00000-1930 LTT 9831 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d00002+0146 WEI 45 HWE 64 is certainly identical with Weisse 45 = ADS 17156. Howe misread the sign of the declination. This was already stated in Cin. Pub v 6, nos 748 and 749, and the mean of the two measures is given in the mean results, assigned to Weisse 45. Nevertheless the pair was given separately in the BDS and 12692 and taken over as ADS 17168. ADS 17156 is misidentified. It is BD+00 5079 (9.1), 9.5, G0, with the position for 1900 (1950) as 23 55.1 (57.6) +01 13 (30). B__1950c00003+1642 HJ 318 A component is PPM 116047. In Tycho catalog magnitude of A is 9.46; in Guide Star Catalogue B is GSC 1178 1031 with magnitude 12.77. Spectral types are K for A component, G5-K0 for B component. Annual proper motion for B: AR= -0.013" and DEC=-0.0005" FMR1999c00006-5238 FIN 294 Spectrum: K1/2III+A/F.00008+0630 GWP 2 XMI 101. Tob2012b00011+6935 STTA253 B is BD+68@1417.00011-2326 LDS2070 B is CD-24@17944.00012-0005 TOK 359 Long-period SB. Tok2013b00012-0312 LDS9082 Old LDS6082.00013+6021 STTA254 A is the semiregular variable WZ Cas.00013+0742 DU 4 HJL 325. HJL198600013-7012 GLI 290 B is CPD-70@3035.00014+3937 HLD 60 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.67 +/- 0.29, 1.79, and 1.65 Msun, respectively. Mlk201200016+6437 MLR 79 Misidentified by Muller as BD +63@2093.00016+3714 ES 2444 Aka ALI 472.00018-0322 LDS9083 Old LDS6083.00018-2548 B 630 Measures uncertain, too close. G266-029. Not resolved in our images Oso2004 HIP 146. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc.00019-0952 LDS5157 NLTT 58812/58813 Chm200400020+4530 J 864 BRT 1164. -22s and +2.4' from BD+44 4541. J__1955 AC: CPM pair. J__195500022+5958 BU 1337 STI 1256.00022+2705 BU 733 85 Peg. Spectral types and masses of primary and secondary assigned by ten Brummelaar et al., based on adaptive optics observations. TtB2000 AB: Additional notes may be found in Baize (1945). Baz1945b AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 1.49 +/- 0.81, 1.58, and 1.56 Msun, respectively. Mlk2012 Soderhjelm notes poor Hipparcos solution. Sod1999 A third star has been detected by infrared speckle interferometry. Mcy1983 HIP 171. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. AC and AD: Optical pairs, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 AC and AD: Additional notes may be found in Burnham (1894). Bu_1894 AD: Rectilinear solution by Friedman et al. (2011). USN2011a00023+1609 BPM 1 [PM2000] 1692 + [PM2000] 1685. Gvr201000023+0732 LDS9084 Old LDS6084.00023-2943 B 631 zet Scl. The companion is very faint and not accurately measured. A is a spectroscopic binary.00024+1429 GWP 4 XMI 102. Tob2012b00024+1047 BGH 1 AB,C: HJL 326. HJL1986 AB,C: SHY 377. Bayesian analysis by Shaya & Olling (2011) indicates Shy2011 very high (near 100%) probability pair is physical.00025-0826 LDS5255 NLTT 2/3 Chm200400026+6606 STF3053 B is BD+65@1988.00026+1841 SHY 378 AB: HIP 201 + HIP 206.00028+1647 BPM 2 [PM2000] 2010 + [PM2000] 1993. Gvr201000028+0208 HJ 998 AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 AC: Rectilinear solution by Friedman et al. (2012). USN2012a00031+0816 STF3054 B component is eclipsing binary of Algol-type, period 2.2604 d. Zas201200032+4508 HJ 1927 Unless the separation has decreased greatly, the measures given in the ADS would seme to refer to the nearby pair ADS 108. B__1963b00032+3315 ES 2400 Pair long unconfirmed due to 1m error in published epoch-1900 coordinates (thanks to Rafael Caballero, private communication)00034+1839 GWP 6 XMI 103. Tob2012b00034-2430 LDS2076 NLTT 53/54 Chm200400037+1851 GWP 7 XMI 104. Tob2012b00037+1134 BPM 3 [PM2000] 2710 + [PM2000] 2680. Gvr201000037-2824 CRZ 1 BDK 1. G 266-33 + 2MASS J00034227-2822410. Distance 39.5 +1.8/-1.6 pc for primary, 26 +/- 3 pc for secondary. Estimated age of system 0.9-1.4 Gyr. Mass of secondary estimated at 0.100-0.103 Msun. Fah201000038-1317 XMI 1 Rectilinear solution by Hurowitz et al. (2013). USN2013a00042+6217 H 5 79 9 Cas.00042-1008 LDS3116 NLTT 86/84 Chm200400044+5804 OSO 1 G217-030. No common proper motion pairs, based on comparison with POSS2 red plates Oso200400045+0045 GWP 10 XMI 106. Tob2012b00045+1851 GWP 9 XMI 105. Tob2012b00046+4206 CHR 122 B is a spectroscopic binary. Hence the system is quadruple.00046-4044 GKI 2 Ba,Bb. GJ 1001BC = LHS 102BC. Spectral types L4.5 and L4.5 Red2006b00047+3416 STF3056 AB is an orbit pair, and D is an unresolved spectroscopic pair (P=68d) Tok2019b so this is a 2+2 hierarchical multiple. C is optical.00049+5832 STF3057 Called a two-spectrum SB in the Bright Star Catalog Supplement. H 1 39. MEv201000049-1320 GAL 295 Object #1 in Gallo's original list. Gal1912a00050+0835 GWP 11 XMI 107. Tob2012b00051+6323 HJ 1933 STI 1265.00052+4514 ES 9001 Previously known as ES 1293a. BU 9001 Previously known as BU 997a.00053-0542 33 Psc Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Harper (1926). Hrp192600054+1620 STTA255 B is BD+15@4934.00054-2559 LDS3119 NLTT 158/159 Chm200400055+3406 HU 1201 A possible close approach about 1980. AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 1.09 +/- 0.63, 2.52, and 1.10 Msun, respectively. Mlk201200056-0141 LDS3012 NLTT 176/175 Chm200400057+4549 STT 547 Premature orbits have been computed. Motion direct. Both A and B have variable RV (ranges 45 and 25 km/s, respectively). Another star (9.9, 330") has common proper motion. AB: Bolometric corrections and component masses determined from M-L relation. A family of possible orbits were determined by Kiyaeva Kiy2001 (2001) for the F component relative to AB pair (Note: only the shortest-period solution is presented in orbit catalog.) AB: NLTT 172/173 Chm2004 AD and AE: Optical pairs, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 AF: HIP 473 + HIP 428. AC and AD: Rectilinear solution by Pavlovic et al. (2013). Pal201300057+4549 POP 217 AP: Rectilinear solution by Cvetkovic (2011). Cve2011d00057+0626 BFR 1 NLTT 182 + 2MASS J00054171+0626300. Baron et al. (2015) estimate spectral types M4.5 +/- 0.5 and L0 +/- 1, distances 62 +38/-23 and 69 +5/-22 pc, masses 0.157-0.181 and 0.079-0.085 Msun. BFr201500059+1805 STF3060 AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 Aka J 3330. HD 108 Hutchings (1975 ApJ 200, 122) presented a preliminary orbit with a period of 4.6d, but subsequent work has cast doubt on the reality of the orbit (Underhill 1994 ApJ 420, 869). Msn1998a LEP 1 AD: HJL1001. HJL1986 AD: SHY 112. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical. AD: the visual binary at 573" is co-moving, same parallax. The D component is ~1.3m below the main sequence in the (K, V-K) color- magnitude diagram. Tok2012a00063+5826 STF3062 One component, designated V640 Cas, is variable, probably due to partial eclipses. P = 1.08 d. See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Secondary is SB, P=47.685d Tok2014d00063-4905 HDO 180 A is a spectroscopic binary. Primary is planet host star, P=339d. B comp is LHS 1021. Pair bound. Photometry suggests companion K8.5-M1.5 with mass 0.59 +/- 0.02 Msun. Egn200700064+4501 UC 320 Aka BVD 170. Skf201300066+2901 STT 549 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 ENG 1 A,CD: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 LAF 1 CHARA Array Limb-darkened diameter of A : CIA2013c R = 0.9172 +/- 0.0090 \rsun, L = 0.6078 +/-0.0090 \lsun, Teff = 5327 +/- 39 K, M = 0.889 \msun, Age = 9.6 Gyr. BU 1338 CD: J 866.00066+1554 GWP 12 XMI 108. Tob2012b Aka GRV1158 with quadrant flip.00067-0706 JNN 11 Estimated age 1000-10000 Myr; masses 0.35 +/- 0.09 and 0.21 +/- 0.05 Msun; a ~5.6 au. Jnn201400068-2106 RSS 41 CPD-21@100068-0853 BUG 15 Burgasser et al. (2012) determine that the pair comprised of LP 704-48 and SDSS J000649.16-085246.3 share cpm, at a projected separation of 820 +/- 120 au, based on a derived distance 30 +/- 3pc. Spectral type of the primary is M7. From near-IR spectroscopy they determine the secondary is SB, orbital period 147.6 +/- 1.5d, e = 0.10 +/- 0.07; spectral types of Ba and Bb are M8.5 +/- 0.5 and T5 +/- 1. Estimated ages of A and B are >8 and >3-4 Gyr; masses 0.092 Msun for A, 0.082-0.083 and 0.049-0.064 Msun for the M8.5 and T5 stars. Bug2012 NLTT 251 + 2MASS J00064916-0852457. Baron et al. (2015) estimate spectral types M6.0 +/- 0.5 and M9.0 +/- 0.5, distances 25 +7/-11 and 37 +5/-11 pc, masses 0.102-0.133 and 0.079-0.085 Msun. BFr201500070+0303 GWP 14 XMI 109. Tob2012b00071+6309 MLR 105 No significant movement since first resolution. Drd200900073+2058 HDS 12 Rectilinear solution by Hartkopf & Mason (2013). Hrt2013b00074-2936 LDS2088 NLTT 296/295 Chm200400076+4009 STF3064 Taken to be the same as H 4 69 (= H IV 69). With error of 1deg in declination it would be the same as STF 3064 rej. BDS 8. Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 Rectilinear solution by Hurowitz et al. (2013). USN2013a00076-2718 LDS2089 NLTT 307/308 Chm200400077+6022 JNN 247 G 217-32. Estimated age 35-300 Myr; masses 0.17 +/- 0.07 and 0.12 +/- 0.06 Msun; a ~9.8 au. Jnn201400078+5723 HJ 3241 HJ 1935.00079+0317 J 301 BAL 1606.00079-2727 LDS 5 Also known as CHM 1. WDS designation in error, apparently due to confusion between CD-28 11 and CPD-28 11.00079-3005 LDS2092 NLTT 319/320 Chm200400080+3123 STTA256 B is BD+30@3.00081+3240 HJ 610 SEI 2. Nsn2017a00082+6217 HJ 1936 Optical pair, since relative motion reflects the proper motion of component A relative to B to high accuracy. Kiy201200082+5933 STI 8 AB: 00083+5934SMA 300082+0937 LDS9085 Old LDS6085.00083+1329 GWP 17 XMI 110. Tob2012b00084+2905 H 5 32 21 And = alp And = Alpheratz AB: H V 32. STFB 15. A is spectroscopic binary, P = 96.7d. AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 MKT 11 Aa,Ab: Separations and magnitude differences derived by model fitting to calibrated squared visibilities, using measurements with the Mark III interferometer. Spectroscopic and photometric data are combined with astrometry from the Mark III interferometer to derive orbital elements for the SB1 by Pan et al. MkT1992a Pourbaix gives combined solution for this resolved SB2, yielding orbital parallaxes and component masses. Pbx2000b Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Pan et al. (1992). MkT1992a Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate astrometric data. Derived component masses are 4.05 +/- 0.50 and 1.71 +/- 0.20 Msun. Ren2010 Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 5.19 +/- 0.18, 4.10, and 3.09 Msun, respectively. Mlk2012 Aa,Ab: Docobo et al. (2014) use the spectroscopic elements of Pourbaix (2000), together with speckle data and the Hipparcos parallax, to Pbx2000b derive the remaining orbital elements. The resulting masses are 3.84 +/- 0.29 and 1.63 +/- 0.26 Msun. Doc2014h00085+3456 HDS 17 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 2.78 +/- 0.89, 2.67, and 1.10 Msun, respectively. Mlk2012 A(B) Teff = 6100+/-50(5940+/-50) K, R = 1.93+/-0.20(1.83+/-0.20) \rsun, AlW2014b L = 4.63+/-0.80(3.74+/-0.70) \lsun, M = 1.35(1.25) \msun. Sp = F8.5IV(G0IV).00085-7134 HLN 18 Also known as TDS1309.00085-0419 GWP 19 AB and BC were originally listed as the triple 00086-0418; now are merged with GWP 18 at the correct WDS designation.00087+5006 ES 443 Identical to ES 744.00088+8647 NLTT 324 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Intermediate Astrometric Data with spectroscopic elements by Latham et al. (2002). They derived component masses 1.06 and 0.59 Msun and an Lat2002 estimated semimajor axis of 7.00 mas. Ren201300088+0801 HDO 2 Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 Rectilinear solution by Friedman et al. (2012). USN2012a00089+3257 SEI 1 Neither component seen on POSS plate; may be flaws on AC Potsdam plate00089+2050 BEU 1 GJ 3010. Estimated age 30-300 Myr; masses 0.20 +/- 0.09 and 0.11 +/- 0.06 Msun; a ~2.0 au. Jnn201400090+2738 GIC 1 AB = G130-046/G130-045.00090-5400 HDO 181 Spectroscopic binary. Quoted errors in P and a are +116/-40y, +0".20/-0".06, respectively. Ary2002b00092+5909 AGC 15 bet Cas = 11 Cas = Caph The primary is a Delta Scuti-type variable. Spectroscopic binary, P = 27 d. AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 NPOI Limb-darkened diameter 2.103 +/- 0.015 mas, Sp = F2III, NOI2018 R = 3.79 +/- 0.04 \rsun, Teff = 6739 +/- 88 K, L = 26.8 +/- 1.4 \lsun, M = 2.02 +/- 0.03 \msun, Age = 1.00 +/- 0.05 Gyr.00092-3035 LDS2093 NLTT 410/401 Chm200400093+7943 STF 2 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 3.97 +/- 2.24, 3.22, and 2.02 Msun, respectively. Mlk201200093+5324 FYM 4 The EF pair reported by Fay (2013) is not seen in Aladin; probably an FyM2013d erroneous identification of their CG pair. BVD 11 CD: Originally listed as separate pair (00096+5325), aka FYM 4CD.00093+2517 GIC 2 LDS 859 = G130-048/G130-047. HIP 754. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. A companion is a close astrometric binary. HIP1997d AB: Primary is SB2, P=463.250d Tok2014d Spectroscopic orbit P=463.44d and radial velocity of B consistent Grf2015b with physicality.00094+6357 BUP 1 V641 Cas, a VV Cep-type system.00094+4819 LDS3128 NLTT 412/405 Chm200400094+1415 CHE 1 Due to poor published coordinates, identification with the coordinates in the WDS is uncertain. Chevalierâ€™s measure does not agree well with Che191 others for this pair. Hrt2012b00094-2759 BU 391 kap 1 Scl00096+3826 PTT 1 This appears to be the same as ALI 473. PTT position 00 10.0 +38 23.00096+0148 GWP 22 XMI 113. Tob2012b00096+1047 GWP 21 XMI 112. Tob2012b00096+1052 GWP 20 XMI 111. Tob2012b00097+3107 GIC 3 G130-050/G130-049. NLTT 433/431 Chm200400100+4623 STF 3 A small star in field: 1831.33 133.0@ 4.57"; Possibly an illusion. Bu_1906 H 2 83. MEv2010 Primary is V342 And, an Algol-type eclipsing binary, P = 2.63934d. Zas201200100+1109 STF 5 34 Psc.00101+5847 STI1287 SMA. Daley (Dal2002c) finds a large B-V for the secondary of 1.52.00101+3825 HDS 23 Da,Db: Cvetkovic et al. (2014) derive spectral types K3 and K4, masses 0.79 and 0.72 Msun. Dynamical parallax is 11.42 +/- 0.70 mas. Cve201400103+7231 HJ 1941 See note to 00138+7233BUP 2.00104+5831 BU 253 Ba,Bb: Rectilinear solution by Rica & Zirm (2012). FMR2012i00104+4952 ES 2576 B is BD+49@17.00105+1716 ALP 1 2MASSI J0010325+171549 Physical companionship to this ultracool dwarf ruled out based on I-J color, using I-band photometry taken at WIYN in August 2002. AlP200700106-7313 I 43 There is a long gap (1931-1977) in the observations.00107+5453 WOR 37 SX Cas, an eclipsing and spectroscopic binary, P = 36.6d. Spectral types A6shell and K3III.00108+5846 BU 485 Ca,Cb: Rectilinear solution by Rica & Zirm (2012). FMR2012i00108-5729 HJ 3350 Primary is BL Phe, a Beta Lyr type eclipsing binary, P = 0.81035d. Zas201200109+4807 LEP 2 NI 1.00109+1705 GWP 24 XMI 114. Tob2012b00110+0058 SKF1821 Initial WDS designation (00110+0913) garbled - dec portion copied from SKF1820.00111+5755 HJ 1003 STI 1291.00112+4933 ES 2577 B is BD+48@28.00113+1435 LDS1072 NLTT 521/522 Chm200400113+0625 GWP 27 XMI 115. Tob2012b00113-2045 LDS 1 G266-060. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. NLTT 525/526 Chm200400114+5850 SKW 1 Aa,Ab. Primary of the Herbig Ae/Be pair LkHa 198. A family of possible SKW2005 orbits are calculated, based on various choices for initial parameters (luminosities, component masses, etc.). Neither a" nor T0 was provided. a" was calculated from other published parameters and T0 was determined by trial and error with comparison to their Figure 3.00116-0305 STF 8 H 2 55. MEv201000116-2748 LDS2099 kap 2 Scl00117+0323 FMR 29 aka UC 332.00121+5337 BU 1026 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 6.13 +/- 1.26, 3.41, and 3.01 Msun, respectively. Mlk2012 CHR 1 AC: Rapid motion, particularly in separation.00121+3327 GII 13 Aka ITF 31.00122+4647 A 802 Not seen 1950-1976. Possibly a whole revolution.00125+1434 LN Peg Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d00126+2143 LDS 861 NLTT 589/592 Chm200400126+1118 BPM 4 [PM2000] 8713 + [PM2000] 8668. Gvr201000130+0257 A 2001 Apparent motion in a highly-inclined orbit.00132+1511 BUP 3 gam Peg = 88 Peg = Algenib Beta CMa variable and spectroscopic binary.00132+0536 PLQ 3 Possibly same star as HDO 5 (Doolittle).00132-1711 HJ 1944 B is BD-17@16.00133+6919 KUI 1 AB: Nechville 6. JNN 248 BC: GJ 11 B. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.10 and 0.26 +/- 0.06 Msun; a ~17.2 au. Jnn201400134+3859 BRT2196 ALI 718, J 2709.00134+3801 ES 2445 ALI 474.00134+2659 STT 2 Hipparcos parallax of 0".00808 yields a mass sum of 1.9 Msun, slightly underestimated for a double star of spectral type F8V. Dynamic parallax is 0".0053, considerably different from the measured one. Sca2000b AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 3.36 +/- 1.29, 4.23, and 1.10 Msun, respectively. Mlk2012 Star C (mag. 10.37, 18") is physical, according to Le Beau. LBu1990c00135-0009 HJ 618 BAL 641 = LDS 4.00136+1356 LDS1073 LDS6086 = LDS9086.00137+7702 MLR 283 Aka TDS1350.00137+4934 STF 9 B is BD+48@42.00137+1537 BPM 5 [PM2000] 9457 + [PM2000] 9535. Gvr201000138+7233 BUP 2 Misinterpretation of a note in Bu_1913 resulted in these three BUP components being associated with 00103+7231HJ 1941, when all three were actually measured relative to a planetary nebula (NGC 40) about 3m following the HJ pair. Since one BUP component was also the primary of the MLR 282 triple system, the BUP component designations were changed to become part of the MLR multiple. The planetary nebula is now the D component in this system.00138+3612 BU 1341 AC: This is a measure of A and BD+35@27.00138+0812 TOK 360 Likely triple system. Tok2013b Primary is unresolved Hipparcos acceleration solution (G-code) binary. Tok2014d00138-7442 HJ 3353 Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 Rectilinear solution by Hurowitz et al. (2013). USN2013a00139+6323 BU 1309 AB: The star is 63@703-62@1909 in Vat. Astrog. Cat. (Van Biesbroeck). VBs1954 AD: D is 63@656-62@1910.00139+1518 LDS1074 NLTT 667/666 Chm200400139-0429 LDS9087 Old LDS6087.00140+2837 BRT 117 MLB 554.00140-1815 BFR 2 NLTT 687 + 2MASS J00135882-1816462. Baron et al. (2015) estimate spectral types M3.0 +/- 0.5 and L1.0 +/- 0.5, distances 42 +26/-16 and 83 +7/-27 pc, masses 0.389-0.412 and 0.072-0.078 Msun. BFr201500141+7601 STTA 1 B is BD+75@5.00141+3957 ES 2544 ALI 1008.00142-0712 MSH 1 Meshkat et al (2015) resolved a faint companion to HD 984. They derive a system age in the range 30-200 Myr. Teff for the primary is 6315 +/- 89K; temperature for the secondary is 2777 +127/-130K or 2900 +/- 200K, depending on adopted scale and synthetic spectra. Spectral types are F7V and M6.0 +/- 0.5. Primary mass is 1.20 +/- 0.06 Msun; secondary mass estimates range from 74 - 90 Mjup, depending on adopted models. Msh201500143-0535 OSO 2 G031-036. Not a common proper motion pair, based on comparison with POSS2 red plates Oso200400144+3609 LDS3140 NLTT 703/704 Chm200400144+1643 BPM 6 [PM2000] 9941 + [PM2000] 9955. Gvr201000144-1424 GAL 296 Object #7 in Gallo's original list. Gal1912a00145-0747 BU 486 Irregular variable, AD Cet.00148-2859 RSS 1 This previously uncataloged double star was a Hipparcos double entry system. The first measure is determined from the individual positions listed by Rousseau et al. Rss199600150+0849 STF 12 35 Psc. A is an Algol-type system, UU Psc, P = 0.84d. Also known as CHE 2. HJL 2. HJL1986 H 3 62. MEv201000150-7251 BRG 1 The AstraLux PSF was strongly asymmetric for this target, hence in addition to the usual PSF fitting, we also performed a customized aperture photometry scheme in order to ensure that the PSF fitting did not provide a biased result (see paper for details). We adopt the aperture photometry values for the differential photometry, and let the errors be represented by the scatter between PSF fitting results and the aperture photometry. Note that the photometry values presented Brg2010 here should replace those in Bergfors et al. (2010). Jnn201200152+5947 FYM 153 Purported AJ pair removed on request of author. FyM2014b00152+3642 LDS3144 pa error = 359 deg. RAO2020b00152+2722 J 868 Rectilinear solution by Rica (2014). FMR2014f Due to the very different parallax in Gaia DR2 for the two components Cve2019b the orbital solution of Novakovic (2007) is no longer plausible and the Nov2007b linear solution is preferred. The orbit solution is retained in ORB6.00152+2717 KUI 2 A is a spectroscopic binary.00152+2722 J 868 Despite having an orbit, this pair determined to be optical. FMR2014d00152+2454 GIC 4 G130-059/G130-060.00153+5304 GIC 5 G217-041/G217-040. NLTT 739/738 Chm200400153+4412 A 1256 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 6.79 +/- 3.58, 5.77, and 2.82 Msun, respectively. Mlk2012 Primary is the Algol-type eclipsing binary V348 And. Zas2009 The A component is a close 27.7-d eclipsing pair, so the pair is at Zas2019b least triple. Based on proper motion C and D are likely optical.00153+1630 BPM 7 [PM2000] 10539 + [PM2000] 10566. Gvr201000153+0936 GWP 30 XMI 116. Tob2012b00153-4006 WG 2 B is CPD-40@14.00154-1134 GAL 297 00153-1133SLE 251. Object #9 in Gallo's original list. Gal1912a00155-1608 HEI 299 L722-22. Astrometric binary now resolved. Too poor astrometric orbit (Innes 1998) and too few resolved Inn1988 observations (cf. Heintz 1990) to give definite orbit. Present Hei1990a solution at least preferable to `X' HIP solution. Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 0.17 +/- 0.02, 0.39, and 0.50 Msun, respectively. Mlk201200157+3516 ALP 2 2MASSW J0015447+351603 Physical companionship to this ultracool dwarf ruled out based on I-J color, using I-band photometry taken at WIYN in August 2002. AlP200700159-0853 SHY 381 HIP 1266 + HIP 118.00160+0415 NLS 1 Nielsen et al. (2012) discovered two low-mass companions to the young A0V star HD 1160. The B component is thought to be a brown dwarf, mass 33 +12/-9 Mjup. The C component is of spectral type M3.5 +/- 0.5, with estimated mass 0.22 +0.03/-0.04 Msun. The age of the system is roughly 50 +50/-40 Myr. Nls201200161+0902 GWP 32 XMI 117. Tob2012b00162+7657 STF 13 A premature orbit has been calculated.00162+1903 J 217 Measures scattered. Additional notes may be found in Couteau (1952) and Cou1952a Van Biesbroeck (1954). VBs195400162-7951 GJ 3021 Combined solution, based on reduction of Hipparcos intermediate astrometric data together with spectroscopic elements from the Geneva Extrasolar Planet Search Programs home page. HaI2001 CVN 14 Companion is a probable mid-M dwarf. Cvn2006 Spectral type of B component M4V +/- 1. Cvn2007 A second candidate companion at 39" is noted in UCAC2 as having much different proper motion, so has been ruled out as a companion. The measured proper motion of the companion between the two SofI observing epochs is (+368 +/- 68 mas, -48 +/- 68 mas). IR spectroscopy suggests a spectral type of M4-M5V for the B component. Mug2007b Co-moving with HIP 107705 at 3.5pc. Shy200100164+5722 TDS1375 Aa,Ab: formerly 00165+5722, WDS designation changed when merged with HJ 1011 into triple00164+1950 LDS 863 AB: NLTT 803/804 Chm200400165-2805 LDS2107 NLTT 834/835 Chm200400167+3910 ES 1936 ALI 719.00167+3638 STF 19 STT 3.00167+3629 STT 4 Hipparcos parallax of 0".01115 yields a mass sum of 2.75 Msun with an uncertainty of 38% overestimated for a double star of spectral type G0. Dynamic parallax is 0".0108, agreeing well with the measured parallax. Sca2000b Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.72 +/- 0.59, 2.35, and 1.05 Msun, respectively. Mlk201200169-5239 GC 333 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Bopp et al. (1970). Evn197000171+3841 CHR 123 theta And = 24 And00171-1205 CBL 202 GWP 34. Tob2012b00171-1406 GAL 298 Object #12 in Gallo's original list. Gal1912a00172-1921 LDS 9 B is BD-20@34.00174+0853 A 1803 Too close 1932, 1946-47, 1965-72. Modern measures show a close approach about 1985. While both 18- and 36-year period orbits have been calculated for this pair, Griffin (Docobo, private communication) determined spectroscopically that the shorter-period high-eccentricity orbit is the correct one. The measure reported for 1976.622 is spurious and has been deleted from the catalogs. McA1982b Large and irregular residuals preclude the correction of an orbit. Tok1985 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 0.02 +/- 0.02, 1.48, and 1.13 Msun, respectively. Mlk2012 STF 22 AB,C: H 2 50. MEv201000174+0221 STF 21 HJL 3. HJL198600176+1300 HJ 3 HJL 4. HJL198600176-1113 GAL 299 Object #13 in Gallo's original list. Gal1912a00177+5126 TRN 8 AO Cas. Classification is from the UV tomographic analysis of Bgn1991 Bagnuolo & Gies (1991). Msn1998a The image rotator was in an unknown state, so two possible theta values are listed for the 2001.7341 observation - one for zenith up and one for north up. Trn200800178+1620 TOK 646 Primary is 39 Psc. B is likely physical, as it moves in the same direction as A in DSS2 image. Tok2014d00180+2057 LDS 864 NLTT 912/910 Chm200400180+0931 AG 1 HJL 5. HJL198600182+7257 A 803 Quadrant uncertain. Wor1967b00182+1209 GWP 38 XMI 118. Tob2012b00183+1646 BPM 8 [PM2000] 12613 + [PM2000] 12602. Gvr201000184+4401 GRB 34 AB: Proper motion of A +2860 +390. Proper motion of B +2884 +410. Premature orbits have been calculated. RV of star A possibly variable. B component is the BY Dra-type variable CQ And and a SB. AB: NLTT 919/923 Chm2004 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d PTI Limb-darkened diameter = 1.014 +/- 0.05 mas, PTI2001 R = 0.389 +/- 0.021 \rsun. VLTI Limb-darkened diameter 1.000 +/- 0.05 mas, LTI2003a M = 0.414 +/- 0.021 \msun, R = 0.383 +/- 0.02 \rsun, T = 3698 +/- 95 K. CHARA Array Limb-darkened diameter of A : 0.988 +/- 0.016 mas CIA2006 R = 0.379 +/- 0.006 \rsun, Teff = 3730 +/- 49 K. CHARA Array Limb-darkened diameter of A : CIA2012f R = 0.3874 +/- 0.0023 \rsun, L = 0.02173 +/-0.00021 \lsun, Teff = 3563 +/- 11 K, M = 0.423 \msun. AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200800184+0344 HDO 12 AB: Appears to be same pair as HDO 13.00185-2757 HJ 1949 B is CD-28@75.00187+4347 STT 5 26 And.00188+5923 HJ 1012 STI 1320.00188-1217 GAL 15 Incorrectly entered in WDS as GAL 5.00188-1258 GIC 6 G158-057/G158-054.00189+5923 HJ 1013 STI 1322.00189-1135 GAL 16 Originally entered with incorrect RA, so also known as 10187-1239GAL 42200190+4301 ES 1483 J 1359.00192+5942 KR 4 A is an irregular variable, V377 Cas.00192+4330 ES 1484 BRT 67. Djurkovic calls this ES 1484BC. Dju1954c00192+0827 GWP 39 XMI 119. Tob2012b00194-0849 HJ 1953 iot Cet = 8 Cet. Variable? NPOI Limb-darkened diameter 3.310 +/- 0.062 mas, Sp = K1III, NOI2018 R = 29.95+/- 0.725\rsun, Teff = 4645 +/- 73 K, L =376.8 +/-22.0 \lsun, M = 3.70 +/- 0.10 \msun, Age = 0.23 +/- 0.03 Gyr.00196-2808 LDS 12 Proper motion -275 -1292.00197+6046 LDS9088 Old LDS6088.00197+1951 GWP 40 XMI 120. Tob2012b 2MASS J00193931+1951050 and J00194303+1951117 are separated by only 53", have very similar proper motions (e.g. Roser et al. 2010) and XXX2010 have similar estimated spectroscopic distances (23 and 21 pc, respectively) in Riaz et al. (2006), hence it is highly likely that Ria2006 they form a physical pair. Jnn201200197+0624 ZUC 5 Primary is white dwarf PG 0017+061 = PHL 790. Zuc199200199+2633 CHE 4 Chevalier's measure was correct, but his published (dx,dy) predict Che1908 different (rho,theta) than published. This was apparently due to a typographic error in dy, which was printed as -0'.0317 rather than -0'.0617. There is also an apparent trigonometric error in his value for position angle. Chevalier gives a value for theta of 154.62 deg, but all later measures in the WDS give values of about 204.0 deg. It appears his value should be 360âˆ’154.62 = 205.38 deg instead. Hrt20100200+3814 S 384 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 AB: H 5 85. MEv201000201+4244 OSO 3 G171-050. AB is not a common proper motion pair, based on astrometry and color. Oso2004 LDS3151 AC: NLTT 1038/1036 Chm200400203-3246 B 1025 Considerable motion, but no measures for more than 30 years.00204+1757 OSO 4 G032-012. Not a common proper motion pair. Oso200400206-2356 WSP 20 Planet-host star found to be close visual binary. Evans et al. (2016) find that the transiting hot Jupiter is probably orbiting the primary, and derive the following properties: A: M = 1.089 +/- 0.047 Msun, R = 1.142 +/- 0.085 Rsun planet: M = 0.378 +/- 0.022 Mjup, R = 1.28 +/- 0.15 Rjup EvD201600206+1219 BU 1015 Hipparcos parallax of 0".00883 yields a mass sum of 2.87 Msun with an uncertainty of 75% slightly in excess for a binary of spectral type F5. The great uncertainty concerning the sum of masses is largely due to the consistent error in the measured parallax. The dynamical parallax is 0".0085, agreeing well with the observed parallax. Sca2000b Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 2.44 +/- 1.04, 2.58, and 1.20 Msun, respectively. Mlk201200207+3159 CCA 1 WSP 1. WASP-1. Duplicity discovered based on low-amplitude radial velocity variation. Spectral analysis plus transit light curves yields an orbital period of 2.520d. Given a spectral type for the primary of F7V, the planet has mass 0.80-0.98 +/- 0.11 Mjup and radius 1.33-2.53 Rjup. Mass of the parent star is 1.06-1.39 Msun. CCA200700207+0738 GWP 41 AB: XMI 121AB. Tob2012b GWP 42 AC: XMI 121AC. Tob2012b00208+2737 CHE 7 MLB 674. Also known as ROE 116.00210+6740 HJ 1018 STF 18. Mlr1955c00210+2647 CHE 9 Chevalier's measure was correct, but his published (dx,dy) predict Che1908 different (rho,theta) than published. This was apparently due to a typographic error in dx, which should be +0'.0708. Chevalier applied his declination offset from the plate center in the wrong direction, leading to an error of over 25' in the coordinates. The image for the pair at the corrected coordinates is elongated on the Aladin image; due to uncertain relative proper motion it's impossible to tell whether his rho and theta values are correct. Hrt2012b00210-7429 OGL 1 SMC139.6.72 + SMC139.6.636 Pli201200211+6443 TDS 13 According to Milburn this pair was originally "found by Aitken Mlb1925 (private letter) in looking for MLB 244". This note went unnoticed A__1925D until long after the Tycho designation had come into usage, however; although the historical measures have been added the original TDS designation has been retained.00212-4246 KO 1 A = LEHPM 494 (spec M6.0 +/0 1.0 V), B = DENIS-P J0021.0-4244 (spec M9.5 +/- 0.5 V). Data sources: UK Schmidt blue survey (1977.6), ESO Schmidt red (1984.8), DENIS I (1996.60), UK Schmidt red (1996.61), UK Schmidt near-IR (1999.6), 2MASS (1999.7). Mean separation (1974-1999) 1.296 +/- 0.012 arcmin. The pair moved 5".7 over 22 years, 80 times the uncertainty in mean rho; concludes is CPM pair. Cab2007a Additional 2003 measure from Spitzer Space Telescope. Cab2007b00214+6700 STT 6 Orbit is very eccentric and very inclined. Scardia's geometrical elements do not differ much from those of Van Biesbroeck and Muller, but the orbit is more eccentric and has twice the period. An Hipparcos parallax of 0".00491 yields a mass sum of 6.6 Msun, overestimated for a binary system of spectral type B8.5V. The dynamical parallax is 0".0054, in reasonable agreement with the measured one. Sca2000b00214+2744 CHE 10 MLB 675.00214-7355 OGL 2 SMC138.6.56 + SMC138.6.104 Pli2012