10000+2433 CHR 145     The primary is DH Leo, a RS CVn system, and spectroscopic binary with           
                       a period of 1.07d (Barden, AJ 89, 683, 1984). Barden observed three K           
                       stars in his spectra of this system. Fekel (1989, private comm.) has            
                       observed the third component of this system and finds no velocity               
                       changes in excess of +/- 2 km/sec from 12 spectra obtained since 1984.          
                       This new speckle component is thought to be this third spectroscopic            
                       component.                                                              McA1990 
10001-1521 GWP1267     ABL 271.                                                                Tob2012b
10002+0615 STF1401     HJL 118.                                                                HJL1986 
10004-0154 GWP1268     ABL 268.                                                                Tob2012b
10005-0250 GWP1269     ABL 269.                                                                Tob2012b
10007+3219 OSO  30     G118-030. Neither AD or AE is a common proper motion pair               Oso2004 
                       Proper motion of A = -1010,-661 (UCAC2).                                        
10010+3155 RAG   7     GJ 376. Raghavan et al. (2010) consider B as possible eclipsing binary  Rag2010 
                       based on Gizis et al. (2000)                                            Giz2000 
10010-0651 GWP1270     ABL 270.                                                                Tob2012b
10011-4154 CPO 279     CPD-41@4230.                                                                    
10012-2309 RSS 221     CD-22@7830                                                                      
10012-5606 HDO 209     B is CPD-55@2795.                                                               
10013+3252 OSO  31     G117-063. Not a common proper motion pair, based on astrometry and              
                       color                                                                   Oso2004 
10015+1807 BPM 567     [PM2000]  965525 + [PM2000]  965511.                                    Gvr2010 
10016+5424 STI2239     MLB 125.                                                                        
10017+1725 RUC   7     Elements from Hipparcos Intermediate Astrometric Data are combined              
                       with a light-travel time analysis of eclipse timings by Bakis et al.    Bks2005 
                       XY Leo. Spectral type of resolved companion estimated at K6V.           Ruc2007 
                       Multiple system including contact binary XY Leo. Pribulla & Rucinski            
                       (2006) estimate the mass of the contact pair at 1.378 Msun and the      Pbl2006 
                       minimum mass of the wider component at 1.00 Msun.                               
10019+1354 BPM 568     [PM2000]  965775 + [PM2000]  965789.                                    Gvr2010 
10019-0045 GWP1272     ABL 272.                                                                Tob2012b
10019-1438 GWP1271     ABL 273.                                                                Tob2012b
10019-2841 HJ 4277     B is CD-28@7839.                                                                
10021-5459 DUN  83     B is CPD-54@3041.                                                               
10022-1946 B   781     Primary is the eclipsing binary OZ Hya, P = 2.04876 day.                Zas2010 
10024-3547 BRT1656     TDS6979.                                                                        
10025+1703 RUC  22     Primary is XZ Leo.                                                              
10025-2814 JNN  71     2MASS J10023100-2814280 has a relatively close (~0.56") companion               
                       which is probably real, although this has yet to be confirmed with a            
                       proper motion test.                                                     Jnn2012 
10027+1635 BPM 569     [PM2000]  966270 + [PM2000]  966274.                                    Gvr2010 
10028+1756 BPM 570     [PM2000]  966320 + [PM2000]  966383.                                    Gvr2010 
10028-0134 GWP1273     ABL 275.                                                                Tob2012b
10028-1248 GWP1274     ABL 279.                                                                Tob2012b
10029+6847 STF1400     Very similar in characteristics to STF 1398. Observers have confused            
                       them.                                                                           
           ODE   7     AC: C is found in 2MASS, matching color, physical?                      Tok2014d
10030+0207 GRV1042     SLW 427.                                                                        
10031-1837 GWP1276     ABL 281.                                                                Tob2012b
10032-0557 GWP1278     ABL 276.                                                                Tob2012b
10032-0658 GWP1277     ABL 277.                                                                Tob2012b
10032-1420 GWP1279     ABL 280.                                                                Tob2012b
10032-5203 HJ 4282     B is CD-51@4435.                                                                
10034+5732 A  1347     The scattered measures show evidence of rapid motion.                           
10034+0203 HJ 1174     BAL 1866.                                                                       
10036-0852 GWP1280     ABL 278.                                                                Tob2012b
10036-2903 TOK 131     HIP 49285.                                                              Tok2011a
10039+0150 HJ 3320     BAL 1867.                                                                       
10040-1806 SHJ 110     AC: H N  25.                                                            MEv2010 
10041-7604 HJ 4288     B IS CPD-75@634.                                                                
10042-0426 GWP1284     ABL 282.                                                                Tob2012b
10043-0142 STF1404     HJL 119.                                                                HJL1986 
10043-0458 GWP1285     ABL 283.                                                                Tob2012b
10043-2823 I   292     A premature orbit has been computed.                                            
10044+5023 REB   1     G196-003. Spectral types are M2.5 +/- 0.5 and L, masses 0.40 +/- 0.05           
                       Msun and 25 +25/-10 Mjup, respectively.                                 Reb1998 
                       Jameson et al.(2008) confirm the CPM nature of this pair.               Jms2008 
10044+3611 GRV1183     SLW 429.                                                                        
10045-5840 MIF   1     MWC 198 = V640 Car. Primary is a B2e star with a complex circumstellar          
                       environment. Millour et al. (2009) resolve a close companion, and               
                       estimate the orbital period as 20-50y; polarisation suggests a high             
                       inclination, and there is also evidence suggesting high eccentricity.   MiF2009 
10046-3335 SEF   2     LHS 5166 + 2MASS J10043929-3335189. Distance to system 19.0 +/- 3.0pc,          
                       mass of L4 companion 0.070 +0.005/-0.015 Msun.                          Sef2005b
10050-5119 HU 1594     1995.1024: Quadrant determined by speckle imaging analysis.             Hor1996 
10056+3105 STF1406     STT 211.                                                                        
10056-8405 HJ 4310     AB + TOK 396Aa,Ab: HIP 49442 = HD 88948 is a nearby dwarf in the 3".9           
                       visual binary HJ 4310 AB. According to GCS, the RV of the main                  
                       component A varies by 3.5km/s. Here it is resolved into a 0".18 Aa,Ab           
                       pair with an estimated orbital period of 25yr. No astrometric                   
                       acceleration was detected, however. The visual secondary B was                  
                       targeted separately and found unresolved.                               Tok2015c
                       AB: A is SB, no orbit.                                                  Tok2014d
10062+4105 TOK 535     A comp is SB2, P=2073d                                                  Tok2014d
10062-3514 SWR  83     CPM pair                                                                Skf2004 
10063-0626 GWP1289     ABL 286.                                                                Tob2012b
10063-1735 GWP1288     ABL 287.                                                                Tob2012b
10064-0046 GWP1290     ABL 284.                                                                Tob2012b
10066-0519 GWP1293     ABL 285.                                                                Tob2012b
10066-1919 TOK  66     Ba,Bb: Estimated masses 0.92 and 0.26 Msun; sep 12.6 au, period 40 y.   Tok2010c
10066-1926 GWP1292     ABL 288.                                                                Tob2012b
10067+1754 HDS1457     The primary is a bright G-type star, mass 1.12 +/- 0.09 Msun, radius            
                       1.55 +/- 0.02 Rsun, Teff 5770 +/- 80K. Hipparcos gives a parallax of            
                       13.59 +/- 1.58 mas (73.58 +/- 9.68pc). Ma et al. (2016) resolve two     MaB2016 
                       close companions, in addition to the HDS companion, and determine some          
                       orbital elements for all three pairs. The Ab companion is likely a              
                       giant planet or brown dwarf, depending on the inclination angle;                
                       mimimum mass is 12.4 +/- 0.7 Mjup. The Ac companion is likely a brown           
                       dwarf; minimum mass 57.7 +/- 3.7 Mjup. The closest companion appears            
                       to be new, so is given the designation MAB 2Aa,Ab. The Ac component             
                       has a separation similar to the unconfirmed companion measured by               
                       Balega et al. (2006) in 2001, so the BAG 23 designation is retained,    Bag2006b
                       although the component pair is changed to Aa,Ac to match that of Ma.            
10067-1234 GWP1294     ABL 292.                                                                Tob2012b
10067-7045 NZO  15     Not found by Heintz at IDS position. The spectral type of -70@964 is    Hei1987a
                       K1/2III/IV.                                                                     
10068+0537 CHR  30     14 Sex.                                                                         
10069+3539 BRT2593     ALI 358.                                                                        
10070-4026 KTK   1     Central star of the planetary nebula NGC 3132.                                  
10070-7129 TOK 397     HIP 49546 is an astrometric binary of 1.5yr period (Goldin & Makarov            
                       2006) with variable RV. The period corresponds to a semi-major axis of  Gln2006 
                       25mas. The star is resolved here tentatively at 26mas. This resolution          
                       is below the diffraction limit and needs confirmation. The measured             
                       position angle of 346deg is close to 342deg predicted by the                    
                       astrometric orbit.                                                      Tok2015c
10071-1119 GWP1295     ABL 291.                                                                Tob2012b
10072-2220 RST3679     CPD-21@4616.                                                                    
10073+1646 WRH  18     eta Leo = 30 Leo. Occultation binary now confirmed by speckle.                  
                       Additional notes may be found in Wilson (1941).                         WRH1941b
10075-3325 SWR  84     CPM pair                                                                Skf2004 
10075-5904 COO  97     B is CPD-58@1922.                                                               
10077-0644 GWP1297     ABL 289.                                                                Tob2012b
10077-0905 RST3681     TDS7042.                                                                        
10077-0916 GWP1298     ABL 290.                                                                Tob2012b
10078+0715 HEI 755     Also known as TDS7045.                                                          
10079+1000 GAN   5     31 Leo.                                                                         
10079-1610 GWP1299     ABL 293.                                                                Tob2012b
10081-6405 RST 471     Aka HRG  48.                                                                    
10083+3136 KUI  48     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.77 +/- 0.22, 2.92, and 1.25 Msun, respectively.  Mlk2012 
                       AB Visual orbit, P=17.765y (Hartkopf et al. 1996). SB period 8.882yr    Hrt1996a
                       (Tremko et al. 2010 CoSka 40, 83)                                       Tok2014d
10084+6620 LDS1235     Primary is NLTT 23425. According to the LSPM, the secondary is                  
                       NLTT 23425; however, no object is visible on Aladin images at its               
                       purported position.                                                             
10084+1158 STFB  6     alp Leo = 32 Leo = Regulus.  LDS 913.                                           
                       AB: H 6  11.                                                            MEv2010 
10084-1945 BU  911     HIP 49668. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB  CfA: A=SB?                                                          Tok2014d
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
10085+6826 ENG  41     B is BD+69@557.                                                                 
10085+1712 BPMA 39     [PM2000]  969450 + [PM2000]  969537.                                    Gvr2010 
10086-0014 GWP1300     ABL 294.                                                                Tob2012b
10086-7500 SWR  86     Late-K/M giants, not G8 dwarfs. CPM pair                                Skf2004 
10087-0951 GWP1301     ABL 296.                                                                Tob2012b
10087-6549 HJ 4292     B IS CPD-65@1250.                                                               
10088+1401 BPMA 40     [PM2000]  969633 + [PM2000]  969471.                                    Gvr2010 
10090-0741 GWP1302     ABL 295.                                                                Tob2012b
10091-3448 HJ 4287     SWR  85.                                                                        
10092+3320 GRV 812     HJL 120.                                                                HJL1986 
10093+2020 A  2145     Composite spectrum binary, classified G2III+A2V by Markowitz                    
                       (1969 Dissertation, Ohio State Univ.), who quotes delta m = 1.1.                
                       It is not known which spectrum belongs to the visual primary.                   
                       Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                       second orbit of Baize (1957).                                           Baz1957a
                       1983.9371, 1983.9372: Interferometric observations are in disaccord     Wor1983 
                       with the 1957 orbital elements of Baize (see Worley & Heintz 1983).     Bnu1984 
                       1984.1861, 1984.2814, 1985.2053: The speckle interferometric                    
                       observations show that Finsen's orbit fails to describe the orbital     Fin1977a
                       motion of this system.                                                  Bnu1986 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 13.28 +/- 8.31, 6.98, and 3.29 Msun, respectively.            Mlk2012 
10095-6841 I    13     AB. 1997.1230: Our reduction does not give the quadrant unambiguously.          
                       We therefore adopt the quadrant consistent with the latest measure in           
                       the WDS.                                                                Hor1997 
10098-0502 GWP1304     ABL 297.                                                                Tob2012b
10098-6001 TDS7075     JAW  13.                                                                        
10099+5420 MLB 126     STI2243.                                                                        
10100+1623 A  2367     AB: HJL 122.                                                            HJL1986 
10100-1901 GWP1305     ABL 298.                                                                Tob2012b
10101-0157 HJ  153     ID uncertain, but appears to be most likely system in region                    
10102-6505 BRT1983     TDS7077.                                                                        
10103+3825 HDS1465     Only one HIP measure, presumably wrong. Component B in 2MASS at                 
                       343.7d, 11.33", likely physical.                                        Tok2014d
10106-1221 BU  593     lam Hya = 41 Hya. A is a spectroscopic binary.                                  
10106-1222 lam Hya     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Jones (1928).                                                           Jon1928f
10110+7508 KUI  47     Not resolved in images.                                                 Oso2004 
                       Poorly determined (long) period, only periastron-part covered.                  
10110-4814 BRT 775     CPD-47@3979.                                                                    
10111-1031 GWP1308     ABL 301.                                                                Tob2012b
10112+7622 HJ 3319     LDS1708.                                                                        
                       HJL 121.                                                                HJL1986 
10113+1001 BU 1425     Early component confusion. The 73" pair was apparently initially                
                       designated AB, but a note in the BDS indicated the pair "is not         Bu_1906 
                       BD+10 2119, but smaller stars 47s f 31 Leo". The pair was redesignated          
                       FG, and as a result the system has no AB pair. The E and F components           
                       are separated by ~34'.                                                          
10113-1949 GWP1309     ABL 302.                                                                Tob2012b
10114+4927 ENG  42     AB: Proper motion of A -1353 -501. Slightly variable.                           
                       Proper motion of B -008-012.                                                    
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           BUP 130     BC: C is BD+50@1723. Proper motion of C is +013-021.                            
10114-0642 GWP1310     ABL 300.                                                                Tob2012b
10114-7428 TOK 132     HIP 49913.                                                              Tok2011a
10116+1321 HU  874     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.39 +/- 0.53, 2.82, and 1.17 Msun, respectively.             Mlk2012 
10116-0447 GWP1311     ABL 299.                                                                Tob2012b
10120+2007 HJ  476     STT 212.                                                                        
10120-0612 HO   44     Motion in a highly-inclined orbit.                                              
10120-2836 B   194     Although Hartkopf et al. (1993) predicted a time of periastron          Hrt1993 
                       around 1989.3, we find the time of periastron to be 2006.2. The                 
                       discrepancy may be explained by three measures not published at the             
                       time of the 1993 paper.                                                 USN2002 
                       1990.3407: Periastron passage apparently occurred about the time of or          
                       shortly before our first speckle observation in 1989.3.                 McA1990 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.43 +/- 0.86, 4.91, and 2.19 Msun, respectively.             Mlk2012 
10121+2118 A  2146     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 11.22 +/- 10.32, 3.02, and 1.10 Msun, respectively.           Mlk2012 
10122-4847 I  1196     Hipparcos suspected non-single.                                                 
10126-3225 LDS 297     LDS5708.                                                                        
10132-0848 LDS 296     NLTT 23709/23710. UC 1896.                                              Chm2004 
10134-1847 LDS3965     NLTT 23731/23733                                                        Chm2004 
10134-5054 HJ 4299     B is CD-50@4922.                                                                
10137-0723 TOK 133     HIP 50100. A is X-ray source 1RXS J101344.5-072301.                     Tok2011a
10140-1429 GWP1314     ABL 307.                                                                Tob2012b
10141-0401 GWP1316     ABL 304.                                                                Tob2012b
10142-0920 GWP1318     ABL 305.                                                                Tob2012b
10142-1615 GWP1317     ABL 308.                                                                Tob2012b
10142-7636 KOH  88     Due to an error in transcribing data from Kohler's paper, a measure of  Koh2001 
                       RST1521 was inadvertently attributed to this system and assigned the            
                       AB component designation, with this pair listed as the Aa,Ab pair.              
10143+2104 BWL  25     Makarov & Kaplan (2005) and Frankoswki et al. (2007 A&A 464, 377)       Mkr2005 
                       found evidence for a close astrometric companion based on differences           
                       between Hipparcos and Tycho-2 proper motions. Two epochs at Keck in             
                       Mar 2011 and Feb 2013 show substantial orbital motion. The system was           
                       unresolved by Subaru in Dec 2011, suggesting the secondary had moved            
                       too close to the primary to be resolved. System is a probable member            
                       of the Carina young moving group, with an age ~30 Myr. Primary is               
                       GJ 2079 = DK Leo.                                                       Bwl2015 
10143-5712 HLN  14     Also known as TDS7133.                                                          
10146-0147 GWP1324     ABL 303.                                                                Tob2012b
10149-0059 GWP1325     ABL 309.                                                                Tob2012b
10149-1328 GWP1327     ABL 313.                                                                Tob2012b
10151-6717 CPO  48     C is probably CPD-66@1208.                                                      
10152+0134 BAL1872     BD +02 2309a.                                                                   
10157-3317 HJ 4300     SWR  87. CPM pair                                                       Skf2004 
10157-5115 HD  89137   The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
10158-0541 GWP1330     ABL 310.                                                                Tob2012b
10159-0613 GWP1332     ABL 311.                                                                Tob2012b
10160-0816 GWP1334     ABL 312.                                                                Tob2012b
10161-2837 TOK 199     This is marked as an SB2 in the GCS, while Latham (2012, private                
                       communication) derived an orbital period of 916d, now independently             
                       confirmed by our orbit.                                                 Tok2015c
10161-5954 HU 1597     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.77 +/- 0.39, 3.33, and 1.82 Msun, respectively.             Mlk2012 
10163-2859 I   851     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.34 +/- 1.03, 3.12, and 1.30 Msun, respectively.             Mlk2012 
10165-0521 WSI 115     Aka FAR  10. Primary is white dwarf WD 1013-050.                        Far2005b
           FAR  10     AC: In this previously known system, 2MASS J10162867-0520320 is a               
                       spectroscopic binary of two M dwarf components, which is in turn a              
                       visual companion at 3.2" separation from a white dwarf (WD).                    
                       Furthermore, the WD is itself a spectral binary, making the system              
                       quadruple, with a demonstrated physical companionship of all four               
                       components (Vennes et al. 1999 ApJ 523, 386). The 3.2" pairing is               
                       easily distinguished in the AstraLux image, but the spectroscopic               
                       pairs remain unresolved. Because the system must primordially have had          
                       a pre-WD primary much more massive than J10162867-0520320 (given that           
                       the main sequence lifetime of an M0 star is longer than the Hubble              
                       time), we do not count it as an M-star binary for any of our                    
                       statistical purposes. The binary is listed as having confirmed proper           
                       motion in Table 4, this is based on the result in Vennes et al. and             
                       not our comparison with the astrometric point in the literature; since          
                       no error bars are listed for that point and since we only get rather            
                       marginally significant results if we assume reasonable errors of 0.1"           
                       and 1deg, we do not draw any new conclusions on the basis of such a             
                       comparison.                                                             Jnn2012 
10166+4117 SHY 552     HIP  50325 + HIP  50327.                                                        
10167+5737 HJ 1176     AB: HJL 123.                                                            HJL1986 
10167+2325 STFA 18     zet Leo = 36 Leo = Adhafera. A spectroscopic binary.                            
                       B is BD+24@2207.                                                                
10169+2552 BUP 131     B is BD+26@2062.                                                                
10171+1309 JMS   2     2MASS J10170754+1308398 + 2MASS J10171515+1307419.                      Jms2008 
10171-4241 SWR  88     CPM pair                                                                Skf2004 
10171-6120 B  1673     Variable, V337 Car.                                                             
10172+2306 STT 523     39 Leo. Mt. Wilson spectral types are F1s and dM1.                              
10173-1140 GWP1337     ABL 314.                                                                Tob2012b
10174-5354 CVN  16     TWA 22. Chauvin et al. (2009) derive spectral types M6 +/- 1 for both   Cvn2009 
                       components. The semimajor axis was calculated from their value for a            
                       (1.77 +/- 0.04au) and distance of 17.5pc. Effective temperatures are            
                       2900 +/- 200 and 2900 +200/-100 K. The system mass is 220 +/- 21 Mjup.          
10176+2155 LDS3973     NLTT 23914/23917                                                        Chm2004 
10178+7104 STF1415     AC: HJL 124.                                                            HJL1986 
                       AB: H N 145.                                                            MEv2010 
10180+0721 FAR  11     AC: Primary is white dwarf WD 1015+076.                                 Far2005b
10182-5049 HU 1598     V340 Vel, Algol (EA) type eclipsing binary, P = 3.55953 d.              Zas2011 
10183-0326 RST4454     Two orbit solutions by Heintz (1997); neither clearly preferable.       Hei1997 
10183-1321 J  2900     BRT 2723.                                                                       
10183-2029 LDS3975     The star is single in the AstraLux images, but has a known wide                 
                       companion at 32" separation (WDS).                                      Jnn2012 
10185-1811 GWP1338     ABL 316.                                                                Tob2012b
10186-3546 UC 1910     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                       Primary is X-ray source, PMS star; also SB2, P=11.410d. Not PMS, just           
                       fast rotator?                                                           Tok2014d
10187-1823 GWP1339     ABL 317.                                                                Tob2012b
10189+4403 ENG  43     B is BD+44@1975.                                                                
10190+1613 BPM 571     [PM2000]  975130 + [PM2000]  975121.                                    Gvr2010 
10191-6441 HJ 4306     1997.0902: The magnitude difference of the system is listed in the WDS          
                       as 0.1.  Our reduction does not give the same quadrant as the latest            
                       measure in the WDS.                                                     Hor1997 
10192-0502 GWP1341     ABL 318.                                                                Tob2012b
10193-0724 GWP1343     ABL 319.                                                                Tob2012b
10196+1952 Ci 20,574   = GJ 388 = AD Leo                                                               
                       Reuyl (1943) orbit rejected from Fourth Orbit Catalog                   Reu1943 
                       ("not confirmed by subsequent observations")                            Wor1983 
10196-5724 FIN 162     A is the Algol-type system HP Car.                                              
10197+1928 WNO  53     GJ 9324 + NLTT 23781. CPM pair.                                         Mkr2008 
                       B = NLTT 23781. Co-moving, not binary.                                  Tok2014d
10198-3036 RST2685     Corrected position and Durchmusterung number                            Hei1987a
10199+1217 FAR  12     Primary is white dwarf WD 1017+125.                                     Far2005b
10200+1950 STF1424     A: gam Leo = 41 Leo = Algieba                                                   
                       Star C is flare star AD Leo = BD +20 2465, 5' distant, and not          Bag1984b
                       related to the pair AB. This companion has been detected only at                
                       7500 Angstroms, and is expected to have a very low mass.                        
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       D is BD+20@2464.                                                                
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           BAG  32     Ca,Cb. 1981.2446: Flare star (M4.5Ve) known as having an unseen                 
                       companion of P ~ 27 yr (Reuyl 1943). Companion has been detected only   Reu1943 
                       at 750 nm.  The companion is expected to have a very low mass.          Bag1984b
           STF1424     AB: H 1  28.                                                            MEv2010 
10201-0327 GWP1346     ABL 320.                                                                Tob2012b
10201-6135 HOA   1     GO Car.                                                                 Plt1934 
10204+6808 HJ 3324     Same as STF1418.                                                                
10205+0626 STF1426     AB,C: H 2  43.                                                          MEv2010 
10206-1128 GWP1349     ABL 321.                                                                Tob2012b
10206-7109 GLI 293     Also known as HDS1486. #144 in the original list of Gilliss.                    
10208-6732 HJ 4314     B is CPD-66@1232, spectrum B9/A0IV/V.                                           
10209-0641 OSO  32     G055-014. Neither is a common proper motion pair, based on astrometry           
                       and color                                                               Oso2004 
10209-1911 GWP1350     ABL 322.                                                                Tob2012b
10209-5603 RMK  13     A has a variable spectrum.                                                      
10210-2844 RSS 233     HIP 50681. No V-band photometry in the WDS.                             Tok2011a
10212-0304 BUG  10     SDSS J102109.69-030420.1                                                        
                       Estimated spectral types are T1 + T5, effective temperatures 1260 +/-           
                       210 and 1130 +/- 190 K.  Masses are estimated at 0.025-0.076 and                
                       0.021-0.074 Msun, and the orbital period (assuming the semi-major axis          
                       = 1.26 * rho) is ~50yr.                                                 Bug2006a
10213+7846 RAS  24     Peculiar SrCuEu star DI Dra.                                            Ras2014 
10215+7647 LDS1711     NLTT 24011/23991                                                        Chm2004 
10215-1621 LDS3984     NLTT 24117/24116                                                        Chm2004 
10217-0946 BU   25     A=SB1. CfA: prelim. orb. P=3056d=8.37y?                                 Tok2014d
10217-6920 RSS  13     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
10218+3555 LDS1240     NLTT 24113/24114                                                        Chm2004 
10218-0023 GWP1352     ABL 323.                                                                Tob2012b
10218-4430 LDS6232     B is CD-43@6191.                                                                
10219+3704 BFR   5     LSPM J1021+3704 + 2MASS J10215386+3704166. Baron et al. (2015)                  
                       estimate spectral types M4.0 +/- 0.5 and L0 +/- 1, distances                    
                       88 +39/-25 and 93 +13/-36 pc, masses 0.207-0.272 and 0.071-0.076 Msun.  BFr2015 
10221+1226 BU 1321     HU 876.                                                                         
10222+4114 WIL   2     Using data from 2MASS, Wilson et al. (2001) conclude AB is probably a   Wil2001 
           MUG   7     physical pair, based on proximity and magnitude (time baseline is               
                       insufficient to confirm). They derive spectral type of L0V and mass             
                       77-80 Mjup for the B component. Mugrauer et al. (2004) conclude that    Mug2004c
                       components C,D,E,F,G (their stars 1-5) are background stars, with E,            
                       F, and G (stars 3,4,5) showing a constant separation. The B component           
                       (star 6) shows common proper motion with planet host star HD 89744,             
                       confirming the Wilson et al. discovery.  The mass of B is estimated at          
                       about 0.074-0.080 Msun, making it either a heavy brown dwarf or very            
                       low-mass stellar companion. Additional information was compiled from            
                       the 2MASS catalog to supplement that in these two papers.                       
           GJ 9326     Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from Korzennik    CPS2000a
                       et al. (2000).                                                          HaI2001 
           WIL   2     No comoving objects found within separation/magnitude range listed.             
                       However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                       background object.                                                              
                       AB: Primary is exoplanet host, P=256d. Chauvin et al. (2006) detect     Cvn2006 
                       only optical companions at VLT with coronagraphic mask. Roell et al.            
                       (2012 A&A 542, A92) list the companion B at 62" as physical.            Tok2014d
           RBR  17     2002.0166: PA is measured in zenith mode. If data collected in                  
                       equatorial mode, PA =  53.6. Confirmation of the pair should establish          
                       the correct theta value.                                                Rbr2011d
10223+4130 mu UMa      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Jackson et al. (1957).                                                  JES1957 
10223-1032 BD-09 3055  SB1. Curvature seen in proper motion components from Hipparcos data,            
                       although period was unknown. Combined spectroscopic/astrometric                 
                       solution, based on echelle spectra and Hipparcos intermediate                   
                       data (abscissa residuals).  Torres derives a parallax of 19.5 +/-       Trr2006a
                       1.8 mas (compared to Hipparcos value of 29.4 +/- 2.7 mas). An                   
                       estimated primary mass of 0.73 +/- 0.05 Msunyield a mass of 0.88 +/-            
                       0.05 Msun for the secondary.                                                    
           TOK 398     HIP 50796 is a single-lined and astrometric binary according to                 
                       (Torres 2006), with period 570.98d (1.56yr), K1=20.76 km/s, e=0.611.    Trr2006 
                       The Hipparcos parallax corrected for binary motion is 20.6+/-1.9mas.            
                       The spectroscopic secondary companion is over-massive, most likely a            
                       close pair of M-dwarfs. If so, the new speckle companion at 1".66 with          
                       a period on the order of 500yr makes the system quadruple. The speckle          
                       companion might contribute to the IR excess found by Torres. The                
                       system is an X-ray source, and is possibly young.                       Tok2015c
10223-5945 HD  90087   LS 1518.                                                                        
                       The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
10224+1209 GIC  92     G043-045/G043-043.                                                              
                       NLTT 24159/24144                                                        Chm2004 
10224-2933 GC 14246    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10227+1521 STT 216     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
10228-1427 GWP1355     ABL 326.                                                                Tob2012b
10231-1525 GWP1356     ABL 327.                                                                Tob2012b
10232+0542 SHJ 115     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
                       H 5  64.                                                                MEv2010 
           TOK 200     The 1".1 speckle companion can explain dmu, but not the acceleration.   Tok2012a
10233-0203 GWP1357     ABL 324.                                                                Tob2012b
10233-1603 GWP1358     ABL 328.                                                                Tob2012b
10236-1721 GWP1359     ABL 329.                                                                Tob2012b
10236-4408 HJ 4315     B is CD-43@6220.                                                                
10237+0237 LAM   7     AB: B is BD+03@2357.                                                            
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
10237-0221 GWP1360     ABL 325.                                                                Tob2012b
10238+1239 BPM 572     [PM2000]  977607 + [PM2000]  977554.                                    Gvr2010 
10238-4415 I   208     AB. 1997.1230: A smaller annulus was used in the power spectrum fit             
                       due to the faintness of the source. As a consequence, the separation            
                       and position angle uncertainties may be larger than other measures.     Hor1997 
10239-1934 GWP1361     ABL 330.                                                                Tob2012b
10244+3411 STTA104     B is BD+34@2122.                                                                
                       The primary is a semi-regular variable.                                         
10245+4008 ES 1542     BRT 106                                                                         
10246+0305 CHE 147     SLE 586.                                                                        
10246-1906 HS Hya      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Torres et al. (1997). They derived component masses 1.39 and 0.61 Msun  Trr1997d
                       and an estimated semimajor axis of 8.48 mas.                            Ren2013 
10247-0612 GWP1362     ABL 332.                                                                Tob2012b
10247-1127 GWP1363     ABL 333.                                                                Tob2012b
10249-3818 GLI 294     Also known as RSS 236 and WFC 104. #145 in the original list of Gilliss.        
10250+2437 STF1429     A premature orbit has been computed.                                            
10251-0059 GWP1364     ABL 331.                                                                Tob2012b
10253-1250 GWP1366     ABL 334.                                                                Tob2012b
10254+1603 BPM 573     [PM2000]  978410 + [PM2000]  978438.                                    Gvr2010 
10254-1034 GWP1370     ABL 336.                                                                Tob2012b
10254-1826 GWP1369     ABL 338.                                                                Tob2012b
10256+0847 STF1431     H 1  29.                                                                MEv2010 
10257-0704 SCA  53     Spectrum: K5:IIIbFe-0.5.                                                        
10258+0312 HJ 1177     BAL 2373.                                                                       
10258-4757 SWR  91     CPM pair                                                                Skf2004 
10260+5237 STF1428     BDS 5386, H I 71 probably same star.                                            
                       H 1  71.                                                                MEv2010 
10262+0356 BU 1280     A is a Delta Scuti-type variable, RX Sex.                                       
10263-5353 HJ 4319     Spectrum M2IabCN0.5, variable in light. B has a B-V color of 0.25;              
                       U-B = -0.67 (Humphreys et al., ApJ 172, 75, 1972)                               
10264+6246 LDS2583     SLW 472.                                                                        
10264+1438 BPM 574     [PM2000]  978935 + [PM2000]  978948.                                    Gvr2010 
10264-0658 GWP1371     ABL 335.                                                                Tob2012b
10266-1728 GWP1373     ABL 337.                                                                Tob2012b
10269+1931 COU 292     1983.9557, 1983.9667: Measurements should be given low confidence.      Bag1985 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.26 +/- 1.05, 2.44, and 1.10 Msun, respectively.             Mlk2012 
10269+1713 STT 217     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.38 +/- 1.55, 2.70, and 1.17 Msun, respectively.             Mlk2012 
10269-0703 GWP1374     ABL 339.                                                                Tob2012b
10270+2638 HIP  51157  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Griffin (1987). They derived component masses 0.86 and 0.30 Msun and    Grf1987b
                       an estimated semimajor axis of 76.15 mas.                               Ren2013 
10271-1756 GWP1375     ABL 340.                                                                Tob2012b
10271-6200 TDS7279     AB,C: SHY 555. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                       very high (near 100%) probability pair is physical.                             
10276+0946 HJ  832     45 Leo. A is an Alpha CVn-type variable, CX Leo, and an SB.                     
10277-0108 LDS3990     NLTT 24410/24411                                                        Chm2004 
10279+3642 HU  879     bet LMi = 31 LMi. G8III-IV.                                                     
                       Combined visual-spectroscopic orbits by Heintz (1981,1982). Visual      Hei1981f
                       observations cover only a narrow apastron arc.                          Hei1982e
                       Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                       orbit of Baize (1950).                                                  Baz1950b
                       Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based   Gon2002a
                       on a combination of ground-based catalogs with Hipparcos.                       
                       This object was misidentified as HO 879 in McAlister & Hendry (1982).   McA1982d
                       Malkov et al. (2012) derive dynamical and spectroscopic masses                  
                       3.37 +/- 0.94 and 2.63 Msun, respectively.                              Mlk2012 
10280+1950 STF1435     HJL 125.                                                                HJL1986 
10282-2548 FIN 308     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.71 +/- 0.53, 2.23, and 0.98 Msun, respectively.  Mlk2012 
                       AB: Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at               
                       request of author.                                                      Tok2015c
10283-0436 GWP1378     ABL 341.                                                                Tob2012b
10284-1517 GWP1380     ABL 343.                                                                Tob2012b
10286-1437 GWP1382     ABL 342.                                                                Tob2012b
10287+4558 A  1993     Derived orbital parallax 0".01274, mass sum 2.01 +/- 0.87 Msun          Lin2004a
10288+6300 OSO  33     G236-030. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
10288-6235 DUN  85     B is CPD-61@1676.                                                               
                       Additional notes may be found in Dunlop (1829).                         Dun1829 
10289+3453 SHY 215     HIP  51312 + HIP  52140.                                                        
10289-0300 FIL  25     BAL 211.                                                                        
10290-1952 GWP1385     ABL 344.                                                                Tob2012b
10294+1211 HDS1507     Cvetkovic et al. (2016) estimate spectral types F0 and F7, masses 1.66          
                       and 1.30 Msun. Dynamical parallax is 10.81 +/- 0.15 mas.                Cve2016b
10294+0346 SLE 494     Error in Soulie (1986) measure apparently due to typo in right                  
                       ascension of primary.                                                   Sle1986a
10294-5034 B  1681     V349 Vel, Algol (EA) type eclipsing binary, P = 3.02447 d.              Zas2011 
10296+3757 HJ 2532     ALI 848.                                                                        
                       AB: HJL 126.                                                            HJL1986 
10296-3036 H N  50     del Ant                                                                         
10297+8415 GC 14305    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10297-1327 GWP1387     ABL 347.                                                                Tob2012b
10299+2835 STTA105     B is BD+29@2056.                                                                
10299-0435 GWP1388     ABL 345.                                                                Tob2012b
10300-0413 LDS3994     NLTT 24512/24515                                                        Chm2004 
10301-4721 HJ 4324     SWR  92.                                                                Skf2004 
10302+5100 STT 219     BDS 5471, HJ 2535 probably same star. The Hipparcos secondary                   
                       magnitude of 7.70 is very different than the visual mean of 11.2.               
10303-0818 GWP1389     ABL 346.                                                                Tob2012b
10306+5559 LDS2863     A: 36 UMa                                                                       
                       B: BD+56@1458.                                                                  
                       Components of these systems (AB and AC) all have common proper          Egg1950 
                       motion and common radial velocity.  Vyssotsky & Reuyl also claim that   Vys1942 
                       this system shares a common proper motion with BD+57 1266, an 8th               
                       magnitude star 4041" from A.                                                    
                       AB: HJL 127.                                                            HJL1986 
                       AB: Raghavan et al. (2010) consider B component possible binary (RV     Rag2010 
                       variable)                                                               Tok2014d
10307-5429 HJ 4327     B is CPD-53@3900.                                                               
10307-6121 DUN  87     B is CPD-60@1944.                                                               
10310-0232 GWP1390     ABL 348.                                                                Tob2012b
10310-0738 STF1441     A is a spectroscopic binary. C is BD-06@3171.                                   
10313-5153 HJ 4328     B is CD-51@4816.                                                                
10314-5343 HJ 4329     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
           LUH   9     AC: GJ 9332 + 2MASS J10313234-5338010.                                          
10315-0605 GWP1391     ABL 350.                                                                Tob2012b
10316+4316 SHY 557     HIP  51536 + HIP  51726.                                                        
10316-0253 GWP1392     ABL 349.                                                                Tob2012b
10316-3956 HJ 4326     B is CD-39@6453.                                                                
10317-4429 B  1161     Measures uncertain, too close. Needs speckle.                                   
10318-6356 HD  91452   The classification is from the LSC; however, Garrison et al. (1977              
                       ApJS 35, 111) assign a type B0 Ia.                                      Msn1998a
10319+3223 HJ  482     33 LMi.                                                                         
10319-8155 HJ 5444     B is CPD-81@448.                                                                
10320+3355 LDS1244     Discrepant Luyten measure appears to be due to a 1' error in dec of     Luy1969 
                       his secondary.                                                                  
10320+2202 STF1442     STT 221.                                                                        
10320-2021 B  2248     J 2655. BHA 13.                                                                 
10320-4504 PZ    3     B is CD-44@6582.                                                                
10321+3240 SKF 317     SLW 487.                                                                        
10323-1827 GWP1395     ABL 352.                                                                Tob2012b
10325-7226 RSS  14     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
                       SHY 558. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
10328+0918 WRH  19     rho Leo = 47 Leo. Possible spectroscopic binary.                                
                       Additional notes may be found in Wilson (1941).                         WRH1941b
                       A is a blue supergiant with multiple pulsation periods.                 IAU2014e
10329-4700 HJ 4330     AB: B is CD-46@6207.                                                            
           YSJ   1     Aa,Ab: 1995.1025: WDS Catalog lists a companion at 40".3 and position           
                       angle 163deg. The component listed here appears to be a new discovery.          
                       Our two observations of this object were forty minutes apart on                 
                       February 7, 1995 (UT).                                                  Dns1997 
                       1997.1176  This is the first measure of this system since the                   
                       discovery measures in 1995 of Dinescu et al. (1997) The difference in   Dns1997 
                       position angle from their last measure is 2.2 deg and the difference            
                       in separation is 0".020.                                                Hor1997 
10330+3033 LDS1246     NLTT 24638/24639                                                        Chm2004 
10332+4026 HJ 2534     A is a spectroscopic binary.                                                    
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
10332-5830 EVS  16     Primary is the Cepheid Y Car.                                           Evs2016a
10334+3410 LDS 916     NLTT 24653/24654                                                        Chm2004 
10335-4659 HJ 4332     B is CD-46@6218.                                                                
10336+1351 BPM 575     [PM2000]  982666 + [PM2000]  982677.                                    Gvr2010 
10339-1750 S   610     B is BD-17@3179.                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
10340+1631 BPM 576     [PM2000]  982873 + [PM2000]  982856.                                    Gvr2010 
10340-0423 GWP1397     ABL 353.                                                                Tob2012b
10340-2345 BU 1269     44 Hya.                                                                         
10341+1251 BPM 577     [PM2000]  982909 + [PM2000]  982959.                                    Gvr2010 
10343-1732 GWP1400     ABL 355.                                                                Tob2012b
10344+4041 LDS3998     SLW 495.                                                                        
10345-0641 GWP1401     ABL 354.                                                                Tob2012b
10345-1753 B  2533     Perhaps identical with HLD 107.                                                 
10347-3524 HJ 4334     SWR  94. CPM pair                                                       Skf2004 
10349-0820 GWP1403     ABL 359.                                                                Tob2012b
10350+0839 STF1450     49 Leo. A is the Algol-type system TX Leo.                                      
                       Individual J,H,K magnitudes are calculated from 2MASS combined                  
                       magnitudes and AO-derived magnitude differences                         Rbr2005 
10351-5741 COO 107     Spectrum of B is A.                                                             
10352-4545 SWR  95     CPM pair                                                                Skf2004 
10352-4755 SWR  96     CPM pair                                                                Skf2004 
10353+4321 LDS4001     SLW 497.                                                                        
10354+2616 STF1451     LDS1249.                                                                        
                       AB: NLTT 24760/24757                                                    Chm2004 
10355-0234 GWP1404     ABL 356.                                                                Tob2012b
10356-0415 GWP1406     ABL 357.                                                                Tob2012b
10356-0508 GWP1405     ABL 358.                                                                Tob2012b
10359+6336 STF1444     Primary is GT UMa, an Algol type eclipsing binary, P = 1.16471d.        Zas2012 
10360+0118 GRV1044     SLW 499.                                                                        
10361+1137 BIG   1     B is BD+12@2234.                                                                
10361-2641 BU  411     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.69 +/- 0.48, 2.42, and 1.17 Msun, respectively.             Mlk2012 
10363-1213 GWP1409     ABL 360.                                                                Tob2012b
10363-1621 BU 1075     phi 2 Hya                                                                       
10364-1223 GWP1410     ABL 361.                                                                Tob2012b
10365-1214 EHR  13     AB: Companion appears to be a background star.                          Ehr2010 
           KUI  51     AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
10366+7849 HJ 5480     Discrepant observation by Pettit originally catalogued at PTT  26,      Ptt1917 
                       although he said it was of HJ 5480.                                             
10366-1246 GWP1411     ABL 362.                                                                Tob2012b
10367+1522 DAE   3     RBS 887                                                                         
                       Daemgen et al. (2007) derive distance of 19.6 +/- 4.6 pc, separations   Dae2007 
                       of 20.8 +/- 6.0 au (AB) and 3.7 +/- 1.1 au (BC), and predicted orbital          
                       periods of 157 +97/-93 yr (AB) and 16 +10/-9 yr (BC). Spectral types            
                       for the three components are M3.5 +/- 0.5, M4.5 +/- 0.5, and M4.5 +/-           
                       0.5; masses 0.29 +0.11/-0.08, 0.16 +0.05/-0.04, 0.16 +0.05/-0.0 Msun.           
10370-0850 TOK  44     Aa,Ab: Tokovinin et al. (2015) derive spectral types G0V and K5V for            
                       the Aa and Ab components; masses are 1.46 and 0.64 Msun. Aa is a 170d           
                       SB; Aa2 is possibly of type M3V.                                        Tok2015b
                       Aa,Ab: SB, P=7.603y.                                                    Tok2014d
           A   556     AB: Tokovinin et al. (2015) derives a spectral type K5V for the B               
                       component; mass is 0.64 Msun. Dynamical parallax is 27.4 +/- 0.6 mas.   Tok2015b
10372+8603 STF1410     AB: STT 214.                                                                    
10373-4814 SEE 119     One component is SB, P = 10.21 d. (#623 in Batten et al., 1989).        Bte1989 
                       According to Evans (1969), this is the primary. Identification of       Evn1969 
                       the ascending node is based on this assumption.                                 
                       The period adopted for the visual orbit utilizes RV and                 Fin1968b
                       interferometric observations.                                                   
                       See also Evans (1969) for residuals, ephemeris,and full discussion of   Evn1969 
                       this interesting system.                                                Fin1970b
10373-5826 JSP 408     TDS7378.                                                                        
10374+3133 LDS1251     NLTT 24861/24863                                                        Chm2004 
10374-5837 SNA  10     Aa,Ab: It is uncertain whether the 33mas companion corresponds to the           
                       SB reported by Sota et al. (2014, ApJS 211, 10). If it does, the                
                       orbital period is at least 5 years.                                     Sna2014 
           HJ 4338     Herschel says "A very neat double star involved in a nebula." There is          
                       perhaps a nebulouse patch running N and S, 5' x 1', but there is no             
                       nebula surrounding this pair as suggested by h. Many small stars near.  I__1916a
                       But what John Herschel was describing was the large (15' diam) object           
                       NGC 3324; Herschel used the pair as the reference position for the              
                       nebula. Innes was probably viewing at quite high magnification to               
                       measure the double, and so missed the nebula. The pair is in fact the           
                       principle source of fluorescing uv photons for the nebula!              Skf2014 
10375+3015 HJ  487     Aka SKF1845.                                                                    
10376+3001 LDS1253     NLTT 24873/24875                                                        Chm2004 
10376-4556 CPO 296     CPD-45@4802.                                                                    
10376-5744 JSP 410     TDS7381.                                                                        
10377-7335 HJ 4344     Algol (EA) type eclipsing binary, P = 2.45763 d.                        Zas2011 
                       B is CPD-72@998.                                                                
                       SWR  97. CPM pair                                                       Skf2004 
10379+3405 36 LMi      SB1. Combined orbit including RV data and Hipparcos Intermediate                
                       Astrometric data. Semimajor axis derived from photocentric a0 plus              
                       stellar evolutionary model. Derived properties for A and B:                     
                       M/Msun = 4.94 + 1.42, L/Lsun = 1296.36 + 5.89, dm = 5.86 mag,                   
                       log age = 8.10.                                                         WaX2015b
10381+4026 STT 223     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
10382-0620 GWP1414     ABL 363.                                                                Tob2012b
10382-0629 GWP1415     ABL 364.                                                                Tob2012b
10383+6007 STT 222     Primary is 2.8d SB1; AB is physical pair, estimated period 3600y.       Tok2006 
10385-1559 GWP1416     ABL 365.                                                                Tob2012b
10386-1653 phi 3 Hya   Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Christie (1936).                                                        Crs1936 
10386-4558 B  2715     CPD-45@4816.                                                                    
10389+0721 J    79     Aitken incorrect; pair is BD+08 2387, not +08 2388.                     J__1949a
10390-0440 GWP1421     ABL 366.                                                                Tob2012b
10390-5849 GLI 152     B is CPD-58@2475.                                                               
10391+0726 J  1351     BRT 2603.                                                                       
                       J  2656.                                                                J__1962a
10392-2551 TOK 135     HIP 52145. A is SB without orbit, dRV= 1.2.                             Nrd2004 
                       A new triple. There is also a bright companion C in the field.          Tok2011a
10395+3142 STF1458     HJL 128.                                                                HJL1986 
                       SEI 521.                                                                Nsn2017b
10397+0851 STT 224     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.81 +/- 0.74, 2.61, and 1.20 Msun, respectively.  Mlk2012 
10398+4209 OSO  34     G146-056. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
10401+1914 STT 225     AC: HJL 129.                                                            HJL1986 
10402-1622 LDS 311     B is BD-15@3101.                                                                
                       NLTT 25010/25005                                                        Chm2004 
10406-1523 GWP1430     ABL 369.                                                                Tob2012b
10406-5933 COO 110     B is CPD-58@2523.                                                               
10409-3545 B  2001     Spectrum composite; G8-K0III+F-G.                                               
10410-1225 GWP1432     ABL 368.                                                                Tob2012b
10412-0811 GWP1433     ABL 367.                                                                Tob2012b
10412-4403 DON 429     TDS7414.                                                                        
10420+6506 GRV1046     SLW 510.                                                                        
10422+3142 BLL  28     A is the semiregular variable RX LMi.                                           
10422-0357 GWP1435     ABL 371.                                                                Tob2012b
10423-1043 GWP1436     ABL 373.                                                                Tob2012b
10424-0114 GWP1437     ABL 370.                                                                Tob2012b
10425-0358 GWP1438     ABL 372.                                                                Tob2012b
10425-3340 NHR   1     The source at 2.4" separation, first reported in Neuhauser et al.       Nhr2000 
                       (2000), is an already known background star (Lowrance et al. 2005), a   Lwr2005 
                       conclusion which we can confirm at ~28 sigma confidence.                Jnn2012 
10425-6158 HZG9001     FV Car.                                                                 Plt1934 
10426+0335 A  2768     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       This object was misidentified as ADS 7986 in McAlister & Hendry (1982)  McA1982d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.37 +/- 1.09, 2.80, and 1.13 Msun, respectively.             Mlk2012 
10426-1555 GWP1439     ABL 374.                                                                Tob2012b
10427-1826 GWP1440     ABL 377.                                                                Tob2012b
10428-0211 GC 14729    Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from the Geneva           
                       Extrasolar Planet Search Programs home page.                            HaI2001 
10430+2620 BU  913     40 LMi.                                                                         
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
10430-6424 the Car     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
10432+0440 A  2769     This pair is the C component of 10433+0445.                                     
10432-1542 GWP1441     ABL 376.                                                                Tob2012b
10432-6110 SIN  55     BD: initially listed incorrectly as AD.                                         
10433+0445 STF1466     35 Sex. A is a spectroscopic binary.                                            
                       Spectrum composite; K3III+K0III.                                                
                       AB: H N  36.                                                            MEv2010 
10434-0352 J    89     Also appears to be the long lost pair HLD  11 = BDS 5534.               Dam2014 
10434-1706 BFR   6     2MASS J10432398-1706024 + 2MASS J10432513-1706065. Baron et al. (2015)          
                       estimate spectral types M4.0 +/- 0.5 and M9.0 +/- 0.5, distances                
                       42 +26/-16 and 75 +6/-23 pc, masses 0.207-0.272 and 0.079-0.085 Msun.   BFr2015 
10435+4612 SMA  75     B is BD+46@1658. B is a spectroscopic binary.                                   
                       AB: NLTT 25147/25160                                                    Chm2004 
                       AB: HJL 130.                                                            HJL1986 
                       AB: SHY 216. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
           MET   7     BE and BF: Primary of 10440+4612 MET   7AB and AC same as B component           
                       of 10435+4612 SMA  75AB; systems merged.                                        
                       Based on proximity, Metchev & Hillenbrand (2004) say the BE pair is     Met2004b
                       probably physical.                                                              
10435-1852 GWP1442     ABL 378.                                                                Tob2012b
10438-0039 GWP1444     ABL 375.                                                                Tob2012b
10438-5933 CP-58 2611  Trumpler 14 FMM 20. This object is designated as Trumpler 14 20 in the          
                       list of Feinstein et al. (1973 A&AS 12, 331)  and as FMM 20 in Penny    Pny1993 
                       et al. (1993).                                                          Msn1998a
10438-5957 HJ 4355     B is CPD-59@2547.                                                               
10440-5932 CP-58 2620  Trumpler 14 FMM 8.  This object is designated as Trumpler 14 8 in the           
                       list of Feinstein et al. (1973 A&AS 12, 331) and as FMM 8 in Penny et   Pny1993 
                       al. (1993).                                                             Msn1998a
10440-5933 NEL   1     See discussion of the system by Sana et al. 2014).                      Sna2014 
           HJ 4356     Both A and B components were observed with the speckle camera and       Pny1993 
                       appeared to be single (Penny et al. 1993).                              Msn1998a
10440-5952 HJ 4357     V661 Car, Algol (EA) type eclipsing binary, P = 23.944 d.               Zas2011 
           SNA  13     Aa,Ab: Primary is V661 Car, a detached Algol-type eclipsing binary.             
                       The 20mas pair probably does not correspond to the 23.9d eclipsing              
                       binary (Otero 2006, Open European Journal on Variable Stars 45, 1),             
                       given the ~2.6kpc distance to the Cr228/Tr16 complex.                   Sna2014 
10441-1536 GWP1445     ABL 382.                                                                Tob2012b
10441-4005 HJ 4349     SWR  98. CPM pair                                                       Skf2004 
10441-5935 HJ 4360     Trumpler 16 MJ 238. Both A and B components were observed with the              
                       speckle camera and appeared to be single. Levato et al. (1991) derive   Lev1991a
                       a single-lined spectroscopic orbit for HD 93161 but they                        
                       do not indicate which component is the binary.  Howarth et al. (1997            
                       MNRAS 284, 265) and Penny (1996) found large radial velocity changes    Pny1996b
                       in closely spaced IUE spectra, and Howarth et al. argue that both               
                       components are short-period binaries.                                   Msn1998a
                       A comp is SB, types O8V and O9V, period 8.566 +- 0.004d. Spectral type          
                       of B component is O6.5V(f) and presents radial velocity variations.     Naz2005 
                       The position angle has been flipped about the E/W axis for the HST      Nel2004 
                       observation.                                                                    
                       The B component is noted as SB1 by Chini et al. (2012). Both A and B    Cii2012 
                       are bright enough for an interferometric analysis of the SAM data, but          
                       no companion was found.                                                 Sna2014 
           SNA  14     Ca,Cb: The C component was reported as SB1 by Chini et al. (2012).      Cii2012 
                       Further observations are desirable to confirm the reality of the tight          
                       Ca/Cb/Cc triple.                                                        Sna2014 
                       This star (component C of HD 93161) was observed with the speckle               
                       camera and appeared to be single.                                       Msn1998a
10442+6111 LDS2320     Pair at precise coordinates matches Luyten's rho/theta, as well as his  Luy1970 
                       BD+61 1312 cross reference, but apparently there was a typographical            
                       error of 2h in his published coordinates.                                       
10442+2927 SLW 515     CVR 572.                                                                        
10442-0732 GWP1446     ABL 380.                                                                Tob2012b
10442-3931 SWR  99     CPM pair                                                                Skf2004 
10443-1227 GWP1447     ABL 381.                                                                Tob2012b
10443-4515 CPO 301     B is CD-44@6765.                                                                
10443-7052 DUN  99     B is CPD-70@1185, spectrum A6IV.                                                
           CHR 227     Ba. Worley (private communication) noted that the systematic binary             
                       star surveys of Rossiter (1955) and van den Bos missed the              Rst1955 
                       declination band -73 to -70 deg. This probably explains why this                
                       half-arcsecond pair remained undiscovered until now.  CHR 227                   
                       represents a new component to the wide (63") common proper motion pair          
                       HR 4211-12 = DUN 99 AB, discovered by J. Dunlap in 1826 (1829) and      Dun1829 
                       last observed nearly 80 years ago (Dawson 1918). A 10th magnitude C     Daw1918a
                       component also lies some 35" from A, discovered by John Herschel in     HJ_1847a
                       1835, but no closer components are known.                               Hrt1996b
10444-6000 DAW   8     Often classified O9 or 9.5. QZ Car. The bright star consists of two             
           HDS1534     eclipsing pairs, P = 20.73d and 6.00d.                                          
                       The classifications are from Morrison & Conti (1980), who describe      Cti1980 
                       this quadruple that consists of a pair of SB1 systems (the shorter              
                       period system is also eclipsing).  Their expressed hope that speckle            
                       interferometry might resolve the pair was not realized in our work,             
                       but the object remains an important target for high resolution work.    Msn1998a
           SNA  15     The primary is QZ Car, a semi-detached beta Lyr type eclipsing binary.          
                       A complex multiple system, with three visual companions. The central            
                       object is itself a quadruple, composed of a pair of SBs, Aa1,Aa2                
                       (O9.7I+B2V, P=20.7d) and Aa3,Aa4 (O8III+O9V, P=60d and eclipsing).      Sna2014 
10445-5734 HDS1535     Classical Cepheid VY Car.                                                       
10445-5944 SEE 513     Noted by See but never added to WDS, this pair was confirmed by USNO    See1897l
                       UCAC1 astrometry. Discoverer designation and data added 12/09/2002.             
10446-5944 BSO   4     A is a spectroscopic binary. B is CPD-59@2584.                                  
                       Primary is V560 Car, an ellipsoidal variable star and eclipsing SB2.    Sna2014 
10446-5945 HD  93205   Trumpler 16 MJ 340.  The classification is from the UV tomographic              
                       analysis of Penny (1996). The companion star, HD 93204 (BsO 4 B) was    Pny1996a
                       also observed and appeared to be single.                                Msn1998a
10447-6001 HJ 4363     B is CPD-59@2593.                                                               
10448-5934 SNA  18     A long-period binary, discussed in Sana et al. (2011). This pair is     Sna2011b
                       one of the tightest resolved binaries in our sample and a non-thermal           
                       radio emitter.                                                          Sna2014 
10449+3224 LDS1258     NLTT 25213/25215                                                        Chm2004 
10451-0207 LDS4012     NLTT 25234/25233                                                        Chm2004 
10451-0735 GWP1450     ABL 379.                                                                Tob2012b
10451-1704 GWP1451     ABL 383.                                                                Tob2012b
10451-5941 B  2256     eta Car = Trumpler 16 MJ 480, an old nova in a nebula with nuclei.              
           I  1092     B and C involved in the nebulosity.                                     B__1951a
           WGT   2     One of these three components found by Weigelt is probably B  2256;     Wgt1986a
           DUN  98     however, it is not clear which one due to the lack of a continuous              
                       series of observations and orbital motion.                                      
                       This famous luminous blue variable is not classified as an O star, but          
                       it is almost certainly a massive object. The inner structure of the             
                       ejecta of this star is described by Davidson et al (1997 AJ 113, 335).          
                       A preliminary set of orbital elements is given by Damineli et al.               
                       (1997 NewA 2, 107), who suggest a 5.5-yr orbit with a maximum angular           
                       separation of 0".004.  The central object appeared single in our                
                       observations. The H component (HDE 303308) was also observed and                
                       appeared to be single.                                                  Msn1998a
                       Powell also measured the distance to 10446-5944BSO   4 (1856.012,       Pwl1857 
                       229.57 deg, 294.77; 1860.297, 229.3 deg, 297.8"), but they are not      Pwl1864 
                       physically related so are not merged.                                           
                       Powell also measured the distance to 10441-5935HJ 4360C (1860.306,      Pwl1864 
                       312.6 deg, 571.1"), but they are not physically related so are not              
                       merged.                                                                         
10453-5945 COO 113     Primary is V731 Car, Algol-type eclipsing binary, period 2.29995d.      Zas2013 
                       B is CPD-59@2633.                                                               
10453-8028 I   294     del 1 Cha                                                                       
10454+7550 HJ 5482     BDS 5530, HJ 3329 same star.                                                    
10454+3831 CHR 191     1983.4277: The AB pair is a new component to the 0".7 pair HO 532.              
           HO  532     This new component was actually first resolved in 1983 (McAlister et            
                       al (1987), but it was believed at the time that the measurement was of  McA1987b
                       the known pair (the wide component laid outside the processor "window"          
                       of our old autocorrelator).  Reprocessing of our archival video data            
                       allowed us to resolve both components in the 1983 and 1984 data sets,           
                       although both early measurements of the AB pair are quite weak.                 
10454-4342 HJ 4362     B is CD-43@6533.                                                                
10457-1907 LDS4013     NLTT 25279/25280                                                        Chm2004 
10457-5924 HD  93403   The classification is from the UV tomographic analysis of               Pny1996a
                       Penny (1996).                                                           Msn1998a
10458-5929 HJ 4369     B is CPD-58@2685. A is an irregular variable, BO Car. B has a B-V               
                       color of 0.16; U-B = -0.21 (Humphreys et al., ApJ 172, 75, 1972)                
10459+3041 S   612     42 LMi. B is BD+31@2181.                                                        
10460-1934 GWP1452     ABL 385.                                                                Tob2012b
10461-5657 HRG 133     B is CPD-56@3776.                                                               
10461-5934 HJ 4370     B is CPD-58@2689.                                                               
10463-1343 GWP1453     ABL 384.                                                                Tob2012b
10463-4128 TOK 137     HIP 52676. A is exoplanet host, P=13.2d, 46.0d                          Tok2014d
10463-6036 RST4463     A is a spectroscopic binary.                                                    
10465-6416 FIN 364     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 7.76 +/- 1.39, 5.61, and 3.71 Msun, respectively.  Mlk2012 
                       AB: Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at               
                       request of author.                                                      Tok2015c
10466-5933 HJ 4371     B is CPD-58@2700.                                                               
10468-4925 R   155     mu Vel. A is a SB.                                                              
10470+1302 STF1472     STTA106.                                                                        
10470-1241 GWP1454     ABL 390.                                                                Tob2012b
10472+7250 BUP9007     NGC 3348. For the record, measures are:                                         
                       10472+7250BUP9007      1888 2000    4  74  72  13.5  13.1 11.2  13.1            
                                         -024-005 +012+005               104710.03+725022.7            
                       10472+7250 1888.38      73.6         13.5                       0.3   1 Enh1906B
                       10472+7250 1910.12      67.8         13.5                       1.0   1 Bu_1913 
                       10472+7250 1999.168     72.8         13.29                      1.3   1 Skf2014b
                       10472+7250 2000.0       71.9         13.13           609  70    0.2   1 Skf2014b
10472+4027 LDS4016     AB: NLTT 25336/25338                                                    Chm2004 
10472-6006 COO 115     B is CPD-59@2700.                                                               
10474-1804 GWP1456     ABL 391.                                                                Tob2012b
10474-6555 R   157     Aka HDS1543.                                                                    
10475-2221 SHY 218     AC: HIP  52787 + HIP  52776.                                                    
10476+2008 LDS4018     NLTT 25362/25363                                                        Chm2004 
10476-0601 GWP1457     ABL 387.                                                                Tob2012b
10476-1516 STF1474     BC: H 2  74.                                                            MEv2010 
10476-1538 STF1473     B is BD-14@3187.                                                                
                       AB: SHY 562. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
10477-0748 GWP1458     ABL 388.                                                                Tob2012b
10478-0337 GWP1459     ABL 386.                                                                Tob2012b
10481-0218 OCC1061     Sign error in published WDS designation.                                OCC2012b
10482-1702 GWP1461     ABL 397.                                                                Tob2012b
10482-3956 NHR   2     DENIS-P J104814-395606                                                          
                       Conclude secondary is background object.                                Nhr2002c
10483+1006 BPMA 41     AB: [PM2000]  990241 + [PM2000]  990072.                                Gvr2010 
           BPMA 42     BC: [PM2000]  990072 + [PM2000]  989991.                                Gvr2010 
10484+3734 HD  93521   The classification is from Hobbs et al. (1982 ApJ 263, 690). Fullerton  Ful1990 
                       (1990) and Howarth & Reid (1993 A&A 279, 148) describe the striking             
                       line profile variations in the spectra apparently due to nonradial              
                       pulsations.                                                             Msn1998a
10484-2014 LDS 315     NLTT 25404/25403                                                        Chm2004 
10485-1537 GWP1462     ABL 396.                                                                Tob2012b
10485-2223 RST2710     CPD-21@4800.                                                                    
10488-0721 GWP1464     ABL 395.                                                                Tob2012b
10489-0102 GWP1465     ABL 393.                                                                Tob2012b
10490-4348 DAW  10     AB = SWR 100. CPM pair                                                  Skf2004 
10491-0058 BVD 147     = GWP1467 = ABL 392.                                                    Tob2012b
10491-0247 GWP1466     ABL 394.                                                                Tob2012b
10492-1823 GWP1468     ABL 398.                                                                Tob2012b
10493-0401 STF1476     40 Sex.                                                                         
10493-4652 BRT 790     CPD-46@4866.                                                                    
10493-5319 LUH  16     WISE J104915.57-531906.1. Nearby (2.0 +/- 0.15pc) high-proper motion            
                       (-2759 +/- 6, +354 +/- 6mas/yr) star resolved as 1.5" (3au) binary by           
                       Gemini Multi-Object Spectrograph. Primary classified as L8 +/- 1,               
                       secondary as late-L/early-T.                                            Luh2013 
                       Based on several spectral indices, Burgasser et al. (2013) determine            
                       spectral types L7.5 and T0.5 +/- 1.                                     Bug2013 
                       Boffin et al. (2014) monitored LUH 16 over 2 months, and detected               
                       perturbation in the relative orbital motion which led them to suspect           
                       a substellar companion around one of the two components.                Bof2014 
                       Kniazev et al. (2013) obtained long-slit spectra and NIR images, and            
                       derive spectral types of L8 +/- 1 and T1.5 +/- 2.                       Kni2013 
                       Bedin et al. (2017) derive masses 32 +/- 11 and 27 +/- 10 Mjup for the          
                       components of this L7.5+T0.5 brown dwarf pair.                          Bdi2017 
10494+0439 GIC  93     G044-038/G044-037.                                                              
10496+1256 STF1477     HJL 131.                                                                HJL1986 
10496-3552 JC   22     B is CD-35@6767.                                                                
10498+3533 BEU  14     PM = -640-1018.                                                                 
                       GJ 1138. This pair has been previously reported as a 300 mas binary             
                       (Beuzit et al. 2004). The fact that it looks single in our AstraLux     Beu2004 
                       images despite the excellent quality of those observations implies              
                       that it must have undergone substantial orbital motion, bringing it to          
                       a much smaller (<100 mas) projected separation in June of 2012.         Jnn2014 
10498-0854 J  2076     Pair is -28s, -1' from BD-08 3018                                       J__1949a
10499-0453 GWP1469     ABL 399.                                                                Tob2012b
10500-1225 GWP1470     ABL 401.                                                                Tob2012b
10503-0854 HJ  838     41 Sex. A is a spectroscopic binary. C is BD-08@3019.                           
10503-1625 GWP1471     ABL 402.                                                                Tob2012b
10504-1326 LDS4023     AC: NLTT 25480/25488                                                    Chm2004 
10504-1459 RST3714     FIN 310.                                                                        
10505+5627 OSO  35     G196-047. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
10506-0611 GWP1472     ABL 400.                                                                Tob2012b
10506-4112 CPO 306     Nys calls A CPD-40@4776, and B CPD-40@4775.                                     
10510-5957 HJ 4378     B is CPD-59@2783.                                                               
10513+3607 BWL  26     Bowler et al. (2012) estimate the spectral type of the companion at             
                       M7 +/- 2. Age of the system is estimated as 25-300 Myr, distance                
                       22 +/- 3 pc, projected separation 4.4 +/- 0.6 au.  Masses of the                
                       primary and secondary are 0.25 +/- 0.5 Msun and 46 +/- 16 Mjup.         Bwl2012b
                       A comp is GJ 3629, spectral type M3.0Ve, mass 0.3-0.5 Msun. B is M7.5           
                       +/- 0.5, mass 41-94 Mjup. Orbital period is estimated at ~30 yr.        Bwl2015 
10514-1329 GWP1475     ABL 403.                                                                Tob2012b
10516-2115 BU 1428     A is the variable V Hya.                                                        
10519-5859 SNA  20     This object is the O8.5 Iaf spectroscopic standard. The Sb2 status              
                       reported by Chini et al. (2012) may rather trace intrinsic variability  Cii2012 
                       due to the string winds of this Iaf supergiant.                         Sna2014 
10520+1606 A  2373     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 29.48 +/- 39.87, 5.40, and 1.20 Msun, respectively.           Mlk2012 
10522+4423 DUP   2     Dupuy et al. (2015) resolved this L/T pair and determined it to be a            
                       J-band flux reversal binary. Parallax is 38.4 +/- 0.7 mas (distance             
                       26.1 +/- 0.5pc); spectral types are L6.5 +/- 1.5 and T1.5 +/- 1.0,              
                       masses 49 +/- 3 and 39 +/- 3 Mjup.                                      Dup2015b
10522+0728 STF1482     GIR   5 was incorrected listed as the AC pair at these coordinates.             
10524-1924 GWP1477     ABL 407.                                                                Tob2012b
10525+0730 GIR   5     Incorrected listed as the AC pair at the coordinates of STF1482.                
10526+0500 A  2773     HIP 53165. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
10526-1807 GWP1479     ABL 406.                                                                Tob2012b
10528-0516 GWP1481     ABL 404.                                                                Tob2012b
10529-1717 HDS1556     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.26 +/- 0.96, 2.06, and 0.94 Msun, respectively.             Mlk2012 
10530+5742 A  1352     This cannot be the close 5.508-d spectroscopic binary.                  Grf2009c
                       NU UMa, Algol (EA) type eclipsing binary, P = 5.50762 d.                Zas2011 
10530+0458 TOK 438     Latham (2012, private communication) identified HIP  5212 = HD 94292            
                       as SB2 with a period of 8.3yr and a highly eccentric orbit. It is               
                       resolved here securely at 50mas.                                        Tok2015c
10531-0311 FIL  27     BAL 214.                                                                        
10531-1439 GWP1484     ABL 405.                                                                Tob2012b
10531-2038 GJ 9336     Triple with inner SB1 of 6.8 days and outer SB system of estimated              
                       3.3 yr period which produces large acceleration. The estimated axis is          
                       40 mas, unresolved with speckle.                                        Tok2012a
10532-0905 LDS4030     NLTT 25623/25624                                                        Chm2004 
10532-1519 LDS4031     SKF   7.                                                                        
10532-3006 SHY 563     HIP  53226 + HIP  53314.                                                        
10533-1506 LDS4032     = GWP1486 = ABL 410.                                                    Tob2012b
10533-4316 CPO  53     BVD  87.                                                                        
10533-6207 WFC 110     JAW  19.                                                                        
10534-0215 S   617     BDS 5610 is probably identical (BDS). B is BD-01@2458.                  Bu_1906 
                       A is a spectroscopic binary.                                                    
           GC 14969    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1980).                                                         Grf1980b
           S   617     HJL 132.                                                                HJL1986 
                       H 5  62.                                                                MEv2010 
10535-2008 BU 1429     b 2 Hya. A is a suspected variable star, CV 101166.                             
10535-5851 DUN 102     B is CPD-58@2830.                                                               
10536-1111 GWP1487     ABL 409.                                                                Tob2012b
10540-0747 GWP1489     ABL 408.                                                                Tob2012b
10540-1958 GWP1488     ABL 412.                                                                Tob2012b
10543-3325 PRO  96     SWR 102.                                                                        
10546-1711 GWP1491     ABL 411.                                                                Tob2012b
10546-3845 HJ 4381     B is CD-38@6819.                                                                
10554-1023 GWP1495     ABL 417.                                                                Tob2012b
10555-0055 GWP1498     ABL 413.                                                                Tob2012b
10555-0813 GWP1497     ABL 414.                                                                Tob2012b
10555-0917 GWP1496     ABL 416.                                                                Tob2012b
10556+2445 STF1487     54 Leo. B is a spectroscopic binary.                                            
                       Measure of 1927.33 made by triangulation of multiple measures.                  
                       H 3  30.                                                                MEv2010 
10556-1246 GWP1499     ABL 418.                                                                Tob2012b
10557+4246 MTR   1     While the proper motion indicates the pair is optical, spectral typing  Mtr2013 
                       and the distance based on colors is consistent with a physical pair.            
                       The optical/physical status of the pair is not certain at this time.            
10557+0044 BU 1076     55 Leo. If T is reasonably accurate, the RV run of the primary in               
                       1919-30 would fit the visual motion with an ascending node in the third         
                       quadrant.                                                                       
10557-4625 CPO 309     CPD-45@5026.                                                                    
10558-0841 GWP1500     ABL 415.                                                                Tob2012b
10559+2339 POU3092     LDS4038 = LDS6234.                                                              
10560-6024 HDS1561     This is the B[e] star GG Car, a supergiant with a rotating disk         IAU2014c
                       structure.                                                                      
10560-7725 REP  15     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = M1.5             Teff = 3630 +- 320        L = 0.50  +- 0.09           
                          Age =  1.6 +2.3/-0.8   M =    0.42 +0.21/-0.12   R = 1.79  +- 0.16           
                       B: SpT = M3               Teff = 3420 +- 250        L = 0.10  +- 0.02           
                          Age =  5.8 +10/-2.5    M =    0.29 +0.13/-0.12   R = 0.91  +- 0.07   Dae2013 
10561-2108 S   618     B is BD-20@3300.                                                                
10562+4802 ES 2636     B is BD+48@1901. One component is variable.                                     
10564-5733 HJ 4387     B is CPD-56@4017.                                                               
10566+2620 BRT3296     Originally published as BRT 156.                                        Brt1928 
10566+1739 STF1490     BDS 5613 same star.                                                             
                       HJL 134.                                                                HJL1986 
                       STF1489.                                                                        
10567-0542 GWP1501     ABL 420.                                                                Tob2012b
10568-3615 SWR 103     CPM pair                                                                Skf2004 
10570-0051 LDS6235     NLTT 25797/25799                                                        Chm2004 
                       HJL 135.                                                                HJL1986 
10570-7121 HJ 4392     B is CPD-70@1261.                                                               
                       SWR 104.                                                                        
10571-0214 GWP1504     ABL 419.                                                                Tob2012b
10571-6840 RMU   1     AB: Companion is a probable giant planet, mass 5 +/- 2 Mjup, located            
                       55.7 +/- 2.5 au from its host star, HD 95086.                           Rmu2013b
                       Galicher et al. (2014) provide a revised L' magnitude difference for            
                       the Rameau et al. (2013b) measure of 1/11/2012, obtained by better      Rmu2013b
                       calibration and derivation of the neutral density filter throughput.    Glc2014 
           KOU   2     AC: C component is a background star.                                   Rmu2013a
10576-1735 GWP1507     ABL 425.                                                                Tob2012b
10576-1955 GWP1506     ABL 428.                                                                Tob2012b
10577+1031 BPM 578     [PM2000]  994707 + [PM2000]  994714.                                    Gvr2010 
10578-0107 GWP1509     ABL 421.                                                                Tob2012b
10578-0555 GWP1510     ABL 423.                                                                Tob2012b
10579-1756 GWP1511     ABL 426.                                                                Tob2012b
10581+0634 GIC  94     G045-024/G045-023.                                                              
10583-7717 GHE  33     Daemen et al derive component properties (units K,Lsun,Myr,Msun,Rsun):          
                       A: SpT = K1               Teff = 5080 +- 490        L = 1.6   +- 0.4            
                          Age = 10.  +12/-7      M =    1.4  +- 0.2        R = 1.65  +- 0.16           
                       B: SpT = M6               Teff = 2990 +- 320        L = 0.06  +- 0.01           
                          Age =  4.2 +5.8/-4.0   M =    0.10 +0.11/-0.07   R = 0.89  +- 0.09   Dae2013 
10585+1711 A  2375     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.93 +/- 1.76, 2.09, and 0.95 Msun, respectively.             Mlk2012 
10585-1046 LDS4041     NLTT 25870/25869                                                        Chm2004 
                       Non-physicality established by CTIOPI parallax (unpublished).                   
10585-1450 GWP1513     ABL 424.                                                                Tob2012b
10585-1816 GWP1512     ABL 427.                                                                Tob2012b
10586+0908 STF1497     ARG  73.                                                                        
10586-0234 GWP1514     ABL 422.                                                                Tob2012b
10590-1555 GWP1515     ABL 429.                                                                Tob2012b
10590-3607 SWR 105     CPM pair                                                                Skf2004 
10594-4308 HJ 4394     B is CD-42@6636.                                                                
10595+4026 47 UMa      = Chalawan. Combined solution, based on reduction of Hipparcos                  
                       intermediate astrometric data together with spectroscopic elements from CPS1996b
                       Butler & Marcy (1996).                                                  HaI2001 
10596+2527 AG  342     NLTT 25925/25926                                                        Chm2004 
10596+1800 HDS1568     Cvetkovic et al. (2016) estimate spectral types K0 and K9, masses 0.90          
                       and 0.48 Msun. Dynamical parallax is 29.33 +/- 3.03 mas.                Cve2016b
10598+5854 STF1495     B is BD+59@1339.                                                                
                       H 5 111.                                                                MEv2010 
10599-4445 CPO 310     LDS 326.