17002-2459 EHR  14     Aa and Ab appear to be comoving, but B component is a background star.  Ehr2010 
                       Primary is 26 Oph.                                                              
17003+3056 ISO   3     eps Her = 58 Her. Spectroscopic binary, P = 4.02d.                              
17003-7612 GLI 232     Spectrum of B: A8/F0.                                                           
17004-4839 SEE 316     Spectrum composite; G8-K0III+G.                                                 
17005+0635 CHR  59     A spectroscopic binary.                                                         
17011+3016 FAR  19     Primary is white dwarf WD 1659+303.                                     Far2005b
17011-0413 ENG  59     30 Oph.                                                                         
17012-3812 SNA  62     A 22.4d SB1, the SB is probably too tight, so not resolved by PIONIER.          
                       Faint companions at 2.0" and 3.4" are deteced in the NACO FOV.          Sna2014 
17013-2808 B   326     Retrograde motion.                                                              
17014+3754 HJ  263     A pair of 12th magnitude stars in field.                                        
17014+3329 BU 1542     Secondary is galaxy IC 4638.                                                    
17016+1457 H 4 122     H IV 122. STF2115. A is the Alpha CVn-type variable V451 Her.                   
17017-2542 HJ 1297     J 1734.                                                                         
17018+1746 BPM 673     [PM2000] 1218945 + [PM2000] 1219146.                                    Gvr2010 
17020+4507 GRV1224     SLW1202.                                                                        
17020+0827 STF2114     A spectroscopic binary.                                                         
17021+0713 STF2113     The AC and AD components which were with this are actually associated           
                       with STF2103.                                                                   
17024-1154 STF3108     B is BD-11@4281.                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
17026-5504 HJ 4905     A is the semiregular variable T Ara. B is CPD-54@7976.                          
17031-5314 HDO 263     eps 2 Ara. Duplicity doubtful.                                                  
           SKF 103     Identified as a double but not measured by Wegner.                      Wgn1973 
                       AC: GJ 2125. C is DA3.2, mass 0.65. Mass(A)=1.41 (Holberg et al. 2013)  Hbg2013 
17031-5833 I   997     Composite-like spectrum: A3/5V+K0III.                                           
17033+5935 STF2128     LDS1437. Mt. Wilson spectral types K5 and M0.                                   
                       NLTT 44134/44135                                                        Chm2004 
                       HJL 243.                                                                HJL1986 
17036+6948 A  1146     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.64 +/- 1.51, 2.42, and 1.20 Msun, respectively.             Mlk2012 
17039+3212 DAE   6     NLTT 44114 = LP 331-57                                                          
                       Daemgen et al. (2007) derive a distance of 18.0 +/- 1.2 pc, separation  Dae2007 
                       of 20.3 +/- 1.4 au, and predicted orbital period of 143 yr. Spectral            
                       types are M2.0 +/- 0.5 and M4.0 +/- 0.5; masses are 0.46 +/-0.02 and            
                       0.22 +0.09/-0.06 Msun.                                                          
17039+1941 BU  822     AB: The Brt1939a measure was initially mis-identified with 17047+1936           
                       PRY   2AB - see note for 17047+1936PRY   2 AB.  The A component is a            
                       spectroscopic binary.                                                           
                       AC: See note for 17047+1936FOX 281 AC.                                          
17039-1956 RST3065     CPD-19@6092.                                                                    
17039-3751 V884 Sco    This is a massive X-ray binary with a neutron star companion.  The      HIP1997a
                       ellipsoidal variation is portrayed in a recent Hipparcos light curve.   Msn1998a
17040-5105 DUN 212     B is CD-50@10977.                                                               
17044+1330 BPM 674     [PM2000] 1222616 + [PM2000] 1222740.                                    Gvr2010 
17046-3800 B   890     CPD-37@6897.                                                                    
17047+1936 PRY   2     AB: The measure was initially mis-identified with the 17039+1941        Fox1925 
                       BU  822AB pair. Due to their similarity in magnitudes, position angle           
                       and separation, there may still be some identification problems in              
                       measures of these two AB systems.                                               
           FOX 281     AC: The Fox, Worley, and Comellas measures were initially               Fox1925 
                       mis-identified with the 17039+1941BU  822AC pair.  This was probably    Wor1967a
                       due to the proximity of these two systems as well as the similarity of  Cll2003 
                       the AB pairs.  The C components of these two systems are also similar           
                       in magnitude and separation, although very different in position angle          
17048+4848 HR 6363     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1991).                                                         Grf1991 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Griffin (1991).                                                         Grf1991 
17048+2805 STF2120     AB: H 3  89.                                                            MEv2010 
17048-3753 HJ 4915     Spectral type K?                                                                
17050-0504 LDS 585     LDS6317. AB: Wolf 531. B is BD-04@4226. Proper motion of A -920,-1138;          
                       PM of B -915,-1130 (UCAC2). Components of this system all have                  
                       common proper motion and common radial velocity                         Egg1950 
                       HIP 83591. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: SHY  85. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
17050-5122 RST5596     CPD-51@10149.                                                                   
17053+5428 STF2130     mu Dra.                                                                 Fat1941 
                       Small motions with 3 or 6 yr periods in one of the components have              
                       been suspected, but from the positional and RV observations Heintz              
                       finds no evidence for them, and points out that the O-C residuals               
                       would be increased by the hypothetical body.                                    
                       AB: H 2  13.                                                            MEv2010 
                       AB: Additional notes may be found in Simonov (1937).                    Smw1937 
                       AB: Prieur et al. (2012) derive a dynamical parallax of 36.3 mas and            
                       (using their orbital elements and the revised Hipparcos parallax of             
                       van Leeuwen 2007 A&A 474, 653) a total mass 2.8 +/- 0.5 Msun.           Pru2012 
                       AB: Low-grade SB orbit for Ba,Bb (P=2270d, K1=2.8km/s), needs           Pbx2004 
                       confirmation (SB9)                                                      Tok2014d
           BU 1088     AC: Star C (mag 13, 13.4" from the center of AB) is in slow retrograde          
                       motion; Cf. Heintz (1966). Mt. Wilson spectral types F5s.               Hei1966 
17054+4803 SDK   1     White dwarf pair = WD 1704+48 0942+24 = EGGR 576/577                    Grn1986 
17054+1244 H 5 133     H V 133. 60 Her.                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
17054-3346 WNO   5     Spectral type of B may be M.                                                    
                       AB + TOK 413Aa,Ab: The RV of HIP 83612 varies by 52km/s (GCS). It is            
                       a very close pair with an estimated period of ~1.5yr, and the measure           
                       near the diffraction limit derived from the elongated power spectrum            
                       is tentative. The Hipparcos parallax is likely biased by the binary.            
                       The visual component B = HIP 83609 (AB = WNO 5) at 25" is optical.      Tok2015c
17055+1033 BU  357     V2626 Oph, an Algol-type eclipsing binary, period 10.87424.             Zas2011 
17056-4106 HLN  41     CPD.                                                                            
17061-2635 EVS  29     Primary is the Cepheid BF Oph.                                          Evs2016a
17062+6438 GIC 146     LDS2730. G240-044/G240-045.                                                     
17064-6829 SWR 214     CPM pair                                                                Skf2004 
17065-0236 STF3110     Also known as BAL 572.                                                          
17065-3527 B   894     This "field" object may belong to the "CLUST 4 " groupof Mel'nik &              
                       Efremov (1995 SvAL 21, 10). An ellipsoidal variation is present in the  HIP1997a
                       Hipparcos data with an unusually long period of 16.11 d.                Msn1998a
           SNA  63     The primary is V1074 Sco, a pulsating variable star and 16.1d EB                
                       (Mason et al. 1998). We do not detect the 2.8" companion at dI=6.3mag,  Msn1998a
                       but do report a 6.7" companion at dKs = 5.9mag.                         Sna2014 
17066+1727 BAR  42     Also known as TDT 215.                                                          
17066+0039 BU  823     AB: Orbits of AB and Ba,Bb may be almost co-planar.                     Tok2014d
17069+2254 KUI 123     Ross 862. Aka KUI  77.                                                          
17070+0648 STF2123     LDS 988.                                                                        
                       HJL 244.                                                                HJL1986 
17073+6440 ALP  19     2MASSW J1707183+643933                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17074-0558 BUG   5     2MASS J17072343-0558249                                                         
                       Noted as binary by Burgasser et al. (2004).                             Bug2004 
                       Spectral types M9 and L3, masses 0.072-0.085 and 0.064-0.077 Msun       McE2006 
17074-3405 V455 Sco    Symbiotic star, spectral type M6.5. Fekel et al. (2008) orbit is a      Fek2008 
                       combined spectroscopic/spectropolarimetric solution. Estimated value            
                       for a" based on their a sin i, i, and estimated distance of 4.3 kpc.            
17075+3810 COU1291     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.39 +/- 0.87, 2.43, and 0.95 Msun, respectively.             Mlk2012 
17075+3557 HJ  264     C component is A component of HU 1176.                                          
17077+0722 YSC  62     GJ 1210. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.06 and 0.13            
                       +/- 0.03 Msun; a ~5.6 au.                                               Jnn2014 
17080+3556 HU 1176     Van de Kamp & Moore point out that Eggen's orbit yields a mass sum      Kam1966 
                       of 52.5, 'an impossible figure'.                                        Egg1945 
                       The speckle observations now resolve the former ambiguity.                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hartkopf et al. (1989).                                                 Hrt1989 
                       Calculated mass sum is 3.32 +/- 0.39 Msun. Spectral types are early A           
                       or F, but spectral class has been reported as either dwarf or giant.            
                       This total mass is more consistent with dwarf stars.                    Mut2010b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.09 +/- 0.14, 3.33, and 1.82 Msun, respectively.  Mlk2012 
17081+3549 BU 1456     This is the same as BU 1455. AC and AD were previously listed as                
                       Aa and Ab, respectively, for that pair. Identical nature noted by               
                       Friedrich Damm.                                                                 
17082-0105 A  1145     The primary is an SB; the observed RV range is 55 km/s.                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.23 +/- 1.93, 3.64, and 3.48 Msun, respectively.             Mlk2012 
17082-3500 SNA  64     The object is a 28.6d SB1, but the SB is too tight, so not resolved by          
                       PIONIER.                                                                Sna2014 
           HD 154643   LS 3941. This "field" object may belong to the "CLUST 4 " group of              
                       Mel'nik & Efremov (1995 SvAL 21, 10).                                           
                       The classification is from Garrison et al. (1977 ApJS 35, 111).         Msn1998a
17084+1738 BPM 675     [PM2000] 1228900 + [PM2000] 1228757.                                    Gvr2010 
17085-3639 EGN  20     System is close to galactic plane, so found to have 12 companion                
                       candidates. The B component is physical, colors are compatible with an          
                       M1.5-M4.5 spectral type and mass 0.27 +/- 0.02 Msun.  The C component           
                       is unbound, and the F component is likely unrelated as well. Single             
                       epoch observations, so nature of D, G, H, I, J, K components unknown.           
                       Nature of E and M are also inconclusive.                                Egn2007 
17088+6543 STA   1     zet Dra = 22 Dra. A premature orbit has been computed.                          
                       Martin et al. (1998) derive component masses 5.940 +/- 1.134 and                
                       3.645 +/- 0.770 Msun.                                                   Mig1998 
17091-3753 B   896     CPD-37@6976.                                                                    
17093+2244 OSO  76     G170-021. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
17096+4047 MCA  45     The equinox-1900 position was incorrectly given as 17093+4054 by                
                       McAlister et al. (1983).                                                McA1983 
                       A: Ren & Fu (2013) calculated an astrometric orbit, combining           Ren2013 
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Griffin (1978).                                                         Grf1978a
17097+3021 STF2131     B is BD+30@2938.                                                                
17098+6821 LDS1438     NLTT 44344/44348                                                        Chm2004 
17098+0804 OSO  77     G139-016. None of the components share a common proper motion, based            
                       on color and comparison with POSS2 red plates                           Oso2004 
17098-1031 TOK 414     HIP 83962 = HR 6375 has a variable RV according to the GCS, while               
                       Gorynya (2013, private communication) detected double lines. It is              
                       resolved tentatively at 33mas with dy=1.8 mag (the 5-ms exposure makes          
                       it unlikely that the asymmetry is caused by vibrations). The                    
                       separation corresponds to an orbital period on the order of 1yr, which          
                       could bias the Hipparcos parallax.  However, Eggleton & Tokovinin               
                       (2008 MNRAS 389, 869) consider the star as single. The new pair was             
                       not resolved in 2014.3, presumably it became closer.                    Tok2015c
17099-8219 HJ 4884     B is CPD-82@701.                                                                
17102+5430 STF2138     B is BD+54@1862.                                                                
                       HJL 245.                                                                HJL1986 
           SHY  89     AC: HIP  83988 + HIP  86141.                                                    
           SHY  89     BC: HIP  83996 + HIP  86141.                                                    
17104+2107 ALP  20     2MASSW J1710255+210715                                                          
                       Physical companionship to this ultracool dwarf ruled out based on i-z           
                       and z-J colors, using photometry from SDSS.                             AlP2007 
17104-1544 BU 1118     eta Oph = 35 Oph = Sabik.                                                       
                       Smyth notes an additional wide companion (1833.61, 260.5deg, 269")      Smy1844 
                       Measure of 1989.388 made by MAPPIT. This measure had an identification  Han1989 
                       error, position error, or misprint in the publication, which has been           
                       corrected. Measure of 1990.37 also made by MAPPIT.                      Rbt1991 
                       Difficult a/e correlation, needs 20 more years of speckle observations  Sod1999 
                       Spectral types and masses of components assigned by ten Brummelaar      TtB2000 
                       et al.                                                                          
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 7.05 +/- 0.51, 3.61, and 4.58 Msun, respectively.  Mlk2012 
17104-1611 FOX 198     Also known as ARA  86.                                                          
17106-1617 KNP   5     The binary at this position, formerly known as FOX 198, is actually of  Fox1915 
                       a different pair first resolved by Knipe. The FOX 198 pair, also known  Knp1965 
                       as ARA  86, is at 17104-1611.                                                   
17107+1427 BPM 676     [PM2000] 1232570 + [PM2000] 1232441.                                    Gvr2010 
17107-4433 I  1312     Spectrum composite; G8-K0III+G.                                                 
17108-6021 B  1846     Spectrum: G8/K0III+A/F.                                                         
17111+3501 LIM   6     Liu et al. (2012) derive near-IR spectral types of T8 +/- 0.5 and T9.5          
                       +/- 0.5. At a derived photometric distance of 19 +/- 3 pc, the two              
                       stars are separated by 15 +/- 2 au. Various evolutionary models yield           
                       masses of 19-23 Mjup for the primary, 8.1-10.7 Mjup for the secondary.  LiM2012 
17111+2414 SHY 713     HIP  84054 + HIP  84070. Primary is V620 Her.                                   
17111+1739 BPM 677     [PM2000] 1233246 + [PM2000] 1233145.                                    Gvr2010 
17113+1246 JNN 152     2MASS J17111769+1245408 and J17111841+1245080, both from the Riaz et    Ria2006 
                       al. (2006) sample, are separated by only 34" and have comparable                
                       estimated distances (69 and 82 pc), as well as similar proper motions   Rsr2010 
                       (e.g. Roser et al. 2010), and thus likely form a physical pair.         Jnn2012 
17113-5641 HD 154857   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                       candidate within separation/magnitude range listed. However,                    
                       further observations are required for verification                              
17115-1630 HU  169     Additional notes may be found in Docobo (1998).                         Doc1998f
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.86 +/- 1.84, 3.07, and 1.91 Msun, respectively.             Mlk2012 
17118+4029 RDN   1     Common proper motion pair G 203-50 + 2MASS J17114559+4028578.                   
                       Spectral types M4.5 + L5, Teff 3114 +/- 115 and 1700 +210/-250 K,               
                       masses 0.146 +- 0.031 and 0.066 +0.008/-0.015 Msun.                             
                       Distance = 21.2 +/- 3.9 pc.                                             Rdn2008 
17118+2232 ALP  21     2MASSI J1711457+223204                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17119-0151 LPM 629     Poor Hipparcos solution.                                                Sod1999 
                       Malkov et al. (2012) derive dynamical and photometric masses of                 
                       0.31 +/- 0.14 and 0.74 Msun, respectively.                              Mlk2012 
17120+3158 LOS   2     Discovered while observing GYL   5. A component is GSC 2595 1004,               
                       B = GSC 2595 956. B component magnitude estimated at 13.3.                      
17121+4540 KUI  79     Proper motion of A +257 -1565.                                                  
                       Poor Hipparcos solution.                                                Sod1999 
                       AB: Martin et al. (1998) derive component masses 0.379 +/- 0.035 and            
                       0.369 +/- 0.035 Msun.                                                   Mig1998 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 0.56 +/- 0.05, 0.68, and 0.65 Msun, respectively.  Mlk2012 
17125+6918 GC 23290    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                       Spectroscopic solution to these astrometric pairs given by Griffin      Grf2013a
                       (2013). Periods match "tolerably well," other common elements less so.          
17125+1035 B  2826     37 Oph.                                                                         
17129+4220 BUP 176     Proper motion of A -1015.19 -354.54. B: -004.6 -009.0                           
17129+2317 POU3263     Aka POU3259.                                                                    
17129-0508 SCE   1     GJ 660.1 = GJ 9588.  Schneider et al. (2011) estimate spectral type of          
                       the secondary as M9 +/- 2. Projected separation is 120 +/- 9 au.        Sce2011 
                       Aganze et al (2016) derive spectral types M1 and d/sdM7 and effective           
                       temperatures 3800 and 2550 +80/-90 K.  Masses are 0.57 +/- 0.07 and             
                       0.084-0.091 Msun, radii 0.53 +/- 0.04 and 0.085 +/- 0.014 Rsun. The             
                       authors suggest the possibility that unusual spectral features of the           
                       B component may arise from contamination due to an additional                   
                       unresolved companion.                                                   Aga2016 
17130-5836 HJ 4920     A is a spectroscopic binary, P = 2.88d.                                         
17131-2532 RST3076     Spectrum: B9/9.5IV/V.                                                           
17133-6712 DUN 214     B is CPD-67@3295.                                                               
17133-7243 HJ 4914     Composite-like spectrum: G5III+A4/5V.                                           
17136+1716 A  2087     Ambiguous orbit?                                                                
17137-5425 R   294     SWR 216. CPM pair. B may be variable.                                   Skf2004 
17140+1621 HO  557     A is the W UMa-type system AK Her.                                              
17141+5608 STT 327     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.77 +/- 0.57, 2.53, and 1.35 Msun, respectively.             Mlk2012 
17142+1911 BU 9029     These pairs are not associated with STF2139 as reported by Burnham.     Bu_1906 
17145-0202 BAL 573     J 2905.                                                                         
17145-3946 HJ 4926     A is the variable V915 Sco.                                                     
17146+1423 STF2140     alp Her = Rasalgethi. Star A is an irregular variable, and B is an              
                       SB1, P = 51.58 d. Spectrum composite; G5III+F2V. Radial velocity                
                       measures by Smith (1988 private comm.) for alp Her A since 1984                 
                       have shown an increase in velocity by about 11 km/sec during a                  
                       three-year interval, then an apparent turnover in velocity during               
                       the fourth year. This suggests a component with a period of the                 
                       order of a decade; it now appears that this system may have at least            
                       5 physical components. Measure of 1927.43 made by triangulation of              
                       multiple measures.                                                              
                       The 1779.66 measure by Herschel was corrected.                          H__1804 
           CHR 139     Aa,Ab: A premature orbit has been computed.                                     
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Radial velocity measures by Smith (1988 private communication) for alp          
                       Her A since 1984 have shown an increase in velocity by about 11 km/sec          
                       during a three-year interval, then an apparent turnover in velocity             
                       during the fourth year.  This suggests a component with a period of             
                       the order of a decade; it now appears that this system may have at              
                       least five physical components.                                                 
                       Aa,Ab:  Resolved 3 times 1986-1991 at separations 0.16-0.19"                    
                       separations, but unresolved by Balega at the 6-m in 1997 and 10 times   Bag1999a
                       1985-1997 at 4m and 2.5m telescopes                                     Hrt2009 
           STF2140     AB: H 2   2.                                                            MEv2010 
17149-7442 SWR 215     CPM pair                                                                Skf2004 
17150+2450 BNU   5     Aa,Ab: del Her = 65 Her = Sarin. A is a spectroscopic binary.                   
                       1983.3180: Measurements were made with the 20-power objective, hence            
                       the accuracy is low.                                                    Bag1984a
           STF3127     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
                       AB: H 5   1.                                                            MEv2010 
17152+3214 COU 805     TDT 292.                                                                        
17153+2423 POU3269     Aka POU3268.                                                                    
17153-2636 SHJ 243     36 Oph = A Oph. AB = HDO 144. Proper motion -480 -1142. A premature             
                       orbit has been computed. A may be a spectroscopic binary.                       
                       Three orbit solutions by Irwin et al. (1996); the shortest-period       Irw1996 
                       orbit is marginally preferable.                                                 
                       AC: NLTT 44415/44446                                                    Chm2004 
                       AC: SHY  87. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       C component = CD-26 12036 (mag. 6.34, 700", K5V), proper motion                 
                       -481 -1134. C has common proper motion.                                         
                       The original AC and BC components in the BDS and ADS were changed               
                       to AD and BD in the IDS to accommodate the discovery by Luyten          Luy1941 
                       (= LDS 588) assigned AC.  This component assignment has been                    
                       maintained.  However, the BC measures from the BDS were erroneously             
                       assigned to the AD component in the IDS and two AC measures were                
                       assigned to the BD.  This has been corrected, as have errors made               
                       in the IDS in the measures of South and Jacob of the AD and BD          S__1824 
                       components. PM of D +003+026.                                           Jc_1848b
                       AD: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
17153-3333 SNA  65     Aa,Ab: The primary is the Be star V1075 Sco. The star was reported to           
                       be single in a RV study by Garmany et al. (1980, ApJ 242, 1063) but             
                       reported as SB2 by Chini et al. (2012). Since no period has been        Cii2012 
                       published so far, one cannot decide if the 24.8mas Aa,Ab companion is           
                       the spectroscopic one.                                                  Sna2014 
17155+1052 HDS2440     Cvetkovic et al. (2014) derive spectral types G4 and  G6, masses 1.07           
                       and 1.02 Msun. Dynamical parallax is 15.31 +/- 0.60 mas.                Cve2014 
17156-1018 BU  957     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.37 +/- 1.47, 2.87, and 1.20 Msun, respectively.             Mlk2012 
17156-3836 FIN 355     Rapid motion.                                                                   
                       New orbit based on few observations, mass-sum too small.                Sod1999 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.29 +/- 0.17, 2.22, and 2.12 Msun, respectively.             Mlk2012 
17157-0949 A  2592     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 20.39 +/- 12.95, 4.49, 1.13 Msun, respectively.    Mlk2012 
                       AB + TOK  53Ba,Bb: This is the triple system HIP 84430. We computed             
                       the first orbit of the secondary subsystem Ba,Bb which was discovered           
                       at SOAR in 2009 and has just completed one full revolution since. Its           
                       separation is always close to the diffraction limit. Adopting a mass            
                       sum of 2.6 Msun for Ba,Bb, the resulting dynamical parallax is                  
                       7.6+/-1.5mas, while the HIP2 parallax is 4.9+/-0.9mas. The latest               
                       orbit of the outer pair A 2592 AB published in Tokovinin et al. (2014)  [Tok2014
                       does not account for the fact that the speckle measurements at SOAR             
                       refer to A,Ba and not to AB. Here we give a more accurate solution              
                       that uses the positions of AB computed from the measures of A,Ba under          
                       the assumption that Ba and Bb have equal masses. After this correction          
                       and orbit adjustment, the weighted residuals are 4.3mas in separation           
                       and 1.3deg in angle. Interestingly, there were a considerable number            
                       of speckle-interferometry measures of this pair obtained in the 1980's          
                       and 1990's at 4-m telescopes, but none of them recognized the                   
                       subsystem Ba,Bb, despite its small dm.                                          
                       Ignoring the multiplicity, the spectroscopic survey of Guillout et al.          
                       (2009 A&A 504, 829) determined a moderate axial rotation V sin i =              
                       10.8km/s and detected the lithium line of 52.8mA equivalent width               
                       which, together with the X-ray detection by ROSAT (RasTyc 1715-0948),           
                       normally indicates youth. These authors do not mention this star in             
                       particular, but discuss a group of active lithium-rich giants in their          
                       sample, to which this system apparently belongs. Even with the larger           
                       dynamical parallax (instead of the HIP2 parallax), all three resolved           
                       components of HIP 84430 are located above the main sequence in the              
                       color-magnitude diagram. This multiple system is peculiar and merits            
                       further study.                                                          Tok2015c
17159-6059 R   295     Also appears to be R   292.                                                     
17161+2316 COU 315     Docobo et al. (2010) derive a dynamic parallax of 21.48 +/- 0.50 mas    Doc2010h
                       and a total mass of 1.60 +/- 0.12 Msun.                                         
17161-2556 RST3082     Spectrum: B9.5/A0IV/V.                                                          
17162+0211 CHR  61     This system, first announced by McAlister and recalled in a later       McA1984b
                       McAlister paper after repeated attempts at confirmation, has been       McA1993 
                       restored. While perhaps still spurious, the subsequent confirmation or          
                       suspected duplicity (by another technique) makes the discovery                  
                       measurement somewhat more probable.                                             
17163-4220 I   408     A is variable.                                                                  
17165+0413 LDS 989     Wolf 661-2.                                                                     
17165+0113 HJ  854     A is the Algol-type system U Oph., spectrum composite;                          
                       B5Vnn+B5V.                                                                      
17166+2635 WHC  15     Probable rapid motion in a highly-inclined orbit.                       Ho_1894b
                       CD: Ambiguous wording in the ADS resulted in this pair being                    
                       incorrectly listed as AE or AB,E in the IDS and in earlier versions of          
                       the WDS.                                                                        
17166+0440 LDS4734     A is Wolf 664.                                                                  
17166+0325 SHY 715     AC: HIP  84515 + HIP  85911.                                                    
17166-0027 A  2984     41 Oph. A premature orbit has been computed.                            Vou1951 
17167+1100 BPM 678     [PM2000] 1242397 + [PM2000] 1242317.                                    Gvr2010 
17169+8902 HJ 2985     lam UMi                                                                         
17171+1806 LDS4735     NLTT 44506/44505                                                        Chm2004 
17173+3306 STT 328     68 Her. A is the Beta Lyrae-type system u Her.                                  
                       Composite spectrum, B1.5Vp+B5III.                                               
17173-3010 BU 1119     Spectroscopic binary.                                                           
17173-3533 HD 156134   Bochum 13 #2.                                                           Bid1976 
                       The classification is from McConnell & Bidelman (1976).                 Msn1998a
17173-4140 CPO  73     LDS 589.                                                                        
17173-6016 B  1853     Spectrum: G8/K1III+A.                                                           
17174-6657 LDS 587     Primary is 1.7d eclipsing SB2 V824 Ara; visual pair has estimated               
                       period of 20,000y.                                                      Tok2006 
                       A component is 1.68d SB2, spectral types G5IV+K0IV/V. System is a               
                       member of the bet Pic moving group.                                     Zuc2001b
17175-2746 TRN  24     AB and AC: The image rotator was in an unknown state, so two possible           
                       theta values are listed for the 2001.4959 observation - one for                 
                       zenith up and one for north up.                                         Trn2008 
           HD 156212   Levato et al. (1988) find the radial velocities to be "probably         Lev1988 
                       variable", but since the total range in 11 measurements is 33 km/sec            
                       we assign it to the "C" category.                                       Msn1998a
17177-2638 H 1  35     H I 35.                                                                         
17178+2844 S   686     B is BD+28@2714.                                                                
17179+3229 BU   45     SEI 541.                                                                Nsn2017b
17180-2417 H 3  25     omi Oph. H III 25.                                                              
17183+0459 SLE  19     Aka UC  226.                                                                    
17184+3240 BU  628     A premature orbit has been computed.                                            
17184+0451 SCJ  14     B is BD+05@3367. Aka SLE  18.                                                   
17185+5346 ES  776     Heintz confirms that the Furner measures listed in ADS belong to this   Hei1983a
                       system, so aka FUR   1.                                                         
17186+3229 L    15     Lewis mentions a pair 2' s: 1900.5, 028@, 5.55".                        L__1896a
                       Position of L 15 revised by Heintz.                                     Hei1987a
                       Observations attributed by Popovic & Pavlovic to new pair 17186+3225    Pop2001 
                       PAL   2 have been assigned to this pair. However, there is some                 
                       uncertainty as to whether these two binaries are the same.                      
17186-3223 PRO 154     CPD-32@4467.                                                                    
17187+2146 STTA152     B is BD+21@3090.                                                                
17189-2400 H 6  54     H VI 54.                                                                        
17190-2034 RSS 435     CPD-20@6531                                                                     
17190-3459 MLO   4     Proper motion +1167 -169. Spectral type of C may be M.                          
                       Good double-solution instead of unuseable HIP-data.                     Sod1999 
                       Identification of ascending node is probable.                                   
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.07 +/- 0.61, 1.37, and 1.40 Msun, respectively.  Mlk2012 
17191-4638 BSO  13     Proper motion of A +1508,+109; PM of B +1417,+138 (UCAC2). Epoch-2000           
                       coords of C = 1718497-463819, current AC separation ~2'.4 at 265deg.            
                       Epoch-2000 coordinates of D = 1718551-463738, current AD separation             
                       ~1'.6 at 290deg.                                                                
                       41 Apri.                                                                        
                       Four orbit solutions by Wielen (1962); only orbit #4 now in catalog.    Wln1962 
17193-5323 DUN 215     B is CPD-53@8531.                                                               
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
17194-4413 HDO 269     Spectrum composite; B9.5V+A6III.                                                
17195-5004 FIN 356     Composite spectrum, F8III+B9V.                                                  
17198-3606 SNA  69     Aa,Ab: OWN indicates a 16.4d SB. SAM resolved it as a 185mas pair; a            
                       distant faint companion is also see in the NACO FOV.                    Sna2014 
17199+2629 OSV   5     Ross 867 = LDS 993. Both components are flare stars, V647 and V639 Her          
17200-0801 CHR 151     Aa,Ab: This newly-discovered pair was unresolved in our earlier survey          
                       for duplicity among high-velocity stars (Lu et al. 1987). Abt &         McA1987c
                       Biggs (1972) list a single radial velocity of -89.3 km/s for this       AbH1972 
                       object, published in 1950. Additional observations, both by speckle             
                       and by spectroscopy, are needed for confirmation of its duplicity and           
                       its high velocity.                                                      Hrt1992b
                       B is BD-07@4426.                                                                
17201+2513 BRT3317     Originally published as BRT 173.                                        Brt1928 
17204+2017 LEP  82     NI   37.                                                                        
17207+3228 DOR   1     72 Her. Struve-Dorpat. Proper motion of A +137 -1041.                           
                       Variable. PM of E -016+041, F -052+021                                          
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
17207-0706 A  2593     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 0.93 +/- 0.32, 1.83, and 0.95 Msun, respectively.             Mlk2012 
           TOK 178     HIP 84866. AB is a visual binary A 953 with P=73.5y and a=0.262".               
17207-5625 FIN 255     AB. 1990.3497: This observation finally confirms the discovery of this          
                       system by Finsen, made in 1931!                                                 
17208+0156 LDS6319     Wolf 672. Colors indicate white and red dwarf stars.                            
17208-0902 A    28     aka HO  631                                                                     
17208-1251 SHJ 247     nu Ser = 53 Ser. B is BD-12@4724.                                               
                       H 5  29.                                                                MEv2010 
17208-3932 RST1951     TDT 315.                                                                        
17209+2430 S   687     70 Her. A is a spectroscopic binary.                                            
17209-3604 SNA  70     The 45mas companion was resolved both by PIONIER and NACO/SAM. RV               
                       variability of 7 km/s is reported by Crampton (1972, MNRAS 158, 85)     Cii2012 
                       but not confirmed by Chini et al. (2012).                               Sna2014 
17210-2107 DON 832     xi Oph = 40 Oph                                                                 
17213-5107 HD156643    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17214+2259 POU3288     Aka WRH   6.                                                                    
17214-3707 BRT1714     CPD-36@7238.                                                                    
17215+2845 CHR 194     Aa,Ab:. 1991.3247: A new close companion to the 0".7 pair KUI 80.               
                       The primary of this system is listed in the preliminary version of the          
                       fifth edition of the Bright Star Catalogue as a G0III SB.               Hof1991 
17215-5628 HJ 4939     B is CPD-56@8164.                                                               
17217+3958 MCA  47     Martin et al. (1998) derive component masses 1.150 +/- 0.229 and                
                       2.624 +/- 0.372 Msun.                                                   Mig1998 
           V819 Her    Ba,Bb: Period fixed from spectroscopic orbit by Scarfe et al. (1994).   Scf1994 
                       The visual secondary is a 2.2d eclipsing binary (V819 Her).                     
                       Ba,Bb: Mass-sum in agreement with Scarfe et al. (1994).                 Sod1999 
                       Ba,Bb: Scarfe et al. (1994) give a combined spectroscopic/speckle               
                       solution, yielding distance, masses, etc.                               Scf1994 
                       Ba,Bb: Muterspaugh et al (2008) combine PHASES astrometry with speckle          
                       and radial velocity data to derive orbits for both the AB and Ba,Bb             
                       pairs of this triple. The parallax is determined at 14.57 +/- 0.19 mas          
                       (distance 68.65 +/- 0.87 pc). Masses of the A, Ba, and Bb components            
                       are 1.799 +/- 0.098, 1.469 +/- 0.040, and 1.090 +/- 0.030 Msun.         Mut2008 
                       Ba,Bb: O'Brien et al. (2011) derive an orbit for the B component via a          
                       chi-square fit to interferometric visibility measurements from                  
                       observations of fringe packets at the CHARA Array. The mutual                   
                       inclination compared with the AB orbit is 33.5 +/- 9.3deg. Combined             
                       with spectroscopy by Scarfe et al. (1994), they derive masses for A,    Scf1994 
                       Ba, and Bb of 2.566 +/- 274, 1.488 +/- 0.181, and 1.079 +/- 0.148 Msun,         
                       respectively. Parallax is 14.5 +/- 0.2 mas, yielding a separation               
                       between Ba and Bb of 0.04573 +/- 0.00163 au. The age of the system is           
                       estimated at 1.9 +/- 1.1 Gyr.                                           CIA2011c
                       Zasche et al. (2014) derive a combined solution, including                      
                       interferometry plus times-of-minimia variations in the Algol-type               
                       eclipsing-binary secondary.  They determine a distance of 68.8 +/-              
                       1.8pc and a mass for the secondary of 1.86 +/- 0.30 Msun.               Zas2014b
17221+2310 COU 415     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.99 +/- 1.24, 2.24, and 1.20 Msun, respectively.             Mlk2012 
17221-7007 FIN 373     iot Aps                                                                         
                       Docobo & Andrade (2013) derive a dynamical parallax of 3.89 +/- 0.26            
                       mas and component masses 3.89 +/- 1.02 and 3.45 +/- 0.90 Msun. See              
                       paper for extensive notes on this system.                               Doc2013d
17222+1358 BPM 679     [PM2000] 1252669 + [PM2000] 1252688.                                    Gvr2010 
17222-5902 HJ 4934     B is CPD-58@7077.                                                               
                       SWR 217.                                                                Skf2004 
17224-3012 HO  413     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
17226-3555 GC 23463    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17228-4537 EVS  30     Primary is the Cepheid V636 Sco.                                        Evs2016a
17232-4937 SWR 218     CPM pair                                                                Skf2004 
17233-4728 HDO 271     iot Ara. A is variable.                                                         
17236+4256 HD157821    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17237+3709 MCA  48     Aa,Ab: rho Her. Suspected of variable velocity, and resolved by                 
                       speckle interferometry.                                                         
           STF2161     AB: H 2   3.                                                            MEv2010 
17238+0219 BAL1936     J 3297.                                                                         
17239+3300 LDS5854     LDS6320.                                                                        
17239-5154 HJ 4941     SWR 220.                                                                        
17240+3835 HU 1179     1985.741: The residuals of these measurements (as well as those of              
                       McAlister) are irregular and do not permit the correction of an orbit.  Tok1985 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.81 +/- 1.50, 3.55, and 1.70 Msun, respectively.             Mlk2012 
17240-0921 RST3972     High mass-sum, sp duplicity?                                            Sod1999 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.80 +/- 0.64, 2.18, and 1.05 Msun, respectively.             Mlk2012 
                       Aa,Ab: Martin et al. (1998) derive component masses 1.791 +/- 0.499             
                       and 1.749 +/- 0.489 Msun.                                               Mig1998 
           TOK 179     HIP 85141. Aa,Ab = RST3972,                                             Tok2011a
17241-5716 BRT2823     SWR 219.                                                                        
17243-3722 RST3091     Spectrum: B8/9III/IV.                                                           
17244-2248 HJ 4948     AC: HJ 4851.                                                                    
17245-3032 HLD  28     SEE 325.                                                                        
17246+3913 WSI   2     Aa,Ab: Hipparcos suspected non-single.                                          
           S   689     STTA153.                                                                        
                       AB: B is BD+39@3124.                                                            
17246-4709 HJ 4944     B is CD-47@11509.                                                               
17247+3802 HSL   1     Aa,Ab. Masses of 0.887+/-0.030 and 0.788+/-0.021 are determined.        Hor2006d
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 2.37 +/- 0.30, 2.12, and 0.95 Msun, respectively.  Mlk2012 
                       Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic             
                       elements are fixed to those of Goldberg et al. (2002 AJ 124, 1132).             
                       Assigned spectral types for Aa, Ab, and Ac are G5V, G8V, and K6V;               
                       derived masses for Aa and Ab are 0.92 and 0.84 Msun.                    Hor2015 
17247-3412 HJ 4936     Primary is eclipsing binary of W UMa-type, period 2.359 day.            Zas2013 
           MZA  36     Aa,Ab: Pismis 24-1. Barr Dominguez et al (2013, A&A 557, A13) reported          
                       a 2.36d photometric period, indicating one of the components of this            
                       pair is an eclipsing binary.                                            Sna2014 
17248-5913 WSI  87     Comparable separations of AB and AD suggest a possibly dynamically      Tok2010b
                       unstable configuration, which is very unlikely. Companion D cannot be           
                       a chance projection: it is too bright and would have been spotted               
                       before.                                                                         
17249+1806 BPMA 50     [PM2000] 1257922 + [PM2000] 1258132.                                    Gvr2010 
17249-4950 CPO 523     CPD-49@9962.                                                                    
17250+0108 RST5431     BAL 1489.                                                                       
17251+3444 HU  922     Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 5.14 +/- 2.29, 1.89, and 1.05 Msun, respectively.  Mlk2012 
           SHY 719     AB: HIP  85238 + HIP  83811.  B component = A component of 17075+3557.          
17252+1355 BPM 680     [PM2000] 1258439 + [PM2000] 1258470.                                    Gvr2010 
17254-5233 LPO  62     SWR 221. CPM pair                                                       Skf2004 
17254-5623 HJ 4942     gam Ara                                                                         
17255+5130 HU  672     Includes GQ Dra, a Beta Lyr type eclipsing binary, P = 0.76590d.        Zas2012 
17259+1655 KUI  81     A is the irregular variable V640 Her.                                           
17260-0139 TOK 180     HIP 85307. A = HR 6489, F3V, PM(A)=(+61,+52). NOMAD: PM(B)=(-62,+75).           
                       The status of B is uncertain, it is not found in the WDS. A,B are ~1            
                       mag above the MS (true parallax ~25mas?). Nothing on B in SIMBAD.               
                       Crowded field, N*=73.                                                   Tok2011a
17260-0245 OSO  78     G019-025. AB is not a common proper motion pair, based on comparison            
                       with POSS2 red plates.                                                  Oso2004 
17260-5038 HDO 313     kap Ara                                                                         
17261+3550 ES 2228     BOW.                                                                            
17261-3718 RST3096     TDT 349.                                                                        
17262+6311 HO   68     TDT 351.                                                                        
17262+3604 GRV1230     SLW1210.                                                                        
17262+2927 STF2165     Called a Delta Del-type star by Bidelman.                                       
17263+0736 GC 23614    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       McLaughlin (1962).                                                      MLa1962 
17264-4837 SHY 297     HIP  85342 + HIP  85326.                                                        
                       AB + TOK 415Ba,Bb: HIP 85342 and HIP 85326 form a physical pair AB at           
                       127" separation (common PM, RV, and parallax). The B component = HIP            
                       85326 has a variable RV and an astrometric acceleration which could             
                       hardly be produced by the 1" speckle companion Bb found here, owing to          
                       its long estimated period of ~300yr. It seems that B is triple and the          
                       whole system is quadruple. This companion Bb was not detected in the            
                       previous speckle observations because it is red: dI = 2.4, dy = 4mag;           
                       its color matches a dwarf star at the same distance as the system.              
                       However, the field is crowded and the newly found companion could               
                       still be optical.                                                       Tok2015c
                       AB: Tokovinin & Lepine (2012) miss B, but list companion at 1373",      Tok2012c
                       likely optical.                                                         Tok2014d
17266-0505 MKT  14     Aa,Ab: 47 Oph. Preliminary elements determined by Hummel (1997), based          
                       on Mark III interferometric results.                                    MkT1997 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.59 +/- 0.21, 3.02, and 1.30 Msun, respectively.             Mlk2012 
                       Wang et al. (2015) derive a combined interferometric/spectroscopic              
                       orbit, including data from the Mark III and NPOI arrays. Derived                
                       physical parameters for the Aa and Ab components include luminosities           
                       7.80 +/- 0.36 and 3.41 +/- 0.25 Lsun, radii 2.06 +/- 0.07 and                   
                       1.36 +/- 0.06 Rsun.                                                     WaX2015 
17266-3258 TOK 416     HIP 85360 is an acceleration and spectroscopic binary. Its preliminary          
                       spectroscopic period (Latham 2012, private communication) corresponds           
                       to a semi-major axis of 80mas. The star is chromospherically active             
                       and possibly young. The faint companion found here at 1".16 is most             
                       likely optical, as the field is extremely crowded. Re-observation               
                       within a year will resolve its status.                                  Tok2015c
17267+3105 LDS 995     B is BD+31@3025.                                                                
                       NLTT 44816/44814                                                        Chm2004 
                       HJL 247.                                                                HJL1986 
                       SHY 720. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
17268-2620 BU  128     HDO 146                                                                         
17270+5718 ES 2658     STI 2351.                                                                       
17272-6105 RSS 441     CD-60@6672                                                                      
17273+1504 BPM 681     [PM2000] 1262856 + [PM2000] 1263009.                                    Gvr2010 
17275+0428 GRV 956     HJL 248.                                                                HJL1986 
17279+1123 STF2166     B is BD+11@3183.                                                                
17279-4702 RST5543     V750 Ara, a light and velocity variable.                                        
17282+4301 OSO  79     G203-068. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
17282+3949 BOY  10     Aa,Ab: 2MASSW J1728114+394859                                                   
                       Aa,Ab: Burgasser et al. (2011) derive spectral types of L5 and L6.5,    Bug2011 
                       masses 0.075 +/- 0.007 and 0.066 +/- 0.008 Msun, and effective                  
                       temperatures 1570 +/- 80 and 1340 +/- 70K.                                      
                       Aa,Ab: Assuming a parallactic distance of 24.1 +/- 2.1 pc                       
                       (Vrba et al. 2004), Konopacky et al. (2010) derive a system mass of     Vrb2004 
                       0.15 +0.25/-0.04 Msun.                                                  Kon2010 
           ALP  22     AB: Physical companionship to this ultracool dwarf ruled out based on           
                       I-J color, using I-band photometry taken at WIYN in August 2002.        AlP2007 
17283-2058 A  2244     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.70 +/- 1.23, 2.64, and 1.20 Msun, respectively.             Mlk2012 
17286+1132 BPM 682     [PM2000] 1265621 + [PM2000] 1265681.                                    Gvr2010 
17287-2304 RST3103     CD-22@12047.                                                                    
17290+5052 STF2180     H 1  66.                                                                MEv2010 
17290-4358 DUN 217     Spectrum of B: A2IV.                                                            
17290-5048 CPO 527     CPD-50@10113.                                                                   
17292-3132 SNA  72     The primary is V1081 Sco, a detached Algol-type eclipsing binary                
                       showing apsidal motion (Otero 2005, IBVS 5631, 1), most probably                
                       because of this third component at 26.8mas. The object is reported as           
                       SB3 and we postulate our detection corresponds to the 3rd component.    Sna2014 
           HD 158186   The classification is from Garrison et al. (1977 ApJS 35, 111). An              
                       eclipsing light curve is presented in the Hipparcos Catalogue for a     HIP1997a
                       for a period of 8.77 d.                                                 Msn1998a
17293+2924 A   351     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.06 +/- 0.24, 1.33, and 0.79 Msun, respectively.  Mlk2012 
           KUI  82     AB,C: Baize measures from 1937-1962 were corrected by the author for a  Baz1966b
                       scaling error. In this same paper Baize extracted three measures from           
                       A.C. data and also calculated a rectilinear fit to all measures.                
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
                       AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
17295+3456 STF2178     BDS 8092. H III 40 may be same star?                                            
17297+6351 LDS5227     LDS6321.  Also known as LEP  84.                                                
                       NLTT 44975/44960                                                        Chm2004 
                       HJL1095.                                                                HJL1986 
                       SHY 298. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
17297+1629 BPM 683     [PM2000] 1268087 + [PM2000] 1267932.                                    Gvr2010 
17299+3035 SLE  29     SLE 29 and GRV 957 may be the same pair, but there appears to be a              
                       major typographical or reduction error by Soulie (1983).                Sle1983 
17300+3035 GRV 957     SLE 29 and GRV 957 may be the same pair, but there appears to be a              
                       major typographical or reduction error by Soulie (1983).                Sle1983 
17301-3343 HWE  39     A is a spectroscopic binary, P = 38.10d.                                        
17304+5218 BU 1090     bet Dra = 23 dra = Rastaban                                                     
17304-0104 STF2173     The eccentricity, inclination, node, and longitude of the node are      Dnc1952 
                       taken from the orbit of Duncombe & Ashbrook (1952) by Wilson (1976).    WRH1976b
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.91 +/- 1.03, 2.05, and 0.95 Msun, respectively.             Mlk2012 
17306+1731 GC 23718    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17308+0349 A  2247     In 1923, 183@, 0.1". Quadrant doubtful.                                         
17308-3726 B   912     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.35 +/- 1.71, 3.78, and 2.24 Msun, respectively.             Mlk2012 
17311-6041 EHR  15     Primary is del Ara. Physical/optical nature of AB,AC,AD all undefined.  Ehr2010 
           HJ 4951     AE: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           del Ara     Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17314+0243 A  2386     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Lucke & Mayor (1982).                                                   Luk1982 
                       1978.6174: This epoch was incorrectly given as 1977.6174 by McAlister           
                       & Hendry (1981).                                                        McA1981b
17315-6026 I   600     Ruymaekers & Nys (1995) noted discrepancies in the orbit of Erceg &     Ruy1995 
                       Olevic (1988), and calculated elements from the Thiele-Innes            Erc1988 
                       elements originally given.                                                      
17316+1654 BPM 684     [PM2000] 1272174 + [PM2000] 1271975.                                    Gvr2010 
17316-2616 CHR 229     Possible confirmation of this pair may be found in Hoffleit & Warren    Hof1991 
                       (1991), who note the following: "Duplicity reported from grazing                
                       occultation observations of 1991 Sep 15. Estimated magnitude of                 
                       comparison 8.6, separation several tenths of an arcsecond in position           
                       angle 160 deg (all rough estimates)".                                   Hrt1996b
                       OCC 821.                                                                        
17316-3018 I   105     SEE 330.                                                                        
17316-3041 LDS 602     NLTT 44935/44933                                                        Chm2004 
17317+3019 STF2181     AB and AC: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
17317+1111 AG  354     HU 179.                                                                         
17318-4953 HJ 4955     alp Ara. A spectroscopic binary.                                                
17320+6808 BU 1458     27 Dra. A is a spectroscopic binary.                                            
17320+0249 STT 331     A: V2373 Oph, a Beta Lyrae eclipsing binary, period 1.08628d.           Zas2010 
           BU 1538     DE: This is a measure of a faint pair 1 minute preceding STT 331.               
17321+3106 LDS4750     NLTT 45001/45000                                                        Chm2004 
17321-2035 LDS5226     NLTT 44964/44965                                                        Chm2004 
17322+5511 STFA 35     A: 25 Dra = nu 2 Dra                                                            
                       B: 24 Dra = nu 1 Dra = BD+55@1944.                                              
                       AB: STTA156. Both components are spectroscopic binaries.                        
                       HJL 249.                                                                HJL1986 
                       SHY 299. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       H 5  11.                                                                MEv2010 
17322+1156 ISO   4     A spectroscopic binary, P = 6.8d.                                               
17324+2848 A   352     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.72 +/- 0.80, 2.79, and 1.35 Msun, respectively.             Mlk2012 
17324-4638 HJ 4957     Nebulous looking star 10' np.                                           I__1909 
17325+1346 BPM 685     [PM2000] 1274391 + [PM2000] 1274440.                                    Gvr2010 
17325+1201 BPM 686     [PM2000] 1274449 + [PM2000] 1274756.                                    Gvr2010 
17326+3445 HU 1181     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.79 +/- 0.33, 2.12, and 1.05 Msun, respectively.             Mlk2012 
17327+7414 29 Dra      Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Fekel et al. (1993).                                                    Fek1993b
17331+0243 BAL1939     TOB 262.                                                                        
17331-3035 CHM   6     NLTT 44988 + 44989.                                                             
17333+4634 ALP  23     2MASSW J1733189+463359                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17333+4037 LDS4753     NLTT 45053/45054                                                        Chm2004 
17334+7414 LDS1871     B is BD+74@718.                                                                 
                       HJL 251.                                                                HJL1986 
17335+5734 MLR 571     1980.7255: This measure was incorrectly attributed to HR 6053 in                
                       McAlister et al. (1983), with an additional factor of two error in the          
                       separation.                                                             McA1983 
17335+1553 BPM 687     [PM2000] 1276763 + [PM2000] 1276893.                                    Gvr2010 
17336+1801 BPM 688     [PM2000] 1277005 + [PM2000] 1277076.                                    Gvr2010 
17336-3547 BRT1725     CPD-35@7036.                                                                    
17336-3706 SEE 334     AB: lam Sco = 35 Sco = Shaula. Variable. Spectroscopic binary.                  
           TNG   1     Aa,Ab: The combined solution orbit by Tango et al. (2006) determines    Tng2006 
                       component masses of 10.4 +/- 1.3 Msun and 8.1 +/- 1.0 Msun. There is            
                       also a pre-MS subcomponent to A with a mass of 1.8 +/- 0.2 Msun. The            
                       dynamical parallax is 112 +/- 5 mas, about a factor of two smaller              
                       than the Hipparcos value of 216 +/- 42. The dynamical value is much             
                       more accurate. Two components have calculated effective temperatures            
                       of 25000 +/- 1000 and 21000 +/- 1000 degrees Kelvin, respectively.              
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 77.47 +/- 30.56, 22.63, 10.96 Msun, respectively.  Mlk2012 
17337+1451 WSI   3     Hipparcos suspected non-single.                                                 
17339+0806 SHY 726     HIP  85940 + HIP  85944.                                                        
17341-0303 TOK 417     HIP 85963 has a variable RV and is an acceleration binary. The 91mas            
                       separation implies an orbital period of ~10yr; the estimated masses             
                       are 1.37 and 0.81 Msun. Despite extensive literature (51 references in          
                       SIMBAD), there is no published spectroscopic orbit, while several               
                       high-resolution spectroscopic studies addressed the abundance.          Tok2015c
17342-1910 B  1863     AB + TOK 418AC: B 1863 is a known close binary which has been                   
                       unexpectedly found to be a triple. The new distant component C is               
                       detectable also in the y filter, but we measured only the inner binary          
                       in y. The star was observed at the Blanco telescope in 2008.5397, and           
                       the pair actually measured then was AC, at 133.8deg, 0".217, dy =3.7.           
                       The inner pair AB with a smaller dm was unresolved in 2008.5, while it          
                       is clearly resolved now. Owing to the large distance from the Sun, we           
                       expect only a slow motion, so even the inner pair observed since 1929           
                       may not yet be ready for computing its first orbit.                     Tok2015c
17342-5454 TOK 419     HIP 85969 has a variable RV according to the GCS and confirmed by               
                       Jones et al. (2002 MNRAS 337, 1170). The 0".55 separation implies a             
                       period on the order of 80yr. The star is on the exo-planet program at           
                       the Anglo-Australian Telescope.                                         Tok2015c
17343-1909 SS 73-90    Symbiotic star, spectral type M6. Fekel et al. (2008) orbit is a        Fek2008 
                       combined spectroscopic/spectropolarimetric solution. Estimated value            
                       for a" based on their a sin i, i, and estimated distance of 4.7 kpc.            
17344+1310 STF2184     AB: H 3  35.                                                            MEv2010 
17345+0335 BAL2443     J 3298.                                                                         
17346+2958 MAB   1     Primary is a slightly evolved subgiant, inferred mass 1.16 +/- 0.11             
                       Msun, and is a 9.009d SB. Minimum mass of close companion is 40.0 +/-           
                       2.5 Mjup. Distance is estimated at 218 +/- 14 pc. A wider possible              
                       companion was discoverd by AO imaging at 643mas, with dm 6.49mag in             
                       K-band. If physically associated, this companions would have an                 
                       estimated mass of 0.13 Msun. Further pm data are needed to determine            
                       its physical or optical association with primary.                       MaB2013 
17346+0935 STFA 34     53 Oph = f Oph. STTA155. B is BD+09@3423.                                       
                       AB: H 5  30.                                                            MEv2010 
17346-5256 CPO 533     B is CPD-52@10710.                                                              
17347-3235 HJ 4962     Central star of cluster NGC 6383, and spectroscopic binary, P = 3.37d           
           ISO   5     Our single observation appears to indicate a single star, so we cannot          
           HDS2480     confirm the reported ISO 5 Aa pair. Nor did we detect the new                   
                       Hipparcos Aa,Ac pair, presumably due to the large magnitude difference          
                       (Delta Hp = 3.2).                                                       Msn1998a
                       Classifications of the Ab and Ac components are from Lindroos (1985).   Lnd1985 
                       Lindroos also notes a wider "X" component (V = 10.8, separation = 25",          
                       photometric classification = B5 IV) which he claims is physical.  This          
                       component is not mentioned in the WDS.  Lindroos finds a distance of            
                       1.8 kpc.                                                                        
           SNA  73     Aa1,2: The primary is V1036 Sco, an ellipsoidal variable star. It is            
                       marginally resolved on two PIONIER observations with minimum                    
                       separation rho>0.9mas on the first epoch and rho=10mas about one month          
                       later.  The known SB2 has an equal mass ration, P=3.36d, and a sin i =          
                       14 Rsun (Stickland et al. 1993; Linder et al. 2007, A&A 474, 193.       Stc1993 
                       Given a probably distance of ~1.5kpc, the expected separation of the            
                       spectroscopic pair is <0.2mas, so we probably detected a 3rd fainter            
                       component. Mason et al. (1998) reported three other companions at       Msn1998a
                       0.27", 0.74", and 5.4". We clearly detect the wider pairs, but not              
                       Aa,Ab. The Ab companion may be a spurious detection (possibly due to            
                       the 10mas Aa1,Aa2 pair), or possibly is too faint for AstraLux and              
                       NACO, implying dm > 5mag.                                               Sna2014 
17348+0601 STF2185     STTA154.                                                                        
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       BC: The 1912 observation was incorrectly attributed to a nonexistent    Dob1927 
                       AD component (apparently the result of an erroneous note in the ADS).   A__1932a
                       Error noted by Burley & Kidd.                                           GSU2002 
                       AB: HJL 250.                                                            HJL1986 
17348-1115 HJ 4964     B is BD-11@4410.                                                                
17349+1234 MCY   4     alp Oph = Rasalhague.                                                           
                       The companion has been detected by infrared speckle interferometry.     Mcy1983 
                       Kamper et al. derive a combined astrometric/spectroscopic solution.     Kpr1989 
                       Gatewood derives a weighted mean parallax of 68.12 +/- 0.75 mas from    Gat2005 
                       MAP and previous results. Masses resulting from solution are 2.842              
                       +/- 0.194 and 0.778 +/- 0.058 Msun; spectral types are A2V and K2V.             
                       This object was incorrectly identified as HD 159571 by Balega et al.    Bag1984b
                       1999: Boccaletti et al. (2001) theta was flipped from 116.3 to 63.7,    Boc2001 
                       as noted by Gatewood (2005).                                            Gat2005 
                       Orbital elements by Hinkley et al. (2011) gives a mass ratio of         Hnk2011 
                       2.76 +0.43/-0.27 and individual masses 2.40 +0.23/-0.37 and 0.85                
                       +0.06/-0.04 Msun, assuming a parallax of 69.1 mas.                              
17349-0044 BAL 891     J 2114.                                                                         
17350+6153 BU  962     26 Dra.                                                                         
                       Magnitude of B underestimated by Burnham.                               Baz1954a
                       A distant companion (mag. 9.95, 740") shares the large proper motion            
                       (Upgren 1962).                                                          VVO1962 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.77 +/- 0.95, 1.80, and 1.05 Msun, respectively.  Mlk2012 
                       AB: GJ 684. A is SB1, P=76.1y (Abt & Wilmarth 2006)                     AbH2006 
           LDS2736     AB,C: SHY  88. Bayesian analysis by Shaya & Olling (2011) indicates     Shy2011 
                       very high (near 100%) probability pair is physical.                             
                       AB,C: C is GJ 685.                                                      Tok2014d
           HZE   3     GJ 684. Heinze et al. (2010) determine that the new companion is a              
                       background object.                                                      Hze2010 
17352+2635 LAW   5     Spectral types M7-L3 and M8-L4, masses 0.077-0.086 and 0.066-0.082              
                       Msun, distance 10-12 pc                                                 Law2006 
17357-6257 HJ 4956     SWR 225.                                                                        
17358-3542 VOU  72     1.6' n, 1.5m f CPD-35 7046.                                             Vou1947a
17359-6427 SWR 226     Probably giants, not dwarfs                                             Skf2004 
17360+2100 STF2190     A is a spectroscopic binary.                                                    
                       Herschel observed this pair and another nearby pair of similar rho and  HJ_1833c
                       theta and same primary and secondary magnitudes he designated HJ 2807.          
                       Offset from his STF2190 coordinates shows no bright star at location            
                       of HJ 2807, however. Burnham says HJ 2807 is "undoubtedly identical     Bu_1906 
                       with STF2190" (= BDS 8082). Herschel's 1830.47 measure was accordingly          
                       reassigned to STF2190. Gauchet disagrees with Burnham, but his          Gau1925 
                       separation does not agree with Herschel's and his coordinates precess           
                       to location of a 7th magnitude star (BD+20@3531) 1.5m east of                   
                       Herschel's. Separation and magnitudes of this pair, designated                  
                       GAU  21, agree with Gauchet's, although the quadrant is reversed.               
17360-2025 BHA  19     CPD-20@6597.                                                                    
17362+5425 ES  637     B is BD+43@2775.                                                                
17362-3330 B   914     Spectral type may be M.                                                         
17362-5538 HJ 4959     B is CPD-55@8221.                                                               
17364+6820 CHR  62     Aa,Ab is also the astrometric binary Ci 18,2354 = GJ 687                        
                       Lippincott orbit rejected from Fourth Orbit Catalog                     Lip1967 
                       ("object still suspected to be binary by some, but no even              Wor1983 
                       approximately reliable or complete elements yet available")                     
           ENG  61     AB: B is BD+68@947. Proper motion of B = -868,-1270 (UCAC2)                     
                       Proper motion of A = +013+084, C -008+005                                       
                       AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
17366-4825 TDT 431     SWR 227.                                                                        
17368+1147 BPM 689     [PM2000] 1285047 + [PM2000] 1285184.                                    Gvr2010 
17368-2057 HU  751     Direct motion.                                                                  
                       1985.4843: autocorrelogram remeasured; new results listed here.                 
17370+6845 FOX 203     ome Dra = 28 Dra. A is a spectroscopic binary.                                  
           ome Dra     Combined spectroscopic/astrometric solution, based on high-resolution           
                       echelle spectra plus archival PTI visibility measurements.                      
                       Derived masses 1.46 +/- 0.16 and 1.18 +/- 0.13 Msun,                            
                       distance 23.65 +/- 0.15 pc.                                             Knc2010 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.49 +/- 4.97, 2.59, and 1.25 Msun, respectively.             Mlk2012 
17372+2754 KUI  83     LDS 997.                                                                        
                       Masses and bolometric magnitudes are derived for the two components             
                       of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                       and available parallaxes.                                                       
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.07 +/- 0.37, 1.37, and 0.55 Msun, respectively.  Mlk2012 
                       AB,C triple solution.                                                   Sod1999 
17373+7105 LDS1872     NLTT 45240/45242                                                        Chm2004 
17373-4300 SEE 510     The confirmation by Hipparcos may be due to taking as a first solution          
                       the measure by T.J.J. See. It is possible that a grid-step error is     See1896c
                       involved here and an NDAC solution of PA = 275, sep = 0.51", and                
                       dm = 3.2 seems better. However, this would seem to contradict See's     Jaw2006b
                       original estimate of the magnitude of B at 13. It is entirely possible          
                       that See's pair is spurious. Given the small dm and how obvious the             
                       Sco is, this could not possibly be, as has been suggested, HJ 4963.             
17374-4022 ARY 107     Author listed WDS position as 17373-4027, but corrected in private      Ary2014b
                       communication on July 2, 2014                                                   
17375+2419 CHR  63     79 Her.                                                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 13.76 +/- 1.34, 3.71, and 2.09 Msun, respectively.            Mlk2012 
17375+2036 GAU  21     See note for 17360+2100STF2190.                                                 
17376+1747 BPM 690     [PM2000] 1287091 + [PM2000] 1286976.                                    Gvr2010 
17376+1556 BPM 691     [PM2000] 1287158 + [PM2000] 1287331.                                    Gvr2010 
17376-1524 ISO   6     xi Ser = 55 Ser. Aa,Ab is a spectroscopic binary, P = 2.29d. The Isobe  Iso1990a
                       pair is not the spectroscopic binary.                                           
17376-4049 EVS  31     Primary is the Cepheid V950 Sco.                                        Evs2016a
17379+1836 Ci 18,2347  = GJ 686                                                                        
                       Bieger orbit rejected from Fourth Orbit Catalog                         Bie1964 
                       ("not confirmed by subsequent observations")                            Wor1983 
17379-3752 I   247     A spectroscopic binary.                                                         
17380+5521 GRV1137     SLW1211.                                                                        
17380+3330 JNN 115     The B component of the system appears to be a close binary itself in            
                       several different epochs of AstraLux imaging, but the suspected Ba/Bb           
                       pair is not sufficiently resolved to get a converging binary fit,               
                       hence we treat the AB system as a regular binary in this study.         Jnn2012 
17380-4837 CPO 542     Heintz reverses the quadrant.                                           Hei1987a
17382+0913 OSO  80     GD 211. Not a common proper motion pair, based on comparison with               
                       POSS2 red plates                                                        Oso2004 
17383+4500 ES 1257     Measures are very discordant, and indicate rapid movement.              Baz1940a
17384-0519 BAZ   8     Erroneously identified by me as new pair; it is in reality RST3983.     Baz1952d
17384-5956 HJ 4961     B is CPD-59@7089.                                                               
17385+4013 OSO  81     G204-020. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
17386+7120 WOR   7     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
17386+5546 STF2199     A premature orbit has been calculated.                                  Dur1944d
17387+6114 HOM   1     Aa,Ab : A 3748-d spectroscopic orbit of this pair has been determined.  Grf2013f
17387+1840 SLO   1     Aka TDT 447.                                                                    
17387+1834 OSO  82     G170-056. CD is not a common proper motion pair, based on color and             
                       comparison with POSS2 red plates                                        Oso2004 
17388+1643 BPM 692     [PM2000] 1290109 + [PM2000] 1290424.                                    Gvr2010 
17389+8403 STF2299     LDS1876. B is BD+84@397.                                                        
17390+1320 GC 23923    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17391+0202 SHJ 251     Spectroscopic binary. Composite spectrum, K0III+F4IV.                           
                       AB: HJL1096.                                                            HJL1986 
17392-5112 HJ 4965     B is CD-51@11033.                                                               
17393+0333 GC 23929    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17394+0103 GIC 147     Ross 534 = LDS 998. G020-007AB.                                                 
17395+4600 BLA   5     Aa,Ab: iot Her = 85 Her. A is a spectroscopic binary, now resolved by           
                       speckle interferometry.                                                         
17397+7256 H 1  41     H I 41.                                                                         
17398+0225 OSO  83     G020-008. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
17398-0458 STF2191     B is BD-04@4324.                                                                
17400+4046 ES 9003     Previously known as ES 1556a.                                                   
17400-0038 BU  631     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 6.97 +/- 4.66, 4.77, and 2.82 Msun, respectively.             Mlk2012 
17401+2646 BRT3320     Originally published as BRT 176.                                        Brt1928 
17402+0909 STF2228     GRV 964.                                                                        
17404+0544 VVO  16     Aka CBL 162.                                                                    
17404-1319 HU  182     aka HO  633                                                                     
17405-2045 DON 856     CPD-20@6623.                                                                    
17407+3117 STTA157     B is BD+31@3077.                                                                
17407+1237 BPM 693     [PM2000] 1295265 + [PM2000] 1295297.                                    Gvr2010 
17408-3052 BSS   1     Primary is pulsar PSR J1740-3052; companion appears to be a                     
                       main-sequence star.                                                     Bss2011 
17411+7225 GIC 148     LDS5225. G258-016/G258-017.                                                     
                       RoboAO resolved Ba,Bb in 2013 at 0.26", but not accepted as real        Tok2014d
17411+2431 STF2194     Spectroscopic binary. Composite spectrum K0III+F4IV.                            
                       AB: HJL 252.                                                            HJL1986 
                       AB: H 3 104.                                                            MEv2010 
17412+4139 STF2203     BDS 8128, STTA158.                                                              
17417+2831 ROE 119     BRT 177.                                                                        
17417-4604 SWR 228     CPM pair                                                                Skf2004 
17418+0458 BAL3011     Not found by Heintz at IDS position.                                    Hei1990b
17418-5402 HJ 4969     B is CPD-53@8734.                                                               
17419+7209 STF2241     psi 1 Dra. LDS1874. B is BD+72@805.                                             
                       A premature orbit has been computed.                                            
                       A family of possible orbital solutions are determined by Romanenko      Rmn1994 
                       (1994), with periods  ranging from 5,200 to 120,000 years, using the            
                       method of apparent motion parameters and incorporating parallax and             
                       radial velocity information.                                                    
           STF2241     AB: H 4   7.                                                            MEv2010 
                       31 Dra. Toyota et al. (2009) monitored the RV of both the A and B               
                       components every 1-2 months between 2003 Mar - 2007 Nov, using a                
                       high-dispersion echelle (precision ~10 m/s). The A component exhibits           
                       a linear trend in RV, with a slope +220 m/s/y. Toyota et al. assert             
                       that these variations are due to an unseen companion. Assuming a                
                       circular orbit, period is estimated at 3200d; minimum mass of the               
                       unseen star ~50 Mjup. Standard deviation of radial velocities for the           
                       B component <40 m/s and velocities show no periodic variation. This             
                       result rejects the association of a planet of mass > 1.8 Mjup           Toy2009 
17420+2127 STF2197     DRD   1 initially entered incorrectly as AC pair; later moved to new            
                       WDS designation 17421+2127.                                                     
17421+2127 DRD   1     Initially entered incorrectly as AC pair in 17420+2127.                         
17421-5248 HRG 124     SWR 229. CPM pair                                                       Skf2004 
17422+3804 RBR  20     Triple system. The Riddle et al. (2015) companion at 2".2 is confirmed  RAO2015 
                       as physical by its fixed position and its location on the CMD. The     .        
                       main star is a double-lined spectroscopic binary with P = 6 yr (D.     .        
                       Latham 2012, private communication) and estimated semimajor axis of    .        
                       0".1. Our standard algorithm, fitstars, produced subpar results on     .        
                       this star and instead we used the deconvolution technique used in      .        
                       Riddle et al. (2015) to analyze this star. It is resolved here at      .        
                       0".07. The magnitude difference of Aa,Ab (dK = 2.43) matches the       .        
                       spectroscopic mass ratio of 0.52 and corresponds to the Ab mass of     .        
                       0.60 Msun. The orbital motion of Aa,Ab can be followed with AO and     .        
                       speckle interferometry.                                                Rbr2015d 
17422-4838 TDT 468     Primary is D component of 17422-4839 ANT   3AD. AD does not appear to           
                       be a physcial pair, so the systems were not merged.                             
17422-4839 ANT   3     D component = 17422-4838 TDT 468.                                               
17424+6501 ES 1910     STI 828.                                                                        
17425+2434 ENG  62     83 Her.                                                                         
17427-5740 RST5544     Spectral type of A may be G5.                                                   
17428+1646 BPMA 51     [PM2000] 1301020 + [PM2000] 1301094.                                    Gvr2010 
17430+1213 BPM 694     [PM2000] 1301421 + [PM2000] 1301372.                                    Gvr2010 
17432+8526 LUH  12     G259-20 + 2MASS J17430860+8526594.                                      Luh2012b
17432-2956 ARG  30     B is CD-29@13894.                                                               
17433+5703 LDS1450     NLTT 45369/45370                                                        Chm2004 
17433+2137 DUQ   1     Aa,Ab: Martin et al. (1998) derive component masses 0.942 +/- 0.166             
                       and 0.337 +/- 0.072 Msun.                                               Mig1998 
17433+1751 BPM 696     [PM2000] 1302167 + [PM2000] 1302018.                                    Gvr2010 
17433+1441 BPM 695     [PM2000] 1302165 + [PM2000] 1302484.                                    Gvr2010 
17433-5743 I   377     A is the semiregular variable V Pav, P = 225d.                                  
17434+1110 BPM 697     [PM2000] 1302568 + [PM2000] 1302697.                                    Gvr2010 
17436+5844 ALP  24     2MASSI J1743348+584411                                                          
                       Physical companionship to this ultracool dwarf ruled out based on I-J           
                       color, using I-band photometry taken at WIYN in August 2002.            AlP2007 
17441-5150 HD 160691   No comoving objects found within separation/magnitude range listed.             
                       However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                       background object.                                                              
17443+1425 HJ 1303     A is the eclipsing binary V624 Her.                                             
17444+4027 ES 9004     Previously known as ES 1556b.                                                   
17446+0235 STF2202     61 Oph. A is a spectroscopic binary. B is BD+02@3391.                           
                       AB: H 4  32.                                                            MEv2010 
17447-4244 FIN 341     Appears to be in rapid motion.                                                  
17449-1839 A  2250     A is the semiregular variable SZ Sgr.                                           
17450-1646 VOU  42     Spectrum: Fm Delta Del.                                                         
17450-4511 HJ 4973     B is CD-45@11856.                                                               
17451-5408 R   303     SWR 230.                                                                        
17453+1049 BPM 698     [PM2000] 1307466 + [PM2000] 1307473.                                    Gvr2010 
17456-2824 SHY 729     HIP  86919 + HIP  86672.                                                        
17457+1743 STF2205     A premature orbit has been computed.                                            
17457-2900 Sgr A*      Semimajor axis in mpc was converted to arcseconds based on a quoted     Eck2002 
                       distance of 8 kpc.  Errors for Eck2002 orbits are as follows:           Sel2002 
                                                                                               Ghe2003 
                       Element       Sgr A* - S1       Sgr A* - S2          Sgr A* - S8        Sel2003 
                       ----------------------------------------------------------------------          
                       P (yr)        100. +184/-54     19.4   +7.4/-3.0     57.   +1060/-0             
                       a (mpc)       18.  +18./-8.     5.6    +0.7/-1.1     10.   +48./-0.             
                       a (arcsec)    0.46 +0.46/-0.21  0.14   +0.02/-0.03   0.26  +1.24/-0.00          
                       i (deg)       60.  +/-5.        70.    +6./-17.      0.    +/-70.               
                       Omega (deg)   -14. +7./-12.     23.    +27./-11.     -65.:                      
                       T (by)        2097 +281/-96     2002.6 +6.8/-22.     2043  +1060/-0             
                       e             0.6  +/-0.3       0.8    +0.15/-0.40   0.95  +0./-0.12            
                       omega (deg)   190. +120/-10     190.   +/-10.        -55.  +32/-0               
                       ----------------------------------------------------------------------          
                       Note: This system has grown more complex as additional stars orbiting           
                       the Galactic Center have been observed. With the number of companions           
                       now exceeding 170, it has become increasingly difficult to maintain             
                       the usual WDS designation/component scheme. All WDS pairs were                  
                       therefore copied to the WDSS (WDS supplemental catalog) in July 2017;           
                       henceforth the standard published designations for Sgr A* companions            
                       will be used for all components.                                                
17459+2153 STT 335     B is BD+21@3209.                                                                
17460+3919 STF2224     A is a spectroscopic binary. Composite spectrum, K3III+F7V.                     
                       It is also variable, V826 Her.                                                  
17461+0532 CHR 157     1991.3275  An 18.92d period orbit in Batten et al. (1989) apparently    Bte1989 
                       refers to a closer component.  Membership of this star in the cluster           
                       IC 4665 is in question: Abt et al. (1964) list it as a member,          AbH1964 
                       Sanders & van Altena (1972 A&A, 17, 193) as a non-member.               Msn1993b
17461-3204 LDS 611     B is CD-32@13297.                                                               
17465+2743 TRN   2     Aa,Ab: Astrometric orbit, P=65yr, e=0.32 (Heintz 1994) implies          Hei1994a
                       a=0.265", does not fit the 1.4" companion of Turner (2001).             Trn2001 
                       Roberts et al. derive a spectral type for the secondary of M4V +/- 1.           
                       Using an estimated mass for the primary, they estimate the mass of the          
                       secondary as 0.32 Msun.                                                 Rbr2016a
                       Inclination of this orbit appears to be the same as that of the         GdF2017 
                       rotation axis of the primary.                                                   
           STF2220     A: mu Her = 86 Her is a large-amplitude astrometric binary, P = 65y.            
                       A,BC: LDS1002. HJL 253.                                                 HJL1986 
                       A,BC: H 4  41.                                                          MEv2010 
                       A,BC: Additional notes may be found in Baize (1964).                    Baz1964 
           AC    7     BC: Prieur et al. (2014) derive a dynamical parallax of 123.0 mas and           
                       a total mass of 0.82 +/- 0.07 Msun (based on the revised Hipparcos      VlF2007 
                       parallax of van Leeuwen 2007).                                          Pru2014 
17465-0305 BRT 471     Not found by Heintz at IDS position.                                    Hei1985a
17468+0534 A  1161     In IC 4665.                                                                     
17469+3555 MLB 936     Not found by Heintz at IDS position.                                    Hei1990b
17471+4737 CHR  64     A spectroscopic binary, P = 2.8d. Hence triple.                                 
17471+1742 STF2215     A spectroscopic binary. A premature visual orbit has been calculated.           
17475-0847 OSO  84     G020-015.                                                                       
17476-2622 J  1732     CPD-26@5975.                                                                    
17476-4008 SEE 338     iot 1 Sco. A is a spectroscopic binary.                                         
17477+2748 GIC 149     G182-026/G182-027.                                                              
17477-8213 WJG   1     BC: Originally 17464-8212 WJG   1, but primary was found to be B                
                       component of 17477-8213 LDS 603.                                                
17478-2211 B   358     CPD-22@6444.                                                                    
17480-5442 I   612     Primary is V537 Ara, Algol-type eclipsing binary, period 1.874351d.     Zas2013 
17482+1339 BPM 699     [PM2000] 1315705 + [PM2000] 1315640.                                    Gvr2010 
17483+1740 BPM 700     [PM2000] 1315759 + [PM2000] 1315895.                                    Gvr2010 
17483+1547 FOX 209     AC: Also known as J   753AC. Identical nature noted by Friedrich                
                       Damm.                                                                           
17483-3525 JSP 732     CPD-35@7269.                                                                    
17489-2219 BRT1508     CD-22@12253.                                                                    
17490+3704 COU1145     1981.333: This observation was incorrectly attributed to COU 1445 in    Tok1982a
                       Tokovinin (1982).                                                       Tok1982b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.84 +/- 0.14, 2.27, and 1.05 Msun, respectively.             Mlk2012 
17491+5047 CHR  65     Aa,Ab: 30 Dra.  Hipparcos Acceleration Double Solution.                         
                       This system, first announced by McAlister and recalled in a later       McA1984b
                       McAlister paper after repeated attempts at confirmation, has been       McA1993 
                       restored. While perhaps still spurious, the subsequent confirmation or          
                       suspected duplicity (by another technique) makes the discovery                  
                       measurement somewhat more probable.                                             
17491+1151 BPM 701     [PM2000] 1318164 + [PM2000] 1318445.                                    Gvr2010 
17492-3618 JSP 734     CPD-36@7625.                                                                    
17494+2651 BRT3322     Originally published as BRT 178.                                        Brt1928 
17496-2000 HJ 2810     AB: The CPD identifications of A and B are -19@6275 and -19@6274.               
                       AD: D component is planetary nebula NGC 6445.                                   
17499-7505 SWR 231     A component not CD-75 9877: +1m CD RA error, thus = CPD-75 1397         Skf2004 
17502+4424 SIG   3     2MASSW J1750129+442404.                                                         
                       Spectral types M7.5, M9.5. Estimated orbital period 36 +10/-9 yrs.      Sig2003 
                       Konopacky et al. (2010) derive a distance of 37.6 +/- 12.3 pc and a             
                       system mass of 0.20 +/- 0.12 Msun.                                      Kon2010 
17502-1339 LDS5856     NLTT 45517/45519                                                        Chm2004 
17502-4005 HDO 279     iot 2 Sco                                                                       
17503+2517 STF2232     H 3  40.                                                                MEv2010 
17503+1737 BPM 702     [PM2000] 1321865 + [PM2000] 1321463.                                    Gvr2010 
17504+5414 OL   89     Aka TDS 888.                                                                    
17504-3652 JSP 737     CPD-36@7660.                                                                    
17505-0603 LAF  59     Due to the large number of components (exceeding the number of upper-           
                       case letters), a non-standard component designation was necessary,              
                       hence the pairings A,Ya; A,Yb; etc. For this pair, as well as LAF  62           
                       and LAF  71, the lower-case designations (such as Ya and Yb) do not             
                       refer to components of a close pair.                                            
17505-4655 CPO 556     SWR 232. CPM pair                                                       Skf2004 
17505-4817 HJ 4982     B is CD-48@12074.                                                               
17505-5337 HJ 4978     A is the Algol-type system V539 Ara.                                            
17506+0714 STT 337     Quadrant uncertain. Star approaching periastron.                        Baz1954a
                       In AJ 63, 68, 1958 I have given a mean of 5 measures of ADS 10828. The  B__1958 
                       first measure is not of this pair, but of the nearby pair ADS 10846.            
                       The result for 10828 should read: 1957.449, 22.7, 0.24, 8.4-8.7, n=3    B__1962a
                       A premature orbit has been computed.                                            
17506-4019 EGN  21     AB pair unbound, but bound/unbound nature of AC pair inconclusive.              
                       Primary is planet host star.                                            Egn2007 
           HD 162020   Chauvin et al. (2006) note finding at least one faint companion         Cvn2006 
                       candidate within separation/magnitude range listed. However, further            
                       observations are required for verification.                                     
17507+0755 STF2230     B is BD+07@3483.                                                                
17507-3444 BRT1741     CPD-34@7161.                                                                    
17509-3342 HDO 280     Classical Cepheid RY Sco.                                                       
17510+5709 STI2360     LDS1455.                                                                        
17515-7748 LDS 609     TSN 104.                                                                        
17518-1336 HU  188     Spectrum: B9.5III/IV.                                                           
17520+1520 STT 338     L    16.                                                                        
                       AB: Prieur et al. (2012) derive a dynamical parallax of  7.9 mas and            
                       (using their orbital elements and the revised Hipparcos parallax of             
                       van Leeuwen 2007 A&A 474, 653) a total mass 12. +/- 11. Msun.           Pru2012 
17520-0114 HR 6659     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Griffin (1980).                                                         Grf1980a
                       SB1. Combined orbit including RV data and Hipparcos Intermediate                
                       Astrometric data. Semimajor axis derived from photocentric a0 plus              
                       stellar evolutionary model. Derived properties for A and B:                     
                       M/Msun = 1.66 + 0.41, L/Lsun = 42.50 + 0.03, dm = 7.88 mag,                     
                       log age = 9.29.                                                         WaX2015b
17521+0107 S   694     STTA159. B is BD+01@3525.                                                       
17523+4057 A   699     Also unresolved 1960.                                                           
17523+3624 OSO  85     G182-031. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
17524+1733 BPM 703     [PM2000] 1327958 + [PM2000] 1327923.                                    Gvr2010 
17525+1530 WLY  17     AC: Previously known as FOX 209. That pair is actually at 17483+1547            
                       and the pair measured here is new. The correct identification was               
                       ascertained by Friedrich Damm.                                                  
17526+1154 BPM 704     [PM2000] 1328639 + [PM2000] 1328474.                                    Gvr2010 
17526-0609 EVS  32     Primary is the Cepheid Y Oph.                                           Evs2016a
17527+1459 BPM 705     [PM2000] 1328958 + [PM2000] 1328887.                                    Gvr2010 
17530+8354 STT 349     Heintz (1978) suspects the presence of an unresolved star.              Hei1978d
                       Unless motion takes place in a very short period these measures are             
                       unusually discordant.                                                   VBs1954 
17530+1521 OSO  86     G183-009. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
17530-0755 STF3128     Separation 0.56" of my single night's measure in 1958 (Pub Yerkes Obs   B__1960b
                       IX, pt I, p 77) should read 0.22".                                      B__1963a
                       Semi-major axis incorrectly given as 0.935 by Popovic & Catovic (1989)  Pop1989b
                       should be 0.985 (erratum noted in Inf. Circ. 108, 1989)                         
                       HIP 87533. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
17532+3713 DAE  11     TrES-4.  Daemgen et al. (2009) estimate spectral types F8 and K5.5-M0,          
                       masses 1.18 and 0.59 Msun, and an orbital period of about 21000y.       Dae2009 
                       Bergfors et al. (2013) estimate spectral types F8V and K4.5-M1.5V.      Brg2013 
17533+4000 BU  130     90 Her.                                                                         
17533+2459 A   235     A 2007 measure was inadvertently confused with a measure for BU 435 in          
                       Mason et al. (2011); this measure has been corrected.                   Msn2011d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.88 +/- 0.44, 1.97, and 0.91 Msun, respectively.             Mlk2012 
17533-3444 BU 1123     A premature orbit has been computed.                                            
17533-3547 BRT3324     AB: Not found by Hinetz.                                                Hei1987a
           BRT3325     CD: CPD-35@7400. Not found by Heintz.                                   Hei1987a
17534+1058 STTA160     B is BD+10@3314.                                                                
17534-2639 HJ 4991     B is CD-26@12487.                                                               
17534-3454 SEE 342     Spectroscopic binary.                                                           
17534-3907 VOU  96     Coordinates are those of DM cross-reference. Original WDS designation           
                       18534-3858 for this pair apparently had 1h error in RA. Unfortunately,          
                       original reference is unknown, so impossible to check.                          
17535+5652 LDS1457     xi Dra = 32 Dra = Grumium                                                       
17535-0355 TOK  54     Primary is V2610 Oph, eclipsing binary of W UMa -type, period                   
                       0.42651 d.                                                              Zas2012 
17536-1726 HDO 147     BHA  59                                                                         
17536-3445 B   362     CPD-34@7283.                                                                    
17537+1702 BPM 706     [PM2000] 1332137 + [PM2000] 1331879.                                    Gvr2010 
17538+1610 BPM 707     [PM2000] 1332342 + [PM2000] 1332598.                                    Gvr2010 
17539-3445 B  1871     One component is a Beta Lyrae-type system, V906 Sco.                            
17540+0303 OSO  87     G020-019. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
17542+1240 BPM 708     [PM2000] 1333651 + [PM2000] 1333727.                                    Gvr2010 
17542+1108 FIN 381     Primary is 0.80d W UMa ecl. bin (V2388 Oph). Called a SB in the                 
                       Bright Star Catalogue; this may be motion in the visual pair.                   
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.83 +/- 1.03, 3.32, and 1.20 Msun, respectively.             Mlk2012 
                       Docobo & Andrade (2013) derive a dynamical parallax of 13.45 +/- 0.38           
                       mas and component masses 1.76 +/- 0.22 and 1.38 +/- 0.18 Msun (based            
                       on photometry of Yakut et al. 2004 A&A 417, 725) or 13.82 +/- 0.39              
                       mas, 1.72 +/- 0.24 and 1.18 +/- 0.16 Msun (based on photometry of               
                       Rucinski et al. 2002 AJ 124, 1738). See paper for extensive notes on            
                       this system.                                                            Doc2013d
                       Zasche et al. (2014) derive a combined solution, including                      
                       interferometry plus times-of-minimia variations in the primary. They            
                       determine a distance of 70.6 +/- 8.9pc and masses of 1.96 +/- 0.03 and          
                       0.54 +/- 0.06 Msun.                                                     Zas2014b
17547+2016 OSO  88     G183-011. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
17551+3745 OSO  89     G182-032. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
17551+3134 AG  215     SEI 551.                                                                        
17555+2250 GRV 970     DAL  25.                                                                        
17555+1322 BPM 709     [PM2000] 1337739 + [PM2000] 1337455.                                    Gvr2010 
17557-1156 HJ 4997     LDS 617.                                                                        
17557-2456 J  2194     May be CD-24@13632.                                                             
17557-3034 I  1011     Spectrum: B9.5II/III.                                                           
17558+3117 SEI 552     ES  342.                                                                        
17559-7032 HJ 4976     B is CPD-70@2439.                                                               
17560-6632 HJ 4983     B is CPD-66@3163.                                                               
17561+2130 STT 339     CfA: A or B is SB?                                                      Tok2014d
17563+6237 STTA163     AB: Pair appears in an appendix list, not part of discoverer's regular          
                       numbering sequence.                                                             
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
17563+0259 A  2189     Systemic mass is estimated at 4.1 +/- 0.5 Msun, assuming a dynamical            
                       parallax of 4.75 +/- 0.15 mas.  The Hipparcos parallax for this pair            
                       is poorly determined (3.67 +/- 1.12 mas)                                Doc2008a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 27.45 +/- 27.60, 6.25, and 2.09 Msun, respectively.           Mlk2012 
17563-1549 HJ 2814     B is BD-15@4723.                                                                
17563-3228 JSP 748     A is the eclipsing binary V453 Sco, P = 12.61d.                                 
17564+1820 MCA  49     Aa,Ab: 1980.4820: This measure was incorrectly attributed to HR 6148            
                       by McAlister et al. (1983).                                             McA1983 
17565-3408 JSP 934     CPD-34@7399.                                                                    
17566+5813 ES   20     A is the Mira-type variable T Dra, BD+58@1772a.                                 
17566+5129 BU  633     gam Dra = 33 Dra = Etamin. A is variable.                                       
                       AF. Smyth's quoted separation is difference in RA only.                 Smy1844 
17567-3255 BRT1743     Not found by Heintz at IDS position.                                    Hei1990b
17568+1736 BPM 710     [PM2000] 1341630 + [PM2000] 1341762.                                    Gvr2010 
17568+0459 V566 Oph    Multiple system including contact binary. Pribulla & Rucinski (2006)    Pbl2006 
                       estimate the mass of the contact pair at 1.828 Msun and the minimum             
                       mass of the wider component at 0.24 Msun.                                       
17568-2036 J  1617     AB: ARA1132.                                                                    
17568-3755 JSP 751     CPD-37@7662.                                                                    
17569+1811 J  1352     Jonckheere notes ADS positions are 1970 and 1920. In his 1952 paper             
                       he uses 1950 ADS position and has a note "two couples?".  There is              
                       indeed a measure that indeed looks different:                                   
                       1951.62, 39.9@, 3.33", 11.3-11.3.                                       J__1952 
                       Observations incompatible. Is there confusion between different pairs,          
                       as thought by Jonckheere (JO 35, p 53)?                                 Cou1952b
17569+0610 HD163642    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17569-1903 FEN  25     17570-1903ARA 718                                                               
17569-3445 JSP 935     Primary is V907 Sco, Algol-type eclipsing binary, period 3.776277d.     Zas2013 
                       Triple star. The orbital planes of the B9.5V eclipsing binary and the           
                       more distant companion (per= 99.3 d.) are not coplanar so the orbital           
                       plane of the eclipsing binary shows nodal regression with a period of           
                       68 years. For about one-third of this time, the close binary is                 
                       eclipsing, the rest of the time the inclination is too small for                
                       eclipses to occur. The earliest observations of the system in the year          
                       1899 show eclipses; the eclipses stopped about 1918, started again              
                       about 1963, and stopped again in about 1986. Eclipses should start              
                       occurring once again in the year 2030+/-5. (Otero, 1999 AJ 117, 541L).          
17569-3514 BRT1744     CPD-35@7528.                                                                    
17571+0004 STF2244     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 8.83 +/- 5.28, 4.60, and 2.00 Msun, respectively.             Mlk2012 
17572+3541 HO   73     Also known as POP  10. HO   73 was at the location of BD+35 3111, the           
                       DM number to which it was assigned and then POP  10 was rediscovered.           
                       All measures have been assigned to HO   73AB and STF2256AC at the               
                       coordinates of POP  10.                                                         
           STF2256     AC: WAL  86CD. The pair 17574+3540 WAL  86AC is not physical, so the            
                       systems have not been merged.                                                   
17572+2400 MCA  50     A close pair of solar-type stars, astrometric binary                            
                       Balega et al. (1984) derive probable period of 940 days                 Bag1984a
                       Culver et al. (1980 BAAS 12, 250) report this to be a spectroscopic             
                       binary with a period of 2.6 years.                                      Bla1987 
                       Determination of these two old measures resulted from new reduction             
                       techniques developed over the past year; these data were reanalysed             
                       for a joint spectroscopic/speckle analysis of this system.              Hrt1992b
                       All our CCD speckle data for this close system have been reprocessed            
                       and examined. In addition, we have listed 7 negative measures dating            
                       from observations made at the KPNO 2.1-m in the 1970's.                         
                       Hartkopf et al. (1994) derive a combined spectroscopic/interferometric  Hrt1994 
                       solution.                                                                       
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       McAlister et al. (1995).                                                McA1995 
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       Orbit determined by fitting revised Hipparcos intermediate astrometric          
                       data. Derived component masses 1.12 +/- 0.17 and 0.72 +/- 0.11 Msun.    Ren2010 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.29 +/- 0.27, 2.15, and 1.79 Msun, respectively.             Mlk2012 
                       Kiefer et al. (2016) generates a combined spectroscopic/astrometric             
                       orbit, yielding masses 1.132 +/- 0.014 and 0.7421 +/- 0.0073 Msun, and          
                       a parallax 36.35 +/- 0.20 mas.                                          Kie2016 
17573+1238 HD163750    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
17573-5212 HJ 4994     B is CPD-52@10926.                                                              
17574+5111 ES   78     Fox also notes a 1" double (12 mag.) 23" from A in 199@.                Fox1915 
17574-3508 JSP 753     CPD-35@7547.                                                                    
17575+1318 BPM 711     [PM2000] 1344016 + [PM2000] 1344347.                                    Gvr2010 
17575+1058 BU 1299     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 9.51 +/- 8.13, 3.18, and 0.65 Msun, respectively.  Mlk2012 
17575-5740 HJ 4992     SWR 234. CPM pair                                                       Skf2004 
17578+4635 BDK   9     G 204-39 + SDSS J175805.46+463311.9. Distance 13.6 +/- 0.3 pc for               
                       primary, 12 +/- 2 pc for secondary. Estimated age of system 0.5-1.5             
                       Gyr. Mass of secondary estimated at 0.020-0.035 Msun.                   Fah2010 
17578+2751 ALL   2     HJL 254.                                                                HJL1986 
17578+1542 BPM 712     [PM2000] 1344986 + [PM2000] 1345358.                                    Gvr2010 
17578+0442 GJ 699      Ci 20,1069 = Barnard's Star                                                     
                       van de Kamp orbits rejected from Fourth Orbit Catalog                   Kam1969c
                       ("object still suspected to be binary by some, but no even              Wor1983 
                       approximately reliable or complete elements yet available")                     
17579-1921 RST5097     CPD-19@6357.                                                                    
17583-3810 I  9004     Previously known as I  1347 1/2.                                                
17584+1812 J  3268     Aka J  3236.                                                                    
17584+0428 KUI  84     In the same field with Barnard's Star.                                          
                       P, T, and e have been taken by Gatewood (1973) from the astrometric     Gat1973 
                       solution. In the same field with Barnard's Star. Two astrometric                
                       mass-ratio determinations showed B to be twice as massive as A. This            
                       has been confirmed by Tokovinin, who finds B to be a SB, P = 34.5d.     Tok1994b
                       A measurement published by McAlister et al. (1987) dating from          McA1987b
                       1985.4872 was misidentified as being of KUI 84; the measurement was             
                       actually of KUI 89 (WDS 18594-1250). In addition, an observation of             
                       KUI 84 dating from 1988.6655 (theta = 270.6 deg, rho = 0".134) was              
                       published by McAlister et al. (1990). The data have been reprocessed,   McA1990 
                       and we now believe the 1988.6655 measurement was spurious.              Hrt1994 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.57 +/- 0.61, 1.41, and 0.58 Msun, respectively.             Mlk2012 
17584-1747 RST3140     TDT 605.                                                                        
17586-1306 HU  190     HIP 88010. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
17587+1530 BPM 713     [PM2000] 1347830 + [PM2000] 1347917.                                    Gvr2010 
17587-2232 B   367     CPD-22@6498.                                                                    
                       Additional notes may be found in van den Bos (1928)                     B__1928b
17588+1330 RUC  10     V508 Oph. Spectral type of resolved companion later than M5V.           Ruc2007 
17589-2850 B  2848     CPD-28@6088.                                                                    
17589-3652 DUN 219     B is CD-36@12058.                                                               
17590+3003 STF2259     H 4  42.                                                                MEv2010 
17590+0259 BAL2462     J 2119. The close pair suspected by BAL is not confirmed.               Hei1985a
                       In Carte du Ciel, primary is listed as a double of 180deg, 0.9", mags           
                       9.9 and 11.4; but it appears single.                                    Cou1953d
17590+0202 STF2252     C is BD+02@3444.                                                                
17591-3015 PZ    6     A is variable.                                                                  
17591-3559 JSP 758     CPD-35@7594.                                                                    
17592+0304 BAL2464     J 2120.                                                                         
17592-3656 HJ 5000     A is the Algol-type system V1647 Sgr.                                           
17593-0651 STF2250     Same as STF2249.                                                                
17594+1151 BPM 714     [PM2000] 1350087 + [PM2000] 1350363.                                    Gvr2010 
17594-1724 RST3144     A is the Algol-type system WX Sgr.                                              
17595+1753 BPM 715     [PM2000] 1350465 + [PM2000] 1350660.                                    Gvr2010 
17595-3601 TRN  25     The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.4960 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
           HD 163758   MR 78. Leep (1978 ApJ 225, 165) also finds a constant radial velocity.  Msn1998a
17597+3624 OSO  91     G206-001. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004