in data prior to 1960,            
                       was not seen after that.                                                        
11035+5432 A  1590     Heintz (1963) determined an orbit from combined visual, spectroscopic,          
                       and transit observations.                                               Hei1963a
11037+6145 BU 1077     alp UMa = 50 UMa = Dubhe.                                                       
                       Soderhjelm (1999) orbit has low incl. fixed at 180 deg; observations    Sod1999 
                       are lacking near periastron. Pair has a giant primary according to              
                       isochrone fit.                                                                  
                       Faint, distant pair at 385", 7.60V. Possible common proper motion               
                       with the SB HD 95638 at 280".                                                   
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       photocentric (astrometric) orbit based on combination of ground-        Gon2002a
                       based catalogs with Hipparcos.                                                  
                       Companion could not be seen any more the following years.               VBs1954 
                       AB: Malkov et al. (2012) derive dynamical and spectroscopic masses              
                       5.56 +/- 0.80 and 2.75 Msun, respectively.                              Mlk2012 
11037+4420 HJ 2554     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
11037+3253 HJ  493     Position by Espin is 1 minute greater in right ascension than John              
                       Herschel's. Used Espin position.                                                
11040+4321 FMR  14     SLW 561.                                                                        
11042-7627 SDT   1     AB: Companion appears to be co-moving with primary CT Cha. Schmidt et           
                       al. (2008) estimate the spectral type of the secondary at M8-L0.; most  Sdt2008b
                       probable mass is 17 +/- 6 Mjup. C component is a background star.               
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = K7               Teff = 4060 +- 180        L = 0.67  +- 0.15           
                          Age =  3.0 +3.0/-1.5   M =    0.78 +- 0.20       R = 1.66  +- 0.07   Dae2013 
11044-6118 PLT   2     EH Car.                                                                 Plt1934 
11045+3814 HO  377     51 UMa.                                                                         
           HZG   8     AC: HJL1060.                                                            HJL1986 
11047-0413 STF1506     A,BC: Star A (mag 7.64, 11", G5) is physical and in slow direct motion          
           A   676     BC: Incorrectly listed by Docobo (1984) as STF1514 (erratum noted in    Doc1984b
                       Inf. Circ. 93, 1984)                                                            
                       BC. Eggen's (1967) orbit for this pair of 11th magnitude M dwarfs       Egg1967 
                       predicts a separation of 0".20 and a position angle of 86deg at this            
                       epoch.  Our measurement is in poor agreement with this prediction.      Hrt1992b
                       BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.36 +/- 0.38, 1.19, and 0.91 Msun, respectively.  Mlk2012 
           LAF  43     Heinze et al. (2010) determine the E component is a background object.  Hze2010 
11049+0634 GIC  95     G045-031/G045-032.                                                              
11049-6103 DUN 105     The classification of the B component is from Lindroos (1985),          Lnd1985 
                       who finds a distance of 3.5 kpc.                                        Msn1998a
11050+0720 KUI  54     chi Leo = 63 Leo                                                                
11052-7711 LAF   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M4               Teff = 3270 +- 110        L = 0.10  +- 0.02           
                          Age =  4.2 +- 1.0      M =    0.22 +0.07/-0.05   R = 1.00  +- 0.03           
                       B: SpT = M3 +- 1          Teff = 3420 +- 150        L = 0.11  +- 0.02           
                          Age =  5.2 +5.0/-0.7   M =    0.30 +- 0.08       R = 0.95  +- 0.04           
                       The primary may be an SB2.                                              Dae2013 
11053+8102 GIC  96     LDS5203 = G253-042/G253-043.                                                    
                       NLTT 26133/26138                                                        Chm2004 
11053-2718 FIN  47     chi 1 Hya.                                                                      
                       Masses and bolometric magnitudes are derived for the two components of  Msn1999a
                       this system by Mason et al. (1999), based on assumed spectral types             
                       and available parallaxes.                                                       
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       van den Bos (1957).                                                     B__1957a
                       A new orbital analysis of this system is in progress, some three                
                       decades after  van den Bos published his solution.                      Hrt1996b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.79 +/- 0.19, 2.70, and 1.41 Msun, respectively.  Mlk2012 
11055+4332 VBS  18     Proper motion -4405 +940. The companion is WX UMa.                              
                       NLTT 26245/26247                                                        Chm2004 
11056-1105 TOK 221     Astrometric binary; dm 5.4 mag, period ~ 30y Orbit (Gontcharov et al.           
                       2000)                                                                   Tok2012b
11057-7727 AHM   1     CHXR 15. Primary spectral type M5.25. Estimated mass ratio 0.64         Ahm2007 
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M5 +- 1          Teff = 3130 +- 140        L = 0.06  +- 0.01           
                          Age =  4.5 +2.5/-0.9   M =    0.16 +- 0.05       R = 0.87  +- 0.04           
                       B: SpT = M5               Teff = 3130 +- 170        L = 0.04  +- 0.01           
                          Age =  6.0 +6.0/-2.0   M =    0.14 +- 0.06       R = 0.71  +- 0.04   Dae2013 
11058+7440 MLR 423     Also known as TDS 616.                                                          
11061+7837 LDS1726     NLTT 26189/26190                                                        Chm2004 
11061+4253 GIC  97     AB: NLTT 26262/26264                                                    Chm2004 
11061+1325 BRT1271     Declination corrected by Heintz.                                        Hei1980a
11061+0702 STF1507     HJL 138.                                                                HJL1986 
                       H 2  78.                                                                MEv2010 
11063+3113 OSO  36     G120-015. AC is not a common proper motion pair, based on comparison            
                       with POSS2 red plates.                                                  Oso2004 
11065-1325 STF1509     B is BD-12@3347.                                                                
11065-5841 HDO 210     A is variable.                                                                  
11065-7738 LUH  17     The primary is the young low-mass star CHXR 73 (mass ~0.35 Msun).               
                       Luhman et al. (2006) conclude that the companion is also a member of            
                       Chamaelon I, and a young pre-main sequence star, spectral type >M9.5,           
                       mass 0.012 +0.008/-0.005 Msun.                                          Luh2006c
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M2.5             Teff = 3490 +- 180        L = 0.09  +- 0.07           
                          Age =  8.  +70/-5      M =    0.32 +- 0.11       R = 0.83  +- 0.04   Dae2013 
11069+0157 BU  599     65 Leo.                                                                         
11072+5711 HJ 2556     Position correction by Heintz.                                          Hei1983a
11072+3204 SEI 523     ID uncertain - no sign of SEI pair, and ALADIN only indicates one               
                       Astrographic Catalog star in vicinity of Scheiner's coordinates.                
11072-5952 SNA  21     The new companion can hardly be the SB1 companion (P=5.5d) from         Stc2001 
                       Stickland & Lloyd (2001).                                               Sna2014 
                       The classification and SB1 orbit are from Garcia (1994 ApJ 436, 705).   Msn1998a
11073+2832 HJ 1185     C is a faint nebula (NGC 3527). Distance 259.4".                                
11073-4238 HJ 4409     The variable V815 Cen.                                                          
11073-7738 REP  17     DI Cha, a quadruple in a star-forming region in Chamaelon. Schmidt et           
                       al. (2013) resolve the primary into a 0.2" G2/M6 pair, with estimated           
                       orbital period of 130y. The B component is a 50mas pair of M5.5 +/-             
                       1.5 dwarfs, with estimated period 65y.                                  Sdt2013 
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = G0               Teff = 6030 +- 290        L = 4.7   +- 1.0            
                          Age =  7.1 +3.0/-0.7   M =    1.7  +- 0.2        R = 2.00  +- 0.10           
                       B: SpT = M5               Teff = 3130 +- 290        L = 0.11  +- 0.02           
                          Age =  3.0 +3.0/-2.8   M =    0.18 +0.06/-0.08   R = 1.13  +- 0.11   Dae2013 
11074-1522 TOK 139     HIP 54366. A is SB1, P=1061d, N04: dRV= 1.6.                            Tok2014d
11074-4815 CPO 316     B is CD-47@6520.                                                                
11075-7651 REP  19     Aa,Ab: VV Cha. Imprecise coordinates led to REP 19 and KSA 42 being             
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       Aa: SpT = M1.5            Teff = 3630 +- 180        L = 0.14  +- 0.03           
                           Age =  7.0 +9.0/-3.0  M =    0.40 +0.14/-0.06   R = 0.96  +- 0.05           
                       Ab: SpT = M3 +- 1         Teff = 3420 +- 150        L = 0.09  +- 0.02           
                           Age =  6.4 +4.7/-2.2  M =    0.29 +- 0.07       R = 0.87  +- 0.04   Dae2013 
           KSA  42     initially catalogued as separate pairs. Although REP 19 was added to            
                       the WDS before KSA 42, its WDS designation was less accurate, so was            
                       changed from 11072-7651.                                                        
11076+2346 BRT3297     Originally published as BRT 159.                                        Brt1928 
11077+5958 PRB   3     Primary is WD 1104+60 = NLTT 26342, secondary is LP 93-311. Possible            
                       CPM pair, according to Probst (1983).                                   Prb1983 
11077-7734 AHM   2     Cha Ha 2. Primary spectral type M5.25. Estimated mass ratio 0.94        Ahm2007 
11079-7727 AGE   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = K7               Teff = 4060 +- 290        L = 1.2   +- 0.3            
                          Age =  1.3 +2.5/-0.5   M =    0.75 +- 0.25       R = 2.21  +- 0.16           
                       B: SpT = M2.5             Teff = 3490 +- 110        L = 0.42  +- 0.09           
                          Age =  1.6 +- 0.4      M =    0.36 +- 0.04       R = 1.78  +- 0.06           
                       The B component may be an SB1.                                          Dae2013 
11080+4100 LDS4062     NLTT 26367/26368                                                        Chm2004 
11080-0509 LDS 852     LDS6239.                                                                        
                       G163-51 / G163-50.  Secondary is white dwarf WD 1105-048.               Far2005b
11080-7739 GHE  34     The primary is Sz 22, embedded in a circumstellar disk or reflection            
                       nebula. Schmidt et al. (2014) resolve the A component into a 0.5"               
                       pair; the Ab component is a co-moving M4.5 +/- 1.5 dwarf.               Sdt2013 
           LAF   8     BC: Daemen et al. (2013) derive the following component properties              
                       (units are K,Lsun,Myr,Msun,Rsun):                                               
                       B: SpT = M0.5             Teff = 3780 +- 400        L = 0.50  +- 0.09           
                          Age =  2.0 +8/-1.1     M =    0.52 +0.38/-0.19   R = 0.47  +- 0.05           
                       C: SpT = M0.5             Teff = 3780 +- 400        L = 0.090 +- 0.006          
                          Age > 23.              M =    0.50 +- 0.2        R = 0.70  +- 0.07   Dae2013 
11080-7742 GHE  35     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = K7               Teff = 4060 +- 460        L = 1.6   +- 0.3            
                          Age =  1.0 +3.0/-0.7   M =    0.75 +0.50/-0.35   R = 2.55  +- 0.29           
                       B: SpT = M0 +- 1.5        Teff = 3850 +- 290        L = 0.76  +- 0.10           
                          Age =  1.5 +2.5/-0.6   M =    0.57 +0.28/-0.19   R = 1.97  +- 0.15           
                       The primary may be an SB2.                                              Dae2013 
11083-7734 GHE  27     IRAS 11068-7717 = PDS 47 = Glass I.                                     Gre1992 
                       CHXR 32 is a triple system, consisting of a single G5 star with an              
                       edge-on disk, and a co-moving pair of M1/M3.5 dwarfs.                   Sdt2013 
                       Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT < M3                                                                     
                       B: SpT = M0.5             Teff = 3780 +- 210        L = 0.57  +- 0.13           
                          Age =  1.8 +2.2/-0.7   M =    0.52 +0.18/-0.14   R = 1.77  +- 0.10   Dae2013 
11084+0313 H 5  68     H V 68. B is BD+03@2462.                                                        
11084-7742 NHR   6     Primary is Cha Halpha 5, a close (50mas) pair of M5-M7 dwarfs, with an          
                       estimated orbital period of 46y.                                        Sdt2013 
11087-5037 CPO 318     TDS7696.                                                                        
11088+2610 LDS4064     AB: NLTT 26415/26414                                                    Chm2004 
11088+2440 A   677     67 Leo.                                                                         
11088-7519 KOH  89     PU Car.                                                                         
11092-1851 B  2007     Difficult pair; measures puzzling.                                      B__1963b
11092-3002 WBB   2     This previously known binary (e.g. Webb et al. 1999) is part of the     Wbb1999 
                       TW Hya association, and is also known as TWA 2.                         Jnn2012 
11092-7729 REP  20     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M2.5 +- 0.5      Teff = 3490 +-  70        L = 0.25  +- 0.05           
                          Age =  2.7 +0.7/-0.5   M =    0.36 +- 0.05       R = 1.37  +- 0.03           
                       B: SpT = M2 +- 0.5        Teff = 3560 +-  70        L = 0.20  +- 0.04           
                          Age =  4.0 +1.3/-1.0   M =    0.38 +- 0.05       R = 1.17  +- 0.02           
                       C: SpT = M2.5 +- 0.5      Teff = 3490 +-  70        L = 0.14  +- 0.03           
                          Age =  4.7 +2.3/-1.2   M =    0.34 +- 0.05       R = 1.04  +- 0.02           
                       The B component is an SB1.                                              Dae2013 
11093-7630 BRR   3     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       Aa: SpT = M2 +- 1         Teff = 3560 +- 150        L = 0.36  +- 0.07           
                           Age =  2.0 +1.0/-0.5  M =    0.38 +0.10/-0.05   R = 1.57  +- 0.07           
                       Ab: SpT = M4              Teff = 3270 +- 110        L = 0.035 +- 0.007          
                           Age = 12.  +8.0/-5.5  M =    0.19 +0.14/-0.04   R = 0.59  +- 0.02   Dae2013 
11095+8306 STF1499     LDS1728.                                                                        
                       HJL 139.                                                                HJL1986 
11095-2559 LDS4067     CPM. B is white dwarf WD1107-257                                        Tok2014d
11098+6320 H 4 106     H IV 106. Also known as STF1513.                                                
11098-7637 GHE  28     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = B9               Teff =10500                                           
                       B: SpT = M3.5 +- 0.5      Teff = 3340 +-  70        L = 0.11  +- 0.08           
                          Age =  4.5 +15/-1.9    M =    0.26 +- 0.07       R = 0.99  +- 0.02   Dae2013 
11098-7731 PSI   3     Perci et al. (2005) found [KG2001] 102 to consist of 4 components,      Psi2005 
                       all within a 2" region. The A component is determined to be                     
                       substellar, with a mass of 33-55 Mjup at a distance of 160 pc. The C            
                       and D components are believed to be physical companions, but the B              
                       component, of spectral type K7V, is probably a background star at a             
                       distance of about 550 pc. Nearby star "Anon1" was also found to be              
                       double.                                                                         
11098-7738 GHE  29     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M1               Teff = 3710 +- 200        L = 0.81  +- 0.15           
                          Age =  1.1 +0.6/-0.3   M =    0.49 +- 0.12       R = 2.18  +- 0.12           
                       B: SpT = M5               Teff = 3130 +- 210        L = 0.10  +- 0.02           
                          Age =  3.3 +2.7/-2.9   M =    0.18 +0.05/-0.06   R = 1.08  +- 0.07   Dae2013 
11099+1456 BPMA 44     [PM2000] 1000317 + [PM2000] 1000217.                                    Gvr2010 
11099+1107 FYM  37     AB and AC were initially incorrectly assigned to 11091+1105 HJ 176.     FyM2014b
11099-7629 LAF  11     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       Aa: SpT = M3.5            Teff = 3340 +- 290        L = 0.29  +- 0.06           
                           Age =  1.8 +1.2/-1.6  M =    0.30 +0.11/-0.10   R = 1.62  +- 0.13           
                       Ab: SpT = M7              Teff = 2880 +- 360        L = 0.05  +- 0.01           
                           Age =  4.0 +4.0/-3.9  M =    0.08 +0.12/-0.07   R = 0.91  +- 0.11   Dae2013 
11100+1237 LDS6240     NLTT 26471/26477                                                        Chm2004 
11103+3840 HJ 2561     A measure by Schembor (1926.08, 172.6@, 23.24") appears instead to be   Sch1927a
                       an additional measure of 11221+3705 STF1533A,BC.                                
11105-3732 REP  21     IRAS 11080-3715 = PDS 50 = TWA 3.                                       Gre1992 
                       This previously known binary (e.g. Brandeker et al. 2003) is part of    Bnk2003 
                       the TW Hya association, and is also known as TWA 3.                     Jnn2012 
11106-7733 GHE  36     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       Aa: SpT = K5.5            Teff = 4210 +- 390        L = 0.72  +- 0.14           
                           Age =  4.5 +9.5/-3.1  M =    0.95 +0.20/-0.42   R = 1.60  +- 0.15           
                       Ab: SpT = K7              Teff = 4060 +- 210        L = 0.47  +- 0.09           
                           Age =  5.5 +6.5/-3.0  M =    0.80 +0.20/-0.22   R = 1.39  +- 0.07           
                       The pair is also an SB2.                                                Dae2013 
11107+3110 HJ 2562     A premature orbit has been calculated.                                  B__1963b
11107-6023 SNA  22     Aa,Ab: The central object was reported as possible SB1 (Thackeray et            
                       al. 1973, MmRAS 77, 199; Chini et al. 2012) but without more            Cii2012 
                       information on the spectroscopic period                                         
                       one cannot decide whether the spectroscopic and PIONIER companions              
                       are identical. The separation and magnitude difference make this a              
                       plausible option, however.                                              Sna2014 
11109-7646 AHM   3     Hn 13. Primary spectral type M5.75. Estimated mass ratio 0.95           Ahm2007 
11110+0625 OSO  37     G010-004. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
11111+3027 STT 231     Mt. Wilson spectral types M1, M2, G5.                                           
                       AB: NLTT 26534/26531                                                    Chm2004 
                       Pair was listed, but in a "rejected" list, not part of discoverer's             
                       regular numbering sequence.                                                     
                       AB Hyperbolic orbit by Hopmann (1960). e = 575.                         Hop1960b
                       sigma = areal constant in the true orbit = 3.75 arcsec^2/yr                     
                       q = periastron distance in the true orbit = 33".73                              
                       All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
11113+6601 S   621     STTA107.                                                                        
                       AB and AC: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
11114+4325 KUI  55     NLTT 26552/26553                                                        Chm2004 
11115+2518 LDS4071     NLTT 26562/26559                                                        Chm2004 
11115+1520 BPM 580     [PM2000] 1001018 + [PM2000] 1001022.                                    Gvr2010 
11116-1459 LTT 4120    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11117+3441 KZA  10     No object at precise coordinates of A component down to >20th mag,              
                       although Kazeza's AB and AC measures from that location do point to             
                       stars of appropriate magnitudes. Conclude A component is probably               
                       plate flaw. CB measure calculated from Kazeza's AB and AC measures.     Kza1984 
11118+4250 ENG  45     AB: NLTT 26576/26564                                                    Chm2004 
                       AB: HJL 140.                                                            HJL1986 
                       AB: SHY 221. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       AB: A is possibly astrometric binary.                                   Tok2014d
11118-3045 BRT2985     SWR 108.                                                                        
11118-6042 B  1182     The star belongs to a group behind Tr 18 (Vazquez & Feinstein 1990              
                       A&AS 86, 209) at a distance of 2.8 kpc; we designate this as "Tr 18B"           
                       in Table 1.                                                             Msn1998a
11118-7620 LAF  14     B is a background star unrelated to A, a young Cha I object.            Laf2008 
11119-7620 LAF  15     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M2.5             Teff = 3490 +- 110        L = 0.20  +- 0.04           
                          Age =  3.4 +1.2/-0.8   M =    0.34 +- 0.06       R = 1.22  +- 0.04           
                       B: SpT = M3.5             Teff = 3340 +- 110        L = 0.15  +- 0.03           
                          Age =  3.4 +1.2/-0.6   M =    0.27 +- 0.06       R = 1.15  +- 0.04   Dae2013 
11121-7126 B  2273     A may be variable.                                                              
11124-7637 REP  22     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = K7 +- 3          Teff = 4060 +- 590        L = 0.76  +- 0.17           
                          Age =  2.5 +13/-1.7    M =    0.78 +- 0.40       R = 1.77  +- 0.26           
                       B: SpT = M2.5 +- 1.5      Teff = 3490 +- 220        L = 0.10  +- 0.02           
                          Age =  7.2 +12/-3.4    M =    0.32 +0.12/-0.09   R = 0.85  +- 0.05   Dae2013 
11125+3549 STTA108     AB and AC: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
                       Primary is MN UMa, variable of BY Dra type.                             Tok2014d
           KIR   3     AE. Data from 2MASS. Kirkpatrick et al. (2001) derive spectral types    Kir2001a
                       G0V and L4.5V, determine is physical pair, separation ~2000 au.                 
           STTA108     BD: Distances are 2083.6" in 1825, 2094.6" in 1910. D is BD+36@2170.            
           BOY   5     Ea,Eb: Originally listed as separate pair WDS 11124+3548, before                
                       association with  WDS 11125+3549 recognized.                                    
                       Dupuy et al. (2014) find a total mass 0.095 +/- 0.003 Msun (99 +/- 3            
                       Mjup), log age 8.87 +/- 0.08. Spectral types are L4.5 and L6.           Dup2014 
11125-1830 BU  220     psi Crt.                                                                        
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 10.78 +/- 6.79, 4.90, and 2.19 Msun, respectively.            Mlk2012 
11125-4905 CPO 319     CPD-48@3801.                                                                    
11127-7722 WOI   1     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = G8 +- 3          Teff = 5507 +- 440        L = 2.0   +- 0.4            
                          Age = 16.  +30/-10     M =    1.3  +- 0.2        R = 1.52  +- 0.12           
                       B: SpT = K7 +- 1.5        Teff = 4060 +- 310        L = 0.35  +- 0.08           
                          Age =  9.0 +16/-6.5    M =    0.80 +0.15/-0.3    R = 1.20  +- 0.09   Dae2013 
           LAF  16     AC: C is a background star unrelated to the close AB pair.              Laf2008 
11128-6410 HJ 4415     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
11131+4011 HJ  494     Same as STF1515.                                                                
11135-5526 HJ 4417     B is CPD-54@4398.                                                               
11136+5525 A  1353     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.68 +/- 1.12, 2.70, and 1.20 Msun, respectively.             Mlk2012 
11137+2506 SHY 567     HIP  54845 + HIP  54217.                                                        
11137+2008 STF1517     Alternate spectral types G5III, G7IV. Slightly variable.                        
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1970 
                       ("period over 4000 years")                                              Wor1983 
           BU 1431     AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
11140-1904 LDS4073     NLTT 26694/26692                                                        Chm2004 
11141+2031 STT 573     AB: del Leo = 68 Leo = Zosma. Variable? Smyth's quoted separations for  Smy1844 
                       both AB and AC are differences in RA only.                                      
11144-2245 LDS 341     NLTT 26721/26720                                                        Chm2004 
11144-7733 BRR   4     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M3.5             Teff = 3340 +- 110        L = 0.11  +- 0.02           
                          Age =  4.5 +2.0/-1.0   M =    0.26 +- 0.05       R = 0.99  +- 0.03           
                       B: SpT = M6.5             Teff = 2940 +- 200        L = 0.030 +- 0.006          
                          Age =  5.5 +4.5/-1.5   M =    0.08 +0.10/-0.05   R = 0.66  +- 0.04   Dae2013 
11145+1823 LDS4074     NLTT 26709/26710                                                        Chm2004 
11145+0516 STF1518     J 1012.                                                                         
11148+2257 POU3098     ELS 3 is identical                                                      Hei1983a
11148-7734 LAF  19     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M2 +- 1          Teff = 3560 +- 150        L = 0.19  +- 0.04           
                          Age =  4.0 +4.0/-1.3   M =    0.37 +0.10/-0.05   R = 1.15  +- 0.05           
                       B: SpT = M4               Teff = 3270 +- 150        L = 0.05  +- 0.01           
                          Age =  8.0 +7.0/-3.2   M =    0.20 +0.07/-0.05   R = 0.71  +- 0.03   Dae2013 
11150+1607 DEA  75     NLTT 26746 + 2MASS J11150150+1607026. Baron et al. (2015) estimate              
                       spectral types M4.0 +/- 0.5 and L5 +/- 1, distances 36 +22/-14 and              
                       37 +3/-35 pc, masses 0.207-0.272 and 0.056-0.073 Msun.                  BFr2015 
11150-5420 BRT2062     CD-53@3941.                                                                     
11151+3735 CHR 192     1987.2666: CHR 192Aa,Ab is a new component to the 0".6 pair STT 232,            
           STT 232     discovered by Otto Struve in 1843. Reprocessing of archival data                
                       (whose 1987 and 1988 measurements for the wide pair were originally             
                       published in McAlister et al. 1989) has allowed us to confirm this      McA1989 
                       discovery and also to note that the system appears to be accelerating           
                       toward periastron.                                                              
11151-3929 SEE 128     Direct motion.                                                                  
11151-6116 B  1184     AE and AF pairs erroneously designated I  1132.                                 
11152+7329 STF1516     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           STT 539     AC: NLTT 26722/26719                                                    Chm2004 
           HDS1603     BD: BD+74  456a.                                                                
11153-0132 LDS4076     NLTT 26765/26766                                                        Chm2004 
11154-1807 LDS 342     B is BD-17@3337.                                                                
11154-5249 HD 97961    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11157+4551 STTA109     B is BD+46@1707.                                                                
11157-1621 SHJ 372     B is BD-15@3226.                                                                
                       H N 104.                                                                MEv2010 
11159+1318 MCA  35     73 Leo. A spectroscopic binary now resolved by speckle interferometry.          
                       1985.1123, 1985.2053: This system has been observed at the limit of             
                       resolution of a 2-m telescope, so delta m is probably < 1.              Bnu1986 
                       Values of P, T, e, and omega for the Ren & Fu (2007) orbit are adopted  RSl2007 
                       from the orbit of Mason et al. (1997). Their derived masses for the     Msn1997b
                       primary and secondary are 1.81 +/- 0.49 and 1.54 +/- 0.42 Msun,                 
                       respectively.  The authors note that these masses are less than the             
                       ones predicted by either the Mason et al. or Mante (2002) solutions,    Mnt2002a
                       but that their secondary mass is in reasonable agreement with the               
                       value expected for an F1 main-sequence star.                                    
                       Martin et al. (1998) derive component masses 2.624 +/- 1.197 and                
                       2.315 +/- 1.075 Msun.                                                   Mig1998 
                       Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                       2.49 +/- 0.65 and 2.40 Msun, respectively.                              Mlk2012 
11159+0205 NLTT 26792  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Carney et al. (2001) They derived component masses 1.18 and 0.60 Msun   Crn2001 
                       and an estimated semimajor axis of 16.36 mas.                           Ren2013 
11161+5246 STF1520     HJL 142.                                                                HJL1986 
                       H N  68.                                                                MEv2010 
                       GJ 421.1                                                                Tok2014d
11165+6913 SHY 569     HIP  55076 + HIP  58483.                                                        
11165+2627 BUP 137     B is BD+27@2000.                                                                
11166-5215 RST9002     Previously known as RST2737a.                                                   
11167-0339 SHJ 121     74 Leo = phi Leo. B is BD-02@3314.                                              
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
                       H 6  79.                                                                MEv2010 
11170-0708 BU  600     A is an Alpha CVn-type variable, SV Crt., and a spectroscopic binary.           
                       AC: H N  26.                                                            MEv2010 
11172-0153 EPI   1     EPIC 201338508 = K2-5. Primary is host star to two planets; planet              
                       periods 5.73 and 10.93d, radii 1.92 Rearth, a 0.05 and 0.08 au.         Mtt2015b
11173-6749 DON 471     A is variable.                                                                  
11175-5906 R   163     Spectrum B9.5/A0III.                                                            
11177-2705 RST1572     TDS7778.                                                                        
11179-4034 I  1538     Measures uncertain.                                                             
11182+3132 STF1523     xi UMa = 53 UMa = Alula Australis. A is known to have an unseen                 
                       companion, P = 1.83y. B is a spectroscopic binary. The first binary             
                       star orbit was computed by Savary, a "librarian-observer" at Paris      Sav1830 
                       Observatory giving courses in "social arithmetic," i.e., statistics.            
                       Spectral types and masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       Preliminary Keplerian AB 2-orbit model by Soderhjelm (1999) gives       Sod1999 
                       good solution (failure in HIP).                                                 
                       Many-body perturbations observable but not yet studied. Cf. Aa,Bb               
                       analysis in Mason et al. (1995)                                         Msn1995 
                       Both orbits are visual and spectroscopic. The orbit of the visible              
                       AB pair includes the secular perturbations in inclination, node,                
                       longitude of periastron, and K. Star B is also SB1, P = 3.98 d.                 
                       The short-period pair has been resolved by infrared speckle                     
                       interferometry                                                          Mcy1983 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       HR 4375 (A component of STF1523) was misidentified as HR 4374 (B                
                       component) in McAlister (1978).                                         McA1978c
                       An orbital analysis of xi UMa, including the AB pair, the astrometric           
                       companion, and the newly-discovered Bc companion, has been published            
                       by Mason et al. (1995).                                                 Msn1995 
                       AB: H 1   2.                                                            MEv2010 
           CHR 178     Bb. Abt & Biggs (1972) note variable RV.                                AbH1972 
                       Given the typical lack of accuracy associated with astrometric orbits   Tok2010b
                       it is possible that in the doubling of peaks CHR 178 is actually the            
                       known Aa,Ab observing when the faint Ab was flaring. In this                    
                       interpretation, the second elongated observation of CHR 178 is assumed          
                       to be false.                                                                    
           WTE   1     AD: Faint T8.5 brown dwarf companion at separation ~4000au exhibits             
                       common proper motion. IR luminosity and color suggest that mass of              
                       companion 14 and 38 Mjup for system ages 2 and 8 Gyr, respectively.     WtE2013H
11183+0746 HEG   1     This  is evidently a lensed quasar and not a double star, or at the             
                       very least with a Z of 1.7, is not a galactic double star.                      
11184-7622 BRR   5     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M0 +- 1          Teff = 3850 +- 180        L = 0.44  +- 0.10           
                          Age =  3.0 +4.0/-1.4   M =    0.58 +0.20/-0.13   R = 1.50  +- 0.07           
                       B: SpT = M1               Teff = 3710 +- 110        L = 0.12  +- 0.02           
                          Age = 12.  +17/-7      M =    0.46 +0.10/-0.18   R = 0.83  +- 0.02   Dae2013 
11185+3306 STF1524     nu UMa = 54 UMa = Alula Borealis                                                
                       H N  53.                                                                MEv2010 
11187+0250 STF1526     B is BD+03@2482.                                                                
                       Primary is eclipsing binary of Algol-type, period 9.1784 d.             Zas2012 
                       HJL 143.                                                                HJL1986 
11188-4812 RST4941     TDS7782.                                                                        
11190+1416 STF1527     A premature orbit has been computed.                                            
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       H N 142.                                                                MEv2010 
                       Prieur et al. (2012) derive a dynamical parallax of 31.2 mas and                
                       (using their orbital elements and the revised Hipparcos parallax of             
                       van Leeuwen 2007 A&A 474, 653) a total mass 1.7 +/- 1.0 Msun.           Pru2012 
                       Hipparcos parallax 32.52 +/- 1.39 mas. Dynamical parallax 34.2 mas,             
                       masses 0.98 and 0.61 Msun. STF 1527 has a long orbital period of 415y,          
                       but it moved fast through the periastron in 2009-2012, allowing us to           
                       compute a better orbit.                                                 Tok2012b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.04 +/- 1.03, 2.06, and 1.07 Msun, respectively.             Mlk2012 
11191+3811 CHR 133     55 UMA. Primary is 2.6d SB1 (#669 in Batten et al., 1989).              Bte1989 
                       The speckle pair must be different, hence a triple.                             
                       Mass-sum in fair agreement with Liu et al. (1997)                       Liu1997 
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       McAlister et al.                                                                
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 5.89 +/- 0.40, 4.71, and 2.09 Msun, respectively.             Mlk2012 
11192-1950 ARA 683     Primary is RV Crt, Algol-type eclipsing binary, period 1.170509d.       Zas2013 
11194-0139 STF1529     NLTT 26997/26995                                                        Chm2004 
11194-6435 LDS6242     A is CD-63@643.                                                                 
11197-0125 LDS4083     NLTT 27027/27026                                                        Chm2004 
11200+6551 TAM   1     Primary is the nearby flar star Gl 424 = SZ UMa. The companion appears          
                       to be a M4.5 dwarf, with a mass of ~0.18Msun. Estimated orbital period          
                       of the system is about 2.5y.                                            Tam2008b
11204+0117 EPI   2     EPIC 201549860. Primary is candidate planet host star; planet period            
                       5.61d, radius 2.20 Rearth, a 0.06 au.                                   Mtt2015b
11205+0530 HJ 2566     G045-048. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
11206+0230 EPI   3     EPIC 201629650 = K2-13. Primary is planet host star; planet period              
                       39.91d, radius 1.89 Rearth, a 0.21 au.                                  Mtt2015b
11206-2718 BRT2986     CPD-26@4502.                                                                    
11210-5429 I   879     pi Cen.                                                                         
                       The spectral lines are very poor; the RV range of 30km/s is probably            
                       mere scatter. A few more speckle obs needed to constrain eccentricity.          
                       1976.474: This system was observed within a few months of periastron.   BLM1978 
                       Hipparcos parallax 9.12 +/- 0.34 mas. Dynamical parallax 9.1 mas,               
                       masses 6.43 and 3.68 Msun.  The orbit by Mason et al. (1999) had to be  Msn1999a
                       revised using our measures near the periastron. The high eccentricity           
                       e = 0.853 is now well established.                                      Tok2012b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 15.29 +/- 3.02, 8.37, and 4.79 Msun, respectively.            Mlk2012 
11211-3531 I  1539     Position angle uncertain. Needs speckle.                                        
11212+5807 GRV1193     SLW 589.                                                                        
11213-3447 SWR 110     CPM pair                                                                Skf2004 
                       RXJ1121.3-3447 = TWA 13. TW Hya association. Both components are                
                       weak-lined T Tauri stars; spectral types are M1 + M2.                   Stz1999 
11214-2027 STN  22     LDS 348.                                                                        
                       NLTT 27132/27131                                                        Chm2004 
11216+5111 LDS5204     LDS6243.                                                                        
11218+2208 LDS4088     NLTT 27148/27149                                                        Chm2004 
11218-1313 FME   1     Dupuy et al. (2009) derive a system mass of 0.146 +/- 0.014 Msun, and           
                       component spectral types M8 +/- 0.5 and L7 +/- 1.                       Dup2009 
                       LHS 2397a. Assuming a parallactic distance of 14.3 +/- 0.4 pc                   
                       (Monet et al. 1992), Konopacky et al. (2010) derive a system mass of    Dah1992 
                       0.144 +/- 0.013 Msun.                                                   Kon2010 
11219+0343 EPI   4     EPIC 201704541. Primary is eclipsing binary, period 0.411d.             SJR2016 
11221+3705 STF1533     B is BD+37@2177.                                                                
                       A,BC: HJL 144.                                                          HJL1986 
11221+0128 UC 2124     Also known as CBL 556.                                                  Skf2013 
11221-2447 GRE   3     Aa,Ab: IRAS 11195-2430 = PDS 54.                                        Gre1992 
           I   507     Variable TV Crt. Tokovinin (1999) gives three possible orbits which     Tok1999b
                       are consistent with visual and IR speckle observations, as well as              
                       radial velocity difference and Hipparcos parallax for stars of this             
                       type (K5V). Inclination is near 90 degrees, but eccentricity is not             
                       high, as predicted by Torres et al. (1995).                             Trr1995b
                       Star has large IR excess. A component is SB1 (P=262 days), while B              
                       component is SB2 (P=315 days).                                          Tok1999b
                       Torres et al. (1995) report radial velocity data and make some                  
                       constraints on possible astrometric orbits.                             Trr1995b
                       See also HST observations and discussion of all components of this              
                       multiple system by Soderblom et al. (1998).                             Sdb1998 
           SHY 228     AC: HIP  55505 + HIP  58029.                                                    
           BOD   1     Ba,Bb. Masses determined at 0.699+/-0.064 and 0.582+/-0.051 Msun by     Bod2005b
                       Boden et al. (2005).                                                            
11222-6119 VOU  47     Aka HRG  58.                                                                    
11224-2713 LDS 350     NLTT 27188/27182                                                        Chm2004 
11225-1028 WHC   9     J 1574.                                                                         
11225-3054 HJ 4428     Herschel's measure moved to HJ 4430 following suggestion by Dawes.      I__1927a
11225-5322 BNS   6     Hen 3-644                                                                       
11226-5134 LDS 351     B is CD-50@5949.                                                                
11230-3054 HJ 4430     Herschel's measure moved to HJ 4430 following suggestion by Dawes.      I__1927a
11231-1020 OL   12     Not found in 1939. Position may be in error                             B__1950c
11237-2831 ARG  25     B is CD-27@8061.                                                                
11238+4307 LDS4093     NLTT 27234/27231                                                        Chm2004 
11239+1032 STF1536     iot Leo = 78 Leo. Mt. Wilson spectral types F3s and F3s. A is a Delta           
                       Scuti-type variable. A small variation in the early RV's was not                
                       confirmed by fairly numerous subsequent observations. From the visual           
                       separations, Baize suggests a subsystem with P = 16 yr.                 Baz1980a
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Combined spectroscopic/astrometric solution of SB1. Calculated masses           
                       1.92 +/- 0.96 and 0.28 +/- 0.92 Msun; values are poorly constrained.    Mut2010b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.67 +/- 1.45, 2.33, and 1.38 Msun, respectively.  Mlk2012 
11239-2319 RST2746     CD-22@8867.                                                                     
11241+3808 RED  23     M4.5 star is ~7" from M8 dwarf 2MASS J11240487+3808054. Distance                
                       estimates for both ~19pc.                                               Red2007a
                       There is a possible brown dwarf companion to 2MASS J11240434+3808108            
                       at 8" separation noted by Reid et al. (2007), but it is single within   Red2007a
                       the AstraLux field of view.                                             Jnn2012 
11244+0620 HJ 2569     Position correction by Heintz.                                          Hei1983a
11245+6807 LDS1260     LDS 1731.                                                                       
11245+3529 OSO  38     G147-050. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
11246+2331 LDS5205     LDS6244.                                                                        
                       NLTT 27298/27299                                                        Chm2004 
11247-4718 WFC 113     SWR 111. CPM pair                                                       Skf2004 
11249-0205 EPI   5     EPIC 201324549. Primary is eclipsing binary candidate, period 2.519d.   SJR2016 
11249-1741 HJ  840     gam Crt = 15 Crt                                                                
11250-3200 CHR 242     Aa,Ab: The 0".1 pair CHR 242 has only 1 observation in the WDS,                 
                       unresolved with speckle. Double lines were noted by the GCS. This star          
                       remains a mystery.                                                      Tok2012a
           UC 2133     AB: CPM candidate does not pass photometry test; likely optical.        Tok2013c
11250-5236 RST9003     Previously known as RST 541a. Also known as TDS7851.                            
11252+1608 HEI 156     There is a third star at 46 deg, 25"                                    Hei1983a
11253+3512 OSO  39     G147-054. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
11254+7817 LDS 920     LDS1732.                                                                        
                       NLTT 27306/27303                                                        Chm2004 
11256+1627 HJ 4433     81 Leo.                                                                         
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           SHY 224     AC: HIP  55765 + HIP  55262.                                                    
           HJ 4433     H 5  61.                                                                MEv2010 
11257-4314 CPO 324     TDS7855.                                                                        
11258-3852 OSO  40     Neither is a common proper motion pair, based on comparison with POSS2          
                       red plates.                                                             Oso2004 
11258-4410 JNN  75     2MASS J11254754-4410267 has a relatively close (~0.55") companion that          
                       is likely physically bound, but so far there is only a single epoch of          
                       data available.                                                         Jnn2012 
11259+6519 GIC  98     LDS2600. G236-068/G236-069.                                                     
                       NLTT 27350/27352                                                        Chm2004 
11261+0114 EPI   6     EPIC 201546283. Primary is candidate planet host star; planet period            
                       6.77d, radius 5.77 Rearth, a 0.07 au.                                   Mtt2015b
11263+1839 ZUC   9     SKF  36.                                                                        
                       Primary is white dwarf PG 1123+189.                                     Zuc1992 
11264+2047 LDS4098     NLTT 27376/27375                                                        Chm2004 
11268+5923 FOX 171     Position of ADS 8161, referred to BD+60@1328.                                   
11268+0301 STF1540     83 Leo = LDS 921. B is BD+03@2503.                                              
                       Hopmann orbit rejected from Fourth Orbit Catalog                        Hop1960a
                       ("period over 4000 years")                                              Wor1983 
                       The C component (mag. 9.9, 90") is also probably physical.              Fin1970b
                       AB: HJL 145.                                                            HJL1986 
                       AB: H 4  13.                                                            MEv2010 
11268-5310 I   883     Spectrum composite; K0III+A2-3V.                                                
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.12 +/- 1.21, 5.03, and 2.88 Msun, respectively.             Mlk2012 
11270-5451 HJ 4436     B is CPD-54@4542.                                                               
11272-1221 KUI  57     kap Crt = 16 Crt                                                                
11272-1539 HU  462     1997.1231: Our reduction does not give the quadrant unambiguously.  We          
                       therefore adopt the quadrant consistent with the latest measure in the          
                       WDS.                                                                    Hor1997 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.65 +/- 0.25, 1.85, and 0.91 Msun, respectively.             Mlk2012 
11272-1604 LDS4100     AB: NLTT 27425/27430                                                    Chm2004 
11274+2042 OSO  41     G120-050. Not a common proper motion pair, based on astrometry and              
                       color                                                                   Oso2004 
11277+4618 STF1541     HJL 146.                                                                HJL1986 
11279+0251 STFA 19     tau Leo = 84 Leo. STTA110. B is BD+03@2505.                                     
                       AB: H 6  12.                                                            MEv2010 
11280-0155 STF3071     Primary is eclipsing binary of Beta Lyr -type, period 1.0143 d.         Zas2012 
11281-6125 COO 269     A is an Algol-type system, MN Cen.                                              
11282+3313 SEI 524     Neither component seen on POSS plate; may be flaws on AC Potsdam plate          
11285+0141 EPI   7     EPIC 201577035 = K2-10. Primary is planet host star; planet period              
                       19.31d, radius 3.92 Rearth, a 0.14 au.                                  Mtt2015b
11286-4240 BSO   6     A is a spectroscopic binary.                                                    
11287+6433 GIC  99     LDS2601. G236-072/G236-073.                                                     
                       NLTT 27479/27490                                                        Chm2004 
11287+3224 COU 781     TDS7880.                                                                        
11291+3920 STF1543     57 UMa. A is a spectroscopic binary.                                            
                       AB: H 3  86.                                                            MEv2010 
11291-5848 COO 125     AC: Hipparcos suspected non-single.                                             
11292-1721 H 4 112     H IV 112. S 627.                                                                
11296-2428 JC   16     HDO 129 = HDO 130.                                                              
11296-3133 BRT2987     LDS 853.                                                                        
11301+2958 STTA111     LDS 5730. B is BD+30@2164. The primary is the eclipsing pair AW UMa,            
                       P = 0.44d.                                                                      
                       NLTT 27565/27566                                                        Chm2004 
                       Pribulla & Rucinski (2006) estimate the mass of the contact pair at     Pbl2006 
                       1.933 Msun and the minimum mass of the wider component at 0.11 Msun.            
                       HJL 147.                                                                HJL1986 
11303+8102 STF1539     B is BD+81@370.                                                                 
11304-6349 SNA  24     HD 100099 is a 21.6d SB2 (Sana et al. 2011)                             Sna2011a
                       LS 2364.                                                                        
                       The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
11308+4117 STT 234     One component is SB P = 7.40 d, and the lines of all three stars                
                       appear in the spectrum. The close pair is very probably the visual              
                       primary; the ascending node is identified on that assumption.                   
11308-1046 LDS4108     GWP1596.                                                                        
11308-5849 FIN 187     Spectrum of B: F.                                                               
11309-2012 B  2280     BHA 14.                                                                         
11313+5942 STF1544     B is a spectroscopic binary.                                                    
                       STF1545.                                                                        
                       H N  70.                                                                MEv2010 
11317+1422 WSI 101     HIP 56242. Provisionally designated WSI9107.                            Hrt2008 
                       Aa,Ab: 88 Leo. Aa,Ab could be a 'ghost' binary. Only 1 speckle res.     Tok2014d
           STF1547     AB: HJL 148.                                                            HJL1986 
                       88 Leo.                                                                         
                       AB: NLTT 27657/27656                                                    Chm2004 
                       AB: H 3  51.                                                            MEv2010 
                       AB: B= LTT 13146, X-ray source                                          Tok2014d
11318-2047 TOK 222     Astrometric binary; dm 4.9 mag, period ~ 200y?                          Tok2012b
11318-5927 HJ 4445     omi 1 Cen. A semiregular variable.                                              
11319+6237 PTT  22     Also known as STI 730.                                                          
11319-3436 ZUC   1     Aa,Ab: Magnitudes in J,H,K by Konacki et al. (2007) based on 2MASS      Kon2007 
                       combined magnitudes plus their flux ratios.  They determine both                
                       components have spectral type M1.5 +/- 0.5; log (Temp) for both is              
                       3.56 +/- 0.01 K, intermediate between temperatures expected for dwarf           
                       and giant stars, thus appropriate for PMS stars. Log (Luminosity) for           
                       Aa and Ab are -0.80 +/- 0.08 and -0.84 +/- 0.08 Lsun, respectively.             
                       Aa,Ab: Schmidt et al. (2008) analyzed all available astrometry and      Sdt2008c
                       concluded TWA 5 exhibited orbital motion, refuting conjecture that              
                       companion was a background object.                                              
           LWR   2     This system has been identified as a member of the TW Hya association           
                       (Kastner et al. 1997 Science 277, 67) and is known as TWA 5. It                 
                       contains a previously known brown dwarf TWA 5B, first suggested by              
                       Lowrance et al. (1999) and later confirmed by e.g. Brandeker et al.     Lwr1999 
                       (2003). The latter also reported the presence of a close companion      Bnk2003 
                       TWA 5Ab at 54 mas from the primary, independently detected by                   
                       Macintosh et al. (2001). We detect TWA 5B in our AstraLux data, but     MBA2001 
                       not TWA 5Ab, which implies that the projected separation was probably           
                       smaller in 2010 than it was in 2000. The orbit of TWA 5Aa/Ab has been           
                       analyzed in detail by Konopacky et al. (2007). Using the orbital        Kon2007 
                       parameters that they determine, we deduce that at epoch 2010.11, the            
                       projected separation should be only about 18 mas, which is well                 
                       consistent with our non-detection of TWA 5Ab. We use the best-fit               
                       total mass of 0.71Msun for TWA 5Aa/Ab from Konopacky et al.             Jnn2012 
                       Kohler et al. (2013) derive new orbits and masses for the young triple          
                       system TWA 5. System mass for the close pair ZUC 1Aa,Ab is 0.90 +/-             
                       0.1 Msun; system mass for the AB pair is 1.1 +/- 0.1 Msun.              Koh2013 
11320-5227 HJ 4446     B is CD-51@5787.                                                                
                       SWR 112. CPM pair                                                       Skf2004 
11321-6357 HJ 4447     B is CPD-63@1914.                                                               
11322+3615 HU 1134     Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                       8.46 +/- 4.04 and 2.63 Msun, respectively.                              Mlk2012 
11323+6105 STT 235     AB. 1979.0369: This measure was incorrectly attributed to ADS 8249 in           
                       McAlister & Hendry (1982).                                              McA1982d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.05 +/- 1.10, 2.34, and 1.10 Msun, respectively.  Mlk2012 
11323-0025 TOK 142     HIP 56282. NOMAD: PM(B)=(0,500), V(B)=16.83 (??). B is physical,                
                       PM(A)=(+43,-158). A is SB without orbit, dRV= 7.4.                      Nrd2004 
                       This is a new triple system.                                            Tok2011a
11323-2916 H 3  96     H III 96.                                                                       
11323-3020 LPR   1     2MASS J11321831-3019518 + 2MASSJ 11321822-3018316. Primary TW Hydrae            
                       Association member TWA 30, companion is distant (~3400) M dwarf.                
                       Spectral types M5 and M4, distance 42 +/- 2 pc, age ~8 Myr.             Lpr2010 
11324+1212 BGH  35     HJL1064.                                                                HJL1986 
11325+5302 HJ 2574     C is a nebula, NGC 3718.                                                        
11326+2419 STF1549     HJL 149.                                                                HJL1986 
11327+0513 GIC 100     LDS 922. G010-032/G010-031.                                                     
11329+5525 A  1593     Primary is HR UMa, an Algol type eclipsing binary, P = 0.73708d.        Zas2012 
11329-3613 I  1544     A is SB, no orbit                                                       Tok2014d
11330+1319 LDS4114     NLTT 27734/27737                                                        Chm2004 
11330-2327 HDO 130     This system, originally identified as HDO 130, is apparently not the            
                       system observed by Pei1882 in 1868. That measure was later attributed           
                       to 11296-2428JC   16, as was HDO 129.                                           
11330-3151 WSI 102     Aa,Ab: Provisionally designated WSI9108.                                Tok2010 
           HJ 4449     AB: xi Hya                                                                      
11334+5948 LDS1262     NLTT 27746/27749                                                        Chm2004 
11336-4035 I    78     1997.1177: The magnitude difference is listed in the WDS as 0.0. Our            
                       reduction does not give the same quadrant as the latest measure in the          
                       WDS.                                                                    Hor1997 
11343-1531 TOK 143     HIP 56441. NOMAD: PM(B)=(-164,0), V(B)=15.71 (??).                              
                       PM(A)=(-92,+1).                                                         Tok2011a
11347+1648 STF1552     90 Leo. B is a spectroscopic binary.                                    Mlr1952a
                       AB: H 1  27.                                                            MEv2010 
11352-4722 RST 548     A is the semiregular variable V763 Cen.                                         
                       Sinachopoulos et al. (2007) noted an additional component at 131deg,    Sin2007 
                       9".2, dm 6.6mag, but felt it was probably an optical pair and not               
                       worth including as a new entry in the WDS (Gavras, private comm.).              
11354-3232 LTT 4290    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11358-6301 RST3746     lam Cen                                                                         
11360+7634 LDS1736     BVD 163.                                                                        
11360-0231 EPI   8     EPIC 201295312. Primary is candidate planet host star; planet period            
                       5.66d, radius 2.16 Rearth, a 0.06 au.                                   Mtt2015b
11362+4843 FAR  35     Primary is white dwarf WD 1133+489.                                     Far2006 
11363+2747 STF1555     A is a SB. A premature visual orbit has been computed                   Wor1956b
                       Quadrant certain in 1951 and 1953. One star is possibly variable.       Baz1954a
                       Data appear equally well fit by rectilinear solution - see catalog.             
           HJ  503     AB,C: According to Le Beau, this pair is physical.                      LBu1990c
11366+5608 STF1553     LDS1265.                                                                        
                       B is SB2, P=4.627y                                                      Tok2014d
11367+2128 STF1558     AB,C: HJL 150.                                                          HJL1986 
11368-1221 BU  456     Prieur et al. (2012) derive a dynamical parallax of 18.6 mas and                
                       (using their orbital elements and the revised Hipparcos parallax of             
                       van Leeuwen 2007 A&A 474, 653) a total mass 1.1 +/- 0.7 Msun.           Pru2012 
11370-3858 DUN 113     B is CD-38@7231.                                                                
11371+6022 LDS2604     NLTT 27985/27990                                                        Chm2004 
11371-0054 EPI   9     EPIC 201403446. Primary is candidate planet host star; planet period            
                       19.15d, radius 2.04 Rearth, a 0.14 au.                                  Mtt2015b
11373-7554 pi Cha      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11374+4728 KU   39     A is a BY Dra-type variable, and also a spectroscopic binary. A                 
                       premature visual orbit has been computed.                                       
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
11378+4150 LDS5735     LDS6246.                                                                        
                       NLTT 28037/28036                                                        Chm2004 
11378-4855 HJ 4459     B is CD-48@6669.                                                                
11378-6319 SNA  26     The primary is V1051 Cen, a detached Algol-type eclipsing binary. A             
                       known O+O SB2 (Gies et al. 2002; P~9.7d). Given the distance to the     Gie2002 
                       IC 2944 cluster, this additional component at 61mas is not the                  
                       spectroscopic companion, thus making HD 101131 a hierarchical triple.   Sna2014 
11379+5037 GC 15947    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin & Griffin (1980).                                               Grf1980d
11380-0016 BAL1160     RST 5356.                                                                       
11380-0136 LDS4125     NLTT 28053/28048                                                        Chm2004 
11383-6322 I   422     Light and radial velocity variable.                                             
                       Primary is eclipsing variable V871 Cen (period 2.0842 day).             Zas2010 
                       This is another complicated multiple system with three visual pairs at          
                       0.36", 1.7", and 9.6". The AB pair further contains an eclipsing                
                       binary (Otero 2007, Open European Journal on Variable Stars 72, 1;              
                       P=2.08d) and a spectroscopic binary with a period of 2.8d (Sana et al.  Sna2011a
                       2011). This brings the number of stars with 10" to six. It is not               
                       currently possible to determine which component of the AB pair is the           
                       eclipsing one and which is the spectroscopic one.                       Sna2014 
11384+6112 LDS2605     SLW 621.                                                                        
11384-6312 HD 101223   IC2944 Tha 49.  Additional similar radial velocities are reported by    Wes1965 
                       Thackeray & Wesselink (1965) and Humphreys (1973 A&AS 9, 85).           Msn1998a
11386+7511 MLR 425     Also known as TDS7973.                                                          
11387+4507 STF1561     AB: Secondary is 23.5d SB1; AB has estimated period of 2100y.           Tok2006 
                       AB: NLTT 28087/28086                                                    Chm2004 
                       AB: H 3  87.                                                            MEv2010 
                       AB: B is SB2, P=23.541d                                                 Tok2014d
                       AC and AE: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
11387-1312 KUI  58     AB: iot Crt = 24 Crt                                                            
           UC 2181     AC: CPM candidate does not pass photometry test; likely optical.        Tok2013c
                       AC: The C CPM component at 93" is not on the MS, too "blue".            Tok2014d
11390+0406 GRV1059     SLW 624.                                                                        
11390-0354 EPI  10     EPIC 201208431 = K2-4. Primary is planet host star; planet period               
                       10.00d, radius 2.37 Rearth, a 0.08 au.                                  Mtt2015b
11391+6630 LIE   1     HS 1136+6646 = WD 1136+667. The A component is a hot young DAO white    Lie2006 
                       dwarf plus K7V in a close detached binary. The wider companion is seen          
                       in SDSS and HST/STIS images, and is estimated to be of spectral type            
                       K4-5V. Similar proper motion of the close pair and the companion                
                       during the 3.84 years between images leads the authors to conclude the          
                       companion is probably physical.                                                 
11391+1051 BPM 581     [PM2000] 1012822 + [PM2000] 1012809.                                    Gvr2010 
11393-3021 RSS 269     IC2944 Tha 53.  Additional similar radial velocities of the primary     Wes1965 
                       are reported by Thackeray & Wesselink (1965).                           Msn1998a
11395+2518 A   678     Slightly elongated, about 263deg, 0".2?                                 Baz1972 
11395-0208 CBL 348     GWP1638.                                                                Tob2012b
11395-6524 B  1705     A spectroscopic binary.                                                         
                       GT Mus is one component of this quadruple. One component of the close           
                       visual pair is an SB, with P~61d, and also an RS CVn-type binary. The    .      
                       other is an EB with period ~2.75d.                                      Zas2009 
11396+3125 SEI 526     Primary not seen on POSS plate; may be either variable star or flaw on          
                       AC Potsdam plate.                                                               
11396+1900 STF1565     B is BD+19@2482.                                                                
                       HJL 151.                                                                HJL1986 
11396-2959 SWR 114     CPM pair                                                                Skf2004 
11398-6329 BSO   7     B is CPD-62@2205.                                                               
                       BSO   7B is the optical companion of HD 101436 (Lindroos 1985).         Lnd1985 
                       Both stars were observed and appeared to be single.                     Msn1998a
                       Additional diverse radial velocities for HD 101413 are reported by      Wes1965 
                       Thackeray & Wesselink (1965) and Conti et al. (1977).                   Cti1977 
           SNA  28     Ba,Bb: HD 101413 is a 3 to 6-month period SB2 (Sana et al. 2011), with  Sna2011a
                       the spectroscopic companion being a likely mid-B star. The 54mas                
                       companion is too far away and too bright to be associated with the              
                       spectroscopic companion.                                                Sna2014 
11399-2045 LDS4129     NLTT 28153/28155                                                        Chm2004 
11401-0326 GAU  13     Gauchet calls this HJ 186, but it seems to be another pair.             Gau1926a
11406-0824 TOK  25     A is SB1, P=4.406d                                                      Tok2014d
11406-6234 SNA  29     Aa,Ab: Given the brightness difference and the fact that the combined           
                       spectrum is an O9.2II star, both Aa And Ab are likely late O stars.     Sna2014 
11407+1745 BPM 582     [PM2000] 1013462 + [PM2000] 1013449.                                    Gvr2010 
11408-2056 LDS4134     NLTT 28216/28215                                                        Chm2004 
11410+0341 EPI  11     EPIC 201702477. Primary is candidate planet host star; planet period            
                       40.74d, radius 7.28 Rearth, a 0.22 au.                                  Mtt2015b
11410-6242 B   799     A is the Cepheid UZ Cen.                                                        
11411+3412 STT 574     61 UMa.                                                                         
11412+3920 OSO  42     G176-046. AB is a common proper motion pair                             Oso2004 
           LDS4135     AC: NLTT 28236/28208                                                    Chm2004 
11414+5855 ES 2638     LDS2609. B is BD+59@1396.                                                       
                       NLTT 28243/28242                                                        Chm2004 
                       HJL 152.                                                                HJL1986 
11416+3145 BNU   3     Aa,Ab: 62 UMa. B is BD+32@2178.                                                 
                       This system is known to have a variable radial velocity.                Bnu1986 
                       Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate               
                       astrometric data. Derived component masses are 1.31 +/- 0.16 and                
                       1.22 +/- 0.14 Msun.                                                     Ren2010 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 2.56 +/- 0.30, 2.91, and 1.25 Msun, respectively.  Mlk2012 
           STT 575     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
11417+0543 LDS5738     Aka LDS6247.                                                                    
11421-2321 MUG  14     Primary is HATS-1. Spectral type of comoving secondary estimated as             
                       M0, mass 0.67 Msun.                                                     Mug2014 
11423+2302 LDS 926     NLTT 28297/28298                                                        Chm2004 
11426+0554 EPI  12     EPIC 201828749. Primary is candidate planet host star; planet period            
                       33.52d, radius 3.83 Rearth, a 0.19 au.                                  Mtt2015b
11431-3601 I  1546     Position angles uncertain, too close. Needs speckle.                            
11432-0330 BRT 435     J 3233.                                                                         
11434+2245 POU3110     Heintz believes HJ 2581 to be identical.                                Hei1983a
11435-5800 MUG   9     Based on astrometry, photometry and H- and K-band spectroscopy,                 
                       Mugrauer et al. (2007) conclude that HD 101930 A and B comprise a       Mug2007 
                       physical pair. The projected separation is 2229 au, which means the             
                       planetary companion to the A component is well within the long-time             
                       stable region.                                                                  
11436+0634 BU  793     AB: EPIC 201862715. Primary hosts an inflated hot Jupiter (WASP-85Ab),          
                       period 1.4786d.                                                         Mtt2015b
           WSP  85     AC: del Valle & Rica (2016) find the star 2MASS J11434596+0635056,              
                       spectral type M2.5V (based on multi-band photometry), appears to have           
                       distance and proper motion similar to WASP-85, and suggest that it              
                       could be a new physical companion.                                      DVG2016c
11437+1331 HJ 2583     B is BD+14@2427.                                                                
11438+1831 BRT2412     HJL 154.                                                                HJL1986 
11441-5332 LDS 360     Typographical error in Luyten's quadrant ("sp")?                        Luy1941 
11441-0448 RST5524     Obviously in rapid motion, but the measures are insufficient to define          
                       the nature of the motion.                                                       
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.56 +/- 0.88, 2.89, and 1.25 Msun, respectively.             Mlk2012 
11443+4032 OSO  43     G122-043. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
11446-4925 RST9004     Originally published as RST3558a and previously listed in the WDS               
                       under duplicate designation RST3558.                                            
                       Assuming the revised Hipparcos parallax of 20.6 +/- 2.1 mas, Wollert            
                       et al. (2014) find the system mass is 2.6 +/- 0.8 Msun, the semi-major          
                       axis 14.9 +/- 1.6 au. Spectral types at K0 +/- 1 and K5 +/- 1. Some             
                       evidence is found for an unseen third component.                        Wol2014 
11448+1123 J  3234     HJL 155.                                                                HJL1986 
11452+1821 GIC 101     G057-017/G057-015.                                                              
11453+0816 VIG  14     Primary is xi Vir. The optical/physical nature of the faint companion           
                       is undefined.                                                           Vig2012 
11456-6644 HJ 4471     lam Mus                                                                         
           lam Mus     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11459+1122 J  1017     The measure in 1910 doubtful. No certain measures since.                        
11460+3149 GIC 102     Primary is white dwarf WD 1143+321 = NLTT 28470.                        Far2005b
                       NLTT 28470/28469                                                        Chm2004 
11460+3015 LDS4143     NLTT 28476/28472                                                        Chm2004 
11465-7055 RSS  15     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. Also known as RSS 272.                        Rss1996 
11466+2231 KER   2     Aa,Ab: RED  12. 2MASSW J1146345+223053                                          
                       HST WFPC2 observations by Reid et al. (2001). Paper includes mass and   Red2001 
                       age estimates, as well as discussion of L dwarf binary frequency and            
                       semimajor axis distribution.                                                    
           ALP  17     AB: Observed in I-band at WIYN in February 2003, but companion not              
                       detected. Ruled out as brown dwarf companion following further                  
                       IRTF/NSFCam H- and methane-band photometry in April 2004.               AlP2007 
           KER   2     Primary is an L3V brown dwarf; LRIS spectrum shows other component is           
                       a background star of much earlier type.                                 Kir1999 
11467-4029 LDS6248     Proper motion -1545 +385.                                                       
                       HIP 57443. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       A is exoplanet host, P=122d                                             Tok2014d
11475+7702 LDS1739     Primary is SB, P=33.776d                                                Tok2014d
11475+2002 SHJ 130     B is BD+20@2651.                                                                
11477+0016 LDS5207     LDS6249.                                                                        
11479+0815 CHR 134     4 Vir.                                                                          
                       Aa,Ab: This pair was observed by CHARA 17 times 1987-1998 and resolved  McA1989 
                       once (1987.26, 0.259", note: "uncertain whether real"). Later resolved  WSI2007a
                       by the USNO 26in (2006.31, 0.40").                                      Hrt2009 
           RBR   2     AD: Individual J,H,K magnitudes are calculated from 2MASS combined              
                       magnitudes and AO-derived magnitude differences                         Rbr2005 
           SHJ 131     AB: H 6 113.                                                            MEv2010 
11480+2013 STFB  7     93 Leo = LDS4146. A is a spectroscopic binary and light variable,               
                       spectrum composite; A7V+G5III-IVe. B is BD+21@2357.                             
                       AB: HJL 156.                                                            HJL1986 
                       AB: H 6  80.                                                            MEv2010 
           MKT   7     Visual orbit by Hummel et al. (1995) based on astrometry from Mark III  MkT1995 
                       interferometer. Additional spectroscopic data yield component masses,           
                       luminosities, radii, effective temperatures, and distance.                      
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1995).                                                   MkT1995 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 3.97 +/- 0.25, 4.97, and 1.66 Msun, respectively.  Mlk2012 
11480-6607 GLI 168     LDS 367.                                                                        
11484-1019 H 6 115     H VI 115. B is BD-09@3368.                                                      
11486+1417 BU  603     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Individual J,H,K magnitudes are calculated from 2MASS combined                  
                       magnitudes and AO-derived magnitude differences                         Rbr2005 
11487-6134 R  9001     Previously known as R   176a.                                                   
11489+1802 LDS5742     LDS6250.                                                                        
11491+1434 BU  604     bet Leo = 94 Leo = Denebola. Possibly variable.                                 
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
11495+1246 LDS4148     NLTT 28662/28663                                                        Chm2004 
11495-1937 LDS 368     11495-1936DAM  75AB. Other members of 11495-1936 moved to 11495-1937.           
11496+1641 BPM 583     [PM2000] 1017041 + [PM2000] 1017018.                                    Gvr2010 
11498+0557 LDS5743     LDS6251.                                                                        
11498-3816 SWR 117     CPM pair                                                                Skf2004 
11500+3612 GRV 842     HJL 157.                                                                HJL1986 
11501+5024 LDS5208     LDS6252.                                                                        
11502-4951 SWR 118     CPM pair                                                                Skf2004 
11503+3741 HJ  510     AB,C component = LDS5209.                                                       
11503+2519 LDS 928     Also known as LDS6253. It was determined that these two pairs were the          
                       same. LDS 928 was at 11504+2519. The true position is closer to that            
                       of LDS6253, but it was given the discovery designation of the earlier           
                       Luyten number.                                                                  
11504+2626 LDS 927     NLTT 28702/28701                                                        Chm2004 
11507+0146 STT 576     bet Vir = 5 Vir = Zavijava                                                      
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
11509-7411 BRR  15     Erroneously listed as BRR   5, a designation already in use.                    
11510+0707 EPI  13     EPIC 201890494. Primary is eclipsing binary candidate, period 2.536d.   SJR2016 
11510-0520 MCA  36     A spectroscopic binary and suspected occultation binary now resolved            
                       by speckle interferometry.                                                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Ginestet et al. (1985).                                                 Gin1985 
                       The pair has been resolved 3 times 1980-1994, but unresolved ~35 times  HIP1997d
                       1980-1998. Published astrometric orbits give a period of ~1.3y and an   Jnc2005 
                       inclination near 90deg.                                                 Hrt2009 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Imbert & Carquillat (2005).                                             Crq2005 
11512+3322 ARG 101     B is BD+34@2263.                                                                
11513+1255 LDS4150     NLTT 28770/28768                                                        Chm2004 
11515+5412 LDS1272     LDS1273. NLTT 28772/28771                                               Chm2004 
11518-0335 J  1581     Probably variable                                                       J__1962a
11518-0546 CHR  36     This is the variable TY Vir.                                                    
11520+0850 STF1575     B is BD+09@2552.                                                                
                       HJL 158.                                                                HJL1986 
                       SHY 581. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       H 4  49.                                                                MEv2010 
11520-0824 HJ  843     J 1580.                                                                 J__1949a
11521+0936 GWP1692     BC: Initially added to WDS incorrectly as AC.                                   
11523+3827 LDS4151     SLW 664.                                                                        
11526-0306 EPI  14     EPIC 201257461. Primary thought to be a planet host star, with planet           
                       period 50.28d, radius 209.52 Rearth, a 0.30 au. Believed to be a                
                       false positive detection, however.                                      Mtt2015b
11528+1526 SHJ 132     AB: HJL 159.                                                            HJL1986 
                       AB: H 5  60.                                                            MEv2010 
11528-0112 EPI  15     EPIC 201384232 = K2-6. Primary is planet host star; planet period               
                       30.940d, radius 2.50 Rearth, a 0.19 au.                                 Mtt2015b
11529+3050 STF1576     HJL 160.                                                                HJL1986 
                       Additional notes may be found in Schmeidler (1940).                     Scd1940a
11529-3354 HJ 4478     bet Hya. A is an Alpha CVn-type variable.                                       
11532-0722 LDS4154     NLTT 28863/28864                                                        Chm2004 
11532-1540 A  2579     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 59.26 +/- 59.23, 4.05, and 1.45 Msun, respectively.           Mlk2012 
11533+8311 LDS1743     B is BD+83@342.                                                                 
11534-2434 HJ 4479     LDS1274.                                                                        
11535+0552 EPI  16     EPIC 201826968. Primary is eclipsing binary candidate, period 0.367d.   SJR2016 
11537+7345 BU  794     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.31 +/- 1.25, 2.52, and 1.10 Msun, respectively.  Mlk2012 
11537+5032 JMS   3     2MASS J11533966+5032092 + 2MASS J11535018+5035593.                      Jms2008 
11538+5342 SHY 227     AB: HIP  58001 + HIP  61100. A component = gam UMa = Phecda.                    
                       B component = GJ 1160 = A component of 12313+5507.                              
11541+7155 A    75     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.98 +/- 0.64, 2.60, and 1.25 Msun, respectively.             Mlk2012 
11545+2154 UC 2230     CE: Not a CPM pair. The proper motion of the E component was incorrect          
                       (Skiff, private comm.)                                                          
11545+1925 STTA112     LDS 929. B is BD+20@2659.                                                       
                       NLTT 28915/28923                                                        Chm2004 
                       AB: HJL 161.                                                            HJL1986 
                       AB: SHY 229. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
11547-6622 SHY 230     HIP  58085 + HIP  58121.                                                        
11550-6235 BSO  20     B is CPD-61@2779.                                                               
11551+4629 A  1777     65 UMa. The primary is the eclipsing binary DN UMa,                             
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Discrepant 1995.3159 speckle measure found not due to a typographical   Hrt1997 
                       error in theta, following reexamination of original data by authors.            
                       Presumably there was an identification error while pointing telescope,          
                       although no probable match to known close pairs in the vicinity has             
                       been found.                                                                     
           65 UMa      After subtracting out the effects of the 118y AB pair, Zasche et al.            
                       (2012) find a 640d variation, which they attribute to a closer Aa,Ab            
                       pair. The 1.7d eclipsing pair DN UMa, then, is assumed to be Aa1,Aa2.           
                       Their analysis determines a distance 234 +/- 29 pc to the system                
                       (compared with 212 +/- 30 pc from the revised Hipparcos reduction of            
                       van Leeuwen 2007), a and total mass of 8.25 +/- 1.85 Msun. Derived      vlF2007 
                       spectral types, masses, and radii of the components are as follows:             
                           Aa1   A7   1.74 +/- 0.06 Msun   1.86 +/- 0.08 Rsun                          
                           Aa2   A7   1.71     0.06        1.81     0.08                               
                           Ab    A1   2.4      0.4                                                     
                           B          2.4      2.0                                             Zas2012b
           STF1579     STTA113 = STFA 20.                                                              
                       AB,C: H 1  72.                                                          MEv2010 
                       May be a physical septuple: the 1.7d eclipsing pair (2), the 640d               
                       spectroscopic component (+1), the 118y resolved pair A  1777 (+1)               
                       and the wider cpm pair (+1) STF1579AB,D. STF1579AB,C also has similar           
                       proper motion and may be physical and the D component has been split            
                       interferometrically (BAG  46Da,Dd).                                             
11551+0313 HD103501    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
11555+7229 MLR 426     Duplicity uncertain.                                                            
11557+1539 H 6  13     H VI 13. 95 Leo. All stars in the field are much more than 90" away.            
                       A is a spectroscopic binary.                                                    
11558+1115 AG  434     No companion seen in 1893 and 1903.                                     IDS1963A
11560+3520 CHR 258     Hipparcos suspected non-single.                                                 
                       Triple system. Spectroscopic orbits of the inner (23-d) and this        Grf2013f
                       more distant 4988-d pair have been determined. Remarkably close to              
                       the initial 15y estimate.                                               Msn1999b
11560+2159 STF1582     HJL 162.                                                                HJL1986 
11560-7701 TOK 145     HIP 58180. A X-ray source RX J1156.0-7700 with small PM(A)=(-45,+1).            
                       B at 13.4" is physical based on CMDs, but the field is crowded, N*=79.  Tok2011a
11561+4533 STF1581     A is a RR Lyrae-type variable. B also variable?                                 
                       Magnitude underestimated in ADS                                         Baz1943b
11563-4546 LDS 373     B is CD-45@7400.                                                                
                       SWR 119. CPM pair                                                       Skf2004 
11566-0437 STF1584     B is BD-03@3206.                                                                
11567-3216 DUN 116     AB = LDS 374. B is CD-31@9364.                                                  
                       AB = SWR 120. CPM pair                                                  Skf2004 
                       HIP 58240. B = HIP 58241. AB is known CPM pair DUN 116 at 19", 82deg.           
                       BC is a new close pair: 3.6" 116deg, dK=5.8, status unknown.            Tok2011a
11568+0521 CHR 220     First detected as an occultation binary by Evans et al.                 Evn1985 
11572+1351 BPM 584     [PM2000] 1020171 + [PM2000] 1020215.                                    Gvr2010 
11572-7922 HUE   3     Aa,Ab:  The primary is T Cha, a weak-lined T Tauri star (spectral type          
                       G8) surrounded by a cold disk. At a distance of 108 +/- 9pc, the                
                       companion detected by Huelamo et al. (2011) is located 6.7 +/- 1.0 au           
                       from the primary, well within the gap in that star's disk.              Hue2011 
           KST   1     AE: Based on optical and X-ray spectroscopy, Kastner et al. conclude            
                       2MASS J11550485-7919108 is a likely CPM companion to the pre-MS                 
                       star/disk system T Cha, with spectral type M3.                          Kst2012 
11578+4518 A  1778     A may be variable.                                                              
11578-7121 HJ 4483     SWR 122. CPM pair                                                       Skf2004 
11580+6520 LDS2620     NLTT 29095/29094                                                        Chm2004 
11581-2930 LDS 375     NLTT 29109/29108                                                        Chm2004 
11582-1045 J  2084     RST 3765. BRT.                                                                  
11582-1120 LDS4162     GWP1719.                                                                        
11583+3338 LDS5210     LDS6254.                                                                        
11585+3811 LDS5211     LDS6255.                                                                        
11585-4155 LDS6256     HIP 58401. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
11589-2555 I   510     Too close. Duplicity doubtful, and/or rapid motion. Needs speckle.              
11594-4219 HJ 4485     A is CPD-41@5660. B is CPD-41@5659.                                             
11596-7813 HJ 4486     eps Cha                                                                         
11598-0315 CBL 365     GWP1724.                                                                Tob2012b
11599+1144 BPM 585     [PM2000] 1021250 + [PM2000] 1021230.                                    Gvr2010