14000-4714 DAW 207     D: AA Cen                                                                       
           HJ 4638     C: ZZ Cen. Both are variables of unknown type.                                  
14004-2708 LDS4424     NLTT 35939/35937                                                        Chm2004 
14006+4741 LDS5803     AC: NLTT 36000/35991                                                    Chm2004 
14007+2404 BRT3304     POU 3156 is identical, and Barton's angle is corrected by Heintz.       Hei1983a
                       Originally published as BRT 166.                                        Brt1928 
14013-4240 SWR 150     CPM pair                                                                Skf2004 
14014-3137 TOK 159     Aa,Ab: HIP 68507 is an acceleration binary with a variable RV resolved          
                       here at 0".06.  The period of Aa,Ab is on the order of 5yr. There is a          
                       faint physical companion B at 6".7 found in 2MASS (Tokovinin 2011).     Tok2011a
                       Another visual companion at 14", SEE 195, is optical, as revealed by            
                       its fast relative motion.                                               Tok2015c
                       Aa,Ab: SB, no orbit.                                                    Tok2014d
           SEE 195     AC: Linear configuration. A is SB without orbit (dRV= 5.4) and          Nrd2004 
                       astrometric binary (Hipparcos).                                                 
14016+0133 SHJ 171     tau Vir = 93 Vir. A is a spectroscopic binary.                                  
                       B is BD+02@2760.                                                                
                       AB: H 6  77.                                                            MEv2010 
14018-6119 LPO  44     Spectral type F0?                                                               
14019+1530 ALD 112     Worley measured this as ALD 118, but also identified it as Vys 149      Wor1962b
                       = ALD 112, which it matches. Measure moved here.                                
14021-4001 WG  172     SWR 151.                                                                        
14022+1608 BPM 610     [PM2000] 1073886 + [PM2000] 1073930.                                    Gvr2010 
14022-0448 LDS4427     NLTT 36043/36042                                                        Chm2004 
14023-6652 LDS 468     A component appears double.                                             Dam2010 
14024+4620 SWI   1     LDS1403.                                                                        
                       NLTT 36091/36092                                                        Chm2004 
14024-0311 LDS4429     NLTT 36057/36053                                                        Chm2004 
14029-3511 I  1574     Measures uncertain, too close.                                                  
14035+1047 GC 18985    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Kamper (1987).                                                          Kpr1987a
                       Combined astrometric/spectroscopic solution by Kamper (1987).           Kpr1987a
                       GJ 538. Martin et al. (1998) derive component masses 1.109 +/- 0.057            
                       and 0.548 +/- 0.033 Msun.                                               Mig1998 
14037+1914 LDS5806     LDS6289.                                                                        
14037+0829 BU 1270     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.36 +/- 0.53, 2.49, and 1.20 Msun, respectively.             Mlk2012 
14037+0243 AG  192     One component is variable.                                                      
14038-6022 RBT   1     Aa,Ab: bet Cen = Hadar. Also, historically known as Agena. The IAU              
                       sanctioned official name is Hadar. Measure of 1995.035 made by MAPPIT.  Rbt1999 
                       Interferometric data from SUSI are combined with spectroscopic data to          
                       yield orbital parameters, masses, and distance.                         Dvs2005 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 29.50 +/- 5.38, 23.82, 12.02 Msun, respectively.   Mlk2012 
           VOU  31     AB: Spectroscopic and interferometric measures indicate a multiple              
                       system.                                                                         
14040+1318 BPM 611     [PM2000] 1074837 + [PM2000] 1074832.                                    Gvr2010 
14044+6423 NOI   4     HR 5291 = 11 alp Dra = Thuban.                                                  
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Elst & Nelles (1983).                                                   Est1983 
                       This pair is also a spectroscopic binary.                               XXX2017a
14046-3539 I   941     Many uncertain measures. It appears nearly a revolution has been                
                       completed.                                                                      
14047+1345 BPM 612     [PM2000] 1075186 + [PM2000] 1075177.                                    Gvr2010 
14048+2549 BGH  50     HJL 196.                                                                HJL1986 
14048-3200 LPR   2     Looper et al. (2010) determine NIR spectral types T1+/-1 and T5+/-1.            
                       Distance is estimated at 23pc, separation ~3.9au, orbital period                
                       28-35y. Total masses, for ages 0.5, 1.0, and 5.0 Gyr, are 50, 70, and           
                       80 Mjup, respectively. Mass ratio is 0.80 +/- 0.9, Teff for A and B =           
                       1390 +/- 90 and 1180 +/- 90K. 2MASS component magnitudes are derived            
                       from their MKO component photometry and spectral type estimates, using          
                       transformations from Stephens & Leggett (2004 PASP 116, 9).             Lpr2008 
14050+0157 LDS5807     LDS6290.                                                                        
14056-1804 S   659     B is BD-17@4003.                                                                
                       SHY 642. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
14057+1537 BPM 613     [PM2000] 1075685 + [PM2000] 1075674.                                    Gvr2010 
14060-1304 HWE  30     Spectrum of A composite; F2, A3.                                                
14061-7259 GLI 199     Also known as R   240.                                                          
14064-5943 HD 122879   The classification is from the LSC; however, Garrison et al. (1977              
                       ApJS 35, 111) assign a type B0 Ia.                                      Msn1998a
14067-3622 DUN 253     the Cen = 5 Cen = Menkent. DUN 253AB was originally known as DUN 156.           
                       When the Dunlop pair was added to the IDS (after publication of the             
                       printed volume but before its transfer to USNO) an ordinal number               
                       following the last Dunlop listing was added, despite already being              
                       assigned. As it has been in use for almost half a century, it will not          
                       be changed.                                                                     
14068+5946 LDS2700     B is BD+60@1512.                                                                
14069+1547 LAW  21     AB: SLW 965.                                                                    
14071-6327 HJ 4642     AB: Spectrum composite; G0+A3.                                                  
                       AD: Hipparcos suspected non-single.                                             
14072-5153 RST 681     CPD-51@6574.                                                                    
14075-5742 HJ 4645     B is CPD-57@6501.                                                               
14076+5322 LDS2922     SLW 968.                                                                        
14077-5341 DUN 155     B is CPD-53@5880.                                                               
14077-5738 R   238     First distance? B is CPD-57@6504.                                               
14077-6609 RSS  21     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 
14081-1256 STF1802     A possible SB, no orbit. CfA has mention of RV variability, however.    Tok2014d
14082-4124 KSA 132     Primary is the T-Tauri type variable V1032 Cen = PDS 70. Companion is           
                       a background star.                                                      KsA2014 
14082-5019 CPO 382     CPD-49@6690.                                                                    
14083+4927 H 6 112     H VI 112. 13 Boo. A is the variable CF Boo.                                     
14083+3708 BFR  10     NLTT 36369 + 2MASS J14081969+3708255. Baron et al. (2015) estimate              
                       spectral types M4.0 +/- 0.5 and M7.5 +/- 0.5, distances 55 +33/-21              
                       and 84 +4/-29 pc, masses 0.207-0.272 and 0.087-0.096 Msun.              BFr2015 
14083+2112 STF1804     H N 115.                                                                MEv2010 
14087+3341 HU  742     A premature orbit has been computed.                                    Cou1956 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
14088+7733 BNU   9     4 UMi. A spectroscopic binary, P = 605.8d, now resolved.                        
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Scarfe (1971).                                                          Scf1971 
                       1984.2791: Halbwachs (1981) predicts an angular separation of about     HJL1981 
                       0".03 and the system appears to be at the limit of resolution of the            
                       6-m telescope.                                                          Bnu1986 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Scarfe (1971).                                                          Scf1971 
14089+7316 LDS1783     NLTT 36481/36478                                                        Chm2004 
14089-4328 SIN  88     BC: initially listed incorrectly as AC.                                         
14090-1020 CHR  40     96 Vir.                                                                         
14095+3549 HJ  540     HJL 197.                                                                HJL1986 
14096+7250 STF1822     Some measures previously listed under H V 178.                                  
14096-5130 HJ 4651     A is a spectroscopic binary and may be variable. B is CD-50@8297.               
14097-3955 WG  176     SWR 153.                                                                        
14098+0822 A  1098     BRT2157.                                                                Brt1938 
14103-4459 LDS 476     HIP 69220. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: SHY 257. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
14104+3932 SHY 644     AB: HIP  69227 + HIP  69166.                                                    
           YSC 151     Aa,Ac: YSC 218Aa,Ac.                                                            
14104+2506 12 Boo      d Boo. SB2. Combined spectroscopic/interferometric solution by Boden    Bod2000 
                       et al. (2000), including mass determinations, and other analysis.               
                       P = 9.604565d +- 7.6e-6, T (MJD) = 51237.779. Orbital period was                
                       converted to hours in the orbit catalog to allow full precision in the          
                       available column width.                                                         
                       Combined astrometric/spectroscopic solution by Boden et al. (2005),     Bod2005a
                       including interferometry data from PTI and NPOI. Derive orbital                 
                       parallax of 27.74 +- 0.05 mas, luminosities 7.76 +- 0.35 and 4.69 +-            
                       0.74 Lsun, and masses 1.4160 +-  0.0049 and 1.3740 +- 0.0045 Msun, as           
                       well as effective temperatures, radii, and other physical parameters.           
                       Combined spectroscopic/astrometric solution, based on high-resolution           
                       echelle spectra plus archival PTI visibility measurements.                      
                       Derived masses 1.4109 +/- 0.0028 and 1.3677 +/-0.0028 Msun,                     
                       distance 35.820 +/- 0.057 pc.                                           Knc2010 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.17 +/- 6.34, 3.14, and 1.10 Msun, respectively.             Mlk2012 
           ISO  14     AB is bogus, unresolved (2010.481, dm>5.22 @562nm, dm>5.46 @642nm) by   Hor2011 
                       Horch et al. (2011), also unconfirmed by RoboAO                         Tok2014d
14104+1116 GWP2257     CD: Incorrectly added as AC pair, but not physically associated with            
                       14104+1116 GWP2256AB. WDS designation maintained, but component                 
                       designations updated.                                                           
14105-0240 HLD  17     BAL 230.                                                                        
14107-6229 SNA  36     The 0.7mas companion marginally resolved by PIONIER may correspond to           
                       the P=60d SB1 reported by Gamen et al. (2008, RevMexAA 33, 54), which,          
                       assuming pi=0.5mas and M=20 Msun (Hohle et al. 2010, AN 331, 349), has          
                       a_app = 0.4mas.                                                         Sna2014 
14109+1513 SKF 343     HIP 69281. Aa,Ab is HDS 1989, 0.6".  It is not seen in the V-band               
                       images, too red and faint. Is this a visual multiple system with four           
                       components or a small cluster?                                          Tok2011a
14109+0653 GIC 116     G065-029/G065-030.                                                              
14110+5015 STF1814     NLTT 36518/36516                                                        Chm2004 
                       HJL 198.                                                                HJL1986 
14110+3152 GC 19140    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14110-0240 BU  803     BAL 231.                                                                        
14113-0320 STF1807     BAL 232.                                                                        
14122+6137 LDS2704     NLTT 36592/36597                                                        Chm2004 
14122+4411 STT 278     Only elements P and T have been amended by Starikova (1980) from the    Sta1980a
                       orbit of Heintz (1976).                                                 Hei1976 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.87 +/- 1.55, 2.93, and 1.45 Msun, respectively.             Mlk2012 
14123+0225 HJ 3343     A is the Alpha CVn-type variable CU Vir.                                        
14124+2843 STF1812     AB,C: HJL 199.                                                          HJL1986 
14124+1335 HJ  234     LDS 952.                                                                        
14125+1646 LDS1408     Recognized to be the same as LDS6291 by John Greaves.                   Grv2006b
14128-3522 SWR 155     CPM pair                                                                Skf2004 
14131+5520 STF1820     Two possible solutions by Kiyaeva et al. (1998), based on a 26-year     Kiy1998 
                       long series of photographic data from Pulkovo.                                  
                       A component is SB1 (P=2.87 yr, e=0.75). Spectral types and                      
                       magnitudes are estimated for all components of this triple system.              
                       A: Ren & Fu (2013) calculated an astrometric orbit, combining                   
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Kiyaeva et al. (1998). They derived component masses 0.84 and 0.52      Kiy1998 
                       Msun and an estimated semimajor axis of 57.65 mas.                      Ren2013 
14131-1056 HJ  541     Herschel coordinates 14 04+/- NPD 100 08 (1830). He notes: "very                
                       unequal, L. white, S. blueish".                                                 
14133+1430 BPM 614     [PM2000] 1079457 + [PM2000] 1079464.                                    Gvr2010 
14133-0827 CHR 221     First detected as an occultation binary by Blow et al.                  Blw1982a
14134+0524 STF1813     H N  98.                                                                MEv2010 
14134-3043 LDS5811     BC = LDS5812BC.                                                                 
14135+5147 STF1821     kap Boo = 17 Boo. A is a Delta Scuti-type system. B is a long-period            
                       spectroscopic binary with P = 1791.2d.                                          
                       The 6101- and 6675-yr period solutions for the AB pair by Kiyaeva       Kiy2006 
                       (2006) assumed total system masses of 4.2 and 3.6 Msun, respectively.           
                       P and T for the astrometric Ba,Bb solutions were adopted from the               
                       spectroscopic solution of Bakos (1986, AJ 91, 1416), as was the                 
                       value of e (0.53) in the first solution.                                        
                       H 3  11.                                                                MEv2010 
14138+3059 COU 606     Systemic mass is estimated at 1.8 +/- 0.5 Msun, assuming an Hipparcos           
                       parallax of 17.21 +/- 1.63 mas. The dynamical parallax of 18.3 mas              
                       lies within about 1 sigma of the Hipparcos value.                       Doc2008a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.20 +/- 0.71, 1.51, and 0.55 Msun, respectively.             Mlk2012 
14139+4620 RED  24     M2, spectroscopic distance 31pc. 83" from G0 dwarf HD 124694 = HIP              
                       69518 = 2MASS J14135135+4619304. Hipparcos distance of the brighter             
                       star is 26.2pc.                                                         Red2007a
                       2MASS J14134677+4618227 is possibly a wide companion to HIP 69518 at    Rad2007a
                       83" (Reid et al 2007), but is single in the AstraLux field of view.     Jnn2012 
14141+1258 CHR  41     14 Boo. A spectroscopic binary with P = 726.6d.                                 
14141-5029 BRT 825     CPD-49@6779.                                                                    
14142+5915 STF1827     HJL 200.                                                                HJL1986 
14142-5111 CPO 383     CPD-50@6728.                                                                    
14144-1521 LDS 483     AC: NLTT 36649/36641                                                    Chm2004 
14145-3910 HJ 4663     SWR 156. CPM pair                                                       Skf2004 
14146-6148 HDS1999     Primary is V997 Cen, a Beta Lyr type eclipsing binary, P = 2.4282d.     Zas2012 
14146-7605 HLN  32     Also known as R   242.                                                          
14148+1006 KUI  66     15 Boo.                                                                         
                       Duplicity uncertain. The companion, 3 mags fainter, was not seen on two         
                       other good nights.                                                      WRH1954b
14148-1254 CHR 231     First detected as an occultation binary by Africano.                    Afr1978 
14150-0511 FAR  39     SKF  43.  Primary is white dwarf WD 1412-049.                           Far2006 
14150-5705 HDO 228     A is the variable V795 Cen.                                                     
14150-6142 SNA  37     Aa,Ab: The new pair is marginally resolved at 1.5mas, and possibly              
                       corresponds to the newly-reported SB2 system (Sota at al. 2014, ApJS            
                       211, 10).                                                               Sna2014 
14152+2216 LDS 954     NLTT 36716/36714                                                        Chm2004 
14153+5232 SHY 645     HIP  69650 + HIP  69917.                                                        
14153+0308 STF1819     Hopmann (1945) orbit is not seen but is quoted from Baize's             Hop1945 
                       catalog.                                                                Baz1950a
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.92 +/- 1.08, 2.15, and 1.05 Msun, respectively.  Mlk2012 
           SHY 261     AC: HIP  69653 + HIP  70782.                                                    
14154+2413 LDS4446     NLTT 36733/36730                                                        Chm2004 
14157+1911 HDS2003     = alp Boo = Arcturus. Proper motion of B -1093 -1999.                           
                       Duplicity questioned by Griffin and subsequently retracted by           Grf1998 
                       Soderhjelm & Mignard                                                    Sod1998 
                       1975.624: Disk not clearly resolved at 600 nm but resolved (0".018              
                       +/- 0".004) at 450 nm.                                                  Bla1977a
                       1975.634: Disk resolved (0".018 +/- 0".005) at 500 nm.                  Bla1977a
14158+1018 A  1101     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.58 +/- 0.71, 1.74, and 0.85 Msun, respectively.  Mlk2012 
14161+5643 STF1831     D. Arnold noted considerable overlap of measures for the two multiple   Arn2004a
                       systems STF1831 and 14157+5640STF1830, with STF1831CE = STF1830DA and           
                       STF1831EF = STF1830AB. They have therefore been combined into one WDS           
                       system, maintaining the WDS and most of the component designations for          
                       STF1831. Designation changes are as follows:                                    
                          STF1830AB --> STF1830EF                                                      
                          STF1830AC --> STF1830EG                                                      
                          STF1830AD --> STF1830CE (with quadrant flip)                                 
                          STF1831CE --> STF1830CE                                                      
                          STF1831EF --> STF1830EF.                                                     
                       Finally, the single measures of AD and CD were misidentified, so these          
                       measures were reassigned to the proper components.                              
14161+5010 BDK   8     G 200-28 + SDSS J141659.78+500626.4. Distance 45.1 +1.6/-1.5 pc for             
                       primary, 44 +/- 31 pc for secondary. Estimated age of system 7-12 Gyr.          
                       Mass of secondary estimated at 0.077-0.078 Msun.                        Fah2010 
14162+5122 STFA 26     21 Boo = iot Boo. STTA128. A is a spectroscopic binary and a Delta              
                       Scuti-type variable, P = 0.027d. B is BD+52@1785.                               
                       Struve suspected a close companion to A (1836.28, 149.9deg, 0".3)       StF1837 
                       as did Smyth (1838.19, 195.0deg, 0".5) but this supposed pair           Smy1844 
                       has never been confirmed with larger telescopes.                                
                       AB: H 5   9.                                                            MEv2010 
14162+3235 HZG  10     B is BD+33@2434.                                                                
14163+0605 STF1824     H N  99.                                                                MEv2010 
14164+4605 VIG  17     Optical/physical nature of the faint companion is undefined.            Vig2012 
14164+1348 SOZ   3     BNG   1. Physical separation 75 au at distance ~8pc. CPM pair.          Soz2010 
                       Burgasser et al. (2010) confirmed the companion as a T7.5 dwarf.                
                       Spectral model fits yield Teff = 650 +/- 60K and high surface gravity           
                       and/or subsolar metallicity.                                            Bug2010 
                       Very cool (d/sdL7 + T7.5p) common proper motion pair found by                   
                       cross-matching UKIDSS against SDSS.                                     Bng2010 
14165+3334 HU 1266     Possibly an ambiguous case, although only one solution has been tested.         
14165+2007 STF1825     A is X-ray source. B is possible astrometric pair (Gontcharov &         Gon2002a
                       Kiyaeva 2002)                                                           Tok2014d
14165-5718 BSO  10     AH: H is CPD-56@6216.                                                           
14166-5955 I   366     A is the Mira-type variable R Cen.                                              
14170+3143 DEL   5     LSPM J1417+3142 = NLTT 36838. Law et al (2008) derive a distance of     Law2008 
                       16.1 +3.4/-3.4 pc and a projected separation of 11.2 +2.4/-2.4 au.              
                       Estimated spectral types are M4.5 and M4.5.                                     
                       GJ 3839. Estimated age 300-1000 Myr; masses 0.43 +/- 0.03 and 0.33 +/-          
                       0.03 Msun; a ~7.1 au.                                                   Jnn2014 
14170-3935 WG  179     SWR 157.                                                                        
14171-4810 HJ 4666     B is CD-47@9026.                                                                
14172+6136 STI 763     LDS2709.                                                                        
14174+3245 VYS  13     HDS2009.                                                                        
14174+1330 LDS4452     SLW 989.                                                                        
14178+4845 HJ 2710     C is BD+49@2286.                                                                
14179+1118 GIC 117     G065-042/G065-041.                                                              
14180+3531 A Boo       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Scarfe & Alers (1975).                                                  Scf1975 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Scarfe & Alers (1975).                                                  Scf1975 
14180-0733 BUP 157     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
14182-2731 HDS3407     AD : This pair missed on initial entry into WDS of HDS stars.                   
                       Added 02/26/01.                                                                 
14182-5130 HD 124979   LS 3219. The classification is from McConnell & Bidelman (1976).        Bid1976 
                       Tobin & Kilkenny (1981 MNRAS 194, 937) place the star at 0.7 kpc from           
                       the Galactic plane, so we have included it in the "runaway" group.              
                       Penny (1996) suggests that the star may be a double-lined binary which  Pny1996b
                       needs confirmation since there are only 2 other knowndouble-lined               
                       binaries among the runaway stars (both B-type systems; see Gies &       Gie1986 
                       Bolton 1986).                                                           Msn1998a
14185+1714 BPMA 47     [PM2000] 1082068 + [PM2000] 1081940.                                    Gvr2010 
14187+6915 LDS1788     NLTT 36996/37003                                                        Chm2004 
14188-6342 RSS  22     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 
14189+7314 OSO  55     G239-012. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
14189+5452 CHR 137     Docobo et al. (2010) derive a dynamic parallax of 9.49 +/- 0.20  mas    Doc2010h
                       and a total mass of 3.81 +/- 0.35 Msun.                                         
14189+1812 LDS 956     LDS1415.                                                                        
                       NLTT 36923/36924                                                        Chm2004 
14190+0142 GRV1099     Aka SLW 991.                                                                    
14190-0636 SHY  71     AC: HIP  69962 + HIP  69701.                                                    
14190-2549 BU 1246     Too faint, if real                                                      B__1951a
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
14191-1322 IOT   1     lam Vir. Combined spectroscopic/interferometric solution by Zhao et al          
                       (2007),including data from IOTA array. Derive masses 1.897 +/- 0.016            
                       and 1.721 +/- 0.023 Msun, luminosities 20.84 +/- 0.25 and 12.58 +/-             
                       0.16 Lsun, and distance 53.16 +/- 0.29 pc (pi = 18.81 +/- 0.10 mas).    Zha2007 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.50 +/- 0.22, 4.20, and 2.19 Msun, respectively.             Mlk2012 
                       aka OCC9018. The OCC2010 solution is ambiguous and one is arbitrarily           
                       "T" coded until the true solution is determined.                                
14192+4223 AG  193     HJL 201.                                                                HJL1986 
14193+2421 LDS 957     NLTT 36958/36967                                                        Chm2004 
14193+1300 ENG  51     18 Boo.                                                                         
14195-6838 I   325     B is CPD-68@2106.                                                               
14196-0509 KUI  67     LDS5815.                                                                        
                       BD-04 3665; CPM pair (0.66" in 261deg) with large parallax.             Kui1937a
14198+1154 BPM 615     [PM2000] 1082740 + [PM2000] 1082764.                                    Gvr2010 
14199+6747 STF1840     AB: H N  71.                                                            MEv2010 
14201+3026 SHY 647     HIP  70051 + HIP  70609.                                                        
14202-6105 SNA  38     Aa,Ab: Given the lack of information, one cannot decide whether the             
                       40mas companion is also the SB2 system reported by Sota et al. (2014,           
                       ApJS 211, 10).                                                          Sna2014 
           HD 125206   This "field" object may belong to the "CLUST 3" group of Mel'nik &              
                       Efremov (1995 SvAL 21, 10).                                             Msn1998a
14203+4830 STF1834     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.78 +/- 1.56, 2.58, and 1.07 Msun, respectively.             Mlk2012 
14206-3753 SEE 204     psi Cen. Primary is an Algol-type eclipsing binary, period 38.81252             
                       days (see 2006A&A...456..651B).                                         Zas2011 
14209-1729 MUG  17     A is exoplanet host, P=4.15d, 502d, 3008d. Roell et al. (2012) list     Rol2012 
                       companion at 90", confirmed by Mugrauer (2009).                         Mug2009 
14211+5725 FAR  40     Primary is white dwarf WD 1419+576.                                     Far2006 
14212+4534 KOI-1408    Some weak evidence for a small-separation (<0".1) companion.            Hor2012b
14217+1334 BPM 616     [PM2000] 1083695 + [PM2000] 1083701.                                    Gvr2010 
14218+0355 BAL2861     A is the Mira-type variable AO Vir.                                             
14218-7634 GLI 201     Also known as TOB 323.                                                          
14225-2518 RST5534     Measures discordant by 90@ in 1951.                                             
14226+1159 FMR   2     BC: Companion of B is the star no. 0975-07459414 of USNO-A2.0 catalog.  FMR1999h
14226-0746 STF1833     AB: A=SB? (Desidera et al. 2006 A&A 454, 553)                           Tok2014d
14226-5828 DUN 159     A is a spectroscopic binary.                                                    
14233+1318 LAW   3     Spectral types M5-M6.5 for both components, masses 0.108-0.122 and              
                       0.099-0.109 Msun, distance 33.1 +/- 3.4 pc                              Law2006 
14233+0114 PIN   2     LHS 2907 + WISE J142320.84+011638.0. Pinfield et al. (2012) discovered          
                       a T dwarf companion to BD+01 2920 through a search of the WISE first            
                       data release. Based on images from VISTA and UKIDSS, they determine             
                       the pair share common proper motion. Spectroscopy yields a spectral             
                       type of T8p for the companion.                                          Pin2012 
                       I-band FastCam lucky imaging of the primary in 2010 by Murray et al.            
                       (MNRAS 414, 575,  2011) shows no evidence of a close companion to the           
                       primary (down to 4-5 maggs at 1").                                              
14234+0827 STF1835     A,BC; Mt. Wilson spectral types A1n and F1s.                                    
                       A,BC triple solution (double A-(BC) in HIP).                            Sod1999 
                       A,BC: H 2  38.                                                          MEv2010 
                       RV may be variable.                                                             
                       BC: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.47 +/- 0.42, 2.74, and 2.79 Msun, respectively.  Mlk2012 
14234-1717 LDS4461     NLTT 37151/37150                                                        Chm2004 
14234-2749 TOK 163     HIP 70330. A is SB without orbit (dRV=7.6).                             Nrd2004 
14237-2622 B  2768     CPD-25 5414. van den Bos notes: "has a faint triple north following".   B__1930a
14238-1646 HJ 2713     LDS 487.                                                                        
14240-1948 HJ 2714     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
14241+1115 STF1838     BDS 6833, H III 20 probably same star.                                          
                       HJL 202.                                                                HJL1986 
                       H 3  20.                                                                MEv2010 
14242+4338 LDS5816     LDS6293.                                                                        
                       NLTT 37241/37240                                                        Chm2004 
14244-3535 UC 2752     Aka SKF1499.                                                                    
14245+6015 LDS2710     NLTT 37282/37283                                                        Chm2004 
14246+4750 STF1843     AB: HJL 203.                                                            HJL1986 
14247+0917 ZUC  12     SKF  44.                                                                        
                       Primary is white dwarf PG 1422+095 = GD 165 = CX Boo.                   Zuc1992 
                       SKF  44.                                                                        
                       Primary is L4V brown dwarf; this is prototype of L-dwarf class.         Kir1999 
14248-0251 OSO  57     G124-035. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
14252+5151 STT 580     the Boo = 23 Boo. A is a Delta Scuti-type variable. A = SB?             Tok2014d
14253-1321 HJ  546     BDS 6823 same star.                                                             
14255-1958 BU  225     BC = HDO 138                                                                    
           SHJ 179     AB: H N  80.                                                            MEv2010 
14257+2338 BU 1442     LDS 960. Proper motion of A = +792,-1114; PM of B = +794,-1119 (UCAC2)          
                       AB: SHY  73. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       Epoch-2000 coordinates of F = 1425269+233745, current AF separation             
                       ~3'.9 at 280deg. Proper motion of C -005+000.                                   
                       AC and AF: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
                       AD and AF are the same pair, so were merged. Abetti (1922) was          Abt1922 
                       apparently confused, due to the very large proper motion of A.                  
14258+2217 HJ 2721     B is BD+22@2700.                                                                
14258-3305 PRO 113     Only one star seen; appears to be either a plate flaw or error in               
                       reduction of Perth source catalog.                                      PrO1912 
14259-2108 BHA  17     CPD-20@5922.                                                                    
14259-3713 RST2904     Spectrum: A8/9II/III.                                                           
14260+4213 COU1757     Elements determined by Mante (1998) were also published by the same     Mnt1998b
                       author in Obs. Trav. SAF 52, 44, 2000.                                          
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.03 +/- 0.76, 2.08, and 0.95 Msun, respectively.             Mlk2012 
14260+3422 GIC 118     AB = G178-026/G178-025.                                                         
14260+0714 STT 282     LDS 959.                                                                        
14261-4513 DUN 160     tau 1 Lup. Variable. B is CD-44@9321.                                           
14262-0950 RST3878     TDS9203.                                                                        
14262-4404 SWR 158     CPM pair                                                                Skf2004 
14262-4523 I   402     tau 2 Lup.                                                                      
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.67 +/- 0.76, 4.55, and 3.11 Msun, respectively.             Mlk2012 
14265+1557 CLO   1     Konopacky et al. (2010) derive a distance of 34 +/- 13 pc and a system          
                       mass of 0.11 +0.08/-0.11 Msun.                                          Kon2010 
14265+1459 LDS5818     LDS6294.                                                                        
                       NLTT 37341/37342                                                        Chm2004 
14265-5034 CPO 388     CPD-50@6917.                                                                    
14266+0208 HJ 1254     LDS5819.                                                                        
                       HJL 204.                                                                HJL1986 
14267+1625 A  2069     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.92 +/- 1.69, 2.50, and 1.10 Msun, respectively.             Mlk2012 
14268-0511 HWD   1     AC: Howard et al. (2010) determined that the extremely metal-rich A             
                       component is orbited by a massive planet (M sin 1 = 0.38 Mjup) in a             
                       3.41y, e=0.41 orbit. The C component is an M dwarf, with estimated              
                       mass 0.32 Msun and a projected separation of 33 AY                      Hwd2010 
                       AC: Ginski et al. estimate the mass of C at 0.307 +/- 0.033 Msun.       Gns2012 
14269-6630 RSS  23     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 
14270-0308 LDS4466     LDS6295.                                                                        
14275+7542 HJ 2733     5 UMi.                                                                          
14276+1343 BPM 617     [PM2000] 1086775 + [PM2000] 1086813.                                    Gvr2010 
14277+5347 GIC 119     G200-040/G200-039.                                                              
14278+0007 BAL1172     RST 5386.                                                                       
14278-0140 BAL 555     J 2105.                                                                         
14279+2123 HO  543     HJL 205.                                                                HJL1986 
                       STF3085.                                                                        
14279-0032 GIC 120     G124-043/G124-044.                                                              
14279-1806 FEN  20     J 2662.                                                                         
14280+3546 COU1266     AC: Aka DAM  80.                                                                
14282-0214 STF1846     phi Vir = 105 Vir. A may be a spectroscopic binary.                             
14282-2929 FIN 306     52 Hya.                                                                         
14283+6349 LDS2343     NLTT 37499/37498                                                        Chm2004 
14284-3922 HRG  95     This is the variable star V1005 Cen                                             
14286+2817 STF1850     B is BD+28@2331, and is a spectroscopic binary.                                 
14287-1012 STF1847     B is BD-09@3946.                                                                
                       A measure of A and BD-09@3950: 1907.26, Delta (delta) 190.80".                  
14291+6917 MLR 170     The scattered measures and quadrant ambiguity make determination of             
                       the direction of motion impossible.                                             
14293+0018 SHY 649     AB: HIP  70845 + HIP  70649.                                                    
14294+8049 GC 19630    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14295+3612 HU 1268     A premature orbit has been computed.                                            
14295+1225 BPM 618     [PM2000] 1087737 + [PM2000] 1087751.                                    Gvr2010 
14298+3510 ALI 128     No secondary seen. Apparently typo or plate flaw in AC catalog.                 
14298+3445 LDS4470     SLW1001.                                                                        
14301+4737 COU2387     Also known as HDS2046. This double was first resolved by Couteau, but   Cou1988b
                       placed in the WDS at the wrong coordinate and not matched with HDS2046          
14303-4931 HDO 232     A is a spectroscopic binary, spectrum composite; A1V+B.                         
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
14308+0446 BU 1443     See BDS 6932. Burnham could not find star measured by Madler. No star   Bu_1906 
                       in or near Madler place. B is BD+05@2885.                                       
14308-0839 BUP 158     Proper motion -1272 -236.                                                       
14308-5029 LDS 490     B is CD-49@8796.                                                                
14310+1120 BPM 619     [PM2000] 1088568 + [PM2000] 1088537.                                    Gvr2010 
14310-0548 RST4529     Two orbit solutions by Heintz (1981), but the long-period, circular     Hei1981a
                       orbit is ruled out by speckle observations.                                     
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.89 +/- 0.22, 1.91, and 0.95 Msun, respectively.             Mlk2012 
14313-1538 BU  117     AB = HDO 139                                                                    
                       AB: A = SB? No orbit.                                                   Tok2014d
14314+3430 HU  904     Van Biesbroeck and Fox identify this pair as BD+35@2575, but Hussey     VBs1936 
                       says it is 5.59s following and 4' 46.4" north of that star.             Fox1925 
                       Match with Tycho star at listed precise coordinates is based on the     Hu_1905a
                       assumption that Hussey meant BD+35@2575 is 5.59s following and                  
                       4' 46.4" north of binary, rather than vice versa.                               
14317+0150 AG  195     Heintz believes HJ 5485 is identical; there is no pair in the place     Hei1983a
                       formerly assigned to Herschel's pair.                                           
14318+3022 HJ 2728     rho Boo = 25 Boo                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
14321+3818 BLM   3     Aa,Ab: gam Boo = 27 Boo. A is a Delta Scuti-type system.                        
                       1975.383: Photometric variable star of tentative period 0.29 day;               
                       also a member of a binary system with separation ~33".4 and delta m             
                       ~ 9.27. This observation apparently resolves the brighter primary into          
                       two stars.                                                              BLM1978 
           BU  616     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
14321-2743 SKF1971     Primary is the eclipsing binary V356 Hya.                               Skf2013 
14323+8020 STTA130     B is BD+80@444.                                                                 
14323+2641 A   570     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Martin et al. (1998) derive component masses 1.892 +/- 0.410 and                
                       1.162 +/- 0.257 Msun.                                                   Mig1998 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.57 +/- 0.72, 3.29, and 1.74 Msun, respectively.             Mlk2012 
14324+3138 STF1855     Same as STF1856.                                                                
                       AB: HJL 206.                                                            HJL1986 
                       AB: SEI 536.                                                            Nsn2017b
14325+3442 HJ  554     AB: HJL 207.                                                            HJL1986 
14326-5653 EVS  23     Primary is the Cepheid V Cen.                                           Evs2016a
14327-1246 GLP   3     B is BD-12@4080.                                                                
14329+4126 HJ 1255     B is BD+42@2510.                                                                
14330+0340 HD127742    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14331+5528 LEP  68     NI   33.                                                                        
14331+2154 WOL   1     WSP  14.                                                                        
14343+2424 STTA129     B is BD+25@2797.                                                                
                       H 6  52.                                                                MEv2010 
14345+0540 J  1122     A measure in 1952: 279.2@, 1.4". The 1957 measure may be inaccurate.            
14345-6317 HJ 4683     Spectrum of B: A8/F0.                                                           
14347+2945 STT 582     sig Boo = 28 Boo. Possibly variable.                                            
14349+2510 LDS4481     NLTT 37790/37787                                                        Chm2004 
14350+0907 RUC   8     Multiple system including contact binary CK Boo. Pribulla & Rucinski            
                       (2006) estimate the mass of the contact pair at 2.012 Msun and the      Pbl2006 
                       minimum mass of the wider component at 1.50 Msun.                               
                       Spectral type of resolved companion estimated at M1V.                   Ruc2007 
14350-2336 LUH  10     2MASS J14345819-2335572 + 2MASS J14351087-2333025.                      Luh2012b
14351-6101 B  2338     A is the Cepheid TX Cen.                                                        
14351-7619 GLI 206     Also known as R   247.                                                          
14354-2954 LDS 492     NLTT 37783/37782                                                        Chm2004 
14358+0620 MAD   6     Not found by Burnham.                                                   Bu_1906 
                       The pair was later rediscovered by Soulie (2007) and coordinates        Sle2007 
                       verified in 2009 by colleague Florent Losse.                                    
14360+0945 HZE   1     GJ 3860. Heinze et al. (2010) determine that the new companion is a             
                       background object.                                                      Hze2010 
14363-4615 HDO 236     A is variable.                                                                  
14369+4813 A   347     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.19 +/- 1.18, 2.79, and 1.35 Msun, respectively.             Mlk2012 
14370-1218 GC 19695    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
14372+5214 MLR 682     Also known as TDS 755.                                                          
14372-6201 EVS  24     Primary is the Cepheid V737 Cen.                                        Evs2016a
14373-4608 FIN 318     Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 5.32              
                       +/- 0.20 mas (based on their orbital elements and masses expected from          
                       spectral types) or 4.65 +/- 0.12 mas (based on their elements and               
                       masses given by Tokovinin 2008 MNRAS 389, 925). See paper for                   
                       extensive notes on this system.                                         Doc2013d
14374+1102 AG  345     LDS 965.  HIP 71505. See Allen et al. (2000) for information on         AlC2000 
                       metallicity, age, galactic orbital parameters, etc.                             
14375+4743 TDS9251     Ca-Cb: Initially listed incorrectly as Aa,Ab.                                   
14375+0217 CHR  42     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 2.28 +/- 0.81, 2.95, and 1.10 Msun, respectively.  Mlk2012 
14375-2941 WNO  19     B is CD-29@11196.                                                               
14376+3652 FAR  41     Primary is white dwarf WD 1435+370.                                     Far2006 
14377+1632 BPM 620     [PM2000] 1092020 + [PM2000] 1091979.                                    Gvr2010 
14379-4926 RIZ  11     Rho Lupi.                                                                       
14380-5431 DUN 163     B is CPD-53@6038.                                                               
14382+1402 TOK 406     HIP 71572 is an acceleration binary without RV data. It is found to be          
                       a tight 90-mas pair with a small dm and an estimated period under 10yr          
                       (some motion is seen in one month). Very likely it can be studied as a          
                       double-lined SB.                                                        Tok2015c
14384+3632 ALI 367     Primary is eclipsing binary GK Boo (period 0.47777day).                 Zas2010 
14384-1940 HJ 2734     LDS4484.                                                                        
14390+6417 KON   1     Koenig et al. (2005) calculate combined speckle/spectroscopic orbital   Kng2005 
                       solution and derive masses of 0.9 +/- 0.1 and 0.5 +/- 0.1 Msun for the          
                       primary and secondary, respectively. The primary is the young active            
                       variable EK Dra.                                                                
14395+5154 LDS4487     SLW1014.                                                                        
14395-6812 MLO  58     The primary is slightly variable.                                               
14396-6050 RHD   1     alp Cen = LDS 494. According to R.G. Aitken, this was discovered by     A__1935f
                       Father Richaud while observing a comet at Pondicherry, India, in        Rhd1729 
                       December 1689. P= 79.9y, a = 17.52", motion direct. Due to the                  
                       proximity of the pair and the eccentricity of the system, the                   
                       separation ranges from 2 to 22". AB is also known as Rigil Kentaurus.           
                       Henroteau notes that a first attempt to measure the relative positions  HFC1928 
                       of binary components was made by Father Louis Feuillee in 1709, when    Feu1714 
                       he estimated the position angle and distance for alp Cen.                       
                       Proper motion -3642 +699. The distant companion, Proxima Centauri,              
                       distance 9000" was discovered by Innes. It is the flare star V645 Cen,  I__1905 
                       (mag. 10.7, 2.2 degrees distant, M5Ve). See Kamper & Wesselink (1978).  Kpr1978 
                       The secular changes of a, i, node, and longitude of periastron have             
                       been allowed for; quoted elements are for 2000.0.                               
                       The semi-major axis has been revised (Heintz 1982).                     Hei1982a
                       Difficult for Hipparcos with secondary (= HIP 71681) at edge of         Sod1999 
                       the sensitivity profile. Present parallax preferable to HIP value.              
                       Mass-ratio from Kamper & Wesselink.                                             
                       Pourbaix gives two combined solutions for this resolved SB2, each       Pbx2000b
                       yielding orbital parallaxes and component masses.                       Pbx2002 
                       AB: Additional notes may be found in van den Bos (1931).                B__1931b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.98 +/- 0.03, 2.04, and 1.79 Msun, respectively.  Mlk2012 
                       Powell also measured a more distant component (CPD-60 5485) which is    Pwl1864 
                       obviously non-physical (1860.312, 353.7 deg, 161.5").                           
           LDS 494     AC: alp Cen + Proxima Cen                                                       
                       The Kervella et al. (2017) orbit is based on the following adopted              
                       physical parameters:                                                            
                       alp Cen A: M = 1.1055 +/- 0.0039 Msun  R = 1.2234 +/- 0.0053 Rsun               
                       alp Cen B:     0.9373     0.0033           0.8632     0.0037                    
                       Proxima  :     0.1221     0.0022           0.1542     0.0045            Kev2017 
           SCZ   1     Ca,Cb: Proxima Cen. Not a binary!                                       Tok2014d
14397+1827 ALP  18     2MASSW J1439409+182637                                                          
                       Physical companionship to this ultracool dwarf ruled out based on i-z           
                       and z-J colors, using photometry from SDSS.                             AlP2007 
14397-2643 BU  805     HIP 71682. Linear configuration, C is between AB.                               
                       AB: A possible astrometric pair (Makarov & Kaplan 2005). No SB orbit.   Mkr2005 
                       AC: SHY 262. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
14400-2435 LDS6297     NLTT 38011/38013                                                        Chm2004 
14403+3027 HJL1088     SHY 655. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
14403-4051 HNK   1     Aa,Ab: Member of Sco-Cen Association. Mass of Aa 3.41 +0.53/-0.75Msun;          
                       mass of Ab estimated at 146 +45/-32 Mjup (for age 10 Myr), or                   
                       217 +67/-47 Mjup (for age 20 Myr).                                      Hnk2015 
14403-4548 SEE 209     The primary is slightly variable.                                               
14404+2159 MCA  40     A spectroscopic triple system, with periods 101.6 and 3320 days.                
                       The long-period pair has covered more than half its orbit; the orbit            
                       may be determinable.                                                    Bag1984a
                       Barlow & Scarfe (1991) give combined spectroscopic/speckle              Scf1991 
                       interferometric solution.                                                       
                       1985.5226: This measure was found to give very large residuals to the           
                       orbit of Barlow & Scarfe (1991). Comments in our reduction log note     Scf1991 
                       the measure was marginal, and after reinspection we have determined             
                       this measure was spurious.                                              Hrt1992b
                       Martin et al. (1998) derive component masses 3.344 +/- 1.000 and                
                       3.289 +/- 0.988 Msun.                                                   Mig1998 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 6.55 +/- 1.65, 4.67, and 1.05 Msun, respectively.             Mlk2012 
14405-4240 HJ 4692     A,BC = SWR 159. CPM pair. B component is 0".5 pair                      Skf2004 
14405-5702 LDS 495     HIP 71735. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
14407+1625 STF1864     pi 1 Boo = 29 Boo A. B spectrum A6V.                                            
                       Both components are spectroscopic binaries.                                     
                       Measure of 1927.36 made by triangulation of multiple measures.                  
                       AB: H 3   8.                                                            MEv2010 
14410+5757 STF1872     LDS1417.                                                                        
                       AB: NLTT 38127/38134                                                    Chm2004 
                       AB: HJL 208.                                                            HJL1986 
14411+1344 STF1865     zet Boo = 30 Boo.                                                               
                       Spectral types and masses of components assigned by ten Brummelaar et           
                       al., based on adaptive optics observations.                             TtB2000 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Errors for orbit of Alzner (2007) provided by author (private comm.)    Alz2007 
                       Hipparcos parallax yields a mass sum 7.95 Msun, rather high for a pair          
                       of A0V stars. Increasing parallax by 1 sigma (1.24mas) yields a more            
                       reasonable mass sum of 6.51 Msun, however.                                      
                       Calculated mass sum is 122  +/- 275 Msun, unconstrained.                Mut2010b
                       AB: Additional notes may be found in Fu et al. (1997)                   McA1997 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 5.60 +/- 1.66, 5.20, and 4.48 Msun, respectively.  Mlk2012 
           H 6 104     H VI 104.                                                                       
14414+1857 BFR  11     LSPM J1441+1856 + 2MASS J14412565+1856484. Baron et al. (2015)                  
                       estimate spectral types M6 and L1 +/- 1, distances 56 +37/-10 and               
                       99 +10/-34 pc, masses 0.102-0.133 and 0.072-0.079 Msun.                 BFr2015 
14415+2957 LDS6298     NLTT 38115/38116                                                        Chm2004 
14416-0946 SEF   1     G 124-62 + DENIS-P J144137.2-094558. CPM with the close L1+L1 pair              
                       MEL   8Ba,Bb. Distance to the system 34+/- 7 pc, age 500-850 Myr.       Sef2005a
                       Jameson et al.(2008) confirm the CPM nature of this pair.               Jms2008 
14417+0932 STF1866     Same as STF1868.                                                                
14417+0523 OL  160     Not found by Heintz.                                                    Hei1995 
14419-4723 HDO 238     alp Lup. Variable.                                                              
14421+6116 STF1878     A is the Delta Scuti-type variable DL Dra.                                      
14424+6603 GKI   4     G239-025 = GJ 9492                                                              
                       Primary has spectral type M3.0, secondary late M. At distance of 9.9            
                       +/- 1.2 pc and assuming primary mass of 0.32 +/- 0.15 Msun, the pair            
                       has an estimated orbital period of 370 +/- 100y.                        Gki2004 
14425-6459 DUN 166     alp Cir. Probably variable.                                                     
14426+1929 HU  575     Identification of the ascending node, based on a few Mt. Wilson                 
                       spectra, is uncertain at this small difference in magnitude.            Mlr1952b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 0.99 +/- 0.19, 1.28, and 0.55 Msun, respectively.  Mlk2012 
14427-0558 STF1869     B is BD-05@3935.                                                                
14430+1310 KU   48     AB: HJL 209.                                                            HJL1986 
14431+1803 GIC 121     LDS5223. G135-087/G135-086.                                                     
14432-4110 LDS 500     UC 2829. Identification of LDS pair is uncertain, however.                      
14433+1708 BRT2419     Secondary is brighter than primary                                      Los2005 
14434+5155 SKF1640     A is SB2, P=6.459d                                                      Tok2014d
14435-6258 B  1759     C is variable.                                                                  
14436-0415 JNN 100     The two components resolved by AstraLux have very similar brightnesses          
                       and colors, hence physical companionship is probable, although common           
                       proper motion has not yet been tested for.                              Jnn2012 
14437+6234 STI 773     The 1902 discovery observation is in error, due to an apparent          Vat1926 
                       typographical error in the original AC catalog entry for the                    
                       declination of the B component.                                                 
14441+6106 STF1882     AB: H 3  61.                                                            MEv2010 
14443-2701 B   276     ADS 9359a.                                                                      
14446-2215 LDS4498     NLTT 38244/38248                                                        Chm2004 
14448+0742 STF1873     H 2  82.                                                                MEv2010 
14449-3423 JNN 157     Secondary appears to be a very low mass star just above the hydrogen-           
                       burning limit. Masses are estimated at 1.4 Msun and 95 +64/-40 (based           
                       on intrinsic brightness) or 45 +/- 15 Mjup (based on temperature).      Jnn2012b
14450+2704 STF1877     eps Boo = 36 Boo = Izar. B is a spectroscopic binary.                           
                       Scardia et al. say the quadrant is unambiguous for their 2004 theta     Sca2005a
                       value of 162.9. This may have been a typographical error on their               
                       part, as other observers find the secondary to be in the opposite               
                       quadrant and a large magnitude difference.                                      
                       AB: H 1   1.                                                            MEv2010 
14452-4955 EGN  14     The AB pair bound. Primary is K3, B component probably M2.5-M5.5 with           
                       mass 0.18 +/- 0.03 Msun. The C and E components are background stars,           
                       but with only a single epoch the bound/unbound nature of the AD pair            
                       is unknown. The D component is a close binary                           Egn2007 
14452-5536 DUN 169     The primary is BU Cir, a Beta CMa-type variable. B is CPD-55 6152.              
14453-3609 I   528     Too close, measures uncertain.                                                  
14455+4223 STT 285     A faint star (mag. 12.46, 50") has common proper motion                 Maa1938 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.59 +/- 0.86, 2.70, and 1.17 Msun, respectively.  Mlk2012 
14455-1311 LDS4501     NLTT 38285/38284                                                        Chm2004 
14457+6701 LDS2349     GIC 114. G239-027/G239-028. A typographical error led to the Giclas             
                       pair being originally entered in the WDS as 13463+6658.                         
                       NLTT 38380/38391                                                        Chm2004 
14459+2344 COU 100     Docobo et al. (2010) derive a dynamic parallax of 19.95 +/- 0.30 mas    Doc2010h
                       and a total mass of 1.52 +/- 0.09 Msun.                                         
14460+3329 FAR  42     Primary is white dwarf WD 1443+336.                                     Far2006 
14460-1528 HLD  20     5 Lib.                                                                          
14460-2527 H 3  97     H III 97. 54 Hya.                                                               
14462-2111 FIN 309     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.51 +/- 0.21, 2.38, and 1.02 Msun, respectively.             Mlk2012 
14463+0939 STF1879     Mason et al (1999) period should be 243, not 253 yrs (Alzner,           Msn1999a
                       private comm.)                                                                  
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.73 +/- 0.35, 2.10, and 1.00 Msun, respectively.  Mlk2012 
14464-3346 HDS2082     AB + TOK 407Ba,Bb: HIP 72235B is located at 9" from the primary star            
                       and shares its proper motion (AB = HDS 2082). Pre-discovery                     
                       measurements of this Hipparcos pair were published by Wycoff et al.             
                       (2006 AJ 132, 50). The RV of A may be variable (Latham, 2012, private           
                       communication). The star B turns out to be a 0".4 binary Ba,Bb with             
                       masses of 0.70 and 0.17 Msun estimated from the luminosity. Its period          
                       is on the order of 100yr. The whole system could thus be quadruple.     Tok2015c
                       AB: Primary is SB?                                                      Tok2014d
14464-7847 HJ 4689     B is CPD-78@889.                                                                
14467-6128 EVS  25     Primary is the Cepheid BP Cir.                                          Evs2016a
14471-7329 HJ 4693     B is CPD-72@1571.                                                               
14475-0017 HD 130322   No comoving objects found within separation/magnitude range listed.             
                       However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                       background object.                                                              
14477+2406 HO  263     Suspected double by Hough, but unconfirmed by many other observers;     Ho_1890 
                       duplicity still in doubt.                                                       
14478+1037 BPM 621     [PM2000] 1097755 + [PM2000] 1097751.                                    Gvr2010 
14479-3325 HJ 2744     SWR 160.                                                                        
14482-3647 HJ 4701     LDS 505.                                                                        
14485+2445 COU 304     Primary is EM Boo, Algol-type eclipsing binary, period 2.446228d.       Zas2013 
14485-1720 BU  346     Primary is SB and astrometric binary, P=1724d                           Tok2014d
14489+0557 STF1883     See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.86 +/- 1.15, 2.41, and 1.17 Msun, respectively.             Mlk2012 
14492+1013 A  2983     Two orbit solutions by Eggen (1967). Long-period solution later ruled   Egg1967 
                       out by speckle observations.                                                    
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.58 +/- 0.89, 1.74, and 0.79 Msun, respectively.             Mlk2012 
                       Double lined spectroscopic binary whose orbit generates masses of       Grf2015c
                       0.308 +/- 0.012 and 0.306 +/- 0.011 Msun.                                       
14492-5924 FIN 298     Motion direct.                                                                  
14493-1409 BU  106     mu Lib = 7 Lib                                                                  
                       AC and AD: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
                       AE: There are two other faint stars in the directions of 74.7 and 56.5          
                       deg, respectively, a little farther than E.                             Bu_1894 
14493-2415 H 6 117     H VI 117.                                                                       
14495+5122 STF1889     Both components are spectroscopic binaries.                                     
                       AB: H N 116.                                                            MEv2010 
14496+2356 JMS   4     2MASS J14493784+2355378 + 2MASS J14493550+2357118.                      Jms2008 
14497+4843 STF1890     39 Boo. B is a spectroscopic binary. Spectral types F6V+F5V.                    
                       H 2  79.                                                                MEv2010 
14497-2605 LDS 508     NLTT 38457/38454                                                        Chm2004 
14497-4300 CPO 402     B is CD-42@9693.                                                                
14503+8231 HZE   2     GJ 3876. Heinze et al. (2010) determine that the A and B components             
                       definitely comprise a CPM pair.                                         Hze2010 
14503+2355 POT   1     GJ 564. Both B and C components are determined to be young contracting          
                       brown dwarfs, spectral type dL2, with masses <0.075 and <0.065 Msun,            
                       respectively.                                                           Pot2002 
                       BC: Assuming an Hipparcos distance of 18.18 +/- 0.08 pc, Konopacky et           
                       al. (2010) derive a system mass of 0.109 +/- 0.002 Msun.                Kon2010 
                       BC: Dupuy & Liu (2011) derive a mass sum of 0.1095 +/- 0.0022 Msun,             
                       and a mass ratio of 0.948 +/- 0.005.                                    LiM2011 
                       BC: Malkov et al. (2012) derive dynamical and photometric spectroscopic         
                       masses 0.11 +/- 0.01 and 0.38 Msun, respectively.                       Mlk2012 
                       BC: Dupuy et al. (2009) derive orbital parameters for the BC pair,              
                       which is comprised of a pair of L4 dwarfs. They determine a mass sum            
                       for the pair of 0.109 +/- 0.003 Msun.                                   Dup2009c
14504-6625 FIN 426     Spectrum: G8/K1(IV)+A/F.                                                        
14505-7032 HJ 4697     B is CPD-70@1824.                                                               
14506-0001 STF1885     H 1  78.                                                                MEv2010 
14507+7409 BUP 159     bet UMi = 7 UMi = Kochab                                                        
14509-0810 BRT 551     J 1612.                                                                         
14509-1603 SHJ 186     alp 2 Lib = 9 Lib = Zubenelgenubi. B is BD-15@3965. A is a                      
                       spectroscopic binary.                                                           
           CAB   1     AD: HIP  72622 + HIP  71743.                                            Cab2010 
14510+6718 LDS2351     NLTT 38643/38642                                                        Chm2004 
14510+0943 STF1886     BDS 7052; MAD same star.                                                        
14511+0557 WSP  40     HTP  27.                                                                        
14511-3706 I   529     A premature orbit has been computed.                                            
14511-6153 JSP 640     CD-61@4558                                                                      
14512+3107 BWL  39     AE: Colors and/or astrometry are inconsistent with a late-type common           
                       proper motion companion based on visual inspection of the field from            
                       2MASS, SDSS, DSS1, and/or DSS2. Primary is G 166-49.                    Bwl2015 
14513-1700 HU 1270     BC: North and fainter of a 30" pair; ADS is not clear on this point.    B__1949c
14514+1906 STF1888     xi Boo = 37 Boo = EO Boo.                                                       
                       Three orbit solutions by Wielen (1962), only orbit #3 is now in the     Wln1962 
                       orbit catalog. The RV difference is small and renders identification            
                       of the ascending node uncertain.                                                
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: H 2  18.                                                            MEv2010 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.59 +/- 0.21, 1.60, and 1.56 Msun, respectively.  Mlk2012 
                       AD: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
14516-4335 FIN 319     omi Lup                                                                         
14517-3053 H N  48     B is CD-30@11767.                                                               
14517-7328 GLI 210     SWR 161. CPM pair                                                       Skf2004 
14519+5147 LDS4513     NLTT 38649/38650                                                        Chm2004 
14522+1638 FAR  16     Primary is white dwarf WD 1449+168.                                     Far2005b
14523-4455 DON 689     CPD-44@7016.                                                                    
14524+1757 A  2071     EQ Boo, Algol (EA) type eclipsing binary, P = 5.43536 d.                Zas2011 
14525+1844 BU   31     HIP 72764.                                                                      
                       AB: A or B are SB? Trapezium (2" and 8")?                               Tok2014d
14525+0007 GIC 122     G066-035/G066-036.                                                              
14526-1151 LDS 511     B is BD-11@3820.                                                                
14526-6349 HDS 2100    Primary is the Cepheid AX Cir. The wide HDS pair has a spectroscopic            
                       orbit, P=6532d, e=0.19 (Evans 2000 AJ 119, 3050).  Gallenne et al.              
                       resolved the primary into a 20mas pair, and find a minimum mass for             
                       Aa+Ab > 9.7 +/- 0.6 Msun.                                               GaA2014 
                       Masses are 5.2 and 5.0 Msun. Estimated period = 17.9y,                          
                       a = 14.8au = 0.03".                                                     Evs2013 
14527+0746 HLD 120     AB. Schlimmer (2008) published linear elements rather similar to those  Smr2008 
                       in the Rectilinear Elements Catalog: x = -1.1407, y  = -0.9315,                 
                       To = 2229.42  +/- 1.74, sep=    1.473 +/- 0.2, PA =  309.24  +/- 0.5            
14533-5220 CPO 403     CPD-51@8545.                                                                    
14534+1909 GC 20037    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Beavers & Salzer (1983).                                                Bvr1983 
14534+1542 STT 288     CfA: A or B have variable RV?                                           Tok2014d
14535-4637 B  2774     A: S Lup                                                                        
                       B: X Lup                                                                        
14540+2335 REU   2     Additional notes may be found in Wilson (1954) and Wilson (1955).       WRH1955 
14540-6333 RST9005     Previously known as RST 730a.                                                   
14543+0312 BAL2401     May be the same as HJ 5491.                                             Dam2010 
14543-3737 CD-37 9777  Listed as possibly resolved by White et al. (1991), but no separation   Whi1991 
                       or position angle given.                                                        
14544-3409 I   226     Wagner et al. (2016) imaged a Jovian exoplanet orbiting the primary at          
                       a distance of ~80au. They also resolved the Innes B component into a            
                       70mas pair, which they designate as B and C. However, the C component           
                       designation is already in use for Innes' 30" companion. Also, their B           
                       designation redefines B from the photocenter of the previously                  
                       unresolved close stellar pair to one component of that pair. We have            
                       therefore designated the two stars as Ba and Bb, in keeping with our            
                       usual hierarchical designation scheme.                                          
                       Wagner et al. derive the following parameters for system components:            
                                          Aa        Ab             Ba         Bb                       
                          --------------------------------------------------------                     
                          Spectral type   A1V       T2–T4          G          K                .     
                          Mass (Msun)     1.82      4+/-1 Mjup     0.96       0.6                      
                          Teff (K)        9300      850 +/- 50     5700       4400             WgK2016 
14545+1606 FRT   1     AB: The companion is of spectral type dM8.5.e. The measure was made in          
                       the infrared.                                                                   
           MEL   2     GJ 569 Ba,Bb. Lane et al. (2001) paper also includes spectroscopic      Lne2001 
                       information and discussion of spectral type, masses, evolutionary               
                       state, etc.                                                                     
                       Zapatero Osorio et al. (2004) give combined spectroscopic/astrometric   Oso2004b
                       solution, yielding masses 0.071 +/- 0.011 and 0.054 +/- 0.011 Msun.             
                       Total system mass is 0.125 +/- 0.007 Msun.                              Smn2006 
                       Incorrectly listed as MEL   1.                                                  
                       Ba,Bb: GJ 569. Assuming an Hipparcos distance of 9.81 +/- 0.16 pc,              
                       Konopacky et al. (2010) derive a system mass of 0.126 +/- 0.007 Msun.   Kon2010 
                       Dupuy et al. (2010) determine system mass 0.140 +0.009/-0.008 Msun;             
                       spectral types are  M8.5 +/- 0.5 and M9.0 +/- 0.5.                      LiM2010b
14546-3318 BU  347     CPD-32@3746.                                                                    
14550+4301 OSO  60     G178-056. Not a common proper motion pair, based on astrometry and              
                       color                                                                   Oso2004 
14551-0906 TOK 164     HIP 72998.                                                              Tok2011a
14557-3351 HO  390     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
14558+3939 A  1627     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.37 +/- 0.49, 2.64, and 1.45 Msun, respectively.             Mlk2012 
14562+1745 HDS2108     AB: Cvetkovic et al. (2016) estimate spectral types K5 and K6, masses           
                       0.65 and 0.60 Msun. Dynamical parallax is 16.63 +/- 1.12 mas.           Cve2016b
           GII  61     AC: GII  85AC.                                                                  
14565+5923 SHY 661     AC: HIP  73105 + HIP  73730.                                                    
           SHY 661     CD: HIP  73730 + HIP  72389.                                                    
14565+1755 LDS4516     Also known as LHS3001/2. Parallax = 56.41 +/- 0.95 mas.                 Rdl2010 
14565-3438 B  2778     AB,C: Star C (approx. mag. 14, 6") is probably physical.                        
           SEE 215     AB,D: CPD-34@6262.                                                              
14565-4753 HJ 4715     The primary is a spectroscopic binary.                                          
14566-1406 HJ  561     B is BD-13@4022.                                                                
14567-6247 FIN 372     the Cir. One component is variable.                                             
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 39.70 +/- 16.09, 22.40, and 5.75 Msun, respectively.          Mlk2012 
14568+7454 S   666     8 UMi. B is BD+75@549.                                                          
14568+5235 LDS4517     Assuming the current identification is correct, it appears Luyten's             
                       separation should have been 230" rather than his published 330". The            
                       distance value has been adjusted accordingly. (WIH, May 2008)                   
14568-7029 R   253     Also known as WFC 158.                                                          
14571+3529 HJ  243     Same as STT 290.                                                                
14574+8529 BU  353     AB: TDS9351.                                                                    
           MLR 342     AC: 14574+8530PKO  12. LDS1808.                                                 
                       AC: The discovery measure by Muller was corrected in one of his later   Mlr1973a
                       papers. Originally 15028+8532 MLR 342 until association with                    
                       14574+8529 noticed.                                                     Mlr1978b
14575+3124 HDS2112     Proper motion of B -695 -1160.                                                  
14575-2125 H N  28     AB: LDS 514. B is BD-20@4123.                                                   
                       AB: NLTT 38872/38871                                                    Chm2004 
                       Proper motion of A +1034.13 -1725.45, B +987.02 -1666.69.                       
                       B is a spectroscopic binary, P = 308d.                                          
                       Statistically different parallax for the components indicates they are          
                       non-physical.                                                                   
                       Hipparcos triple solution together with A (= HIP 73184). P,T,e,         Duq1988 
                       omega, and q fixed from Duquennoy & Mayor (1988), cf orbit in           Mar1990 
                       Mariotti et al. (1990).  Poor Hipparcos solution.                       Sod1999 
                       Strand (1943) suspects a perturbation with P = 2.2y, a = 0".020,        Str1943 
                       and Omega = 30 deg.                                                             
                       Hyperbolic orbit by Hopmann (1967).                                     Hop1967 
                       sigma = areal constant in the true orbit = 2.540 arcsec^2/yr                    
                       q = periastron distance in the true orbit = 20".388                             
                       All hyperbolic orbits rejected from Fourth Orbit Catalog                Wor1983 
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       AF: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       Ba,Bb: Erroneously entered as BC, although C component is a very wide           
                       companion.                                                                      
                       Ba,Bb: Combined solution (spectroscopic/visual/parallax) by Forveille   Frv1999 
                       at al. (1999) for this low-mass interferometric SB2. P = 308.884 +/-            
                       0.004 days, T0 = JD2450270.220 +/- 0.011. Accurate masses are                   
                       determined for these  M dwarfs, as well as J, H, K, and L magnitudes.           
                       1987.455, 1987.756, 1988.312, 1988.499: Vector separations from the 1D          
                       data are combined to give 2D theta and rho values for these 4 dates.    Mar1990 
14575-2914 UC 2880     Spurious pair - primary has zero motion, and secondary is irresolved    Skf2013 
                       pair also with zero motion.                                                     
14576+6556 RR UMi      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Batten & Fletcher (1986).                                               Bte1986 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by Batten &           
                       Fletcher (1986).                                                        Bte1986 
14576-0010 H 6  51     1 Ser. H VI 51. Erroneously called 2 Ser.                               Bu_1875 
14579+2953 LDS5827     LDS6299.                                                                        
                       NLTT 38930/38926                                                        Chm2004 
14580-6333 HJ 4714     B is CPD-63@3460, spectrum B8/A0III/IV.                                         
14581-4852 WSI  80     The 14.9 yr SB1 orbit is mentioned by Raghavan et al. (2010).           Rag2010 
                                                                                               Tok2012a
14581-6317 LDS 856     The same as LDS6300. Determined by Richard Jaworski.                            
14582-3142 LDS5826     LDS6301.                                                                        
14583+1702 BPM 622     [PM2000] 1103818 + [PM2000] 1103757.                                    Gvr2010 
14584+4403 STF1896     AB: Radial velocity variations, based on 10 years of monitoring,                
                       indicate the presence of a giant planet orbiting the B component, with          
                       P = 1544 +/- 34d, a = 2.62 +/- 0.04 au. M sin i = 1.49 +/- 0.09 Mjup.           
                       The primary is an SB in an eccentric orbit with period 25-30 y; mass            
                       of Ab 0.5-0.6 Msun. No companions were detected by AO imaging.          Des2011 
14585+1024 LIM   5     Liu et al. (2011) use IR imaging to determine the components are                
                       likely physical, and determine the distance to the system at 23.1 +/-           
                       2.4pc. The orbital period is estimated at 20-35y. Spectral type of the          
                       primary is T9.5, that of the secondary is >T10, and possibly the first          
                       member of spectral type Y. Mass estimates are strongly dependent on             
                       age: for ages < 0.5Gyr the masses are <9 and <4 Mjup; for ages >2 Gyr           
                       these increase to >20 and >10 Mjup.                                     LiM2011 
                       Liu et al. (2012) derive near-IR spectral types of T9 +/- 0.5 and Y0            
                       +/- 0.5. At a derived photometric distance of 31.9 +/- 2.5 pc, the              
                       two stars are separated by 3.5 +/- 0.3 au.                              LiM2012 
14585-2843 TOK  30     Visual pair has estimated period 175,000y; primary is 14d SB1.          Tok2006 
14585-4726 CPO  62     B is CD-46@9704.                                                                
14587-2739 BU  239     59 Hya. Alternative spectra:; A4V+A6V.                                          
                       1976.474: The observed separation is much larger than that derived              
                       from the elements given by Mourao (1965), which gives a period of       Mro1965b
                       339.3 yr. These elements yield a total mass of 13.65 Msun, which seems          
                       too large for a pair of A5 stars.                                       BLM1978 
14588+3551 COU1136     Docobo et al. (2010) derive a dynamic parallax of 8.68 +/- 0.50 mas     Doc2010h
                       and a total mass of 1.96 +/- 1.04 Msun.                                         
14589+2238 HU  906     TDS9356.                                                                        
14589-1109 STF1894     18 Lib.                                                                         
                       AB: H 4  56.                                                            MEv2010 
14592+0649 HJ 1263     AC = LDS 971.                                                                   
14592-4206 I  1260     kap Cen. A spectroscopic binary and variable star.                              
14593+4649 COU1760     One component is ET Boo, a beta Lyr eclipsing binary.                   Zas2009 
14594+1530 BPM 623     [PM2000] 1104464 + [PM2000] 1104440.                                    Gvr2010 
14595+4528 DAM  30     SHY 264. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
14595+0851 DAY   2     LSPM J1459+0851 + ULAS J1459+0857. Primary is a cool hydrogen-rich              
                       white dwarf, mass 0.585 Msun. Secondary is a T dwarf (T4.5 +/- 0.5),            
                       distance 43-69pc, mass 0.060-0.075 Msun, depending on model.            Day2011 
14596+5352 SHJ 191     STTA132 = H N  63. B is BD+54@1724.                                             
14597+3506 HJ  562     Also known as STF1900.                                                          
14597-7831 HJ 4703     Primary is astrometric binary?                                          Tok2014d
14598-2201 Ci 18,1988  Alden (1938) orbit rejected from Fourth Orbit Catalog                   Ald1938b
                       ("not confirmed by subsequent observations")                            Wor1983