18001+1517 BPM 716     [PM2000] 1352292 + [PM2000] 1352563.                                    Gvr2010 
18002+8000 STF2308     AB: LDS1882. HJL 257. Statistically the same parallax within the        HJL1986 
                       errors would indicate the components are physical.                              
                       Linear elements fit nicely at present, but this is a physical pair and          
                       an orbit can be computed at some future date.                                   
                       AB: H 4  67.                                                            MEv2010 
                       AB: A,B are 2.6 mag above MS, both evolved, both SB systems. Orbital            
                       parallax 23.0+-2.2mas. Masses 1.39,1.30,1.32,1.20.                      Tok2014d
           BAG   6     A: 41 Dra. Spectroscopic binary, P = 1247.2d, with the highest known            
                       eccentricity to date, e = 0.975.                                                
                       Elements P, T, and e for the Balega et al. (1997) orbit were adopted    Bag1997a
                       from the spectroscopic orbit of Tokovinin (1995).                       Tok1995b
                       Combined spectroscopic/speckle solution by Tokovinin et al. (2003),     Tok2003 
                       deriving masses (1.28 +/- 0.15, 1.20 +/- 0.14 Msun) and orbital                 
                       parallax (23.0 +/- 2.2 mas). Authors note earlier elements and discuss          
                       possibility of orbital evolution.                                               
                       Effective temperatures for the two components are 6370+/-20 and                 
                       6410+/-20K, log g 4.05+/-0.10 and 4.20+/-0.10. Abundances for both              
                       components are very near solar.                                         Bag2005b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 7.75 +/- 5.22, 3.34, and 2.24 Msun, respectively.  Mlk2012 
                       B: 40 Dra = BD+79@570. B is also a spectroscopic binary, P = 10.53d.            
18002+0851 STTA161     B is BD+08@3556.                                                                
18003+5251 STF2271     AB: B is SB2, P=18.888d                                                 Tok2014d
18003+2154 A  1374     Angle decreasing.                                                               
                       AB: Additional notes may be found in Baize (1945).                      Baz1945b
18003+0038 RAS  26     Peculiar SrCuEu star V2126 Oph, type A3. Companion likely                       
                       late-G/early-K; orbital period perhaps 10y.                             Ras2014 
18005-3742 I   230     CPD-37@7765.                                                                    
18006+2934 LDS6413     NLTT 45789/45791                                                        Chm2004 
18006+0256 BU 1124     67 Oph.                                                                         
           H 6   2     H VI 2. STTA162.                                                                
18009+2633 STF2263     H 2  90.                                                                MEv2010 
18011+3558 POP 210     Codiscovered by Olevic.                                                 Ole1970b
18015+2136 STF2264     95 Her. B spectrum G8III.                                                       
                       Measure of 1927.47 made by triangulation of multiple measures.                  
                       H 3  26.                                                                MEv2010 
18015+0448 OSO  92     G140-031. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
18015+0006 WTT   1     The primary is of type G5V, with mass 1.10 +/- 0.01 Msun. Based on              
                       isochrone fitting, Wittrock et al. (2016) estimate the mass of the              
                       secondary at 0.42 +/- 0.03 Msun, and type likely an M dwarf.            Wtt2016 
18015-3612 BRT1750     CPD-36@7919.                                                                    
18015-3732 JSP 763     CPD-37@7798.                                                                    
18017+3714 GCB  29     J 3212.  Also known as BRT2222.                                                 
18018+0118 BU 1125     68 Oph. A spectroscopic binary.                                                 
18019-1906 HD 164438   We found a possible binary companion at a separation of 0".05 which             
                       needs confirmation. The classification is from Garrison et al. (1977            
                       ApJS 35, 111).                                                          Msn1998a
18022-3616 BRT1751     CPD-36@7937.                                                                    
18024+1758 BPM 717     [PM2000] 1359934 + [PM2000] 1359490.                                    Gvr2010 
18024-2302 SNA  77     Aa,Ab: HD 164492A is the center of a wide multiple system. We detected          
                       two additional faint companions at 3.1" and 6.5", and further resolved          
                       A into a 25mas pair with a rather faint companion (dH=3.2). The         Cti1977 
                       object was reported as RV variable by Conti et al. (1977) but this is   Cii2012 
                       not confirmed by Chini et al. (2012).                                   Sna2014 
18025+4414 BU 1127     A premature orbit has been computed.                                            
                       L 18 is probably the same star                                          VBs1960 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       L    18.                                                                        
18025+2619 HO  564     Burnham measured BD+26@3146, 26s preceding and 4' south of HO 564:      Bu_1913 
                       1905.8, 185.4@, 23.22", 8.3-11.5.                                               
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
18026+0429 LDS5859     LDS6323.                                                                        
18028+7547 STF2302     STN  45 (with 1h error in RA).                                                  
18028+0137 BU  635     C is BD+01@3566.                                                                
18029+5626 STF2278     STTA166.                                                                        
                       AB: The BD numbers of A and B may be reversed. D is reversed.                   
                       DS: Also known as ES 1745.                                                      
18030-2243 RSS 468     CD-22@12473                                                                     
18031+4828 STF2277     Mt. Wilson spectral type of B is G8.                                            
18031+1654 BPM 718     [PM2000] 1362136 + [PM2000] 1362258.                                    Gvr2010 
18031-0811 STF2262     tau Oph = 69 Oph. A is a SB. RV of the primary may be variable.         Wrz1959 
                       Primary giant according to isochrone fit.                               Sod1999 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: H 1  88.                                                            MEv2010 
18032-0543 HR 6940     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Scarfe et al. (1983).                                                   Scf1983 
18032+2522 STF2268     AC : 1909.56: Measure unpublished in orbit quotation.                   Dob1927 
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
18032+0755 STTA164     B is BD+07@3536.                                                                
18032+0047 BAL1192     J 1371.                                                                         
18033+3921 STF2275     Not the same as L    19, though some measures were misidentified.               
18034+2324 POU3344     LDS1004.                                                                        
18034+0825 GC 24579    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18035+4032 COU1785     Systemic mass is estimated at 3.0 +/- 0.6 Msun, assuming a dynamical            
                       parallax of 7.32 +/- 0.10 mas.  This is consistent with a pair of F5            
                       dwarfs. There is no Hipparcos parallax for this star.                   Doc2008a
18037-2423 SBE   1     Aa,Ab: Herschel 36 is a young massive system located at 1.3kpc in the           
                       Hourglass high-mass star-forming region in the central part of the M8           
                       nebula. The Ab component is comprised of two stars, spectral types O9V          
                       and B0.5V, in a close orbit with period 1.54d. The Aa component is of           
                       type O9.5V, and is the most luminous star of the system, dominating             
                       its ionizing flux. Aa and Ab are in an orbit with estimated period              
                       500d and projected semi-major axis 3.5mas. The minimum spectrosopic             
                       predicted mass of the Aa+Ab1+Ab2 system is 45,2 Msun. Arias et al.              
                       (2010, ApJ 710, L30) label the components A, B1, and B2 in their                
                       spectroscopic study of the system.                                      SBe2014 
18039+2639 HO  426     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
18039-2419 SNA  79     The faint but clear companion at 57mas is not the known SB2 system              
                       (P=3.8d, a sin i = 16Rsun), which is separated by 0.07mas assuming a            
                       distance of 1 kpc (Trepl et al. 2012, MNRAS 427, 1014). Moreover, the           
                       SB2 has nearly equal masses, while the resolved pair has dH=3.4,                
                       pointing to quite different masses. The object is also detected in X            
                       rays. Trepl et al. identified a soft X-ray excess and 10sec pulsation           
                       which they interpret as the signature of a neutron star in the system.          
                       Our detection is probably an active later-type object, which may                
                       provide an alternaitve explanation to the X-ray excess.                 Sna2014 
18039-2422 SNA  78     9 Sgr. The primary is an emmission-line star. PIONIER clearly resolves          
                       the long-period SB2 discussed by Rauw et al. (2012, A&A 542, A95) at a          
                       separation of ~5mas.                                                    Sna2014 
18040+3923 L    19     Not found by van den Bos in 1958. Not the same as STF2275, although     B__1960b
                       some measures were misidentified.                                               
18040-2529 HDO 148     EGB   6.                                                                        
18042-2846 BRT3058     J 1644.                                                                         
18043+4206 COU1786     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.80 +/- 1.44, 3.07, and 1.45 Msun, respectively.             Mlk2012 
18043-4019 WG  222     CPD-40@8381.                                                                    
18044-2423 RBR   8     The X ray flux of the closer E and W companions indicate they are M and         
                       K dwarfs, identifying them as young stars that are physical companions          
                       rather than field stars.                                                        
18044+0337 A  2257     Systemic mass is estimated at 2.9 +/- 0.6 Msun, assuming a dynamical            
                       parallax of 4.73 +/- 0.20 mas.                                          Doc2008a
18044+0329 STF2266     AB: HJL 255.                                                            HJL1986 
18044-5953 RST5099     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.92 +/- 2.31, 2.17, and 0.97 Msun, respectively.             Mlk2012 
18046+5053 STF2279     HJL 256.                                                                HJL1986 
18046-1702 HU  194     Spectrum: Fm Delta Del.                                                         
18047-5913 HJ 5006     LDS 622.                                                                        
                       A is SB1, P=108.55d, incl. brown dwarf SB component: Tinney et al.              
                       (2001 ApJ, 551, 507)                                                    Tok2014d
18048+1253 BPM 719     [PM2000] 1368153 + [PM2000] 1368073.                                    Gvr2010 
18049+0311 BAL2471     J  3341.                                                                        
18050-2935 BLM   5     Aa,Ab: gam 1 Sgr. A is the Cepheid W Sgr, spectrum also variable.               
                       It is a long-period spectroscopic binary and speckle/occultation pair           
                       1976.477: This measurement resolves the variable star.                  BLM1978 
                       Masses are 5.8 and 2.2 Msun. Estimated period = 173y, a = 63au = 0.15". Evs2013 
18051-4040 CPO 571     CPD-40@8400.                                                                    
18053+8129 STF2326     B is BD+81@618.                                                                 
                       Additional notes may be found in Dembowski (1883).                      D__1883 
18053+1400 BPM 720     [PM2000] 1369739 + [PM2000] 1369615.                                    Gvr2010 
18054+1527 BPM 721     [PM2000] 1370110 + [PM2000] 1369687.                                    Gvr2010 
18054-2140 TOK 365     The faint red companion at 6".6 is likely optical. This is a very               
                       crowded field in the direction of the Galactic center. We see another           
                       companion at 10".8, but only in the red channel.                        Tok2013b
18055+0230 STF2272     70 Oph = p Oph. A complicated multiple system with high proper motion,          
                       which has led to some confusion in component identification. A 1924             
                       measure by Burton supposedly of AW was not to the same W component as   Btn1929b
                       measured in earlier VW observations. The Burton secondary is now named          
                       Y. Similarly, See supposedly measured the BR pair; this pair is now     See1911 
                       labelled BZ.                                                                    
                       A component is 70 Oph.                                                          
                       Spectral types K0V,K4V. Proper motions of A and B are (+276,-1092) and          
                       (+442,-1253), respectively. Proper motion of other components follow:           
                          C : -019-012     D : -002+002     R : -007-007                               
                          S : +005-004     T : +001-006     U : -013-010                               
                          V : +002-014     Y : -023-028     Z : -022+007                               
                       The existence of a third body, for which orbits have been computed, is          
                       now generally discounted as the strong photographic coverage fails to           
                       show any such variation. Batten & van Dessel (1976) discuss the radial  Bte1976 
                       velocities.                                                                     
                       Pourbaix gives combined solution for this resolved SB2, yielding                
                       orbital parallaxes and component masses.                                Pbx2000b
                       1995.559: Absolute quadrant determined by triple-correlation technique  Pru2002b
                       AB: H 2   4.                                                            MEv2010 
                       AB: Additional notes may be found in Simonov (1937) and                 Smw1937 
                       Fatou (1941).                                                           Fat1941 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.60 +/- 0.22, 1.61, and 1.56 Msun, respectively.  Mlk2012 
                       AC, AD, AR, AS, AT, AU, AV: Optical pairs, based on study of relative           
                       motion of components using the method of apparent motion parameters.    Kiy2008 
                       From their combined speckle/spectroscopic solution, Eggenberger et al.  Egn2008 
                       (2008) derive masses 0.89 +/- 0.02 and 0.73 +/- 0.01 Msun and a                 
                       parallax of 194.2 +/- 1.2 mas. Adopting both asteroseismic and                  
                       non-asteroseismic observational constraints with several models, they           
                       derive an age of 6.2 +/- 1.0 Gyr, an initial helium mass fraction Y =           
                       0.266 +/- 0.015, and an initial metallicity (Z/X) = 0.0300 +/- 0.0025.          
                       AS: Additional notes may be found in Burnham (1894).                    Bu_1894 
18057+1200 STF2276     A is a spectroscopic binary, and B is a variable of the Beta CrB-type.          
                       AB: H 3  56.                                                            MEv2010 
18057-3437 HJ 5012     B is CD-34@12450.                                                               
18058+2127 STT 341     Triple solution with C (HIP 88639). Primary is 0.88d RS CVn-type                
                       variable or eclipsing binary (V772 Her).                                Sod1999 
                       Combined visual-spectroscopic orbits by Heintz (1982); the lines were   Hei1982b
                       separated at periastron passage. Star A is an eclipsing SB1, P = 0.88d  Hei1982e
                       (Batten et al. 1979).                                                   Bte1979 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.47 +/- 0.51, 2.06, and 2.00 Msun, respectively.  Mlk2012 
                       AB: A is SB1E, P=0.870d. AB is SB2, P=20.081y                           Tok2014d
                       AB,C: C is SB2, P=25.763d                                               Tok2014d
18059-2134 ARA1507     Aka J  1736.                                                                    
18060+0434 STTA165     B is BD+04@3594.                                                                
18060-0807 A  2595     A is SB, no SB orbit.                                                   Tok2014d
18060-1412 HD 165319   The classification and distance are from Crampton & Fisher (1974 Pub            
                       DAO 14, 283).                                                           Msn1998a
18060-2238 BRT1513     J 2099.                                                                         
18061+1257 BPM 722     [PM2000] 1372670 + [PM2000] 1372512.                                    Gvr2010 
18061-2412 SNA  81     Aa,Ab: We detect a third companion to this SB2 4.6d eclipsing binary            
                       system (Otero 2007, Open European Journal on Variable Stars 72, 1;      MyP2013 
                       Mayer et al. 2013).                                                     Sna2014 
18062+1427 BPM 723     [PM2000] 1373116 + [PM2000] 1372803.                                    Gvr2010 
18063+6543 LDS1461     NLTT 45993/45994                                                        Chm2004 
18063+3824 HU 1186     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.00 +/- 0.69, 2.28, and 1.10 Msun, respectively.             Mlk2012 
18064-4145 HJ 5011     B is CD-41@12402.                                                               
18065+0920 HZG  12     B is BD+09@3560.                                                                
18066+4616 HD166067    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18067+1359 AG  358     AB = J    94.                                                                   
18068+0853 BUP 179     Soulie (1984) misidentified Burnham's C component; this pair has been   Sle1984 
                       designated SLE 133AF. There is apparently an error in the declination           
                       of Soulie's D component.                                                        
                       BG: This pair was erroneously identified as BC.                                 
           GC 24683    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18068-4325 HJ 5014     Quoted errors in P and a for the Argyle et al. (2002) orbit are         Ary2002b
                       +170/-97y, +0".66/-0".41, respectively.                                         
                       Member of the bet Pic moving group.                                     Zuc2001b
18069+1712 BPM 724     [PM2000] 1375827 + [PM2000] 1375834.                                    Gvr2010 
18070+3034 AC   15     99 Her.                                                                         
                       Identification of the ascending node is not very certain.               Hei1972 
                       Kennedy et al. (2012) derive a system mass of 1.4 Msun, using the van           
                       Leeuwen(2008) distance 15.64pc. Using the spectroscopic mass function   VlF2008 
                       of Abt & Willmarth (2006), this yields component masses 0.94 and 0.46   AbH2006 
                       Msun for A and B, respectively.                                         Knd2012 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.73 +/- 0.23, 1.85, and 1.13 Msun, respectively.  Mlk2012 
18071+4943 STT 344     A is a spectroscopic binary.                                                    
18071+3223 HJ 1314     SEI 557.                                                                Nsn2017b
18071-4949 I  1350     I 1350a.                                                                        
18073+0934 STT 342     72 Oph. Spectroscopic binary.                                                   
18074+1817 BPM 725     [PM2000] 1377794 + [PM2000] 1377731.                                    Gvr2010 
18074-3011 B  1350     Spectrum: B9.5/A0IV/V.                                                          
18074-4644 SHY 737     HIP  88782 + HIP  87887.                                                        
18075+4552 KUI  85     Nova Herculis. Not a true visual double star, but the system contains           
                       the eclipsing binary DQ Her.                                                    
18075+2846 STA   2     omi Her = 103 Her. A spectroscopic and interferometric binary.                  
                       1981.373: Result needs further confirmation.                            Tok1980 
18075+1443 BPM 726     [PM2000] 1377872 + [PM2000] 1377790.                                    Gvr2010 
18078+2606 CHR  67     100 Her. One component is variable.                                             
           STF2280     AB: H 3  41.                                                            MEv2010 
18078+1304 H 5  74     H V 74.                                                                         
18079+0153 OSO  93     G020-024. AC, AD, and AE are not common proper motion pairs, based on           
                       color and/or comparison with POSS2 red plates                           Oso2004 
18079-2141 ARA1513     J  2195.                                                                        
18080-1637 RST3996     There was a large change, angle decreasing, during the unobserved               
                       interval 1951-1990.                                                             
18081+3449 POP 211     Aka POP1223.                                                            Dam2015 
                       Codiscovered by Popovic and Olevic.                                     Ole1970b
18081+1232 BPM 727     [PM2000] 1380283 + [PM2000] 1380212.                                    Gvr2010 
18081-2827 WRH  22     Removed from WDS as probably not real.                                          
18082+1059 BPM 728     [PM2000] 1380774 + [PM2000] 1381049.                                    Gvr2010 
18083+2941 LAF  60     Aa,Ab: YSC  65.                                                                 
18088+2049 AGC   8     102 Her. A is a suspected spectroscopic binary.                                 
18089+1802 BPM 729     [PM2000] 1383311 + [PM2000] 1383424.                                    Gvr2010 
18089-2528 WNO  21     One component is a Beta Lyrae-type system, V3792 Sgr.                           
18090+2409 TOK 318     A is possibly SB, no orbit.                                             Tok2014d
18090+1610 BPM 730     AB: [PM2000] 1383786 + [PM2000] 1384274.                                Gvr2010 
           BPM 731     BC: [PM2000] 1384274 + [PM2000] 1384683.                                Gvr2010 
18090-3617 SHY 738     AB: HIP  88920 + HIP  88351.                                                    
18091+3101 BLL  31     A is the Mira-type system T Her. B is BD+31@3185.                               
18092+1458 BPM 732     [PM2000] 1384749 + [PM2000] 1384733.                                    Gvr2010 
18092-2211 RST3157     Poor fit for visual observations, speckle needed.                               
                       Soderhjelm notes poor Hipparcos solution.                               Sod1999 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.04 +/- 1.19, 1.48, and 0.73 Msun, respectively.             Mlk2012 
18093+1648 BPM 733     [PM2000] 1384997 + [PM2000] 1385231.                                    Gvr2010 
18093+1105 BPM 734     [PM2000] 1385001 + [PM2000] 1384518.                                    Gvr2010 
18093+0909 RUC  24     Primary is V839 Oph.                                                            
18093-2359 V3903 Sgr   The classification and orbit are from Niemela & Morrison (1988 PASP             
                       100, 1436).                                                             Msn1998a
18093-2607 B   379     HIP 88937. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
18096+3827 LUH  13     GJ 706 + WISE J180901.07+383805.4. Companion is likely not physical,            
                       based on proper motion.                                                 Luh2012b
18096+1255 BPM 736     [PM2000] 1386179 + [PM2000] 1386086.                                    Gvr2010 
18096+1106 BPM 735     [PM2000] 1386060 + [PM2000] 1386113.                                    Gvr2010 
18096+0400 STF2281     73 Oph. AB: H 1  87.                                                    MEv2010 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.21 +/- 1.75, 3.00, and 1.35 Msun, respectively.  Mlk2012 
18099+2128 LAW   6     Spectral types M5-M6 for both components, masses 0.124-0.109 and                
                       0.101-0.112 Msun, distance 41.8 +/- 4.4 pc                              Law2006 
18099+0307 YSC 132     Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic             
                       elements are fixed to those of Griffin (1999). Assigned spectral types  Grf1999d
                       for Aa and Ab are F7V and F7.5V; derived masses 1.26 and 1.23 Msun.     Hor2015 
                       Aa,Ab: SB2, P=199.55d                                                   Tok2014d
           BU  637     AB: A is a spectroscopic binary.                                                
                       HIP 89000. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
18100-4852 HJ 5017     B is CD-48@12312.                                                               
18101+1629 STF2289     A premature orbit has been computed.  The positional elements - not             
                       given by Hopmann - were reconstructed from his ephemeris.               Hop1964b
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       1995.553, 1998.657: Absolute quadrant determined by triple-correlation          
                       techniques.                                                             Pru2002b
18101-3044 BU  245     HDO 149                                                                         
18102+3402 STF2291     SEI 558.                                                                Nsn2017b
18102-7859 HJ 4988     SWR 236. CPM pair                                                       Skf2004 
18103+0235 BU  638     BC: No measures since 1929. Probably unchanged. IDS estimates for dm            
                       incorrect.                                                              Wor1967b
18106+1155 BPM 737     [PM2000] 1389911 + [PM2000] 1389794.                                    Gvr2010 
18106-1645 S   700     A 4th star "nearly south".                                                      
                       Primary is eclipsing binary of Algol-type, ecc, period 7.8075 d.        Zas2012 
18107-4032 HJ 5025     B is CD-40@12231.                                                               
18111+3241 TOK 615     BC: UC 3529.                                                                    
18112-1723 RST3161     Composite spectrum G5+A0.                                                       
18112-1951 BU  132     Same as SEE 501. A third component is indicated by lunar occultation.           
18112-4557 HDO 286     eps Tel                                                                         
18114+3506 ALI 140     Also known as POP  78.                                                          
18115+1455 OSO  94     G140-044. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
18115+1307 BPM 738     [PM2000] 1393525 + [PM2000] 1393886.                                    Gvr2010 
18116+1126 BPM 739     [PM2000] 1394117 + [PM2000] 1393941.                                    Gvr2010 
18116-4035 WG  227     BRT1029.                                                                Brt1933 
18117-2342 HJ 5030     11 Sgr.                                                                         
18118+3327 B  2545     Called a spectroscopic binary. Variation undoubtedly due to motion in           
                       the visual orbit.                                                               
                       1979.360: Theta incorrectly given as 42.4 deg in McAlister & Hendry.    McA1982d
                       1980.4768: Rho incorrectly given as 0".091 in McAlister et al (1983)    McA1983 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 6.14 +/- 2.37, 7.96, and 2.00 Msun, respectively.  Mlk2012 
18118+1147 BPM 740     [PM2000] 1394874 + [PM2000] 1394617.                                    Gvr2010 
18118-1825 HJ 2820     Aka OL  163.                                                                    
18120+2640 BRT3329     Originally published as BRT 180.                                        Brt1928 
18121+0207 BAL1957     J 1829.                                                                         
18122+0453 BAL2918     Another yet fainter pair os 1' NW of this.                              Hei1978b
18124+0524 OSO  95     G140-046. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
18125+1701 BPMA 52     [PM2000] 1397712 + [PM2000] 1398923.                                    Gvr2010 
18125-1852 VAT   2     J 1737.                                                                         
18126+4033 OSO  96     G204-049. Common proper motion pair.                                    Oso2004 
18126+3836 BU 1091     Prieur et al. (2012) derive a dynamical parallax of  6.0 mas and                
                       (using their orbital elements and the revised Hipparcos parallax of             
                       van Leeuwen 2007 A&A 474, 653) a total mass 2.2 +/- 0.9 Msun.           Pru2012 
18126+1107 BPM 741     [PM2000] 1398075 + [PM2000] 1397943.                                    Gvr2010 
18127+5446 MLR 585     GZ Dra - Algol (EA) type eclipsing binary, P = 2.25335 d.               Zas2011 
18128+1329 BPM 742     [PM2000] 1398813 + [PM2000] 1398870.                                    Gvr2010 
18128+1151 BPM 743     [PM2000] 1399144 + [PM2000] 1399290.                                    Gvr2010 
18128+0356 J  3270     Heintz equates this with BAL2482.                                       Hei1995 
18128-1618 HJ 2821     Spectrum: B5/7II/III.                                                           
18129-4959 HRG 128     B  2434.                                                                        
18130+4251 ES  473     B is BD+42@3026.                                                                
18130+2815 H 5  93     H V 93. B is BD+28@2956.                                                        
                       HJL 258.                                                                HJL1986 
                       SHY 739. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
18130+1138 BPM 744     [PM2000] 1399708 + [PM2000] 1399455.                                    Gvr2010 
18130-2307 EVS  34     Primary is the Cepheid AP Sgr. 12 Sgr.                                  Evs2016a
18130-2704 J  2199     CPD-27@6260.                                                                    
18131+2602 BWL  48     AD: Colors and/or astrometry are inconsistent with a late-type common           
                       proper motion companion based on visual inspection of the field from            
                       2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 4044.                     Bwl2015 
18131-2025 ARA1141     Aka J  1621.                                                                    
18133-4410 BRT1031     CPD-44@9008.                                                                    
18133-6513 NZO  89     SWR 238. CPM pair                                                       Skf2004 
18136+3249 GIC 150     G206-017/G206-018.                                                              
                       NLTT 46138/46139                                                        Chm2004 
                       NLTT 46138.  White dwarf pair = WD 1811+33 = EGGR 373/330               Grn1986 
18138+6235 ES 1836     LDS2408.  WDS designation for ES 1836 was incorrect, so designation             
                       for LDS pair was adopted.                                                       
18138-1904 ARA 735     The primary is the planetary nebula NGC 6567.                           Skf2013 
18138-2104 H 5   7     H V 7. mu Sgr = 13 Sgr. A is an Algol-type system and occultation               
                       binary.                                                                         
18140+2017 HO  268     "Always seen single Flower Obs."                                        Bu_1906 
18140-2052 J  1622     CPD-20@6887. ARA1142.                                                           
18141-1912 CHR 234     First detected as an occultation binary by Evans & Edwards              Evn1981 
18141-2201 BRT1520     CD-22@12732.                                                                    
18142+6445 COM   4     B is BD+64@1251.                                                                
18143+1333 BPM 745     [PM2000] 1404868 + [PM2000] 1404985.                                    Gvr2010 
18143-4309 SHY 740     HIP  89373 + HIP  89274.                                                        
18144+2127 HJ 2828     B is BD+21@3356.                                                                
                       HJL 259.                                                                HJL1986 
18145+1752 BPM 746     [PM2000] 1405737 + [PM2000] 1406209.                                    Gvr2010 
18145-6929 GLI 242     Also known as TOB 347.                                                          
18146-4625 CPO 578     SWR 239.                                                                        
18146-4722 HJ 5031     B is CD-47@12140.                                                               
18147+5635 BU 1274     A is a spectroscopic binary.                                                    
18147-1939 J  1623     CPD-19@6670.                                                                    
18148-0441 HJ  856     B is BD-04@4423.                                                                
18150+3840 LDS4781     NLTT 46179/46180                                                        Chm2004 
18150+1338 BPM 747     [PM2000] 1407711 + [PM2000] 1408069.                                    Gvr2010 
18150-1955 HJ 2823     B is BD-19@4922.                                                                
18150-5018 I   429     Measures scattered, but probable rapid motion.                                  
18151+1415 BPM 748     [PM2000] 1408129 + [PM2000] 1408042.                                    Gvr2010 
18151-5751 HJ 5029     A=SB? no SB orbit.                                                      Tok2014d
18152+1446 BPM 749     [PM2000] 1408559 + [PM2000] 1408870.                                    Gvr2010 
18152-2023 BU  286     16 Sgr. A is a spectroscopic binary.                                            
           CHR 255     Aa,Ab: Garmany et al. (1980 ApJ 242, 1063) observed a smoothly-varying          
                       velocity indicating that the A component is probably a single-lined             
                       binary with a period of 11 d.                                                   
                       Lindroos (1985) provided the classification of the B component and      Lnd1985 
                       determines a distance of 1.2 kpc.                                       Msn1998a
           SNA  83     16 Sgr. SB. See discussion of system by Sana et al. 2014).              Sna2014 
18152-2044 SNA  82     Aa,Ab: 15 Sgr. The primary is a blue supergiant star. PIONIER resolved          
                       a close pair at ~3mas at three epochs, revealing evidence of orbital            
                       motion. This pair likely corresponds to the 668d SB1 obtained by OWN            
                       (Sota et al. 2014, ApJS 211, 10).                                       Sna2014 
18154+3836 MLB 852     Aka ALI 869.                                                                    
18154-4851 HJ 5033     AD: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
18155+1825 BPM 750     [PM2000] 1409823 + [PM2000] 1409869.                                    Gvr2010 
18155-0220 LDS6324     NLTT 46171/46172                                                        Chm2004 
18155-1840 SEE 349     Component not seen in 1934 with 36-inch.                                Kui1961b
18156+1614 LDS1008     A possible wide companion to 2MASS J18153459+1614253 at 13" is noted            
                       in WDS. The star is however single within the AstraLux field of view.   Jnn2012 
18157-6233 B  1880     AB = SWR 240. CPM pair                                                  Skf2004 
18157-6303 HJ 5024     B is CPD-63@4344.                                                               
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
18158+4107 ES 1651     A is the Beta Lyrae-type system TZ Lyr, P = 0.52d.                              
18158+1516 BPM 751     [PM2000] 1411272 + [PM2000] 1411318.                                    Gvr2010 
18159-2716 J  2201     CPD-27@6313.                                                                    
18159-4412 GC 24892    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18160-1006 HU   58     A    38 is identical                                                    Hei1978b
18160-5333 HJ 9004     Previously known as HJ 5453a.                                                   
18162+0434 STTA167     B is BD+04@3677.                                                                
18163-2253 BRT1522     CD-22@12777.                                                                    
18164+2912 OSO  97     G206-020. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
18164+1201 BPM 752     [PM2000] 1413857 + [PM2000] 1414013.                                    Gvr2010 
18164-4638 SWR 241     CPM pair                                                                Skf2004 
18165+2324 BUP 180     BC: Determined to be the same as 18166+2327 POU3376 by Clif Ashcraft.           
18165-1652 HJ 2826     Also known as J  1625 or WHC  16.                                               
18165-2748 RST2043     CPD-27@6328.                                                                    
18166-2033 MCA  51     17 Sgr.                                                                         
18168-1631 SNA  84     We detect three previously unreported distant companions in the NACO            
                       FOV, but lack PIONIER observations to investigate possible closer               
                       companions. The object was reported as SB1? by Abt et al. (1972), a     AbH1972b
                       fact not confirmed by Chini et al. (2012), who prefer a RV stable       Cii2012 
                       classification.                                                         Sna2014 
           HD 167633   LS 4864. Additional radial velocities are reported by Crampton &                
                       Fisher (1974 Pub DAO 14, 283).  The star appears within the boundaries          
                       and at the same distance of Ser OB1 in the LSC.                         Msn1998a
18170-1858 SNA  85     Aa,Ab: Both NACO/SAM and PIONIER resolved the A componnet as a 50mas            
                       pair, which probably corresponds to the 80mas pair detected through     Rad1980 
                       occultation (Radick & Lien 1980). The object may further be an SB1              
                       (Gamen et al. 2008, RevMexAA 33, 54)                                    Sna2014 
           HD 167659   Hilt 730. The 3 speckle observations all indicate a single star, so we          
                       cannot confirm the existence of a companion found by lunar occultation  Msn1998a
                       (Radick & Lien 1980).                                                   Rad1980 
18170-1933 B  2862     J 1626.                                                                         
18171+1706 BPM 753     [PM2000] 1416611 + [PM2000] 1416469.                                    Gvr2010 
18171-1700 WSI 143     AD: Originally assigned to HJ 2826.                                     WSI2010 
                       Correct ID provided by Friedrich Damm.                                  Dam2012 
18172+1517 BPM 754     [PM2000] 1417297 + [PM2000] 1417367.                                    Gvr2010 
18172+0735 J  2514     Pair is BD+07 3619.                                                     J__1948 
18174-1920 B  2863     CPD-19@6748.                                                                    
18174-4929 HDS2586     SHY 743. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
18175+1647 BPM 755     [PM2000] 1418633 + [PM2000] 1418360.                                    Gvr2010 
18175-1638 HJ 2829     Spectrum: B2/3II/III.                                                           
18175-1828 RST3170     The classification of the close spectroscopic pair is from Morrison &   Cti1978 
                       Conti (1978), and that of the B component of the optical pair is from   Lnd1985 
                       Lindroos (1985). Lindroos also gives a distance of 2.0 kpc.             Msn1998a
18176-3406 HJ 5036     A is the Algol-type system RS Sgr.                                              
18176-3646 BU  760     eta Sgr. A is an irregular variable.                                            
18177+4122 LDS4783     NLTT 46260/46265                                                        Chm2004 
18180+3846 GIC 151     G204-058/G204-057 = GJ 4048A/4049B. PM of A -330-1039, B -330-1039              
                       NLTT 46274/46272                                                        Chm2004 
18181+1559 BPM 757     [PM2000] 1421149 + [PM2000] 1421222.                                    Gvr2010 
18181+1454 BPM 756     [PM2000] 1421047 + [PM2000] 1421519.                                    Gvr2010 
18181-1215 TRN  27     The image rotator was in an unknown state, so two possible theta                
                       values are listed for the 2001.7447 observation - one for zenith up             
                       and one for north up.                                                   Trn2008 
           HD 167971   Leitherer et al. (1987 A&A 185, 121) argue that this is a triple                
                       system consisting of a close eclipsing pair and a brighter, distant O           
                       star; the spectral classification presumably applies to the latter              
                       star.                                                                   Msn1998a
           DBK   1     Aa,Ab: System includes a 3.3d eclipsing binary, unresolved in the VLTI          
                       observations. De Becker et al. (2012) assume the components of the              
                       close pair are both O6.5V, and the wide component is O8I. V=7.35 for            
                       the system yields a distance of about 1.8 kpc, in good agreement with           
                       the 1.7 kpc distance determined by Reipurth (2008 Handbook of Star              
                       Forming Regions, vol 2, 590) for the NGC 6604 open cluster.  The Aa,Ab          
                       orbit is thought to be very eccentric.                                  DBk2012 
18186-1348 DCH  26     The AB pair is visible as SBA in spectroscopy, although no orbital              
                       motion is detected (Sana et al. 2009), inagreement with the large       Sna2009 
                       separation, hence very long period.  Five other faint companions are            
                       detected in the NACO FOV.                                               Sna2014 
18186+1538 BPMA 53     [PM2000] 1423159 + [PM2000] 1423708.                                    Gvr2010 
18187-1206 SNA  90     Aa,Ab: Object is a non-thermal radio emitter (DeBecker et al. 2004).    DBk2004 
                       PIONIER clearly resolved it into a tight pair (3.3mas) with almost              
                       equal brightness (dH=0.17 +/- 0.19).                                    Sna2014 
18187-1837 BU  639     There was a close approach around 1900.                                         
                       Large divergences in estimated distance due to considerable southern            
                       declination.                                                            Vou1951 
                       1994.5191: Quadrant determined by speckle imaging analysis              Hor1996 
18188+4510 WOL   2     WSP  58.                                                                        
18189-1348 SNA  91     Aa,Ab: The A component is an O7V+O8V 912d SB (Sana et al. 2012) that    Sna2012 
                       we marginally resove with PIONIER at 6mas separation.                   Sna2014 
18189+3918 MLB1078     ES 2570.                                                                        
18192+2427 105 Her     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Radford & Griffin (1977).                                               Grf1977b
18192+1116 BPM 758     [PM2000] 1426022 + [PM2000] 1425922.                                    Gvr2010 
18196+3915 MLB 754     Not found by Heintz at IDS position.                                    Hei1985a
18196-1944 WRH  30     SEE 501 is probably BU 132.                                                     
18197+1016 HU  197     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.20 +/- 0.69, 1.95, and 1.05 Msun, respectively.             Mlk2012 
18197-4542 CHR 148     HD 167954 is a SB, with P = 120d (Bopp et al. 1970 MNRAS, 147, 355).            
                       With rho = 0".031, the speckle pair is probably not the SB.             McA1990 
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Bopp et al. (1970).                                                     Evn1970 
18198-0458 SCJ  16     A = QS Ser, false HIP variable (GCVS), artifact of scanning binary.     Tok2014d
18199+1524 BPM 759     [PM2000] 1429486 + [PM2000] 1429612.                                    Gvr2010 
18201+2532 STF2309     H 1  86.                                                                MEv2010 
18201-0936 GJ 4052     No comoving objects found within separation/magnitude range listed.             
                       However, Chauvin et al. (2006) note finding at least one faint          Cvn2006 
                       background object.                                                              
                       HD 168443. Combined astrometric/spectroscopic solution, using                   
                       spectroscopic elements (P,T,e,omega) from Wright et al. (2009 ApJ 693,          
                       1084).                                                                  SaJ2011 
18202-3601 BRT1769     CPD-36@8160.                                                                    
18204-1011 HER   2     A post-T Tauri star, FK Ser.                                                    
18205-5107 BRT1043     SWR 242.                                                                        
18205-5344 FIN 264     Spectrum: G0/5III+A7/F0.                                                        
18206+1608 OSO  98     G184-004. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
18207+2530 BRT3330     Originally published as BRT 181.                                        Brt1928 
18208+7120 STT 353     phi Dra = 43 Dra. A premature orbit has been computed.                  D__1883 
                       Almost rectilinear relative motion, long period!                        Ole1975b
                       Period of A (SB1) is 127.99d.                                           Lis2016 
                       An Alpha CVn type variable.                                                     
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Also an unresolved 128.165d spectroscopic binary.                       XXX2017a
18208+2732 BU  640     Measure by Van Biesbroeck in 1932 is undoubtedly in error.              Baz1944a
                       CfA: A is SB, P=long. Triple or not? Makarov & Kaplan (2005): dmu=20.4  Mkr2005 
                       (HIP2:20.1), implies triple.                                            Tok2014d
18209+1153 BPM 760     [PM2000] 1434041 + [PM2000] 1433558.                                    Gvr2010 
18209+0323 HJ 5495     74 Oph.                                                                         
18210-0101 VKI  46     LP 630-1.                                                                       
18210-1714 J  1627     J  1739.                                                                J__1962a
18210-2950 SEE 350     del Sgr = 19 Sgr = Kaus Media                                                   
18211+7244 LAB   5     Aa,Ab: chi Dra = 44 Dra. Astrometric, interferometric, and                      
                       spectroscopic binary.  See discussion of the RV's by J. Vinter Hansen           
                       (Lick Obs. Bul. 19, 141, 1942).                                                 
                       See discussion and orbital elements by Labeyrie et al. (1974).          Lab1974 
                       P, T, and e for Alden (1936) solution taken from spectroscopic orbit    Ald1936c
                       Speckle and spectroscopic orbit by Tomkin et al. (1987), used P,e       Tom1987 
                       fixed from spectroscopy. Positional elements disagree somewhat with             
                       those of the astrometric orbit (prior to resolution of the companion)           
                       by Breakiron & Gatewood (1974).                                         Brk1974 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Analyses of the spectroscopic/interferometric orbit are given by        McA1980b
                       McAlister (1980) and McA1980c and Tomkin et al. (1987).                 Tom1987 
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Tomkin et al. (1987).                                                   Tom1987 
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       The Farrington et al. (2010) orbit is based on speckle plus K'-band     CIA2010 
                       CHARA Array separated fringe packet observations. An orbital parallax           
                       of 123.4+/-1.9 mas is determined.  Based on the mass ratio                      
                       determination of Nordstrom et al. (2004 A&A 418, 989), derived masses           
                       are 0.96+/-0.03 and 0.75+/-0.03 Msun, well below the expected masses            
                       for an F8IV-V and late-G/early-K dwarf pair. The aperture and method,           
                       8m and speckle, are set to give the resolution capability of this               
                       technique, which is less than classical interferometric methods.                
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.71 +/- 0.06, 2.07, and 1.13 Msun, respectively.  Mlk2012 
18211-0102 WOR  35     This is the nearby star G 21-10 = GJ 1226 = LHS 463.                            
18211-1339 RST9006     Previously known as RST4585a.                                                   
18212+5917 LDS2411     LDS5235.                                                                        
18213-0254 STFB  8     eta Ser = 58 Ser                                                                
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
                       H 6  14.                                                                MEv2010 
18214+1259 BPMA 54     [PM2000] 1436289 + [PM2000] 1436037.                                    Gvr2010 
18214-1852 EVS  35     Primary is the Cepheid Y Sgr.                                           Evs2016a
18216+3842 LDS5861     LDS6327.                                                                        
18216-2052 BRT1530     ARA1148.                                                                        
18218+3038 L    21     Appears to be 10deg error in converting Lewis' NPD to Dec for IDS.      L__1900 
18218-1155 EGN  22     AB, AC, and AF pairs unbound; D, E, G, H, and R likely unrelated as             
                       well. Bound/unbound nature of other components is inconclusive.                 
                       Primary is planet host star.                                            Egn2007 
18219+1631 BPM 761     [PM2000] 1438334 + [PM2000] 1437857.                                    Gvr2010 
18220+1621 BPM 762     [PM2000] 1438974 + [PM2000] 1438640.                                    Gvr2010 
18220+1348 BPM 763     [PM2000] 1439257 + [PM2000] 1439185.                                    Gvr2010 
18220-2233 J  2208     CPD-22@6959.                                                                    
18221+5336 BEM  32     ES  649.                                                                        
18222-5534 DUN 220     B is CPD-55@8630.                                                               
                       Primary is QW Tel, a W UMa type eclipsing binary, P = 0.411928d.        Zas2012 
18223+1713 BPMA 55     [PM2000] 1440461 + [PM2000] 1440291.                                    Gvr2010 
18223+1547 BPM 764     [PM2000] 1440458 + [PM2000] 1440241.                                    Gvr2010 
18223-1437 J   519     Additional companion at 222deg, 15", mag 14.5                           J__1946 
18223-2018 BHA  27     J  1628.                                                                Nsn2016 
18224+4545 A   700     Round 1951-1954. Possible quadrant change.                                      
18226+0852 SLE 163     There is apparently a 7s typo in RA of primary by Soulie (1984).        Sle1984 
18228-1727 J  2210     This pair had the wrong coordinate. The correct coordinates were found          
                       by Brian Skiff (Lowell) and the pairs recovered in the 2MASS data.      Skf2004 
18228-1843 CHR 235     First detected as an occultation binary by Africano.                    Afr1978 
18229+1458 HU  581     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.18 +/- 1.48, 2.25, and 1.05 Msun, respectively.             Mlk2012 
18229-1726 J  2209     This pair had the wrong coordinate. The correct coordinates were found          
                       by Brian Skiff (Lowell) and the pairs recovered in the 2MASS data.      Skf2004 
18231+1125 BPM 765     [PM2000] 1444071 + [PM2000] 1444438.                                    Gvr2010 
18231-6235 CPO  79     SWR 244.                                                                        
18232-6130 GLE   2     xi Pav. A is a long-period spectroscopic binary.                                
                       Dynamical elements for Alden's orbit were obtained from a               Ald1946 
                       spectroscopic orbit. Alden's orbit was rejected from the Fourth                 
                       Orbit Catalog ("amplitude below noise level")                           Wor1983 
18236-2610 HO  566     If the quadrants are correct, a revolution has been completed.                  
18237+2146 STT 587     AB: 109 Her.                                                                    
18237-2209 BRT1534     J 2126.                                                                         
18237-5841 SWR 246     CD-58@ 7043. CPM pair                                                   Skf2004 
18238+5139 ES  187     AB: B is SB1, P=126.38d                                                 Tok2014d
18239+5848 STF2323     39 Dra. STTA169 = STFA 36. A is a double-lined spectroscopic binary.            
                       C is a spectroscopic binary, P =2.71d.                                          
                       AC: HJL1098.                                                            HJL1986 
                       AB: H 1   7.                                                            MEv2010 
18240+3844 HO  432AB   This cannot be the close 2347.9-d spectroscopic binary, who postulated  Grf2010d
                       a dm of 6 and a separation of 6 mas.                                            
18241-1734 J  2127     Jonckheere gives angle as 40@ in his 1962 catalog.                      J__1962a
18242-3423 SEE 351     eps Sgr = 20 Sgr = Kaus Australis.  Infrared excess and probable                
                       circumstellar disk. Spectral peculiarities lead to classification               
                       problems. Alternative types B9IVp, A0II(shell)                                  
18243-0405 YSC  67     AB + TOK 420Aa,Ab: The neglected pair YSC 67 turned out to be a new             
                       triple. The outer 0".35 binary AB was known previously, now we detect           
                       elongation that implies an inner subsystem Aa,Ab. We compared with              
                       stars in the same area of the sky observed before and after to assure           
                       that the elongation is not of instrumental origin; it is seen in two            
                       filters.                                                                Tok2015c
18243-4407 DUN 221     B is CD-44@12570.                                                               
18244-2932 RSS  31     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determined from the individual positions          
                       listed by Rousseau et al.                                               Rss1996 
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
18250+2724 STF2315     A is a spectroscopic binary.                                                    
                       AC: 1898 distance probably in error.                                            
18250-0135 AC   11     Spectrum composite; A9III+F6III.                                        Egg1947 
                       Additional notes may be found in Eggen (1947) and Voute (1951).         Vou1951 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 9.58 +/- 9.12, 4.69, and 1.45 Msun, respectively.             Mlk2012 
18251+3016 GIC 152     G206-030/G206-031.                                                              
                       NLTT 46462/46463                                                        Chm2004 
18251+1623 BPM 766     [PM2000] 1454337 + [PM2000] 1454586.                                    Gvr2010 
18251+1152 BPM 767     [PM2000] 1454346 + [PM2000] 1454212.                                    Gvr2010 
18251+0258 BAL1965     J 2579.                                                                         
18252+0720 LDS1011     LDS5236.                                                                        
18253+4846 HU   66     Van Biesbroeck (1954) was unable to resolve this system in 1943,                
                       1944 or 1945 on the 82-inch telescope at the McDonald Observatory.              
                       However, since he resolved the system successfully in 1946 with the             
                       same telescope, and in 1940 with a smaller (40-inch) telescope, the             
                       non-resolution is probably due to bad seeing or ID error.               USN2002 
           STT 351     AC: Additional notes may be found in Muller (1955).                     Mlr1955c
18253+4653 BU  134     Also known as STT 543.                                                          
18254+1142 BPM 768     [PM2000] 1455453 + [PM2000] 1455388.                                    Gvr2010 
18254-1631 HU   64     Mt. Wilson spectral classes F5s and G0.                                         
18254-2033 JC    6     21 Sgr.                                                                         
18255-1241 RY Sct      This massive binary and its surrounding gas torus are described by              
                       Gehrz et al. (1995 ApJ 439, 417). A light curve from  Hipparcos is now  HIP1997a
                       available.  The system mass and the nature of the secondary are still           
                       controversial (Skulskii 1992 SvA 36, 411; Skulskii & West 1993 Astron.          
                       Rep. 37, 594; Golovatyi & Skul'skii 1992 SvA 36, 550).  We found a              
                       possible binary companion at a separation of 0".2 which needs                   
                       confirmation.                                                           Msn1998a
18255-6301 ARY 108AC   Author listed the B component as a new component of 18231-6235 CPO 79.  Ary2014b
                       Corrected by USNO.                                                              
18255-6605 HJ 5039     B is CPD-66@3337.                                                               
18256+0802 STT 348     V2291 Oph                                                                       
18256-3628 OL   19     BRT1777.                                                                Brt1936a
18257+1339 BPM 769     [PM2000] 1457131 + [PM2000] 1456591.                                    Gvr2010 
18259+1458 CHR  70     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.                                             
18259+0541 J  2130     SLE 174.                                                                        
18260+2606 L    22     Appears to be a 10m error in Lewis' epoch-1900 coordinates.             L__1900 
18260-4541 LDS 638     TSN  95.                                                                        
18261+0047 BU 1203     1980.4794  This measure was incorrectly attributed to ADS 11524 by              
                       McAlister et al. (1983).                                                McA1983 
18262+0847 LDS1012     LFT 1415/1416.                                                          Bgh1958 
                       HJL1099.                                                                HJL1986 
                       B is BD+08@3692.                                                                
                       Hipparcos stochastic double solution.                                           
                       A is SB1, P=293.35d (Halbwachs et al. 2012) and astrometric binary,     HJL2012b
                       P=0.827y (Goldin & Makarov 2007).                                       Gln2007 
                       SHY 306. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
18262-1832 CHR 236     First detected as an occultation binary by Africano.                    Afr1978 
18263+1313 BPM 770     [PM2000] 1460131 + [PM2000] 1460594.                                    Gvr2010 
18264+4649 STT 352     B is BD+46@2489.                                                                
18264+1216 BPM 771     [PM2000] 1460407 + [PM2000] 1459847.                                    Gvr2010 
18266+1147 BPM 772     [PM2000] 1461257 + [PM2000] 1460960.                                    Gvr2010 
18266+0627 GCB  31     BRT2838.                                                                Brt1947 
18267+2627 BU 1326     A is a spectroscopic binary.                                                    
18267-3024 TOK 421     HIP 90397 is an acceleration binary with a variable RV (GCS), resolved          
                       here at 69mas (estimated period ~4yr). The star is targeted by                  
                       exo-planet programs.                                                    Tok2015c
18268+0123 BAL1501     RST 5449.                                                                       
18268-1814 FEN  30     DON 902.                                                                        
18269+1308 BPM 773     [PM2000] 1462688 + [PM2000] 1462619.                                    Gvr2010 
18271+2754 TDS 921     Appears to be the same star as L    23, based on coordinates and                
                       astrometry by Lewis (1911).                                             L__1911 
18272+1543 BPM 774     [PM2000] 1464147 + [PM2000] 1464406.                                    Gvr2010 
18272+1533 BPM 775     [PM2000] 1464561 + [PM2000] 1464426.                                    Gvr2010 
18272+0404 FAR  20     Primary is white dwarf WD 1824+040.                                     Far2005b
18272+0012 STF2316     59 Ser. A is a triple spectroscopic binary, and B may be an SB also.            
                       A is an irregular variable, d Ser.                                              
                       Aa,Ab: Examined for visual duplicity of its components, which are               
                       long-period SBs.                                                        WRH1952 
                       AB: H 1  12.                                                            MEv2010 
18273+0820 J  2911     TDT 882.                                                                        
18273-2503 LDS 639     LDS 640.                                                                        
                       NLTT 46491/46490                                                        Chm2004 
18274+1141 BPM 776     AB: [PM2000] 1465466 + [PM2000] 1465190.                                Gvr2010 
           BPM 777     BC: [PM2000] 1465190 + [PM2000] 1464574.                                Gvr2010 
18275-1522 J  1631     CD is probably AB of 18275-1524 with quadrant reversed.                         
18277-3207 I  1023     Measures uncertain, too close. Duplicity dubious, but needs speckle.            
18278+2442 STF2320     Eclipsing and spectroscopic multiple (periods 1.42001 & 2.08327 days).  Zas2010 
                       An updated orbit predicts that the two close pairs may be resolvable            
                       by interferometry, with predicted separations ~17mas and a magnitude            
                       difference of ~1.4mag.                                                  Zas2016b
18278-2949 GC 25175    Combined solution, based on reduction of Hipparcos intermediate                 
                       astrometric data together with spectroscopic elements from the Geneva           
                       Extrasolar Planet Search Programs home page.                            HaI2001 
           RAG   2     Primary is exoplanet host, P=225.6d                                     Tok2014d
18279-1444 J  1651     Aka TDT 892.                                                                    
18280+0612 CHR  71     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 10.53 +/- 3.67, 5.69, and 3.20 Msun, respectively.            Mlk2012 
18280-2525 WFC 208     lam Sgr = Kaus Borealis.                                                        
18281-2048 RSS  32     This previously uncataloged double star was a Hipparcos double entry            
                       system.  The first measure is determinedfrom the individual positions           
                       listed by Rousseau et al.                                               Rss1996 
18284-1527 FOX  82     May be component of multiple 18275-1524.                                        
18285-1013 HJ 5497     Herschel coordinates 18 19, NPD 100 19 17 (1830). Colors orange and             
                       green. RA is described as "precarious".                                         
18286+0451 STTA168     B is BD+04@3759.                                                                
18287+0016 SHC   2     Primary is young stellar object [HMH2007] 20. The companion shows IR            
                       excess, and is identified as a young low-mass companion candidate.      ShC2011 
18288+0009 LI    1     Due to an error in cross-referencing, this pair was originally                  
                       entered into the WDS as 18288-2715.                                             
18289+0019 SHC   6     Primary is young stellar object [HMH2007] 43. The companion shows IR            
                       excess, and is identified as a young low-mass companion candidate.      ShC2011 
18289+0020 SHC   3     Primary is young stellar object [HMH2007] 36. The companion is a young          
                       brown dwarf, mass ~80 Mjup.                                             ShC2011 
18289+0029 SHC   4     Primary is young stellar object [HMH2007] 37. The companion shows IR            
                       excess, and is identified as a young low-mass companion candidate.      ShC2011 
18289+0030 SHC   5     Primary is young stellar object [HMH2007] 40. The companion shows IR            
                       excess, and is identified as a young low-mass companion candidate.      ShC2011 
18290-2635 WNO   6     Variable? B is CD-26@13205.                                                     
18290+0017 SHC   7     Primary is young stellar object [HMH2007] 48. The companion is a                
                       low-mass YSO.                                                           ShC2011 
18292+1142 TOK 321     Spectral type of comoving secondary estimated as M1, mass 0.52 Msun.    Mug2014 
                       AB: A is exoplanet host P=1145d                                         Tok2014d
                       AC: white dwarf candidate at 167", likely optical.                      Tok2012c
18293+1624 BPM 778     [PM2000] 1474812 + [PM2000] 1474553.                                    Gvr2010 
18293-3431 B  1364     CPD-34@7858.                                                                    
18296+0034 SHC   8     Primary is young stellar object [HMH2007] 112. The companion shows IR           
                       excess, and is identified as a young low-mass companion candidate.      ShC2011 
18296+1639 BPM 780     [PM2000] 1476424 + [PM2000] 1476961.                                    Gvr2010 
18296+1553 BPM 779     [PM2000] 1476312 + [PM2000] 1476163.                                    Gvr2010 
18297+5740 LDS2414     LDS2743.                                                                        
18298+1201 BPM 781     [PM2000] 1477006 + [PM2000] 1476757.                                    Gvr2010 
18299+2639 HD170737    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1980).                                                         Grf1980c
18299+1345 BPM 783     [PM2000] 1477579 + [PM2000] 1477791.                                    Gvr2010 
18299+1222 BPM 782     [PM2000] 1477520 + [PM2000] 1477271.                                    Gvr2010 
18300-1257 HU   69     Spectrum: B9.5II/III.                                                           
18301+1127 BPM 784     [PM2000] 1478740 + [PM2000] 1478561.                                    Gvr2010 
18301+0404 CHR  72     Aa,Ab: 1985.8424: This autocorrelogram was remeasured; the new results          
                       are listed here.                                                                
18305+1408 BPM 785     [PM2000] 1480330 + [PM2000] 1479915.                                    Gvr2010 
18306+2805 ES  476     MLB 649 is identical                                                    Hei1983a
18306+1337 BPM 786     [PM2000] 1481254 + [PM2000] 1480624.                                    Gvr2010 
18307+0431 STTA170     B is BD+04@3775.                                                                
                       Pair appears in an appendix list, not part of discoverer's regular              
                       numbering sequence.                                                             
18308+1803 BPMA 56     [PM2000] 1482352 + [PM2000] 1483143.                                    Gvr2010 
18308-1309 BRT2754     Aka J  1652.                                                                    
18309+3840 STF2338     C is the semiregular variable KP Lyr.                                           
18310+0648 SLE 349     AC: The Soulie (1985) C component is not seen; possibly due to a 2s             
                       error in the published RA?                                              Sle1985 
18312+6526 KUI  86     A is a spectroscopic binary.                                                    
18312+1311 STF2330     B is BD+13@3668.                                                                
18313-1306 EVS   8     Classical Cepheid X Sct.                                                        
18313-4821 HJ 5046     SWR 247. CPM pair                                                       Skf2004 
18313-5532 HJ 5044     B is CPD-55@8709.                                                               
18314+0628 STF2329     Same as STF2331.                                                                
18314-1048 STF2325     H N  54.                                                                MEv2010 
18314-4322 CPO  81     AB = LDS 641.                                                                   
18316+1204 BPM 787     [PM2000] 1486217 + [PM2000] 1486275.                                    Gvr2010 
18317+2310 HU  321     Mt. Wilson spectral type of B is G0.                                            
18318+0641 J  1372     Appears to be the same as KRU   6.                                      Dam2010 
18319+0836 OSO  99     G141-015. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
18319-1908 BU  966     Cluster M 25. A is the Cepheid U Sgr.                                           
                       Identifications on Hyd. ph. -19@, 18:28 are as follows:                         
                       A  51273   G  51291   P  51300                                                  
                       B  51272   H  51271   Q  51299                                                  
                       C  51297   J  51270   R  51274                                                  
                       D  51298   K  51267   S  51263                                                  
                       E  51266   L  51268   T  51292                                                  
                       F  51265   M  51269   U  Close comp. to B.                                      
                       The C of the BC pair is not the same as the C of the CD, CG, and CQ             
                       pairs. Therefore, it has been re-designated Ba,Bb. Aa, aB and aC are            
                       now designated AI, IB and IC. Bb is designated BQ (the identity of CQ           
                       and Bb was first noted by Dave Arnold).                                         
18320+2031 LAW  18     LSPM J1832+2030. Law et al (2008) derive a distance of 20.6 +9.6/-3.9   Law2008 
                       pc and a projected separation of 27.0 +14.6/-4.0 au. Estimated                  
                       spectral types are M4.5 and M5.                                                 
18323-1439 CHR  73     1989.3041: Due to typographical error, measurement was incorrectly      McA1990 
                       attributed to 18444+3937 = CHR 77 in McAlister et al. (1990).           Hrt1996b
18326-1542 RBR   9     2001.7364: PA is measured in zenith mode. If data collected in                  
                       equatorial mode, PA = 218.1. Confirmation of the pair should establish          
                       the correct theta value.                                                Rbr2007 
18326-4936 RST9007     Previously known as RST2060a.                                                   
18327+0504 BAL3014     Epoch-1900 coordinates not precessed in creating WDS designation.               
18329+6343 STF2357     Also known as STF2363.                                                          
18329+3850 STTA171     B is BD+38@3211.                                                                
18329+1418 BPM 788     [PM2000] 1492426 + [PM2000] 1492794.                                    Gvr2010 
18330+3136 STF2340     AB: SEI 565.                                                            Nsn2017b
18330+2420 POU3427     J 1886.                                                                         
18331-1042 HDS2632     The motion of AB is reflex of PM(A), crowded field N*=641, optical!     Tok2014d
18331-1918 J  2215     CPD-19@6927.                                                                    
18332+4010 STT 356     AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
18333+3203 SLE 201     Nothing at Soulie (1984) published coordinates. A pair 25s east                 
                       appears to be the most likely candidate.                                Sle1984 
18333+1437 BPM 789     [PM2000] 1494752 + [PM2000] 1494587.                                    Gvr2010 
18333+1309 OSO 100     G141-019. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
18334+5842 ES  188     Primary is HI Dra, a W UMa type eclipsing binary, P = 0.59742d.         Zas2012 
18334+3727 ES 2481     Not found by Heintz at IDS position.                                    Hei1985a
18334-3004 I  1370     Variable companion?                                                     Jsp1964 
18334-3844 DUN 222     kap 2 Cra. B is CD-38@12896, kap 1 Cra.                                         
18335+2102 COU 204     Also known as TOR   4.  The similarity of these systems was first               
                       noted by Dave Arnold.                                                           
18335+0726 SCJ  18     B is BD+07@3740.                                                                
18338+7003 STF2370     HJL 260.                                                                HJL1986 
18338+1744 HU  322     Distance less than 0.1" in 1960.                                                
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 10.48 +/- 51.06, 3.98, 1.17 Msun, respectively.    Mlk2012 
18339+5221 A  1377     Mt. Wilson spectral classes A is G5, C is B8n.                                  
                       AB. This appears to be part of a triple system.  The elements given by          
                       Wilson (1950) and by Baize (1958) are different, possibly due to the    WRH1950b
                       long period of the system. This 1975.533 separation is less than that   Baz1958 
                       derived from either ephemeris but it and the position angle are closer          
                       to Baize's values.                                                      BLM1978 
                       2003.6: Differential astrometry by Lane & Muterspaugh (2004) was        Lne2004 
                       originally published as follows, but converted to BY, rho, and theta            
                       by WIH for inclusion in our catalogs:                                           
                              MJD            dRA (arcsec)           dDEC (arcsec)                      
                          52862.30085   0.222109 +/- 0.000143  -0.119309 +/- 0.00000839                
                          52863.28229   0.222233 +/- 0.000143  -0.119302 +/- 0.0000155                 
                          52864.31096   0.222134 +/- 0.000197  -0.119323 +/- 0.0000189                 
                          52865.29921   0.221981 +/- 0.000155  -0.119361 +/- 0.0000148                 
                       AB: Additional notes may be found in Wilson (1955).                     WRH1955 
18339+5144 ZUC  16     TOK  31.                                                                        
                       GJ 719. Primary is 6d SB2; period of wide pair esimated at 3800y. The           
                       114-day astrometric orbit by HIPPARCOS is not supported by RV. This is          
                       a PMS spotted binary BY Dra.                                            Tok2006 
           BY Dra      Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
                       Combined spectroscopic/astrometric (Palomar Testbed Interferometer)             
                       solution by Boden & Lane (2001), including determination of distance,   Bod2001 
                       masses, luminosities, etc.                                                      
                       Low-mass SB2. Helminiak et al. calculate a combined spectroscopic/              
                       astrometric orbit by combining precise RVs with archival astrometric            
                       data from the Palomar Testbed Interferometer. They derive masses 0.792          
                       +/- 0.026 and 0.697 +/- 0.023 Msun, radii 7.400 +/- 0.016 and 8.414             
                       +/- 0.016 Rsun, parallax 60.43 +/- 0.12 mas.  They conclude it is not           
                       a pre-main sequence system, despite its high orbital eccentricity       Hel2012 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 9.00 +/- 32.45, 1.36, and 0.62 Msun, respectively.            Mlk2012 
18342+0341 ABT9001     Previously known as ABT  13.                                                    
18344+2615 BUP 183     D component = A component of 18352+2616 BUP 184.                                
18346+1739 BPM 791     [PM2000] 1501242 + [PM2000] 1501100.                                    Gvr2010 
18346+1134 BPM 790     [PM2000] 1501189 + [PM2000] 1501042.                                    Gvr2010 
18346-2734 I  1026     AB +  TOK 422Aa,Ab: HIP 91075 was noted as a double-lined binary by             
                       the GCS (one observation only). The separation of 86mas implies a               
                       period of ~10yr, while the double-lined observation matches the                 
                       moderate magnitude difference (estimated masses 1.04 and 0.77 Msun.             
                       The star is an X-ray source, so a future combined orbit could                   
                       determine masses for testing evolutionary models of young stars. The            
                       sky around the object is quite crowded; the 9" companion I 1026 is              
                       optical (it moves too fast).                                            Tok2015c
           I  1027     CD: CPD-27@6461.                                                                
18346-3753 JSP 780     CPD-37@8199.                                                                    
18347-6557 I   634     Spectrum: G3/6III+(A).                                                          
18349-0043 RST5119     Primary is eclipsing binary of Algol-type, period 1.953876 day.         Zas2013 
18349-1442 STF2337     B is BD-14@5117. B spectrum B9/A0II/III.                                        
18349-4801 HJ 5047     B is CD-48@12597.                                                               
18351+0003 RST5120     V413 Ser, Algol (EA) type eclipsing binary, P = 2.25977 d.              Zas2011 
18352+6342 STF2365     Primary is SB2, P=4.738y                                                Tok2014d
18352+2616 BUP 184     A component = D component of 18344+2615 BUP 183.                                
18352+1812 CHR  74     A well-known speckle binary whose first interferometric observations            
                       date from the CHARA speckle program in the mid-1980's, this object              
                       went unobserved from 1996 until the present work. The new data suggest          
                       that nearly half an orbit has been completed since the first speckle            
                       observation. The primary is probably close to an A0V star, and with a           
                       magnitude difference of perhaps 2-2.5, we estimate that the secondary           
                       is an F2V star. This would suggest a mass sum in the range 4-5 Msun,            
                       which is lower than what is implied by the value of P and a we derive,          
                       together with the Hipparcos parallax of 5.04 +/- 0.39 mas. We expect            
                       that the next decade will provide an opportunity to improve upon the            
                       orbit presented here since the separation will be above 0.1 arcsec and          
                       the position angle is expected to cover about 30deg. We encourage               
                       other observers to put this object back on their observing lists for            
                       the next few years.                                                     Hor2015b
18353+2842 OSO 101     G206-034. None of the components share a common proper motion, based            
                       on color and/or comparison with POSS2 red plates.                       Oso2004 
18354+0649 J   100     Van Biesbroeck calls this Toulouse +7@, 18h 28m                         VBs1954 
                       No. 300. Jonckheere gives BD+06@3866.                                   J__1910d
18354-2118 ARA1544     Aka J  1747.                                                                    
18355+4546 LDS6329     NLTT 46716 + 46720.                                                             
                       Also known as GJ 720 A, this star has a wide companion with a                   
                       demonstrated common proper motion at about 112" according to Lepine &   Lep2007 
                       Bongiorno (2007).                                                       Jnn2012 
18355+2336 STT 359     Spectrum composite; G9III+G7III.                                                
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.80 +/- 1.54, 4.11, and 1.85 Msun, respectively.             Mlk2012 
18355+1005 BRT1945     J 2134; also J 2137. Jonckheere noted BRT1945 = J 2134 and suspected    J__1942d
                       J 2137 at 18356+1007 was probably the same star as well. Identity               
                       concluded after search of region, despite fair amount of discrepancy            
                       in some measures.                                                               
18356+0456 BU  643     A is the Alpha CVn-type variable FR Ser.                                        
18358+2522 HDS2637     Fekel et al. (2013) derive a spectroscopic orbit for the primary, with          
                       P=14.685d and e=0.2495. Estimated masses are 2.5 and 2.35 Msun.         Fek2013a
18359+1659 STT 358     Alternative spectrum: G2V+G2V                                                   
                       Identification of the ascending node is uncertain due to weak data.     Hei1954 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
           RED  25     AB,E:  M3.5, 35" from G0/F8 binary HD 171746 = HIP 91159 = 2MASS                
                       J18355323+1658316. Proper motion for the brighter star +049-071.                
                       From measurements of DSS POSS and 2MASS plates Reid et al. derive a             
                       proper motion of +080-070 for the M dwarf. Trigonometric parallax               
                       for the G dwarf gives a distance ~34pc, significantly larger than               
                       the spectroscopic distance of 21pc for M star. It is uncertain                  
                       whether the stars are associated.                                       Red2007a
                       AE: 2MASS J18355276+1659057 is possibly a wide companion to HIP 91159   Red2007a
                       at 35" separation, as noted in Reid et al. (2007).                      Jnn2012 
18360+1144 STT 357     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 8.78 +/- 7.73, 4.26, and 1.66 Msun, respectively.             Mlk2012 
18360+0452 J  2138     BAL2930.                                                                        
18361+6405 MLB 214     Position corrected by Heintz.                                           Hei1983a
18362+6529 GC 25491    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18362-1053 EGN  23     System is only 21deg from galactic center, so 12 companion candidates           
                       were detected. The B, C, H, I, J, K, L, and M components are unbound;           
                       D is likely a background star as well. Single epoch, so the nature of           
                       E, F, and G are unknown.                                                Egn2007 
18362-1407 SNA  92     The object was clearly resolved with PIONIER as a 1.5mas pair. The      Cti1977 
                       possible RV variability reported by Conti et al. (1977) was not         Cii2012 
                       confirmed by Chini et al. (2012).                                       Sna2014 
18363+2143 COU 206     Docobo et al. (2010) derive a dynamic parallax of 3.15 +/- 0.30 mas     Doc2010h
                       and a total mass of 3.72 +/- 2.07 Msun. The mass is excessive for the           
                       spectral types.                                                                 
18364-4952 CPO 592     CPD-49@10659.                                                                   
18366+3328 STF2349     A is possibly a spectroscopic binary. Variable.                                 
18367+3841 H 4  59     H IV 59. Also known as STF2354.                                                 
18367+0640 CHR  76     A is a spectroscopic binary, now resolved by speckle.                           
           J    99     AB: Optical pair, based on study of relative motion of the                      
                       components using the method of apparent motion parameters.              Kiy2008 
18368+1151 L    39     The Sternberg measure evidently does not belong to this pair.           Srb1969 
18369+3846 H 5  39     AB: H V 39. alp Lyr = 3 Lyr = Vega                                              
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
           STFB  9     AE: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
           MET  11     Metchev & Hillenbrand say the F, G, H, I, J, and K components are all   Met2003 
                       probably optical companions of Vega. Physicality of the Ia,Ib and               
                       Ka,Kb pairs is unknown.                                                         
           MBA   2     Macintosh et al. (2003) made a K-band search for extrasolar planets in  MBA2003 
                       the dust surrounding Vega, using Keck, NIRC2, and AO. The relative              
                       motions for these 7 objects between 2002 Feb and 2002 Aug were all              
                       well below expected motions for true companions, leading to the                 
                       conclusion that all these faint companions are background stars.                
                       Identities of the objects discovered by Metchev et al. and Macintosh            
                       et al. are as follows:                                                          
                           MET  11AF     = Met2003 object 1 = MBA2003 object 1                         
                           MET  11AG     = Met2003 object 2 = MBA2003 object 2                         
                           MET  11AH     = Met2003 object 3 = MBA2003 object 3                         
                           MET  11A,Ia   = Met2003 object 4                                            
                           MET  11A,Ib   = Met2003 object 5                                            
                           MET  11AJ     = Met2003 object 6 = MBA2003 object 7                         
                           MET  11A,Ka   = Met2003 object 7                                            
                           MET  11A,Kb   = Met2003 object 8                                            
                           MBA   2AL     =                    MBA2003 object 4                         
                           MBA   2AM     =                    MBA2003 object 5                         
                           MBA   2AN     =                    MBA2003 object 6                         
18369+1506 BPM 793     [PM2000] 1512466 + [PM2000] 1511835.                                    Gvr2010 
18369+1129 BPM 792     [PM2000] 1512306 + [PM2000] 1512288.                                    Gvr2010 
18370+3452 STF2352     AB: SEI 566.                                                            Nsn2017b
18372-0236 BAL 248     BRT1946.                                                                Brt1936b
18374-4704 HJ 5049     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
18378+1752 BPM 794     [PM2000] 1516606 + [PM2000] 1517111.                                    Gvr2010 
18379-0648 LDS5239     HIP 91360. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
18379-1111 BRT2755     J 2139.                                                                         
18380+1107 BPM 795     [PM2000] 1517796 + [PM2000] 1518152.                                    Gvr2010 
18380-0648 TOK  32     Allen et al. (2000) list a CPM companion at 37.1", confirmed as CPM     AlC2000 
                       and ptm by 2MASS. Primary is 21d SB1.                                   Tok2006 
18381+1245 BPM 796     [PM2000] 1517997 + [PM2000] 1517765.                                    Gvr2010 
18381+1229 BPM 797     [PM2000] 1518189 + [PM2000] 1518302.                                    Gvr2010 
18383-0236 BRT3333     Originally published as BRT1947.                                        Brt1936b
18384+6708 STF2384     Unobserved periastron can be covered by speckle in near future.         Sod1999 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.03 +/- 0.58, 2.10, and 0.95 Msun, respectively.  Mlk2012 
18384+0850 HU  198     Variable X Oph; it is the northern component that varies.               Baz1954a
                       The M5e star is the Mira-type variable X Oph, P = 334 d, and at                 
                       minimum often fainter than the K1 star. Motion so far is rectilinear.           
                       Spectrum composite; K1III+M6IIIe.                                               
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       A measure on 1980.4794, incorrectly attributed to ADS 11524 by                  
                       McAlister et al. (1983), actually belongs to ADS 11339.                 McA1983 
18384-0312 A    88     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.42 +/- 0.32, 2.50, and 1.07 Msun, respectively.  Mlk2012 
                       A 4432-d spectroscopic orbit has been determined for this pair.         Grf2013e
18385+1107 BPM 798     [PM2000] 1520282 + [PM2000] 1520283.                                    Gvr2010 
18386+3046 STF2359     Kamper erroneously assigned the wide pairs to 18386+3043 = STF2358.     Kpr1992 
                       The C and D components are A and B of STF2358.                                  
18386+3043 STF2358     The A and B components are also the C and D components of STF2359.              
18386+2422 POU3450     Secondary (from AC catalog) not seen in Aladin - probably plate flaw            
                       or typographic error.                                                           
18386+1632 HO   87     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.52 +/- 2.14, 2.99, and 0.95 Msun, respectively.  Mlk2012 
18387+2858 L    53     Aka SLE 100.                                                                    
18387+2847 L    25     L 25a.                                                                          
18387+2439 HJ 1332     B is BD+24@3479.                                                                
18387-4127 HJ 5052     SWR 249. CPM pair                                                       Skf2004 
18389+5221 STF2368     Mt. Wilson spectral classes A1n and G0.                                         
                       AB: H 2  31.                                                            MEv2010 
18389+1715 BPM 799     [PM2000] 1522179 + [PM2000] 1522332.                                    Gvr2010 
18390+0624 SLE 498     Typographical error (1 arcmin error in coordinates of B component) led          
                       to error in rho and theta by Soulie (1986).                             Sle1986a
18394+0111 BAL1503     J 2519.                                                                         
18395+3009 LDS4794     NLTT 46821/46824                                                        Chm2004 
18395+1225 BPM 800     [PM2000] 1524582 + [PM2000] 1524944.                                    Gvr2010 
18396-3207 PRO 208     SWR 250. CPM pair                                                       Skf2004 
18401+4100 SLE  93     There appears to be a ~90" error in the declination of the primary by           
                       Soulie (1983).                                                          Sle1983 
18404+0942 S   704     B is BD+09@3814.                                                                
18405+1936 OSO 102     G184-017. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
18406+0307 STF2361     B is BD+02@3649.                                                                
18408+1214 HJ 1334     Probably same as J 2142. Jonckheere gives BD as +12@3414; perhaps a     J__1942d
                       misprint for BD+12@3614.                                                        
18409+6633 LDS2419     LDS5242. UC 3635.                                                               
18409+3132 HJ 1337     G206-038. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       NLTT 46857/46858                                                        Chm2004 
18411+2447 LDS6330     Aka POU3485.                                                                    
                       GJ 1230. Estimated age 30-300 Myr; masses 0.40 +/- 0.18 and 0.12 +/-            
                       0.03 Msun; a ~40.0 au.                                                  Jnn2014 
18411+1035 BPMA 57     [PM2000] 1532102 + [PM2000] 1533512.                                    Gvr2010 
18412+1747 BPM 801     [PM2000] 1532364 + [PM2000] 1531960.                                    Gvr2010 
18412+1128 BPM 802     [PM2000] 1532425 + [PM2000] 1532577.                                    Gvr2010 
18413+3018 STF2367     Bidelman classifies AB as composite gK+A:.                                      
                       Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       Only elements P and T have been amended by Starikova (1977) from the    Sta1977a
                       orbit of Baize (1950).                                                  Baz1950b
18413-0727 J  1748     Aka J  2918.                                                                    
18414+7001 GNO   2     Distance is estimated at about 40.2 +/- 4.9 pc, giving a projected              
                       component separation of 2.8 +/- 0.7 au. Estimated orbital period is             
                       ~11 yr, for an assumed age of 1 Gyr. Masses are ~60Mjup for each of             
                       these T5 components.                                                    Gno2011 
18414+1133 BPM 803     [PM2000] 1533639 + [PM2000] 1533477.                                    Gvr2010 
18417+1029 BPM 804     [PM2000] 1534975 + [PM2000] 1535121.                                    Gvr2010 
18417-5514 SWR 251     Southern component not red?                                             Skf2004 
18418+3314 KU  119     SEI 569.                                                                Nsn2017b
18418+1033 BPM 805     [PM2000] 1535637 + [PM2000] 1535209.                                    Gvr2010 
18421+3445 B  2546     A is called a spectroscopic binary, but the variation is likely caused          
                       by motion in the close visual pair.                                             
                       B is BD+34@3286.                                                                
           STF2372     AB: H 4  94.                                                            MEv2010 
           STF2372     AB: SEI 571.                                                            Nsn2017b
18422-1022 J  2522     J 1655 is probably identical                                            Hei1985a
18423-0903 RST4594     A: del Sct = 2 Sct, prototype of the Delta Scuti variables.                     
           H 5  36     AC: H V 36.                                                                     
18424+7550 LDS1890     NLTT 46982/46986                                                        Chm2004 
18425+0334 J   464     AB pair not confirmed by Jonckheere (1962).                             J__1962a
18426+5532 ISO   7     46 Dra. A spectroscopic binary, P 9.87d. Abundance peculiarities.               
           H 6  37     H VI 37.                                                                        
18426-0704 GC 25586    Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1982).                                                         Grf1982b
18426-4740 HJ 5054     B is CD-47@12469.                                                               
18427+1354 JNN 280     There is a point source at 3.7" separation from GJ 4071. The system             
                       has only been observed in one epoch, but based on the colors of the             
                       candidate (dz' = 5.8 +/- 0.1 mag and di' = 5.7 +/- 0.1 mag), it counts          
                       as a probable background contaminant in our analysis.                   Jnn2014 
18428+5938 STF2398     AB: Mt. Wilson spectral classes M4 and M4. Proper motion -1298 +1879.           
                       B is variable. Also known as LDS1466.                                           
                       Optical pair.                                                           Doo1901 
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
                       Parabolic orbit by Wieth-Knudsen (1953).                                Wie1953b
                       sigma = areal constant in the true orbit = 2.207 arcsec^2/yr                    
                       q = periastron distance in the true orbit = 16".603                             
                       A short-period motion in one of the components has been suspected               
                       repeatedly, but photographic measures do not show it. (Heintz 1978)     Hei1978d
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AC: Same as ADS 11632 AB.                                                       
18429+4456 STF2380     B is BD+44@2974.                                                                
18430-7126 HJ 5048     zet Pav                                                                         
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
18431+1318 BPM 806     [PM2000] 1542850 + [PM2000] 1543469.                                    Gvr2010 
18431+0742 LDS1013     B is BD+07@3814.                                                                
18432+1017 BPM 807     [PM2000] 1543666 + [PM2000] 1544209.                                    Gvr2010 
18433+3918 BLL  35     A spectroscopic binary. B is BD+39@3504.                                        
18433+2506 POU3503     COU 509.                                                                        
18434-5252 HJ 5055     SWR 252. CPM pair                                                       Skf2004 
                       Primary is QZ Tel, a W UMa type eclipsing binary, P = 1.03099d.         Zas2012 
18434-5546 HJ 5053     Also known as R   310.                                                          
           B   398     AB: Tokovinin & Lepine (2012) miss AC, but list 2 optical companions    Tok2012c
                       at 697" and 1340".                                                      Tok2014d
                       AB: Gomez et al. (2016) derive dynamical parallax and component masses          
                       for both short- and long-period solutions:                                      
                       short: 16.93 +/- 0.41 mas, 1.126 +/- 0.013 Msun, 0.896 +/- 0.010 Msun.          
                       long:  14.33 +/- 0.47 mas, 1.219 +/- 0.019 Msun, 0.970 +/- 0.015 Msun.  Doc2016i
18435+1247 BPM 808     [PM2000] 1545429 + [PM2000] 1546011.                                    Gvr2010 
18435-0817 J   104     eps Sct                                                                         
18436+1439 BPM 809     [PM2000] 1545884 + [PM2000] 1545616.                                    Gvr2010 
18436-5138 RST5451     A is variable. Spectral type A2/3III/IV.                                        
18437+3141 A   253     Only elements P, T, and a have been amended by Starikova (1978) from    Sta1978c
                       the orbit of Muller (1956).                                             Mlr1956b
18438+1200 BPM 810     [PM2000] 1546793 + [PM2000] 1546974.                                    Gvr2010 
18438-3819 COO 227     11 Cra. Variable?                                                               
18439+1601 OSO 103     G184-020. None is a common proper motion pair                           Oso2004 
18439-0649 YSC 133     A first orbit for this system was reported recently in Tokovinin et     Tok2015c
                       al. (2015), but those authors assumed a quadrant flip of one data               
                       point taken by Horch et al. (2008). That was not an unreasonable        Hor2008 
                       assumption based on the relatively small magnitude difference, but the          
                       points presented here give support to an "alternate" orbit where no             
                       quadrant flips are needed and the period is about half of that derived          
                       in the earlier calculation. Given the revised Hipparcos parallax of             
                       13.55 +/- 0.43 mas, the new orbit gives a mass sum of 3.5 +/- 1.0Msun,          
                       which is somewhat high for a system of composite spectral type F7, but          
                       with substantial uncertainty at this stage. In contrast, the Tokovinin          
                       orbit gives a mass sum of about 1 Msun, which would seem to be too low          
                       by roughly the same amount.                                             Hor2015b
18440+1820 BPM 811     [PM2000] 1548500 + [PM2000] 1548937.                                    Gvr2010 
18442+1030 BPM 812     AB: [PM2000] 1549644 + [PM2000] 1550217.                                Gvr2010 
           BPM 813     BC: [PM2000] 1550217 + [PM2000] 1550653.                                Gvr2010 
18443+3940 STF2382     A: eps 1 Lyr = 4 Lyr                                                            
                       AB: A premature orbit has been computed.                                        
           STFA 37     AB,CD: See ADS for notes of components.                                 A__1932a
                       AB and CD form the physical quadruple eps Lyrae, separation                     
                       208". The observed small RV variations in each pair are probably                
                       merely scatter due to the very poor lines.                                      
                       BD: SHY 307. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
           STF2383     C: eps 2 Lyr = 5 Lyr                                                            
           CHR  77     Ca: See note for 18323-1439 = CHR 73.                                   Hrt1996b
                       Ca is an Alpha CVn-type variable.                                               
                       The measures show a large scatter and there are many observations of            
                       the wider pair without a measure of this close companion. The nature            
                       of the motion or even the reality of this pair is in question.          Tok2010b
           STF2383     The longitude of periastron in the orbit of CD has been corrected.      Gzl1956a
           SHJ 277     EF, EG, etc.: A preliminary sketch of the motions of the SHJ group              
                       show the G component may be flying away in position angle ~190          Dal2002a
           STF2382     AB: H 2   5.  STF2383CD: H 2   6.                                       MEv2010 
18444+2003 GRV 238     B component is +19 3770.                                                        
18444-4657 HU 1528     V359 Tel, Algol (EA) type eclipsing binary, P = 19.2449 d.              Zas2011 
18445+3400 STTA172     B is BD+33@3191.                                                                
18445+1913 J   466     TDT1030.                                                                        
18446+1138 BPM 814     [PM2000] 1552151 + [PM2000] 1551797.                                    Gvr2010 
18448+3736 BU  968     A: zet 1 Lyr = 6 Lyr. A is a spectroscopic binary and variable.                 
           STFA 38     D: zet 2 Lyr = 7 Lyr                                                            
                       AD: STTA173. According to Henroteau, the wide pair zet 1 + zet 2 Lyr    HFC1828 
                       was first by Bianchini in 1737.                                         Bia1737 
                       AD: SHY 308. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
                       AD: H 5   2.                                                            MEv2010 
18448+1036 BPM 815     [PM2000] 1553946 + [PM2000] 1553909.                                    Gvr2010 
18448-3449 BRT1786     CPD-34@8050.                                                                    
18448-5354 HRG 139     SWR 253.                                                                        
18449+1606 HEI 173     A third star at 323 deg, 62"                                            Hei1983a
18450+1255 BPM 816     [PM2000] 1555247 + [PM2000] 1555413.                                    Gvr2010 
18451+4746 ES 1161     KIC 10514430 = KOI 263.                                                         
18451+1415 BPM 817     [PM2000] 1556143 + [PM2000] 1556451.                                    Gvr2010 
18452+4227 KOI  10     AB: Adams et al. (2012) theta values corrected to 360-theta             Adm2012 
                       (reported by Dressing et al. (2014).                                    Dre2014 
18452+3819 STF2393     Also known as STF2387.                                                          
                       AB: H 3  81.                                                            MEv2010 
18452+3532 STF2386     B is BD+35@3350.                                                                
18453+1434 BPM 818     [PM2000] 1557759 + [PM2000] 1558675.                                    Gvr2010 
18453-2039 EVS  37     Primary is the Cepheid V350 Sgr.                                        Evs2016a
18454-6452 SKF 105     Member of the bet Pic moving group.                                     Zuc2001b
18454-5025 R   313     B is CD-50@12120.                                                               
18455+1024 BPMA 58     [PM2000] 1559344 + [PM2000] 1559289.                                    Gvr2010 
18455+0530 STF2375     This remarkable quadruple system is comprised of two close (0".14)              
                       pairs of similar position angle, discovered by Finsen with his          Fin1953c
                       eyepiece interferometer.  Our 1982 observations (McAlister et al.       McA1987b
                       1987) were made at lower magnification and included all four stars in           
                       the field. The resulting overlapping autocorrelation peaks precluded            
                       measurement of the Aab or Bab pairs directly, but did permit measures           
                       of the AB; Aa,Bb; and Ab,Ba configurations.  In later observations              
                       made at higher magnification we observed the A and B components                 
                       separately, enabling measurement of Aa,Ab and Ba,Bb but not AB.                 
                       Listed in the first speckle catalogue as STF 2375 AB,CD.                McA1984b
           FIN 332     Aa,Ab: Listed in the first speckle catalogue as Fin 332 AB.             McA1984b
           FIN 332     Ba,Bb: Listed in the first speckle catalogue as Fin 332 CD.             McA1984b
18456+1604 BPM 820     [PM2000] 1560170 + [PM2000] 1560342.                                    Gvr2010 
18456+1041 BPM 819     [PM2000] 1559506 + [PM2000] 1559263.                                    Gvr2010 
18457+2033 HJ 2839     110 Her.                                                                        
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
18457-1624 J  1656     J 1749.                                                                         
18458+4647 KOI1537     Primary is Kepler exoplanet host star.                                  Adm2013 
18458+3431 STF2390     H 2  67.                                                                MEv2010 
18460+1124 BPM 821     [PM2000] 1562588 + [PM2000] 1562091.                                    Gvr2010 
18460+2422 SLE 508     One degree error In Soulie (1986a) declination.                         Sle1986a
18461+2734 SLE 366     Apparently a typographical error in Soulie's RA for the secondary led   Sle1985 
                       to his discrepant measure.                                                      
18462+1432 BPM 822     [PM2000] 1564514 + [PM2000] 1563801.                                    Gvr2010 
18462+1034 BPM 823     [PM2000] 1564654 + [PM2000] 1564191.                                    Gvr2010 
18463+1030 BPM 824     [PM2000] 1565096 + [PM2000] 1565598.                                    Gvr2010 
18463-2224 SEE 360     28 Sgr.                                                                         
18463-7249 HIP  92103  The NICI images are of poor quality resulting in a shallow detection            
                       limit (at 0".2, dK < 3 and dH < 2).                                     Tok2012a
18464+3116 HJ 1345     Recognized to be the same as SLE 121 by Francisco Romero                FMR2006c
18464+1240 BPM 825     [PM2000] 1565889 + [PM2000] 1565812.                                    Gvr2010 
18464-3559 BRT1787     CPD-36@8476.                                                                    
18465-0058 MCA  53     Aa,Ab: 5 Aql. A suspected spectroscopic binary, now resolved by                 
                       speckle interferometry.                                                         
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 12.98 +/- 5.76, 5.05, and 2.09 Msun, respectively. Mlk2012 
           STF2379     AB: H 3  33.                                                            MEv2010 
18466+3821 HU 1191     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.47 +/- 0.12, 1.69, and 0.88 Msun, respectively.             Mlk2012 
18467-0916 JNN 118     The primary star has two candidate companions in the field of view.             
                       The fainter candidate C is most likely a background star, since its             
                       color is entirely inconsistent with a late M-type star. The brighter            
                       candidate B is more uncertain. It's colors are fully consistent with            
                       the brightness contrast to the primary for a physical companion,                
                       implying a spectral type of M5. It is also visible in 2MASS (Skrutskie          
                       et al. 2006 AJ 131, 1163), which enables to perform a rough CPM test.           
                       The test indicates that B is inconsistent with a static background              
                       object, again implying physical companionship. However, the motion is           
                       also poorly consistent with orbitalmotion, with a sky-projected speed           
                       of order 2 au per year - highly unlikely for such a wide and low-mass           
                       binary. This implies either under-estimated uncertainties in the data,          
                       or an unusual astronomical coincidence. With the small separation and           
                       relatively high brightness difference of the candidate companion, it            
                       is just at the detection limit of 2MASS, and is only reliably                   
                       detectable in K-band. Perhaps there is a systematic noise component             
                       beyond the quoted astrometric 2MASS error in this circumstance. If all          
                       the data are taken at face value, another possible interpretation is            
                       an unfortunate chance alignment with a local M-dwarf, which has a               
                       signficant proper motion of its own. In any case, due to all these              
                       uncertainties, we tentatively treat the pair as a candidate binary              
                       here, but emphasize that more data is needed to test physical                   
                       companionship.                                                          Jnn2012 
18467-2930 TOK 366     Triple system. The wider C component is confirmed as CPM by 2MASS.      Tok2013b
                       AB: A is astrometric binary, P=20.828y (Makarov & Kaplan 2005)          Mkr2005 
18468+4224 KOI 2914    This system hosts a 2.0 Rearth planet with a 21.1 day period (Burke et  KOI2014a
                       al. 2014).                                                              Dre2014 
18468-1428 RST4596     Primary is possible SB, no orbit.                                       Tok2014d
18468-3636 NHR  10     AB: KOH 108.                                                                    
18469+1105 BPM 826     [PM2000] 1569882 + [PM2000] 1569114.                                    Gvr2010 
18469-1222 BRT2757     Possibly BD-12@5164. J 2147.                                                    
18470+1811 ENG  64     AB: 111 Her. BC: Hipparcos acceleration double solution.                        
           SMA  80     Also known as ENG  64CD.                                                        
           ABH 103     All ABH pairs were incorrectly identified with the C component rather           
                       than B. In addition, three early measures of BI were actually of the            
                       new pair, now labelled ENG  64DJ.                                               
18471+5523 SIG   5     Konopacky et al. (2010) derive a distance of 29.8 +/- 7.1 pc and a              
                       system mass of 0.18 +0.35/-0.13 Msun.                                   Kon2010 
18471+1328 BPM 827     [PM2000] 1572182 + [PM2000] 1572776.                                    Gvr2010 
18471-2331 LDS4798     NLTT 46980/46981                                                        Chm2004 
18472+1227 BPM 828     [PM2000] 1572338 + [PM2000] 1573212.                                    Gvr2010 
18472-0445 NOI   5     HR 7063 = bet Sct.                                                              
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Young (1927).                                                           YRK1927 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Young (1926).                                                           YRK1926 
18473+0323 LDS5866     LDS6331.                                                                        
18474+1122 BPMA 59     [PM2000] 1574643 + [PM2000] 1574494.                                    Gvr2010 
18474-2108 B  1889     Spectrum: B9.5II/III.                                                           
18475+4926 BU  971     The primary is a spectroscopic binary, and is also the semiregular              
                       variable S Sct.                                                                 
                       Algol (EA) type eclipsing binary, P = 4.243 d.                          Zas2011 
18476+4450 KOI  68     AB, AC, AD: Adams et al. (2012) theta values corrected to 360-theta     Adm2012 
                       (reported by Dressing et al. (2014).                                    Dre2014 
18476+2903 DAM 679     Typographic error in initial WDS designation (18376+2903)                       
18476+2335 HJ 2841     POU3552.                                                                        
18476+1234 BPM 829     [PM2000] 1575822 + [PM2000] 1575179.                                    Gvr2010 
18476+1121 BPM 830     [PM2000] 1576469 + [PM2000] 1576881.                                    Gvr2010 
18476-0156 LUQ   1     Primary is the Wolf-Rayet star WR 121a, in the W43 star-forming                 
                       complex; this confirms  earlier spectroscopic suspicion of a companion          
                       star, as well as the colliding wind binary scenerio invoked to                  
                       interpret X-ray emission.                                               Luq2011 
18476-0157 LUQ   2     Primary is an O star in the W43 star-forming complex; it appears to             
                       concide with the peak in non-thermal emission by the cluster.           Luq2011 
18477+3600 ALI 142     A is the RR Lyrae-type variable EZ Lyr.                                         
18477+1539 BPM 831     [PM2000] 1577255 + [PM2000] 1576842.                                    Gvr2010 
18478+1725 BPM 832     [PM2000] 1577924 + [PM2000] 1576931.                                    Gvr2010 
18479+1403 BPM 833     [PM2000] 1579102 + [PM2000] 1579251.                                    Gvr2010 
18479+1110 STTA174     B is BD+10@3660.                                                                
18481+1656 BPM 834     [PM2000] 1580332 + [PM2000] 1581229.                                    Gvr2010 
18481+1557 BPM 835     [PM2000] 1580795 + [PM2000] 1579735.                                    Gvr2010 
18481+1231 BPMA 60     [PM2000] 1580760 + [PM2000] 1582659.                                    Gvr2010 
18482+1039 STT 362     Also known as STT 546.                                                          
18483-1935 B  2461     J 1635, J 1750.                                                                 
18483-2033 DON 924     CPD-20@7194.                                                                    
18483-6856 JAO   8     The fainter source in the STIS UV data is the red dwarf primary; the            
                       brighter blue companion is a faint white dwarf with a mass >0.5Msun.    Jao2014a
                       Primary is SCR 1848-6855, a high-proper motion M5.0V dwarf at 24.6pc.           
                       Astrometric observations spanning 8.5 years reveal large photocentric           
                       perturbation due to an initially unseen companion. The pair was                 
                       subsequently resolved by HST/STIS.                                      Jao2014b
18484+1542 BPMA 61     [PM2000] 1582816 + [PM2000] 1585071.                                    Gvr2010 
18485+1045 STF2396     AB, AC, and AD: Optical pairs, based on study of relative motion of             
                       the components using the method of apparent motion parameters.          Kiy2008 
18486+1344 BPM 836     [PM2000] 1584779 + [PM2000] 1584834.                                    Gvr2010 
18487+2053 RAS  27     Main component is poorly-studied silicon star, type A1; companion               
                       late-G/early-K.                                                         Ras2014 
18487+1803 BPM 840     [PM2000] 1585768 + [PM2000] 1586803.                                    Gvr2010 
18487+1426 BPM 838     AB: [PM2000] 1585727 + [PM2000] 1586604.                                Gvr2010 
           BPM 839     BC: [PM2000] 1586604 + [PM2000] 1585866.                                Gvr2010 
18487+1137 BPM 837     [PM2000] 1585336 + [PM2000] 1586244.                                    Gvr2010 
18487-0600 STF2391     AB: H 6  50.                                                            MEv2010 
18487-1702 J  2235     Spectrum: G6/8III/IV.                                                           
18488-0120 BAL 585     J 1373.                                                                         
18489+1615 STF2400     AC: Mt. Wilson spectra are F5s for A and A4n for C.                             
                       AD: D not seen in 1901 and 1919.                                                
                       BC: Additional notes may be found in Burnham (1894).                    Bu_1894 
18489+1219 BPM 841     [PM2000] 1587296 + [PM2000] 1587585.                                    Gvr2010 
18490-0828 STF2388     C component is of spectral type K0:III                                  AbH2000 
18491+1524 BPM 842     [PM2000] 1589068 + [PM2000] 1588083.                                    Gvr2010 
18492+2503 CHR  79     Hipparcos Suspected non-single.                                                 
                       A spectroscopic binary, P = 13.08d. Hence triple.                               
                       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.                                             
18493+2606 BRT3334     Originally published as BRT 184.                                        Brt1928 
18493+1416 BPM 845     [PM2000] 1590859 + [PM2000] 1591945.                                    Gvr2010 
18493+1214 BPM 844     [PM2000] 1590851 + [PM2000] 1590883.                                    Gvr2010 
18493+1206 BPM 846     [PM2000] 1591164 + [PM2000] 1591513.                                    Gvr2010 
18493+1144 BPM 843     [PM2000] 1590805 + [PM2000] 1590470.                                    Gvr2010 
18494+5811 STI2392     MLB 76.                                                                         
18494+1400 BPM 847     [PM2000] 1591238 + [PM2000] 1591692.                                    Gvr2010 
18494+1252 BPM 848     [PM2000] 1591568 + [PM2000] 1591349.                                    Gvr2010 
18496+1621 BPM 849     [PM2000] 1593370 + [PM2000] 1592493.                                    Gvr2010 
18496+1313 SHY 309     HIP  92388 + HIP  92638.                                                        
18497+1238 BPM 852     [PM2000] 1594564 + [PM2000] 1593619.                                    Gvr2010 
18497+1147 BPM 850     [PM2000] 1594069 + [PM2000] 1594283.                                    Gvr2010 
18497+1038 BPM 851     [PM2000] 1594230 + [PM2000] 1593700.                                    Gvr2010 
18497-0555 H 6  50     H VI 50. C is BD-06@4923.                                                       
                       A is a long-period spectroscopic binary.                                        
18497-2019 SEE 362     29 Sgr. Spectroscopic binary.                                                   
18497-7300 R   314     A is a spectroscopic binary.                                                    
18498+3249 H 5  40     A: nu 1 Lyr = 8 Lyr.  H V 40. A is a Beta Lyrae-type system.                    
18498+1639 BPM 853     [PM2000] 1594694 + [PM2000] 1594986.                                    Gvr2010 
18499+3233 HO  440     A: nu 2 Lyr = 9 Lyr                                                             
18499+2806 OSO 104     G184-032. None is a common proper motion pair                           Oso2004 
                       The 2002 measure by Osorio was mistakenly added as a different pair,    Oso2004 
                       designated AC. Pairs have been merged.                                          
18500+2043 HU  328     A is the Algol-type system AD Her.                                              
18500+1733 BPM 855     [PM2000] 1596993 + [PM2000] 1596377.                                    Gvr2010 
18500+1519 YSC  12     Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos            
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Nidever et al. (2002). They derived component masses 1.21 and 0.10      Nid2002 
                       Msun and an estimated semimajor axis of 34.92 mas.                      Ren2013 
                       HD 174457. Combined astrometric/spectroscopic solution, using                   
                       spectroscopic elements (P,T,e,omega) from Nidever et al. (2002 ApJS             
                       141, 503).                                                              SaJ2011 
18500+1420 BPM 854     [PM2000] 1596486 + [PM2000] 1595844.                                    Gvr2010 
18501+3322 STFA 39     STTA175. A is 10 Lyr = Sheliak = bet Lyr, the prototype variable of             
                       its class. B is BD+33@3224.                                                     
                       AB: H 5   3.                                                            MEv2010 
           CIA   3     Aa1,2: bet Lyr. Eclipsing binary (P=12.9d) resolved by CHARA Array              
                       (Zhao et al. 2008). Reductions by two techniques (MACIM and BSMEM) and  CIA2008b
                       a model fit listed in paper; MACIM and BSMEM results given in WDS and           
                       Interferometric Catalog. Three possible orbital solutions also given,           
                       adopting period and Tmin from Ak et al. (2007 A&A 463, 233) and e=0             
                       (Harmanec 2002 ANac 323, 87). These yield distance estimates ranging            
                       from 271 to 313 pc; masses for the gainer and donor are 12.76 +/- 0.27          
                       and 2.83 +/- 0.18 Msun, respectively.                                           
                       Aa1,2: Malkov et al. (2012) derive dynamical and spectroscopic masses           
                       19.84 +/- 11.13 and 15.84 Msun, respectively.                           Mlk2012 
                       In addition to the close pair there is also a hot spot with a size of   IAU2014b
                       22-33 solar radii. What is unknown is where the mass is lost and how            
                       much matter is in the jets.                                                     
18501+2949 HJ 1352     J   109.                                                                        
18501+1230 BPM 856     [PM2000] 1597921 + [PM2000] 1598622.                                    Gvr2010 
18502+1339 BPM 857     [PM2000] 1598720 + [PM2000] 1598294.                                    Gvr2010 
18502-3708 SWR 254     CPM pair                                                                Skf2004 
18503+1626 BPM 859     [PM2000] 1599627 + [PM2000] 1598472.                                    Gvr2010 
18503+1229 BPM 858     [PM2000] 1599448 + [PM2000] 1600027.                                    Gvr2010 
18503-0754 BU  969     S Scuti, variable 9.7-10.9, 148 days.                                           
18503-3736 SWR 255     CPM pair                                                                Skf2004 
18504+1554 BPM 860     [PM2000] 1600232 + [PM2000] 1600303.                                    Gvr2010 
18504+1336 BPM 861     [PM2000] 1600353 + [PM2000] 1599901.                                    Gvr2010 
18504+1241 J  469      Pair is +1m16s, -3" from BD+12 3661. In 1911 Jonckheere noted the               
                       companion was magnitude 10.0, and in 1915 14.0.                         Cou1955a
18504+1210 BPMA 62     [PM2000] 1600642 + [PM2000] 1600936.                                    Gvr2010 
18506+1525 BPM 862     [PM2000] 1601565 + [PM2000] 1600976.                                    Gvr2010 
18506+1458 BPM 863     [PM2000] 1601827 + [PM2000] 1600984.                                    Gvr2010 
18507+1233 BPM 864     [PM2000] 1602976 + [PM2000] 1603469.                                    Gvr2010 
18508+1301 BPM 865     [PM2000] 1603392 + [PM2000] 1602522.                                    Gvr2010 
18508+1059 STF2404     A spectroscopic binary. Composite spectrum, K5III+K3III.                        
18508-2210 BU 1300     30 Sgr.                                                                         
18509+1751 BPM 867     [PM2000] 1604886 + [PM2000] 1604822.                                    Gvr2010 
18509+1109 BRT1312     Also known as COU  16.                                                          
18509+1107 BPM 866     [PM2000] 1604810 + [PM2000] 1605623.                                    Gvr2010 
18510+1505 BPMA 63     [PM2000] 1605089 + [PM2000] 1604284.                                    Gvr2010 
18510+1339 BPM 868     [PM2000] 1605715 + [PM2000] 1605908.                                    Gvr2010 
18510+1041 BPM 869     [PM2000] 1605785 + [PM2000] 1605090.                                    Gvr2010 
18510-2018 PLT   3     A is BB Sgr, B is V 4088 Sgr.                                           Plt1934 
                       Primary is a Cepheid variable.                                          Evs2016a
18511+1421 BPMA 64     [PM2000] 1605963 + [PM2000] 1603708.                                    Gvr2010 
18511-1421 RST4602     J 1659.                                                                         
18512+5923 STF2420     omi Dra = 47 Dra. A is a spectroscopic binary and also variable.                
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AB: H 4  20.                                                            MEv2010 
           omi Dra     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Young (1920).                                                           YRK1920 
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Young (1920).                                                           YRK1920 
           CIA   8     Aa,Ab: Roettenbacher et al. (2015) resolve the RS CVn binary omi Dra            
                       and determined a combined spectroscopic/astrometric orbit. The orbital          
                       parallax is 9.36 +/- 0.10 mas (106.8 +/- 1.1pc), flux ratio in H is             
                       370 +/- 40, the system age 3.0 +/- 0.5 Gyr. Radii are 25.1 +/- 0.3 and          
                       1.0 +/- 0.1 Rsun, luminosities 220 +/- 30 and 1.3 +/- 0.2 Lsun.                 
                       Derived masses are 1.35 +/- 0.05 and 0.99 +/- 0.02 Msun.                CIA2015c
18515+1700 BPMA 65     [PM2000] 1609645 + [PM2000] 1607904.                                    Gvr2010 
18515+1507 OL  105     Not found by Heintz at IDS position.                                    Hei1985a
18517+1600 BPM 870     [PM2000] 1611210 + [PM2000] 1610854.                                    Gvr2010 
18518-2141 DON 929     CPD-21@7088.                                                                    
18519-5756 HJ 5065     B is CPD-58@7511.                                                               
18520+5951 STI 866     LDS2752.                                                                        
18520+4243 LEH   1     Lehmann et al. (2016) find that KIC 7177553 is a quadruple system,              
                       consisting of two close binaries of nearly equal magnitude, separated           
                       by about 0.4". They estimate the distance to the quadruple as 406 +/-           
                       10 pc, giving a physical separation of the wide pair 167+/- 5 au and            
                       an orbital period >1000y.  One close pair is an eclipsing binary with           
                       orbital period 18.00d. The other pair is an SB with period 16.5d. All           
                       four stars are of similar mass and spectral type (main-sequence G).     Leh2016 
18520+1047 STF2408     Also known as GAN   6.                                                          
18520-5418 TOK 325     Triple system. The inner astrometric binary is resolved here; the CPM   Tok2012c
                       companion at 146 is found by Tokovinin & Lepine (2012).                 Tok2013b
18521+2431 COU 510     Previously classified as an Algol-type system, JZ Her, Petr Zasche              
                       (personal corres.) reports that Couteau must have confused it with      Cou1972a
                       the nearby HS Her. This pair is non-variable and is often used as a             
                       check star in variability analyses.                                             
18521+1635 BPM 871     [PM2000] 1615013 + [PM2000] 1614900.                                    Gvr2010 
18522+1409 BPM 872     [PM2000] 1615303 + [PM2000] 1616136.                                    Gvr2010 
18522+1203 BPM 873     [PM2000] 1615368 + [PM2000] 1615921.                                    Gvr2010 
18522-6211 HJ 5062     lam Pav. A is a Cepheid.                                                        
18523+3926 WEI  33     B is BD+39@3557.                                                                
18523+2126 ISO   8     112 Her. A spectroscopic binary, P = 6.36d. The interferometric pair            
                       cannot be this object, so the system is triple.                                 
18523+1432 STF2411     B spectrum F7V. It is called a spectroscopic binary.                            
18523+1357 BPM 874     [PM2000] 1616566 + [PM2000] 1617001.                                    Gvr2010 
18524+1445 BPMA 66     [PM2000] 1617269 + [PM2000] 1616881.                                    Gvr2010 
18525+1644 BPM 875     [PM2000] 1618619 + [PM2000] 1618464.                                    Gvr2010 
18526+1414 BPMA 67     [PM2000] 1619286 + [PM2000] 1619792.                                    Gvr2010 
18528+3125 A   257     Also a faint unequal pair about 28" from CD in 226@.                            
18528+1357 BPM 876     [PM2000] 1621241 + [PM2000] 1620626.                                    Gvr2010 
18528+1234 AG  365     B is BD+12@3695.                                                                
18528-1725 HU  257     Spectrum: Fm Delta Del.                                                         
18528-5057 HJ 5067     SWR 256.                                                                        
18529-5708 LUH  14     LHS 3421 + 2MASS J18525777-5708141.                                     Luh2012b
18530+5816 ES 1746     MLR 359.                                                                        
18530-0935 CHR  81     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.                                             
18531+7405 GC 26011    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18531+1412 BPM 877     [PM2000] 1623188 + [PM2000] 1622811.                                    Gvr2010 
18531-5011 MUG  10     Aa,Ab: PZ Tel. Companion shows common proper motion and detected                
                       orbital motion. Infrared magnitudes are consistent with companion               
                       being a brown dwarf of mass 28 +12/-4 Mjup and Teff = 2500-2700K.       Mug2010 
                       Biller et al. (2010) derive spectral types K0, M7 +/- 2, estimated      Bil2010 
                       masses 1.25 +0.05/-0.20 Msun and 36 +/- 6 Mjup. Age 12 +8/-4 Myr,               
                       distance 51.5 +/- 2.6 pc. Their JHK magnitudes are derived from 2MASS   TMA2003 
                       photometry, combined with their magnitude differences.                          
                       PZ Tel. Member of the bet Pic moving group.                             Zuc2001b
18533+1737 BPM 878     [PM2000] 1624711 + [PM2000] 1625113.                                    Gvr2010 
18533+1557 BPM 879     [PM2000] 1625218 + [PM2000] 1625017.                                    Gvr2010 
18534+1851 LDS5867     LDS6332.                                                                        
18535+7547 STF2452     233 Dra. A spectroscopic binary.                                        D__1883 
                       Aka H 2  31 = S   713.                                                  Bu_1906 
18535+0912 ROE 112     J 2930. Roe and Jonckheere measures of AB were earlier erroneously      Roe1918 
                       attributed to BC.                                                       J__1962a
18535-2030 DON 933     CPD-20@7296.                                                                    
18536-1941 RST3203     Spectrum: A2/3II/III.                                                           
18537+3658 H 6   3     H VI 3. del 1 Lyr = 11 Lyr. A is a SB. B is BD+36@3308.                         
18537+1353 BPM 880     [PM2000] 1628451 + [PM2000] 1628755.                                    Gvr2010 
18537-0533 A    93     Wilson's value for omega was corrected by Muller.                       WRH1954c
                                                                                               Mlr1954d
18538+1756 BPM 881     [PM2000] 1628952 + [PM2000] 1628974.                                    Gvr2010 
18540+1516 L    40     Hipparcos acceleration double solution.                                         
                       J  2585.                                                                Nsn2016 
18541+1500 HD175292    Hipparcos astrometric solution assumed circular orbit (e = omega = 0)   HIP1997d
18541-5131 RST1008     V362 Tel, Algol (EA) type eclipsing binary, P = 1.21125 d.              Zas2011 
18541-5421 HJ 5068     LDS 656.                                                                        
18542-2245 BU 1033     nu 1 Sgr = 32 Sgr                                                               
           nu Sgr      Henroteau notes that Ptolemy (Magna compositio. Venetiis 1515, lib      HFC1928 
                       VIII, cap 1) called the 14' pair nu 1 + nu 2 Sgr a double star.                 
                       This is perhaps the earliest description of a double star.                      
18543+4259 OSO 105     G205-042. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
18543+1158 BPM 882     [PM2000] 1633715 + [PM2000] 1634697.                                    Gvr2010 
18545+4823 WOL   4     KOI1725.                                                                        
18545+3654 ES 2028     del 2 Lyr = 12 Lyr. A is an unclassified variable.                              
18545+1149 BPM 883     [PM2000] 1634622 + [PM2000] 1634682.                                    Gvr2010 
18546+2754 BRT3335     ADS 11819a. Originally published as BRT 185.                            Brt1928 
18547+2239 BU  646     113 Her. The G-type component is a long-period spectroscopic binary.            
           MKT   9     Visual orbit by Hummel et al. (1995) based on astrometry from Mark III  MkT1995 
                       interferometer. Additional spectroscopic data yield component masses,           
                       luminosities, radii, effective temperatures, and distance.                      
                       Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Hummel et al. (1995).                                                   MkT1995 
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.71 +/- 3.27, 5.64, and 4.08 Msun, respectively.  Mlk2012 
                       Aa,Ab: Ren & Fu (2013) calculated an astrometric orbit, combining       Ren2013 
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Luyten (1936).                                                          Luy1936 
18547-1946 OL   80     DON 934. J 1752.                                                                
18549+3358 STT 525     A is a spectroscopic binary. C is BD+33@3256.                                   
18549+1201 BPM 884     [PM2000] 1637865 + [PM2000] 1638783.                                    Gvr2010 
18549-2157 RSS 495     CD-22@13417                                                                     
18550+4822 KOI2754     This system hosts a 0.7 Rearth planet candidate with a 1.3 day period           
                       (Burke et al. 2014). Our ARIES observations revealed a companion 2.11   KOI2014a
                       J mags and 1.65 Ks mags fainter than KOI2754 at a 0".763 separation.            
                       The predicted Kp mag of the companion star is Kp = 15.3 (dKp = 3.0)             
                       if the star is a dwarf and Kp = 15.2 (dKp = 2.9) if the star is a               
                       giant. The companion star was also detected in the WIYN speckle                 
                       imaging acquired with DSSI. The companion is 3.12 mag. fainter than             
                       KOI2754 at 692 nm and 2.56 mags fainter at 880 nm. Assuming that the            
                       planet orbits the target star and that all of the light from the                
                       companion is captured in the Kepler aperture, then the planet radius            
                       should be increased by 3% to account for dilution. KOI2754 does not             
                       exhibit a significant source offset during transit.                     Dre2014 
18550+1136 BPM 886     [PM2000] 1638955 + [PM2000] 1638009.                                    Gvr2010 
18550+1119 BPM 885     [PM2000] 1638777 + [PM2000] 1638092.                                    Gvr2010 
18550-6356 NZO  93     Not found by Heintz at IDS position. Position since corrected.          Hei1990b
18551+4051 HEI  73     KIC 5598639. Primary is Algol type elipsing binary, period 1.29755d.    Zas2017b
18551+1537 BPM 887     [PM2000] 1639912 + [PM2000] 1640333.                                    Gvr2010 
18551+1522 BPMA 68     [PM2000] 1639841 + [PM2000] 1637903.                                    Gvr2010 
18552+4409 GIC 153     G205-045/G205-044.                                                              
18553+1304 BPMA 69     [PM2000] 1641172 + [PM2000] 1641740.                                    Gvr2010 
18553-2341 B   412     Spectrum: B9.5III/IV.                                                           
18553-2618 BED   1     Aa,Ab: Measure of 1991.566 made by MAPPIT.                              Bed1994 
           SMY   4     AB: sig Sgr = 34 Sgr = Nunki. B is CD-26@13591.                                 
18554+1331 BU  647     Also DU    2, BDS 8899. Identification, position corrected by Heintz.   Hei1983a
18555+1413 BPM 888     [PM2000] 1643332 + [PM2000] 1643189.                                    Gvr2010 
18555+0816 J  1191     BRT3336.                                                                        
18556+1413 BPM 889     [PM2000] 1643867 + [PM2000] 1642939.                                    Gvr2010 
18557+1254 COG   1     CD: OL  189.                                                                    
                       J   810.                                                                Nsn2016 
18557+1216 BPM 890     [PM2000] 1644364 + [PM2000] 1643759.                                    Gvr2010 
18558+1243 BPM 891     [PM2000] 1645258 + [PM2000] 1644843.                                    Gvr2010 
18558+0327 A  2192     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.52 +/- 2.27, 3.68, and 1.82 Msun, respectively.             Mlk2012 
18559+1258 BPM 892     [PM2000] 1646011 + [PM2000] 1645924.                                    Gvr2010 
18559+0323 A  2193     Quadrants uncertain.                                                            
18560+4414 STT 365     AB: Duplicity doubtful, needs speckle.                                          
           STF3130     Lewis  measures a pair 1m following and 1' south:                       L__1897 
                       1897, 37@, 3.1", 10.0-11.0.                                                     
18560+3347 STF2421     B is BD+33@3264.                                                                
18560+1147 BPM 893     [PM2000] 1646644 + [PM2000] 1647444.                                    Gvr2010 
18560-2503 B   413     A is SB, no orbit.                                                      Tok2014d
18561+1709 BPM 894     [PM2000] 1647451 + [PM2000] 1647696.                                    Gvr2010 
18562+0412 STF2417     A: the 1 Ser = 63 Ser A = Alya                                                  
                       B: the 2 Ser = 63 Ser B = BD+04@3917.                                           
                       AC: C component = A component of 18566+0416 TOK 620.                            
                       BC: This system was analysed in detail by Teague, who determined the    Tea2001 
                       source of the errors in all three historical measures (Labitzke,        Lbz1929 
                       Przbyllok, and Kamper), which actually belong with the AC pair of this  Prz1926 
                       system.                                                                 Kpr1992 
                       BC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AB: H 4   6.                                                            MEv2010 
18562-5049 RST1011     Spectral type G8/K0 II/III.                                                     
18563+5432 GIC 154     AB = G229-018/G229-019. The B component is GJ 4091B.                            
18563+1435 BPM 896     [PM2000] 1648823 + [PM2000] 1649237.                                    Gvr2010 
18563+1344 BPM 895     [PM2000] 1648725 + [PM2000] 1648525.                                    Gvr2010 
18563-0425 LDS 659     HIP 92960. See Allen et al. (2000) for information on metallicity,      AlC2000 
                       age, galactic orbital parameters, etc.                                          
18564+4530 HJ 1356     B is BD+45@2796.                                                                
                       HJL 261.                                                                HJL1986 
18564+1710 BPM 897     [PM2000] 1649308 + [PM2000] 1650135.                                    Gvr2010 
18564-4040 WG  238     CPD-40@8697. SWR 258.                                                           
                       CPM pair. ASAS J185622-4040.6 (spurious variable?)                      Skf2004 
18565-0511 BRT 485     LEO 43.                                                                         
18565-5313 SWR 257     CPM pair                                                                Skf2004 
18566+1545 BPM 898     [PM2000] 1650833 + [PM2000] 1651015.                                    Gvr2010 
18566+0416 TOK 620     A component = C component of 18562+0412 STF2417AC.                              
18567+5014 JNN 153     2MASS J18564143+5014071 and J18564286+5013483 are separated by only             
                       23" and have similar estimated spectroscopic distances (79 and 77 pc,           
                       respectively) in Riaz et al. (2006), as well as very similar proper     Ria2006 
                       motions (e.g. Roser et al. 2010), hence it is likely that they form a   Rsr2010 
                       physical pair.                                                          Jnn2012 
18567+1657 BPM 899     [PM2000] 1651939 + [PM2000] 1652523.                                    Gvr2010 
18568+1733 BPM 901     [PM2000] 1652793 + [PM2000] 1653380.                                    Gvr2010 
18568+1505 BPM 900     [PM2000] 1652502 + [PM2000] 1651646.                                    Gvr2010 
18569+3112 ES 2422     A is the irregular variable OQ Lyr.                                             
18569+1546 L    42     Baize questions BD identification.  Heintz and Worley were unable to    Baz1944a
                       locate this pair. Identical to OL 180?                                  Hei1983a
18569-3320 GLP  15     B is CD-33@13738.                                                               
18570+3254 BU  648     Identification of the ascending node is somewhat uncertain.             Stk1939 
                       AB: Primary is SB1 and exoplanet host, P=1016d, in a 61y binary         Mut2010e
                       (Muterspaugh et al. 2010). Wobble 1016d, 0.24mas - planet? Astrometric          
                       orbit gives mass 1.5 Mjup if planet around B, 3 Mjup if around A.       Tok2014d
                       AB,C: Optical pair, based on study of relative motion of the                    
                       components using the method of apparent motion parameters.              Kiy2008 
18570+1752 BPM 902     [PM2000] 1653997 + [PM2000] 1654609.                                    Gvr2010 
18571+5143 SHY 749     HIP  93029 + HIP  92467.                                                        
18572+3845 COU1611     TDT1145                                                                         
18573+6224 STF2440     Spectrum of A also called composite; G5IV+G8V.                                  
18573+1800 BPMA 70     [PM2000] 1655946 + [PM2000] 1654297.                                    Gvr2010 
18573+1724 BPM 904     [PM2000] 1656031 + [PM2000] 1655503.                                    Gvr2010 
18573+1644 BPM 903     [PM2000] 1655854 + [PM2000] 1656255.                                    Gvr2010 
18574+2129 HU  329     Many negative results, but probably double.                                     
18574+1517 BPM 905     [PM2000] 1657245 + [PM2000] 1657814.                                    Gvr2010 
18575+5814 STF2438     H 1  43.                                                                MEv2010 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.95 +/- 1.38, 3.19, and 2.19 Msun, respectively.             Mlk2012 
18575+1306 BPMA 71     [PM2000] 1657465 + [PM2000] 1659069.                                    Gvr2010 
18576+7250 OSO 106     G260-013. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
18576+1420 BPM 906     AB: [PM2000] 1658704 + [PM2000] 1659034.                                Gvr2010 
           BPM 907     BC: [PM2000] 1659034 + [PM2000] 1658470.                                Gvr2010 
18577+1731 BPM 908     [PM2000] 1658828 + [PM2000] 1659154.                                    Gvr2010 
18577+1509 OL  180     Position and Durchmusterung correction by Heintz.                       Hei1980a
                       OL  191.                                                                        
18577+1312 BPM 909     [PM2000] 1659281 + [PM2000] 1658736.                                    Gvr2010 
18577+0942 HJ 5505     B is BD+09@3942.                                                                
18578-3802 B   414     Spectral type K?                                                                
18579+4424 KOI 122     Adams et al. (2012) theta values corrected to 360-theta                 Adm2012 
                       (reported by Dressing et al. (2014).                                    Dre2014 
18579+4214 COU1795     TDT1149.                                                                        
18579-2524 B  2871     Spectrum: F2/3III/IV.                                                           
18580+1543 BPM 910     [PM2000] 1661167 + [PM2000] 1660955.                                    Gvr2010 
18581+4711 AG  366     Astroseismology determines Mass and Radius for A(B) as 0.95+/-0.02      WeT2017 
                       (0.93+/-0.01) \msun and 0.93+/-0.01 (0.89+/-0.01) \rsun and an age of           
                       3.0+/-0.5 Gyrs for both stars.                                                  
18581+3813 STF2427     B is BD+38@3377. BC is also known as ALI 875.                                   
18582+1722 CHR  82     Aa,Ab is the Cepheid FF Aql. The system is also a long-spectroscopic            
                       binary, now resolved by speckle.                                                
18582+1644 BPM 911     [PM2000] 1662278 + [PM2000] 1661343.                                    Gvr2010 
18582-2025 HO  271     A is a double-lined spectroscopic binary.                                       
                       Classification of the B component is from Lindroos (1985), who also     Lnd1985 
                       gives a distance of 1.9 kpc to the system.                              Msn1998a
18583+4857 GII  46     Gili (2016) described this pair as the B component of 18582+4858                
                       KOI 258, but the systems differ in position by over 1'.                 Gii2016 
18583+1705 BPM 912     [PM2000] 1663427 + [PM2000] 1663942.                                    Gvr2010 
18583+1654 BPMA 72     [PM2000] 1662798 + [PM2000] 1664716.                                    Gvr2010 
18584+4750 BD+47 2730  Spectroscopic orbit of 858.1d corresponds to this astrometric pair.     Grf2014d
18584+3625 STF2429     H 1  58.                                                                MEv2010 
18584+1459 BPM 913     [PM2000] 1663987 + [PM2000] 1664237.                                    Gvr2010 
18585+1429 BPM 914     [PM2000] 1664713 + [PM2000] 1664939.                                    Gvr2010 
18586+1703 BPMA 73     [PM2000] 1664953 + [PM2000] 1663498.                                    Gvr2010 
18586+1653 BPM 916     [PM2000] 1664901 + [PM2000] 1664659.                                    Gvr2010 
18586+1514 BPM 915     [PM2000] 1664752 + [PM2000] 1665020.                                    Gvr2010 
18588+4041 STF2431     BDS 8981, H IV 93 is identical. A spectroscopic binary.                         
                       H 4  93.                                                                        
18588-0648 J   111     J 2684.                                                                         
18589+3241 AGC   9     gam Lyr = 14 Lyr = Sulafat. Variable? Also known as STT 544.                    
                       AC. Smyth's quoted separation is difference in RA only.                 Smy1844 
18590+1542 BPM 917     [PM2000] 1667679 + [PM2000] 1667227.                                    Gvr2010 
18591+1338 STF2424     11 Aql.                                                                         
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AB: H 3  32.                                                            MEv2010 
18591-2609 B   415     J 1733.                                                                         
18594-1250 KUI  89     A light variable.                                                       Baz1954a
                       1985.4872: This measurement was incorrectly attributed to Kui 84                
                       (WDS 17584+0427) by McAlister et al. (1987).                            McA1987b
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.80 +/- 1.84, 4.41, and 5.25 Msun, respectively.             Mlk2012 
18595+1631 BPM 918     [PM2000] 1670405 + [PM2000] 1670058.                                    Gvr2010 
18595+1420 BPMA 74     [PM2000] 1670255 + [PM2000] 1671086.                                    Gvr2010 
18596+1504 ENG  65     13 Aql = eps Aql. A is a spectroscopic binary.                                  
                       Spectral type K1IIICN0.5Ba0.2.                                                  
           eps Aql     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Griffin (1982).                                                         Grf1982c
18596+1317 BPM 919     [PM2000] 1670767 + [PM2000] 1670975.                                    Gvr2010 
18597+1345 BPM 920     [PM2000] 1671285 + [PM2000] 1671690.                                    Gvr2010 
18597+1206 BPMA 75     [PM2000] 1671862 + [PM2000] 1670609.                                    Gvr2010 
18599+1937 L    43     Not found by Heintz at IDS position.                                    Hei1985a
                       Position in ADS and later WDS was erroneously given as 18597+1036,              
                       although pair also not seen at "correct" coordinates.                           
18599+1454 STF2428     AB: H 2  93.                                                            MEv2010