23003+6755 GIC 187     G241-034/G241-035.                                                              
23004+0353 J  1797     BAL 2575.                                                                       
23005-2619 RST1154     AB: B is PMS star. Member of AB Dor moving group (see Lopez-Santiago            
                       et al. 2006 ApJ, 643, 1160)                                             Tok2014d
           SHY 364     AC: HIP 113597 + HIP 113579.                                                    
           CVN  67     CD: Originally 23003-2609 CVN  67, but primary was found to be the C            
                       component of 23005-2619 SHY 364AC.                                              
                       This is the more massive component of the WDS 23005-2619 system.        Skf2013 
23005-3345 B   582     A = TZ PsA, var. RS CVn type. Strassmeier (1993 A&AS 100, 173) gives            
                       P=1.642d.                                                               Tok2014d
23006-0704 RST4712     The B component is an unresolved composite spectrum binary harbouring           
                       the close hot white dwarf WD 2253-073. Spectral types of A, Ba, and Bb          
                       are G3V, K0V, and DA1.4, respectively; masses are 0.96, 0.79, and               
                       0.58 +/- 0.02 Msun; Teff 5670, 5236, and 37200 +/- 300K.                Hbg2014 
23006-2358 LDS5035     NLTT 9310 + NLTT 9315. CPM pair.                                        Mkr2008 
23008+7453 HJ 3162     H N  35.                                                                MEv2010 
23009-2216 BU  179     CD-22@16154.                                                                    
23005-2619 SHY 364     The more massive component of this multiple system is 23003-2609.       Skf2013 
23010+2646 STF2969     V416 Peg - Algol (EA) type eclipsing binary, P = 1.424797 d.            Zas2011 
23015+1658 BPMA256     [PM2000] 2625556 + [PM2000] 2625433.                                    Gvr2010 
23015+1202 BPM2473     [PM2000] 2625580 + [PM2000] 2625480.                                    Gvr2010 
23016+6912 OL  224     Also known as MLB 435.                                                          
23018-0351 GC 32089    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23019+4220 BLA  12     Aa,Ab: omi And = 1 And. Spectrum composite: B6IIIpe+A2p.                        
                       There appear to be both short and long period light variations.                 
                       Zhuchkov et al. (2010) generated a new orbital solution based on        Zhu2010 
                       published astrometry and new spectroscopic data.                                
           WRH  37     AB: P = 68.6y, a = 0.277", motion retrograde. B has been reported               
                       to be a double-lined spectroscopic binary, P = 33.01d.                          
                       Orbital elements by Olevic & Cvetkovic (2006) for SB:                   Ole2006a
                       P = 33.01 +/- 0.02 d, Tper = 2446925.3 +/- 0.2, e = 0.24 +/- 0.01,              
                       omega = 226.2 +/- 2.3deg, a sin i = 0.161 +/- 0.003 and                         
                       0.211 +/- 0.002 au, M sin3i  = 3.74 +/- 0.05 and 2.86 +/- 0.05 Msun.            
                       This component was first reported in McAlister & Hendry (1982) for      McA1982b
                       1976.61, after which earlier French data were reprocessed to yield the          
                       1975 measures.                                                                  
                       Zhuchkov et al. (2010) generated a new orbital solution based on        Zhu2010 
                       published astrometry, new 6m speckle data, and new radial velocities.           
                       LSC 104.                                                                        
23020+4800 A   194     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.24 +/- 2.37, 3.50, and 2.24 Msun, respectively.             Mlk2012 
23020-2151 B  1018     HDO 174                                                                         
23021+1026 J   294     J 1731.                                                                         
23023-6418 DUN 244     B is CPD-64@4310.                                                               
23024-1119 STF2970     H N 135.                                                                MEv2010 
23026+4946 ES 1185     LDS5999.                                                                        
23026+4245 BU 1147     2 And. The RV of the primary is probably variable.                              
                       Observations seem to confirm suspicion of van den Bos that the B                
                       component is variable.                                                  Baz1972 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       The equinox-1900 position was incorrectly given as 22590+4213 in                
                       McAlister & Hendry (1982).                                              McA1982b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.49 +/- 1.11, 5.85, and 2.00 Msun, respectively.  Mlk2012 
                       The physical nature of star C (mag. about 13, 90") unknown.                     
23028+5718 HJ 1843     STI 2929.                                                                       
23028+4404 STF2973     A variable, LN And.                                                             
23032+1558 BPM2474     [PM2000] 2627151 + [PM2000] 2627137.                                    Gvr2010 
23034+6027 STT 486     A is a spectroscopic binary. B is BD+59@2630.                                   
23035-3445 pi PsA      Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Bopp et al. (1970).                                                     Evn1970 
23036-5618 HJ 5379     B is CPD-56@9990.                                                               
23037+5119 DBR  40     DBR  45.                                                                        
23038+2805 HJ 1842     bet Peg = 53 Peg = Scheat. A is an irregular variable, spectrum                 
                       M2.5II-III.                                                                     
                       AB and AC: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
23039+5123 DBR  44     DBR  54.                                                                        
23039+0056 J  1798     BAL 1247.                                                                       
23040-0233 OSO 188     G028-031. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
23042+5121 DBR  52     DBR  76.                                                                        
23045+5126 DBR  53     DBR  65.                                                                        
23045+5125 DBR  46     DBR  66.                                                                        
23045+3123 ES  396     BRT 293.                                                                Brt1929b
23046-2611 B   587     Measures uncertain, too close. Needs speckle.                                   
23047+2355 POU5775     J 1898.                                                                         
23049+1539 WRH   2     BRT 1363 is probably identical.                                         Hei1983a
23051+5118 HJ 1846     Secondary is about 0.09 mag brighter than primary                       Los2005 
23052+6323 KR   62     The B component is V711 Cep, an Algol-type eclipsing binary with                
                       period 1.30436d.                                                        Zas2011 
23052-0742 A   417     83 Aqr. Alternative spectral type: F2IV+F0V.                                    
                       1977.9134: Rho was incorrectly given as 0".211                          McA1982b
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.62 +/- 0.55, 2.86, and 1.79 Msun, respectively.  Mlk2012 
23054+5825 HJ 1847     Also known as STI2935.                                                          
23054+5453 HJ 3172     STI2934.                                                                        
23054-0911 LDS2965     NLTT 55790/55791                                                        Chm2004 
23060+1323 BPM2475     [PM2000] 2629594 + [PM2000] 2629619.                                    Gvr2010 
23061+6356 LAF  71     Due to the large number of components (exceeding the number of upper-           
                       case letters), a non-standard component designation was necessary,              
                       hence the pairings A,Za; A,Zb; etc. For this pair, as well as LAF  59           
                       and LAF  62, the lower-case designations (such as Za and Zb) do not             
                       refer to components of a close pair.                                            
23064+1235 GIC 188     AB = G029-001/G067-047.                                                         
                       AB: NLTT 55834/55835                                                    Chm2004 
           HDS3291     In addition to the previously known binary companion seen in the                
                       AstraLux images, 2MASS J23062378+1236269 is also a spectroscopic                
                       binary with a semi-major axis smaller than 0.31 au (Shkolnik et al.             
                       2010 ApJ 716, 1522), and has the additional wide companion 2MASS                
                       J23062530+1236570 (also in the sample, a single star in the AstraLux            
                       images) at 37.6" with confirmed proper motion (Lepine & Bongiorno       Lep2007 
                       2007), hence the system is likely quadruple in reality.                 Jnn2012 
23064-2152 HJ 3166     CD-22@16189.                                                                    
23065+4655 STTA242     B is BD+46@3933.                                                                
23067+3302 STF2975     Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
23067-0412 HJ  978     Also known as CHE 435.                                                          
23068+1448 BPM2476     [PM2000] 2630304 + [PM2000] 2630364.                                    Gvr2010 
23069-4331 JC   20     the Gru. Spectrum F5m delta Del.                                                
                       AB: Additional notes may be found in van den Bos (1956).                B__1956a
                       AC: SHY 366. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
23071-2310 LDS5047     NLTT 55857/55860                                                        Chm2004 
23072-5041 DUN 246     B is CD-51@13470.                                                               
                       A comp is possible astrometric pair; however, no SB orbit for A. No             
                       acceleration in original HIP.                                           Tok2014d
23073-3216 PRO 238     B companion is a non-existing star but is scattered light from a                
                       nearby bright star.                                                             
23075+3250 STF2978     H N  11.                                                                MEv2010 
23075+2108 LWR  19     V342 Peg.  Based on the proper motion of A and change in relative               
                       position, Close et al. (2010) conclude B and C are background objects.  Clo2010 
                       AD: Found in SDSS data. Position angle estimated by catalog editor              
                       based on Aladin image.                                                          
           MAR   1     The Ab, Ac, and Ad components are Jovian-mass planets in orbit around           
                       HR 8799. Projected separations are 68, 38, and 24 au; orbital periods           
                       (assuming pole-view circular orbits) are estimated at 460, 190, and             
                       100 years.  Masses are 5-11, 7-13, and 7-13 Mjup, respectively.         Mar2008 
                       The Aa, Ab, Ac, and Ad components all appear to be co-moving.           Vig2012 
23077+4623 HJ 1849     4 And.                                                                          
23077+0636 STF2976     AB: HJL 313.                                                            HJL1986 
23078+6338 HU  994     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 98.34 +/- 19.03, 12.26, and 6.92 Msun, respectively.          Mlk2012 
23078-2042 HJ 3169     Durchmusterung identification not certain.                                      
                       Aka ARA1595.                                                                    
23079+7523 STT 489     pi Cep = 33 Cep. Visual primary (G2 III) is 557d SB1 (#1425 in Batten   Bte1989 
                       n et al.). A spectroscopic orbit was published by Scarfe et al.         Scf1983 
                       AB: Additional notes may be found in Dembowski (1883) and               D__1883 
                       Muller (1950).                                                          Mlr1950b
           pi Cep      Aa,Ab: Astrometric orbit by Gatewood et al. (2001) found by combining   Gat2001b
                       Hipparcos and Multichannel Astrometric Photometer data with the                 
                       spectroscopic elements of Scarfe et al. (1983). The photographic        Scf1983 
                       semimajor axis estimated at 39.0 +/- 3.9 mas. Masses are determined             
                       for all three components of this triple.                                        
                       This object was misidentified as HR 8815 by McAlister (1978).           McA1978c
                       Aa,Ab: Ren & Fu (2013) calculated an astrometric orbit, combining       Ren2013 
                       Hipparcos Intermediate Astrometric Data with spectroscopic elements by          
                       Scarfe et al. (1983).                                                   Scf1983 
23079-5938 NZO 104     Spectral type G0?                                                               
23080+4151 OSO 189     G190-010. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23082+4038 COU1344     TDT3897.                                                                        
23083+0439 GIC 189     G029-006/G029-007.                                                              
23086-6352 B   590     No certain elongation.                                                  B__1951a
23087+0208 5 Psc       Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23088+1058 A  1238     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.89 +/- 1.95, 2.96, and 1.17 Msun, respectively.  Mlk2012 
                       AB: Prieur et al. (2014) derive a dynamical parallax of 9.8 mas and a           
                       total mass of 3.7 +/- 1.7 Msun (based on the original Hipparcos         HIP1997a
                       parallax) or 5.0 +/- 1.9 Msun (based on the revised Hipparcos parallax  VlF2007 
                       of van Leeuwen 2007).                                                   Pru2014 
23091-0233 HIP 114313  SB1 with P = 3.1 yr, estimated q > 0.15. The orbital axis is 31 mas,            
                       too close for NICI. Large acceleration.                                 Tok2012a
23092-0719 STF2980     H N  88.                                                                MEv2010 
23093+4939 HDS3296     1996.5352: Very weak detection, possibly an artifact.                   Msn1999b
23093-8224 HJ 5378     B is CPD-83@745.                                                                
23094+1350 BPM2477     [PM2000] 2632370 + [PM2000] 2632371.                                    Gvr2010 
23094+0701 OSO 190     G028-042. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23095+0841 STF2982     57 Peg. A is an irregular variable, GZ Peg. Spectrum composite;                 
                       M4IIIs+A2V.                                                                     
                       AB: H N  16.                                                            MEv2010 
23096+0045 GAU  20     ZoSe 13964-13965. Proper motion -210 -1270.                                     
                       We do not confirm it using our data and images from the Digitized Sky           
                       Surveys                                                                 Oso2004 
23097+5920 KUI 115     2 Cas.                                                                          
           S   823     AC: H 6  55.                                                            Dam2011 
23099-2057 LDS5052     NLTT 55994/55997                                                        Chm2004 
23099-2227 RST3320     89 Aqr.                                                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 7.05 +/- 2.92, 5.61, and 3.35 Msun, respectively.             Mlk2012 
23100+4758 STF2985     B is BD+47@4058.   AB has a period of ~6300y.                           Tok2006 
                       HJL 314.                                                                HJL1986 
                       AB: B is KZ And, var. of BY Dra type.  B is SB2, P=3.033d               Tok2014d
23100+3651 S   825     STTA243. B is BD+36@5011.                                                       
23100+1426 STF2986     LDS1066.                                                                        
                       A comp is SB1, P=3.632d (Griffin, 2001 Obs 121, 221)                    Tok2014d
23104+4901 STF2987     NLTT 56040/56041                                                        Chm2004 
23104-4515 iot Gru     Hipparcos astrometric solution adopted some elements from the orbit of  HIP1997d
                       Jones (1928).                                                           Jon1928e
                       Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Pourbaix et al. (2004).                                                 Pbx2004 
23105+1502 BPM2478     [PM2000] 2633240 + [PM2000] 2633157.                                    Gvr2010 
23106-0550 LDS2970     NLTT 56037/56038                                                        Chm2004 
23110+6555 AG  290     B is BD+65@1855.                                                                
23111+5304 HD 218915   Aslanov et al. (1984 SvAL 10, 278) discuss the radial velocities and            
                       the possibility of a low-mass companion.  We found a possible binary            
                       companion at a separation of 0".08 which needs confirmation.            Msn1998a
23112+0500 HJ  980BC   Aka BAL2988.                                                                    
23114+3924 MLB1102     ALI 1003.                                                                       
23114+3813 HO  197     Star C (BD +37 4784, mag. 9, 40") may be physical.                              
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 11.98 +/- 6.99, 3.26, and 1.20 Msun, respectively. Mlk2012 
23114-4259 B   594     A premature orbit has been calculated. Needs speckle.                           
                       Likely a spurious pair. Last measured 1963 and unresolved by SOAR on 3          
                       occasions 2008–2012.                                                    Tok201
23116+3654 RUC  26     Multiple system including contact binary AB And. Pribulla & Rucinski            
                       (2006) estimate the mass of the contact pair at 1.656 Msun and the      Pbl2006 
                       minimum mass of the wider component at 0.40 Msun.                               
23118+2651 BUP 234     60 Peg.                                                                         
23121+4517 BU 1528     See star at 23108+4531. Burnham thinks this star more likely to be      Bu_1913 
                       HJ 1853.                                                                        
23121+2656 LEP 113     AC: As noted in Lepine & Bongiorno (2007), 2MASS J23120603+2655579      Lep2007 
                       forms a probable wide (14") pair with HIP 114543, which is itself a 1"          
                       binary. Hence, with the additional component seen in the AstraLux               
                       images, the system is likely quadruple.                                 Jnn2012 
23126+0241 A  2298     Pourbaix gives combined solution for this resolved SB2, yielding        Pbx2000b
                       orbital parallaxes and component masses.                                        
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 3.43 +/- 0.64, 2.39, and 0.95 Msun, respectively.  Mlk2012 
23128+1526 BPM2479     [PM2000] 2635121 + [PM2000] 2635106.                                    Gvr2010 
23128-5240 TOK 682     2MASS has 3 point sources within 10" of A.                              Tok2014d
23129+1233 HJ 3176     BDS 12223, HJ 3177 same star.                                                   
23131+4000 STF2992     Same as STF2994.                                                                
                       AB: HJL 315.                                                            HJL1986 
23133+5710 STT 599     A is variable. Proper motion +2075 +296.                                        
                       B is BD+56@2967. Proper motion of B +009 +006.                                  
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
23134+0241 SCA 144     AB: Eclipsing binary of Algol type, SZ Psc.                                     
           TOK  37     AC has estimated period 50,000y; Evolved primary is 4d eclipsing SB2.           
                       G-solution in Hipparcos. The K1III subgiant primary likely transfers            
                       mass to the MS secondary. Kalimeris et al. (A&A 293, 371, 1995) find            
                       period changes, apparently explained by the mass transfer and magnetic          
                       fields. Any potential tertiary period should be longer than 56y.        Tok2006 
23137+0212 STT 491     ADS notes that the A component (= STT 491 rej) was excluded as single   A__1932a
                       in the 2nd edition of the Pulkova Catalog.                              Stt1878 
23141-0855 STF2993     LDS 802.                                                                        
                       AB: NLTT 56207/56208                                                    Chm2004 
                       B component is 7.1d SB1; period of AB estimated at 18,000y.             Tok2006 
                       B possibly close pair, sep 0.053"?                                      Tok2014d
           S   826     AC and BC: Optical pairs, based on study of relative motion of the              
                       components using the method of apparent motion parameters.              Kiy2008 
23142-1938 LDS5060     NLTT 56210/56211                                                        Chm2004 
23144+2946 ARN  26     AC: C component = primary of 23144+2943 HJ 1858.                                
23144+2943 HJ 1858     Primary = C component of 23144+2946 ARN  26AC.                                  
23146+2555 COU 335     TDT3949.                                                                        
23147-1041 BU  715     The Cincinnati observers in 1877 measured the large star as a close             
                       pair, 1.5deg, :0".32. This was carefully looked for in the 36inch and           
                       there was no trace of any elongation at any time.                       Bu_1894 
23149+4320 MRZ   2     Aka HDS3309.                                                                    
23150-6334 LDS 803     Spectral type K0?                                                               
23151+8327 STF3003     B is BD+82@712.                                                                 
23152+6027 DOO  21     STI 1158. The fainter component is a Wolf-Rayet star.                           
23154+5937 STI9964     Erroneously identified as STI2964. This pair retained.                  Skf2017o
23154+5936 STI2964     Erroneously identified and here corrected.                              Skf2017o
23156+5829 MLR 365     Not the same as the nearby and similar J   860.                         Dam2013 
23156+5756 J   860     Not the same as the nearby and similar MLR 365.                         Dam2013 
23157+0118 CHR 141     Suspected occultation binary.                                                   
                       It has been speculated that the 468d companion is not the speckle       Grf2014d
                       companion. Only measured once.                                                  
23157-1221 LDS2977     NLTT 56270/56279                                                        Chm2004 
23159-0905 STFB 14     91 Aqr = psi 1 Aqr.  LDS 805.                                                   
                       Burnham and Aitken both labelled this pair STFB 12; corrected by Weis   Bu_1906 
                       ("F.G.W. Struve's Double Stars").                                       A__1932 
                       A,BC: NLTT 56282/56278                                                  Chm2004 
           STFB 12     A,BC: H 4  12.                                                          MEv2010 
           BU 1220     AD: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       BC: A pair in motion in a high-inclination orbit.                       Wor1967b
23160-3309 B   596     Spectrum: Fm delta Del.                                                         
23161+4801 ES  694     ES 1186.                                                                        
23162-2823 LDS5062     NLTT 56294/56292                                                        Chm2004 
23162-5947 TOK 217     Tentatively resolved on 2011.85 at 147deg, 0".10, dK=2.5, but not               
                       confirmed here. As the RV is variable, we suppose the pair was                  
                       actually resolved last year but has closed in.                          Tok2013b
23163+1324 BRT1366     Aka ITF  92.                                                                    
23164+6407 BU  992     A premature orbit has been computed.                                            
23164+3739 ES 2537     J 3189.                                                                         
23165+6158 HDS3314     1991.9043: This observation confirms the Hipparcos solution at a                
                       similar epoch (1991.25). An elongated secondary peak yielded an                 
                       inaccurate value for rho, however.                                      Msn1999b
23166-0135 STF2995     LDS 808.                                                                        
23166-0558 OCC 731     BRT 561.                                                                Brt1931 
23167+3441 HDS3315     Cvetkovic et al. (2014) derive spectral types K1 and  K2, masses 0.85           
                       and 0.81 Msun. Dynamical parallax is 10.98 +/- 1.07 mas.                Cve2014 
23167+1937 HDS3316     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 0.78 +/- 0.19, 1.09, and 0.95 Msun, respectively.             Mlk2012 
23167-3635 HDS3317     A single star reported double due to a grid-step error according to             
                       Fabricius.                                                              Fab2000b
23170-6200 EHR  20     Companion appears to be a background star.                              Ehr2010 
23171+3144 OSO 191     G128-043. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
23171-1349 BU  182     Van Biesbroeck (1961) reports a companion with cpm (mag. 17, 15").      VBs1961 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 2.21 +/- 0.99, 1.83, and 1.29 Msun, respectively.  Mlk2012 
           LDS6393     G273-001. AB component not resolved in our data                         Oso2004 
                       HIP 114962. See Allen et al. (2000) for information on metallicity,     AlC2000 
                       age, galactic orbital parameters, etc.                                          
23173-6655 LDS 807     B is CPD-67@3959.                                                               
                       HIP 114980. See Allen et al. (2000) for information on metallicity,     AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       SHY 368. Bayesian analysis by Shaya & Olling (2011) indicates very      Shy2011 
                       high (near 100%) probability pair is physical.                                  
23174+3813 HDS3319     Due to the large proper motion of the secondary, the 1929 measure was           
                       initially ascribed to a supposed AC pair in this system.                        
23176+1818 HU  400     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 5.46 +/- 2.34, 3.74, and 1.45 Msun, respectively.             Mlk2012 
23176-0131 BU   79     HIP 115012. See Allen et al. (2000) for information on metallicity,     AlC2000 
                       age, galactic orbital parameters, etc.                                          
23177+4901 BU  717     8 And.                                                                          
23179-1112 LTT 9469    Hipparcos astrometric solution assuming circular orbit (e = omega = 0)  HIP1997d
23180+4006 MLB 505     ALI1185.                                                                        
23180+3132 OSO 192     G128-045. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23180+0904 OSO 193     G029-020. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
23180-6100 DUN 247     B is CPD-61@6734. B spectral type A5/7V.                                        
                       Statistically the same parallax within the errors would indicate the            
                       components are physical.                                                        
23181+6017 STI1165     B is called BD+59@2698 by Bacchus.                                              
23181-0721 LDS2978     LDS6023.                                                                        
23185+7014 LDS2034     NLTT 56462/56463.                                                               
23185-0916 LDS 810     NLTT 56435/56436.                                                       Chm2004 
23186+6807 STF3001     omi Cep = 34 Cep. A premature orbit has been computed.                          
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       System mass 3.65 +-0.60 Msun. G8III spectral type of primary                    
                       confirmed.                                                              Doc2003d
23186-5818 HJ 5392     B is CPD-58@8063.                                                               
                       Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
23187+1324 HJ 1866     34s f and 1' s of BD+12 4966.                                           Doo1915a
23188+0510 STF2999     AB: H 6  61.                                                            MEv2010 
23189+0524 BU   80     Lewis and Leavenworth measures attributed to CE actually were of a new  L__1902a
                       pair, designated CF.                                                    Lv_1930 
                       AB: The Heintz (1996) orbit predicts a separation of 0.374"; however,   Hei1996c
                       the secondary may have been too faint for the CHARA camera.             Hrt2009 
                       AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 1.44 +/- 0.44, 1.71, and 0.85 Msun, respectively.  Mlk2012 
                       AE: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
23190-0937 HO  199     psi 3 Aqr = 95 Aqr                                                              
23191+4855 ES 2725     B is BD+48@3994.                                                                
23191-1328 MCA  74     94 Aqr. A is a long-period spectroscopic binary now resolved by                 
                       speckle interferometry.                                                         
                       Soderhjelm give triple solution with B (HIP 115125) instead of poor     Sod1999 
                       Hipparcos solution. The primary is overmassive, probably sp. bin.,              
                       cf. analysis of the spectroscopic/interferometric orbit by McAlister            
                       & Hendry (1982)                                                         McA1982c
                       Analysis of this observation by the techniques in use in 1985 was               
                       unable to yield a useable result.                                       Hrt1992b
                       1977.6350: This epoch was incorrectly given as 1977.6359.               McA1982b
                       Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and                  
                       spectroscopic masses 1.55 +/- 0.87, 1.98, and 1.20 Msun, respectively.  Mlk2012 
           STF2998     AB: H 3  34.                                                            MEv2010 
23193+4343 SMA 188     J 2381.                                                                         
23194+7900 LDS2035     AB: Also known as MLR 271.                                                      
23194-0507 HJ 5394     96 Aqr. This cannot be the close 21.24-d spectroscopic binary.          Grf2009b
                       NLTT 56477/56476                                                        Chm2004 
23195+1325 HJ  308     15s f and 1' s of HJ  307.                                              Doo1915a
23195+1326 HJ  309     9s f and 3' s of HJ 307.                                                Doo1915a
23196+0322 SCA 152     We do not confirm it using our data and images from the Digitized Sky           
                       Surveys                                                                 Oso2004 
23197+4823 STTA244     B is BD+47@4111.                                                                
23205+3037 GIC 190     G128-049/G128-050. The A component is Ross 243.                                 
                       NLTT 56545/56551                                                        Chm2004 
23205+1259 LDS5070     NLTT 56546/56548                                                        Chm2004 
23208-5018 RST5560     Spectrum F5m Delta Del.                                                         
23209+3811 ENG  86     12 And.                                                                         
23209+1643 HEI  88     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.93 +/- 0.65, 2.10, and 1.13 Msun, respectively.             Mlk2012 
23210-0148 DAE   7     NLTT 56566 LP 642-48                                                            
                       Daemgen et al. (2007) derive a distance of 22.6 +/- 6.7 pc, separation  Dae2007 
                       of 2.2 +/- 0.7 au, and predicted orbital period of 6 +/- 3 yr.                  
                       Spectral types for both stars are M4.0 +/- 0.5; masses are                      
                       0.25 +0.18/-0.11 and 0.21 +0.17/-0.09 Msun.                                     
                       Although the close binarity of 2MASS J23205766-0147373 was reported in          
                       Daemgen et al (2007) and our AstraLux data have a similar sensitivity,  Dae2007 
                       the star appears single in our images. Since the separation was only            
                       99 mas in 2005, it has presumably moved inward since then.              Jnn2012 
23212+6737 OSO 194     G241-052. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23213+6926 LDS5078     Primary is white dwarf WD 2319+691  = GD 559.                           Far2005b
23215+3730 ES 2540     J 2407, ALI 469.                                                                
23217+0853 HJ 3185     Primary is galaxy NGC 7634.                                                     
23218-1217 HU   95     Combined magnitude from HD. Some visual observers report the pair               
                       to be brighter.                                                                 
23219+3149 BU  718     64 Peg. A is a spectroscopic binary, perhaps as a consequence of                
                       motion in the visual pair.                                                      
23221+6120 B  2907     AC: The very faint companion C may have been a ghost, though it looked          
                       real on all three nights.                                               B__1963b
23224-4636 CPO 637     LDS 812.                                                                        
23226+1706 BPM2480     [PM2000] 2643200 + [PM2000] 2643193.                                    Gvr2010 
23227+6050 STI1171     SMA 189.                                                                        
23227-1502 HU  295     97 Aqr.                                                                         
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 4.54 +/- 0.93, 3.73, and 1.82 Msun, respectively.             Mlk2012 
23228+2208 GIC 191     G068-012/G068-007.                                                              
23228+2034 STF3007     AB: NLTT 56671/56672                                                    Chm2004 
                       AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
23231+1219 HO  300     Removed from WDS as probably not real.                                          
23232+1226 BU 1529     CD: This measure is from the galaxy NGC 7671 near BU 1529 to            Dam2013 
                       BD+11 5002. Redesignated from AC (which was wrong) to CD and X coded.           
                       The measure of AC here is not this CD pairing.                          FyM2013 
23235+4548 STF3010     AB: NLTT 56707/56708                                                    Chm2004 
                       AB: HJL 316.                                                            HJL1986 
23237-1430 HJ 5397     B is BD-15@6411.                                                                
23238-0828 STF3008     An optical pair. A pair was measured by Harvard Observatory near        Pei1882 
                       ADS 16725: 1867.92, 194.4@, 34.09".                                             
                       H N 112.                                                                MEv2010 
23239-1747 TOK 218     dmu is explained by the newly resolved 0".5 pair. Triple, with                  
                       companion at 13".8 in 2MASS. This companion is measured with NICI as            
                       well at the same position, its colors matching a low-mass dwarf.                
                       Considering the low density of background stars, the companion is               
                       physical, although we cannot confirm it as CPM owing to the small PM            
                       of the main target.                                                     Tok2012a
23239-5349 DUN 249     B is CPD-54@10280.                                                              
23241-2146 I  1058     Reality of companion doubtful.                                                  
23244+1429 BU  719     There is an error in the declination in the original catalogue. The             
                       correct place is 231822+1349. HO 301 is identical with this pair.       Bu_1894 
23244-0827 HDO9001     This is the pair described in the STF3008 note recovered.               Dam2010 
23246+4139 CHE 452     There are no obvious errors by Chevalier in applying the offset from    Che1911 
                       his plate center, but there are no pairs at Chevalier’s coordinates,    .     
                       nor coordinates found by reversing the sign of either or both offsets.  Hrt2012b
23246+0617 HJ 3190     13s f and 6' n of BD+05 5165.                                           Doo1915a
23248+6217 H 6  24     AB: H VI 24. 4 Cas.                                                             
                       CD: STI1174.                                                                    
23249+6137 STI1176     According to ADS, Stein also notes a close component (1905.79,          A__1932a
                       91.9deg, 1".2, magnitudes 10.5, 11.3)                                           
23249+4149 CHE 454     AC: A 10' error (23249+4139) in copying declination to catalog led              
                       to assigning a different designation to this companion of CHE 453.              
23256+3326 AG  292     BDS: 11713, AG 282.                                                             
23259+4232 HJ 1877     C component is planetary nebula NGC 7662, "Copeland's Blue Snowball".           
23263+3311 OSO 195     Known companion (= 23263+3311LDS1067)                                   AlC2000 
                       at 4.33'                                                                Oso2004 
           LDS1067     G128-064. See Allen et al. (2000) for information on metallicity,       AlC2000 
                       age, galactic orbital parameters, etc.                                          
                       AB: NLTT 56856/56847                                                    Chm2004 
23263+2752 JNN 139     A very close (~0.15") companion is detected, which is most likely               
                       physically bound, although this has yet to be confirmed with common             
                       proper motion.                                                          Jnn2012 
23263+0527 SCA 158     Aka BAL2991.                                                                    
23265+6038 OSO 196     G217-008. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
23266+5709 LEO  31     STI 2980.                                                                       
23266+4520 GIC 192     The pair HJ 1867 were improperly precessed before, so observers may             
                       have been looking in the wrong patch of sky. Component A of this                
                       optical triple has a very high proper motion. The proper motion of              
                       component B is quite small. The proper motion of component C is                 
                       unknown. At some point during the 20th century, the B and C components          
                       were in approximately the same position, which probably contributed to          
                       the lack of early epoch AC measures. It is possible that some of the            
                       early AB measures may have actually been measures of A,BC. A detailed           
                       analysis of this system is in Bur2003. AB = G216-044/G216-043.                  
                       AB: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
                       AC: NLTT 56881/56879                                                    Chm2004 
23266-5243 EHR  21     omi Gru. Pair appears to be comoving.                                   Ehr2010 
                       WDS designation initially corrupted to 23255-6243.                              
23269+0115 S   830     8 Psc = kap Psc. Spectrum A0pCrSi:Sr:.                                          
                       AB: H 6  62.                                                            MEv2010 
23270-0024 GRV1154     GRV1245.                                                                        
23272-5017 DUN 250     B is CD-50@13978.                                                               
23274+6027 SMA 198     A is an irregular variable.                                                     
23274+5016 OSO 197     G216-045. AF comprise the only common proper motion pair in this                
                       multiple system                                                         Oso2004 
23274+1623 BPMA257     [PM2000] 2647015 + [PM2000] 2647110.                                    Gvr2010 
23274-1736 HJ 3194     Aka ARA 511.                                                                    
23278+0451 DEA  65     NLTT 56936 + 2MASS J23274947+0450583. Primary is VZ Psc. Baron et al.           
                       (2015) estimate spectral types K2+K5 and M9 +/- 0.5, distances                  
                       64 +/-9 and 57 +3/-17 pc, masses 1.46 +/-0.09 and 0.079-0.085 Msun.     BFr2015 
23281-0228 CBL 194     AC: Originally 23281-0227 CBL 194, but secondary found to be primary            
                       of 23281-0228 RST4724. Systems merged, with quadrant flip.                      
23283+0604 H 5  48     H V 48. B is BD+05@5174.                                                        
23284+1432 BPM2481     [PM2000] 2647834 + [PM2000] 2647948.                                    Gvr2010 
23286+1301 BPM2482     [PM2000] 2647997 + [PM2000] 2647988.                                    Gvr2010 
23287+1157 A  1239     CHE, ADS 16834 is identical to A 1239 with a mistake in position.               
23287+0703 CRB  22     BC: Originally listed as separate pair 23288+0703, before its                   
                       affiliation with CBL 549 was noted.                                             
23289+1741 BPM2484     [PM2000] 2648224 + [PM2000] 2648201.                                    Gvr2010 
23289+1720 HJ  311     AC: The C component is n the galaxy NGC 7681.                           Dam2013 
23289+1626 BPM2483     [PM2000] 2648199 + [PM2000] 2648240.                                    Gvr2010 
23294+4128 GIC 193     G190-028/G190-027 =  GJ 4337A+4338B                                             
23297+5457 STI2987     V357 Cas. Primary is Beta Lyr type eclipsing binary, period1.58867d.    Zas2017b
23299-5213 BRT2104     CD-52@10438.                                                                    
23300+5833 STT 496     AC: BDS 12349. A is the Algol-type system AR Cas.                               
           DA    2     CD: Additional notes may be found in Worley (1967).                     Wor1967b
23300-5419 HJ 5401     B is CPD-55@10034.                                                              
23301+3557 J  3197     ALI 238.                                                                        
23304+3050 BU 1266     Triple-lined; both visual components are double-lined spectroscopic             
                       binaries, P = 1.92 and 13.04d resp. Suspected light variation of the            
                       system is unconfirmed.                                                          
           STF3018     Fekel (1986 private communication) reports that he has now detected             
                       four components in the spectrum of this star.                                   
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
23305-2231 ARA2289     AC: Also known as AOT 123.                                                      
23306+1432 BPM2485     [PM2000] 2649501 + [PM2000] 2649488.                                    Gvr2010 
23307+0515 STF3019     H N 137.                                                                MEv2010 
23309+5825 STF3022     AB: H 4  65.                                                            MEv2010 
                       AB: Additional notes may be found in Burnham (1894).                    Bu_1894 
23309+2747 LDS5097     NLTT 57090/57088                                                        Chm2004 
23309-5807 SHY 833     AC: HIP 116056 + HIP 116387.                                                    
23310-6905 HJ 5402     B is CPD-69@3324.                                                               
                       Primary is PMS star, X-ray source.                                      Tok2014d
23311+0841 GIC 194     G029-039/G029-040.                                                              
23313+5225 STT 498     Aa,Ab: The Guillaume 1913 measure is supposed to refer to this object.  Gui1932A
23313+3914 WIS 387     = 14 And = Veritate.                                                            
23315-0405 KO    3     Triple, with wide pair a CPM pair. The primary is an F8 dwarf, the BC           
                       pair (CLO   4BC) comprised of an M8.0V+L3.0V. Data sources: Palomar             
                       Sky Survey red (1951.9), UK Schmidt blue (1982.8), UK Schmidt red               
                       (1988.8), UK Schmidt near-IR (1994.5), 2MASS (1998.8), DENIS I                  
                       (1999.8).  Mean separation of wide pair (1951-1999) 7.530 +/- 0.007             
                       arcmin. Masses of the three components estimated at 1.02 +0.07/-0.06,           
                       0.088 +/- 0.002, and 0.072 +/- 0.001 Msun, respectively                 Cab2007b
23315-2857 B   602     Measures uncertain, too close. Needs speckle.                                   
23317+1956 WIR   1     This is the flare star EQ Peg. Component B is suspected to be the               
                       source of the flares, although both components may be flare stars.              
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       AB: Additional notes may be found in Wilson (1954).                     WRH1954a
23317-0245 LWR  20     AF Psc                                                                          
                       There is a possible companion at 19" noted in Lowrance et al. (2005),   Lwr2005 
                       but it has not been checked for common proper motion.                   Jnn2012 
23319+5401 ES  109     A and B are 1mag below MS in (J,J-K). Parallax <16mas or subdwarfs?     Tok2014d
23320+4349 STF3024     H 2  94.                                                                MEv2010 
                       Primary is V389 And, an Algol type eclipsing binary, P = 25.77827d.     Zas2012 
23322+0705 HU  298     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.47 +/- 0.60, 2.85, and 1.13 Msun, respectively.             Mlk2012 
23323+5111 OL   84     Aka TDT4088.                                                                    
23324-2155 LDS5098     NLTT 57164/57165                                                        Chm2004 
23325+2200 HLM  41     Aka GRV 670.                                                            Dam2010 
23328+2205 ELS   6     Aka DAM 252                                                                     
23328-1645 VOU  28     BC: The 1962 measure by van den Bos may not refer to this pair.         B__1963b
23328-1651 LDS 816     See BC (VOU 28) at 23328-1645                                           Kui1943 
                       A,BC: NLTT 57183/57180                                                  Chm2004 
           SHY 110     AE: HIP 116215 + HIP 116003.                                                    
23331+4556 OSO 198     G216-052. Neither AB nor AD is a common proper motion pair, based on            
                       comparison with POSS2 red plates                                        Oso2004 
23331-2127 HDO 177     BD-22@6147?                                                                     
23332+5724 STT 499     A,BC: HJL 317.                                                          HJL1986 
23333-2055 B  1900     101 Aqr.                                                                        
23334+4251 HDS3356     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.84 +/- 0.20, 1.83, and 1.05 Msun, respectively.             Mlk2012 
23334-1240 LDS2989     NLTT 57205/57204                                                        Chm2004 
23336+6028 STFA 60     AB: Pair appears in an appendix list, not part of the discoverer's              
                       regular numbering sequence.                                                     
23336+3234 OSO 199     G128-077. AB is a common proper motion pair, but AC is not, based on            
                       astrometry and color                                                    Oso2004 
23336+1749 LOS   1     Discovered while observing HO  655. A component is GSC 1723 2167.               
                       Magnitude of B estimated at 11.5.                                               
           HO  655     AC: Optical pair, based on study of relative motion of the components           
                       using the method of apparent motion parameters.                         Kiy2008 
23339-3340 SEE 491     Jessup claims A is double, but gives no data.                           Jsp1964 
23340+3120 BU  720     Variable?                                                               Egg1947 
                       Only elements P and T have been amended by Starikova (1982) from the    Sta1982b
                       orbit of Baize (1976).                                                  Baz1976 
                       Elements published for this long-period system differ: Costa (1966              
                       Urania, Barcelona 51, 73) quotes P = 198.6 yr, while Tel'nyuk-Adamchuk  TkA1966 
                       gives P = 425 yr. The observed theta and rho for 1975.953 are in                
                       reasonable agreement with either uncertain orbit.                       BLM1978 
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
23340+0334 BAL2581     2001 speckle measure actually a new pair, 23344+0331 = WSI 155.         WSI2014 
23341+5947 HJ 1892     KR   65.                                                                        
23342+0218 A  2499     Companion only seen in 1911, and not in 1921, 1933, and 1934.                   
23344+2739 LDS1069     This star has a possible wide companion at about 63" as noted in the            
                       WDS. It is however single in the separation range covered by the                
                       AstraLux data.                                                          Jnn2012 
23344+0331 WSI 155     2001 speckle measure of 23340+0334 = BAL2581 is actually this new pair. WSI2014 
23346-1647 LDS2990     NLTT 57262/57259                                                        Chm2004 
23347+3748 YSC 139     Data at hand suggest that this F8 pair with small magnitude difference          
                       is viewed nearly edge-on. The mass implied by the spectral type is              
                       perhaps 2-2.5 Msun, if the system were to have solar metallicity,               
                       again lower than that implied by the orbital elements. The metallicity          
                       of the system is -0.31 according to the Geneva-Copenhagen Catalog               
                       (Nordstrom et al. 2004), which would tend to lower the mass at a given  Nrd2004 
                       spectral type, thus making the discrepancy worse. Nonetheless, given            
                       the large uncertainty in dynamical mass, it is no worse than a 2 sigma          
                       difference at this point. The mass ratio in the Geneva-Copenhagen               
                       catalog is 0.9, so this at least is consistent with the small                   
                       magnitude difference obtained from speckle measures.                    Hor2015b
                       Orbit determined by fitting revised Hipparcos intermediate astrometric          
                       data. Derived component masses 1.64 +/- 0.29 and 0.90 +/- 0.15 Msun.    Ren2010 
23349+1124 BPM2486     [PM2000] 2652674 + [PM2000] 2652662.                                    Gvr2010 
23350+3302 OSO 200     G128-080. Not a common proper motion pair, based on color and                   
                       comparison with POSS2 red plates.                                       Oso2004 
23350+0136 MEL   9     GJ 900                                                                          
                       Malogolovets et al. (2007) combine all data to derive I-, K-, and       Mlg2007b
                       H-band absolute magnitudes for all three components, as well as                 
                       spectral types and masses:                                                      
                               I  +/-     K  +/-    H   +/-   spec   mass (Msun)                       
                         A:  6.66 0.08  4.84 0.08  5.11 0.08  K5-K7  0.64 - 0.67                       
                         B:  9.15 0.11  6.76 0.20  6.85 0.09  M3-M4  0.28 - 0.34                       
                         C: 10.08 0.26  7.39 0.31  7.54 0.15  M5-M6  0.16 - 0.24                       
                       BC probably form inner short-period (~20y) pair moving with A around            
                       mass center; A,BC period ~80y. Observed configuration may be due to             
                       relative tilts of orbital planes. 2MASS images show faint objects ~12"          
                       northeast and 15" south of primary; stars are probably late M dwarfs            
                       and possibly members of the GJ 900 system.                                      
23351-4237 B   603     iot Phe. A variable of the Alpha CVn-type, spectrum A2VpSrCrEu.                 
           SHY 834     AC: HIP 116389 + HIP 116370.                                                    
23352+1240 BPM2487     [PM2000] 2652884 + [PM2000] 2652864.                                    Gvr2010 
23352-1135 BU   81     Spectrum: Fm Delta Del.                                                         
23352-6441 HJ 5403     B is CPD-65@4149.                                                               
23355+3101 LDS6405     HIP 116421. See Allen et al. (2000) for information on metallicity,     AlC2000 
                       age, galactic orbital parameters, etc.                                          
23355+0850 BRT3372     J 2408.                                                                         
23356+1524 BPM2488     [PM2000] 2653195 + [PM2000] 2653232.                                    Gvr2010 
23356+0823 VIG  22     The B component appears to be a faint background star.                  Vig2012 
23357+3425 ES 2273     ES 2397.                                                                        
23357-2729 SEE 492     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.03 +/- 0.32, 2.10, and 1.07 Msun, respectively.             Mlk2012 
23358+0027 OSO 201     G029-050.                                                                       
23358-5832 RST5174     CD-59@8165.                                                                     
23359+1440 GRV1246     SLW1327.                                                                        
23361-3237 B   604     CM Scl, Algol (EA) type eclipsing binary, P = 10.28857 d.               Zas2011 
23363-0707 BU  721     Elongations real, but too slight for reliable angles.                   B__1959a
23364+0206 THP   1     16 Psc                                                                          
                       SB, period 45d, according to Cayrel de Strobel (1974 A&A 37, 179).              
                       Observed during occultation by asteroid 7 Iris. Separation and                  
                       position angle for 2006.342 constrained to two possibilities, under             
                       assumption asteroid has circular silhouette.                            Thp2006 
23366+5958 OSO 202     G241-060. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
23370+0630 BRT2195     J 1730.                                                                         
23371+3927 A  1492     Closely sf BD+38@5037.                                                          
23373-2056 RSS 580     CPD-21@8282                                                                     
23375+4426 STT 500     A premature orbit has been computed.                                            
23375-4021 WG  289     BRT1133.                                                                Brt1933 
23376+5516 STI3010     SMA 202.                                                                        
23376+4627 STT 600     lam And = 16 And. A is a spectroscopic binary and light variable.               
23376+1236 HJ  315     HJL 318.                                                                HJL1986 
23377+1650 ENG  87     74 Peg. A is a spectroscopic binary.                                            
23377-1304 HJ  316     Aka H N  35 = BDS 12465.                                                Bu_1906 
           BU 1530     CD: This measure is from the galaxy NGC 7723 near BU 1530 to a nearby   Dam2013 
                       star. Redesignated from AC (which was wrong) to CD and X coded.                 
23379+1824 KUI 117     75 Peg. A is a spectroscopic binary.                                            
23382+5514 A  1493     A premature orbit has been computed.                                            
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.23 +/- 2.09, 3.30, and 2.24 Msun, respectively.             Mlk2012 
23386+1124 BPM2489     [PM2000] 2655505 + [PM2000] 2655562.                                    Gvr2010 
23387+1544 BPM2490     [PM2000] 2655551 + [PM2000] 2655564.                                    Gvr2010 
23388+4424 D    26     V392 And, Algol (EA) type eclipsing binary, P = 4.046275 d.             Zas2011 
23388-2816 B   608     Direct motion? Measures uncertain, too close. Needs speckle.                    
23389+2101 LDS5108     NLTT 57506/57507                                                        Chm2004 
23389-0310 BRT 525     Aka J  3354.                                                            Dam2016d
23389-4537 SHY 836     HIP 116602 + HIP 116699.                                                        
23390+3932 MLB 911     ALI 1004.                                                                       
23392-1831 BHA  55     J 1425.                                                                         
23393+7738 NHR   9     = Gam Cep = Errai.                                                              
                       Neuhauser et al. (2007)resolved the wide pair of the gam Cep triple             
                       system using the Subaru AO system. Their combined solution yielded              
                       masses for Aa and B of 1.40 +/- 0.12 and 0.409 +/- 0.018 Msun, plus a           
                       mass function for the planetary companion (M_Ab sin i) of 1.60 +/-              
                       0.13 Mjup. Physical separation for the AB pair is 20.18 +/- 0.66 au.    Nhr2007 
23393+4543 CHR 149     1986.8914: This "prediscovery" confirmation was found by reexamination          
                       of archival data.                                                       McA1990 
                       Balega et al. (2004) notes that it is the B component of A   643, not   Bag2004 
                       the A component, which is comprised of the CHR 149 pair. The component          
                       designation has been changed from Aa,Ab to Ba,Bb accordingly.                   
                       Zhuchkov et al. (2008) give combined spectroscopic/astrometric orbits   Zhu2008 
                       for both wide and close pair.  Spectral types for A, Ba, and Bb are             
                       determined as G0III, F3III, and sdO-BVIII, respectively.  Magnitudes            
                       (assuming an integrated system magnitude of 7.63) are 8.53 +/- 0.03,            
                       8.66 +/- 0.04, and 9.51 +/- 0.05, while indiviual masses are estimated          
                       at 1.3 +/- 0.3, 1.3 +/- 0.3, and 0.7 +/- 0.4 Msun.                              
23395+6658 HJ 1897     Proper motion from Greenwich possibly reversed.                                 
23395-4638 DUN 251     the Phe                                                                         
23397+1153 BPM2491     [PM2000] 2656281 + [PM2000] 2656234.                                    Gvr2010 
23397+0331 BAL2069     HJL 319.                                                                HJL1986 
23398-0420 HWE  99     B is BD-05@6031.                                                                
23399+6419 ES  149     AB: HJL 320.                                                            HJL1986 
23399+5517 STI3015     SMA 203.                                                                        
23399+0538 BUP 240     iot Psc = 17 Psc.                                                               
23400+5446 STI3016     Also known as SMA 204.                                                          
23404+4420 HJ 1898     kap And = 19 And.                                                               
           CSN   1     Aa,Ab: Carson et al. (2012) discovered a "super Jupiter" orbiting kap           
                       And. Spectral types are B9IV and L2-L8, masses 2.4-2.5 Msun and 12.8            
                       +2.0/-1.0 Mjup, assuming a system age 30 +20/-10 Myr (Marois et al.             
                       2010 Nature 468, 1080).                                                 Csn2013 
                       Aa,Ab: Hinkley et al. (2013) derive a spectral type L1 +/- 1, Teff =            
                       2040 +/- 60K, mass 50 +16/-13 Mjup, and age 220 +/- 100 Myr for the Ab          
                       companion of the B9IV star kap And. The primary has a mass of 2.8               
                       +0.1/-0.2 Msun, Teff 11361 +/- 66K, radius 2.29 +/- 0.06 Rsun, age              
                       the same as that of Ab. Results are based on spectroscopy obtained              
                       using a high-contrast imaging platform. They also conclude that the B           
                       and C stars in this system are not comoving with the A component.       Hnk2013 
                       Aa,Ab: Bonnefoy et al. (2014) derive spectral types B9IVn and M9-L3:,           
                       plus log luminosities 1.83 +/- 0.04and -3.76 +/- 0.06. The mass of the          
                       primary is estimated at 2.6 +/- 0.2 Msun; the secondary is 0.013                
                       +0.022/-0.001 Msun for a "hot-start" evolutionary model, >0.011 Msun            
                       for a "warm-start" model.                                               Bnf2014 
23406+5513 HJ 1899     BDS 12513, HJ 1901 same star.                                                   
23407-0023 STF3030     H N  91.                                                                MEv2010 
23409+2022 HO  303     Hough notes that STT 503 follows 1m13s and 3' S.                        Ho_1890 
                       AC: The C component measured by Burnham may be one of two stars in the  Bu_1913 
                       field. However, neither is in very good agreement with his measure,             
                       even after accounting for changes due to proper motion.                         
23411+4613 MLR   4     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.16 +/- 0.28, 2.61, and 1.13 Msun, respectively.             Mlk2012 
23412+1647 GRV 683     HJL 322.                                                                HJL1986 
23412+0616 STF3031     B is BD+05@5208.                                                                
                       HJL 321.                                                                HJL1986 
                       H N 136.                                                                MEv2010 
23413+4954 ES 2732     Also known as ES 2731.                                                          
23414+5925 OSO 203     G241-064. None is a common proper motion pair, based on comparison              
                       with POSS2 red plates.                                                  Oso2004 
23414-3205 LDS2992     NLTT 57627/57628                                                        Chm2004 
23418-1749 HJ 5413     104 Aqr. A spectroscopic binary. B is BD-18@6359.                               
23419-0559 LDS5112     NLTT 57682/57675                                                        Chm2004 
                       AB: Primary is exoplanet host, P=572d. A=SB?                            Tok2014d
           GC 32912    A: Combined solution, based on reduction of Hipparcos intermediate              
                       astrometric data together with spectroscopic elements from Vogt et al.  CPS2000c
                       (2000).                                                                 HaI2001 
23424+4956 HJ 1903     Herschel's 1828 measure than with Espin's in 1912.                      Es_1914 
23424-1357 LDS2995     NLTT 57711/57710                                                        Chm2004 
23427-1433 BU  279     ome 2 Aqr = 105 Aqr. A is a spectroscopic binary.                               
23430-2407 LDS 823     Proper motion +1270 -2200.                                                      
                       NLTT 57749/57756                                                        Chm2004 
23431+1150 A  1242     A premature orbit has been computed.                                    Baz1944a
23432+5455 ES 1048     DE: Also known as STI3022.                                                      
23432-0837 FOX 276     J 1426.                                                                         
23433-7049 HJ 5415     Optical pair, based on study of relative motion of the components               
                       using the method of apparent motion parameters.                         Kiy2008 
23434+0532 J   299     Jonckheere unable to recover.                                           J__1962a
23438-1517 HEG   2     R Aqr. Binary system consists of a Mira and a white dwarf companion,            
                       estimated P=44yr (Willson, L.A., Garnavich, P., & Mattei, J.A. 1981             
                       IBVS 1961, 1). Hollis et al. (1997) give preliminary orbital elements   HJM1997 
                       for the AB pair: P=44y, e=0.8, T=JD2442100.0, i=70deg, Omega~90deg,             
                       omega = +/-90dega = 2.54e14cm for system mass 2.5 Msun, 2.69e14cm for           
                       3.0Msun.                                                                        
23439+3232 LDS1070     Listed as double in ApJ 112, 214. L 1512-34a.                                   
                       AB: Secondary is white dwarf WD 2341+322.                               Far2005b
23440+2922 AGC  14     78 Peg.                                                                         
23441+6147 STI1204     A is a semiregular variable, PZ Cas. B is a Cepheid.                            
                       Also known as MLR 515.                                                          
23442+4923 LDS5116     NLTT 57825/57826                                                        Chm2004 
23445+4623 STF3034     Primary is V395 And, eclipsing binary of W UMa -type, period 0.6847 d.  Zas2012 
23448+5627 BAR  64     BC: STI3024                                                                     
23449+4831 ES  549     AB: Later measures were incorrectly added as the new pair ABH 179AD,            
                       due to the high proper motion of the primary and the long timespan              
                       between observations.                                                           
23449+1543 BPM2492     [PM2000] 2660049 + [PM2000] 2660092.                                    Gvr2010 
23450+3020 OSO 204     G130-007. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23451+1459 JNN 140     G 68-39.                                                                        
                       Due to the compact configuration of the three components resolved by            
                       AstraLux, this is almost certainly a physically bound triple system.            
                       Only one epoch of images exist so far, hence common proper motion has           
                       not yet been demonstrated.                                              Jnn2012 
23454+1547 BPM2493     [PM2000] 2660398 + [PM2000] 2660323.                                    Gvr2010 
23456+1309 HJL1116     A combined interferometric/spectroscopic solution by Halbwachs et al.           
                       (2016) yields masses 1.686 +/- 0.021 and 1.390 +/- 0.034 Msun.          HJL2016 
23459+1941 GRV 691     HJL 323.                                                                HJL1986 
23460+4625 MCA  75     psi And = 20 And. R.H. Wilson reported a wide, faint companion.         WRH1950a
                       H. McAlister resolved the primary into a triple system.                 McA1978b
                       Aac: It is not established whether this third component belongs to Aa           
                       or Ab.                                                                          
                       Based on mean motion of Aa,Ac a period of ~300 years is postulated.     Tok2010b
                       Based on the separation of Aa,Ab relative to this dynamic stability             
                       is questioned, however Aa,Ab has only been measured four times while            
                       Aa,Ac has been measured 39. Is Aa,Ab of a larger delta-m and if not             
                       why is it so infrequently measured. Could it be spurious?                       
23460-1841 H 2  24     H II 24. 107 Aqr = i 2 Aqr. Alternative spectrum: F2III+F2V.                    
23461+6028 STF3037     E is BD+59@2769a.                                                               
23461+5040 STTA248     B is BD+49@4216.                                                                
23462+6240 STF3038     The John Herschel measure identified with this pair may go with         HJ_1831 
                       23463+6201STI1209 which it fits a little better. The measure is "T"             
                       coded with both systems.                                                        
23462+3515 OSO 205     G130-010. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23463+6201 STI1209     The John Herschel measure identified with this pair may go with         HJ_1831 
                       23462+6240STF3038, which Herschel identified the measure with. It               
                       fits better here.                                                               
23464+1324 BPM2495     [PM2000] 2661188 + [PM2000] 2661265.                                    Gvr2010 
23464+1243 BPM2494     [PM2000] 2661128 + [PM2000] 2661130.                                    Gvr2010 
23464-2302 TOK 375     First resolution at 0".15; estimated period 12 y.                       Tok2013b
23465+1724 BPM2496     [PM2000] 2661247 + [PM2000] 2661243.                                    Gvr2010 
23465-7159 HJ 5419     B is CPD-72@2782.                                                               
23466-0900 TOK 220     Resolved on 2011.85 and found here at nearly the same position,                 
                       despite estimated period of 20yr. Seen in projection?                   Tok2013b
23467+6236 VBS  40     STI 1212.                                                                       
23469+2825 STF3039     AB: H 4 107.                                                            MEv2010 
23471-1921 DON1053     BHA 56.                                                                         
23472-2624 LDS5121     NLTT 57957/57958                                                        Chm2004 
23474-2217 I   696     CD-22@16450.                                                                    
23475+2535 BU  727     In my Tenth Catalogue where this pair originally appeared, the printed          
                       distance should be multiplied by two.                                   Bu_1894 
23476+4650 BU  995     A is a spectroscopic binary. One component is variable.                         
23479+1703 STF3041     STTA249.                                                                        
23479+0624 GIC 195     G030-015/G029-067. The B component is variable star DO Psc.                     
23479-0246 S   835     20 Psc.                                                                         
23484-2141 ARA1950     Possibly = HDO 179, suspected binary of Win1882.                                
23485+2539 DSG   8     For the Horch et al. (2015) combined solution, spectroscopic elements           
                       are fixed to those of Griffin (2007). Assigned spectral types are       Grf2007 
                       F5V and F5.5V; derived masses 1.40 and 1.37 Msun.                       Hor2015 
23487+6453 STT 507     STTA250.                                                                        
23488+6213 STT 508     6 Cas. The variable V566 Cas.                                                   
                       Aitken notes that Guillaume gives his 1923 measure without              Gui1932A
                       identification and that the other Guillaume measure goes with           A__1932a
                       STT 508AC. The pair was assigned the designation GUI 39, but nothing            
                       matching his separation and angle can be found in the vicinity of STT           
                       508. The GUI 39 designation has therefore been removed, under the               
                       assumption that Guillaume's measure was of STT 508 but there was some           
                       typographical error in his original reference. This assumption is               
                       supported by the fact that his angle of 19.5 could instead be 195, in           
                       good agreement with contemporaneous measures of the Struve AB pair, as          
                       well as the match of his wider pair with the Struve AC pair.                    
23489-2509 SHY 839     HIP 117454 + HIP 117720.                                                        
23489-2808 BU 1013     del Scl                                                                         
23492+0459 TOK 376     First resolution at 0".20, dK=3.2.                                      Tok2013b
23496+6052 STI1222     B is BD+60@2625a.                                                               
23496-2212 B   619     CD-22@16466.                                                                    
23498+2741 A   424     Only elements P, T, and a have been amended from the orbit of           Sta1978c
                       Morel (1969).                                                           Mrl1969c
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 7.21 +/- 3.53, 5.19, and 1.40 Msun, respectively.             Mlk2012 
23500+4829 OSO 206     G171-023. Not a common proper motion pair, based on comparison with             
                       POSS2 red plates.                                                       Oso2004 
23500+0843 OSO 207     G029-071. Not a common proper motion pair                               Oso2004 
23505+0807 CHE 505     Chevalier gave an incorrect Durchmusterung number for this pair,        Che1910 
                       leading to incorrect coordinates being added to the WDS.                Hrt2012b
23506+5412 SHY 840     AC: HIP 117573 + HIP 117733.                                                    
23506+4705 A   793     Often too close. Possible quadrant reversal about 1925.                         
23506-5142 SLR  14     High but rather imprecise mass-sum.                                     Sod1999 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.28 +/- 0.37, 1.92, and 0.95 Msun, respectively.             Mlk2012 
23509+4730 A   794     A is the semiregular variable TZ And.                                           
23509-7954 UC 5034     CPM candidate confirmed physical by photometry (2MASS and V mags).      Tok2013c
                       Primary is SB2                                                          Tok2014d
23511+0214 HIP 117607  Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos    Ren2013 
                       Intermediate Astrometric Data with spectroscopic elements by                    
                       Udry et al. (1998).                                                     Udr1998 
23512+5123 ALD   7     Not found by Heintz at IDS position.                                    Hei1990b
23513+1757 J   627     Aka COU  72.                                                            Dam2010 
23514+2344 BWL  61     AE:  Source appears spatially extended; probably a background galaxy.           
                       Primary is G 68-46.                                                     Bwl2015 
23515+2501 POU5863     J  1799.                                                                        
23516+3844 ES 2541     ALI1006.                                                                        
23516+3127 BWL   1     AB: Bowler et al. (2012) determined this pair shares CPM. At a          Bwl2012a
                       photometric distance of 50 +/- 10 pc, the projected separation is 119           
                       +/- 24 au. Spectral types are M2.0 +/- 0.5 and L0 +2/-1, masses 0.45            
                       +/- 0.05 Msun and 32 +/- 6 Mjup. Additional JHK photometry of both              
                       components was derived via synthetic photometry from spectrum                   
                       (calibrated to 2MASS), combined with NIRC2 differential photometry.     TMA2003 
                       AB: A comp is active M2.0 star. B is L0-L3, mass 32 +/- 3 Mjup.         Bwl2015 
23516+2502 POU5865     J  1800. Same as POU5866.                                                       
23516+0841 CHE 506     Chevalier gave an incorrect Durchmusterung number for this pair,        Che1910 
                       leading to incorrect coordinates being added to the WDS.                Hrt2012b
23518+1614 BPM2497     [PM2000] 2665067 + [PM2000] 2665069.                                    Gvr2010 
23518-0637 A  2700     Masses and bolometric magnitudes are derived for the two components             
                       of this system by Mason et al. (1999), based on assumed spectral types  Msn1999a
                       and available parallaxes.                                                       
                       See Baize & Petit (1989) catalog of doubles with variable component.    Baz1989d
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 1.82 +/- 0.51, 1.91, and 1.17 Msun, respectively.             Mlk2012 
23521+5845 ES 1804     Spectrum is variable G2-K.                                                      
23522+6427 MLB 236     Aka STI1226.                                                                    
23524+7533 BU  996     A is a spectroscopic binary.                                                    
23525-0924 OSO 208     G273-152. Common proper motion pair.                                    Oso2004 
23527+6042 BU 1153     D component is primary of 23531+6042 STT 511.                                   
23527-0328 LDS3001     NLTT 58251/58250                                                        Chm2004 
23528+5548 HJ 1914     STI3050.                                                                        
23529-0309 FIN 359     24 Psc.                                                                         
                       Mason et al. (1997) orbit includes mass determination.                  Msn1997a
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.87 +/- 0.56, 2.69, and 2.75 Msun, respectively.             Mlk2012 
23530+4121 ARG 108     B is BD+40@5169.                                                                
23530+1155 STF3044     A purported FYM 5AC pair has been removed on request of the author.     FyM2014b
23532-0830 LDS3003     NLTT 58273/58274                                                        Chm2004 
23536+5131 STTA251     AB: Pair appears in an appendix list, not part of the discoverer's              
                       regular numbering sequence.                                                     
23537-0140 HJ 3223     B is BD-02@6055.                                                                
23537-4926 I  1476     Measures uncertain, too close.                                                  
23537-6557 HJ 5428     Pair bound. Near-IR colors indicate B component has a K9.5-M2.5                 
                       spectral type and a mass of 0.53 +/- 0.01 Msun.                         Egn2007 
           SHY 108     AC: HIP 117815 + HIP 114996. C component is gam Tuc.                            
23538-3729 LDS 825     LDS6407.                                                                        
23541+3917 HO  205     V413 And. Primary is eclipsing binary of Algol type, period 53.1d.      Zas2017b
23541-3317 LDS 826     AB: Primary is white dwarf WD 2351-335.                                 Far2005b
           SOZ   2     AC: CPM companion to red dwarf / white dwarf pair LHS 4039 / 4040 is            
                       an M8.5 dwarf; estimated distance 19.5 pc.                              Soz2004 
23542+3739 OL    7     ES 2004.                                                                        
23544-2703 LAL 192     phi Scl, a spectroscopic binary. Originally known as DUN 253 in         Dun1829 
                       Dunlop's original list and the ADS, the discovery designation of this   A__1932a
                       was changed at Lick for an unknown reason.                              IDS1963 
23545+2938 LEP 115     NI   50.                                                                        
23549+2929 STTA252     B is BD+28@4667.                                                                
23553+5144 ES 2735     AC: Measures in 1911 by Espin, and in 1919 by Olivier, disagree, as     Es_1912 
                       noted by Aitken. The Olivier measure was later assigned to              Ol_1920a
                       23562+5138 ALD 123.                                                     A__1932a
23554-5845 HJ 5432     B is CPD-59@7939.                                                               
23555+1755 BFR  14     TYC 1725 00344 1 + 2MASS J2355345 +175404. Baron et al. (2015)                  
                       estimate spectral types G5III and M9.0 +/- 0.5, distances 40 +28/-15            
                       and 103 +10/-37 pc, masses 1.91 +/-0.11 and 0.079-0.085 Msun.           BFr2015 
23555-7749 JSP 854     aka TDT4274.                                                            Dam2016f
23556+0042 LEP 116     NI   51.                                                                        
23558+1718 BPM2498     [PM2000] 2667910 + [PM2000] 2667843.                                    Gvr2010 
23561+2520 A   426     Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 2.14 +/- 1.55, 2.44, and 1.05 Msun, respectively.             Mlk2012 
23562+5946 OSO 209     G217-024. Neither is a common proper motion pair, based on comparison           
                       with POSS2 red plates.                                                  Oso2004 
           LEP 117     AD: CPM pair. D component is white dwarf candidate.                     Tok2014d
23564-0930 STF3046     AB: NLTT 58475/58476                                                    Chm2004 
23565-0035 HJ  994     Aka WEI  44.                                                                    
23566+1855 BRT2518     Aka J  3355.                                                            Dam2016d
23566-5018 TOK 377     First resolution; estimated period 75 yr.                               Tok2013b
23568+0444 A  2100     This system has a Delta m of 0.9 +/- 0.4 in the blue, as determined             
                       from lunar occultation measures by Africano (1975).                     Afr1975 
                       Malkov et al. (2012) derive dynamical, photometric, and spectroscopic           
                       masses of 3.41 +/- 0.66, 3.38, and 1.45 Msun, respectively.             Mlk2012 
23568-4304 CPO 101     LDS 829.                                                                        
23570+2305 GIC 196     G129-045/G129-046.                                                              
23570-2836 LDS2065     NLTT 58501/58508                                                        Chm2004 
23572-1631 LDS 831     NLTT 58517/58518                                                        Chm2004 
23573+6102 STT 512     CD: Also recorded as D 28, BDS 12659 and TDS1229.                               
23573-1259 LDS 830     NLTT 58528/58527                                                        Chm2004 
23575+1131 BPMA258     [PM2000] 2669134 + [PM2000] 2669021.                                    Gvr2010 
23576-6418 EHR  22     Primary is eta Tuc.                                                     Ehr2010 
                       Ba,Bb: Physical/optical nature unknown.                                         
23578+2508 MCA  76     psi Peg = 84 Peg                                                                
23579+1557 RUC  16     U Peg. Spectral type of resolved companion later than M5V.              Ruc2007 
23579-1700 LDS5143     NLTT 58570/58571                                                        Chm2004 
23581+6112 LEO  55     Both components are Cepheid variables, CE and CF Cas.                           
23581+2840 HJ  995     Decided change; probably the measures of HO in 1893 belong to this.     Doo1915a
23581+2420 STF3048     AB: NLTT 58582/58579                                                    Chm2004 
                       AB: HJL 324.                                                            HJL1986 
           GIC 197     DE: NLTT 58602/58601                                                    Chm2004 
23582-1725 DAE   8     NLTT 58589 = LP 746-40                                                          
                       Daemgen et al. (2007) derive a distance of 26.1 +/- 2.0 pc, separation  Dae2007 
                       of 49.7 +/- 3.8 au, and predicted orbital period of 477+/- 58 yr.               
                       Spectral types are M2.0 +/- 0.5 and M2.0 +/- 0.5; masses for both are           
                       0.45 +/- 0.05 Msun.                                                             
23582-2756 HJ 3228     LDS2067.                                                                        
23582-5712 GC 33239    Hipparcos astrometric solution assumes circular orbit (e = omega = 0).  HIP1997d
23584+5123 ES   37     R Cas                                                                           
23581+2420 GIC 197     DE: NLTT 58602/58601                                                    Chm2004 
23586-1408 RST4136     AB: Malkov et al. (2012) derive dynamical, photometric, and                     
                       spectroscopic masses 4.86 +/- 1.99, 3.15, and 1.35 Msun, respectively.  Mlk2012 
23587-0333 BU  730     27 Psc                                                                          
23588+3345 RAO 77      Triple system. The inner SB has P = 25.4 days (Latham et al. 2002),    Lat2002  
                       the Robo-AO companion at 5" is seen at a constant position despite     .        
                       PM(A) = 0".3/y, while its color places it on the MS.                   Rbr2015d 
23588+3156 RAO  76     A is SB and astrometric binary.                                         Tok2014d
                       Previously thought to be a binary, but our observations reveal that    .        
                       it is actually a triple system. The outer component B at 4".8 was      .        
                       discovered by Robo-AO and confirmed by the 2MASS image and by the new  .        
                       data presented here. It is located near the low end of the MS. The     .        
                       main star with astrometric acceleration (Makarov & Kaplan 2005) is     Mkr2005  
                       now resolved at 0".4, corresponding to an orbital period of ~100 yr.   .        
                       The new component Ab is too faint for its detection in the i' band     .        
                       with Robo-AO.                                                          Rbr2015d 
           RBR  31     Aa,Ab: incorrectly labelled RBR 30 in Table 1 of Roberts et al.        Rbr2015d 
23590+5545 STF3049     AB: sig Cas = 8 Cas                                                             
                       AB: H 1   5.                                                            MEv2010 
23592+4112 HO  207     Aka COU 1500.                                                                   
           HJL1113     AC: SHY 376. Bayesian analysis by Shaya & Olling (2011) indicates very  Shy2011 
                       high (near 100%) probability pair is physical.                                  
23595+3343 STF3050     AB: H N  58.                                                            MEv2010 
                       AB: Additional notes may be found in Couteau (1952).                    Cou1952a
23597-3500 B  2511     BC: WSP   8.                                                                    
23598+1744 BPM2499     [PM2000] 2670806 + [PM2000] 2670809.                                    Gvr2010