02000+1334 LDS5181 old LDS6130.02003-0138 BAL 9 J 3333. Nsn201602004-0831 HJ 3476 AB: A is AR Cet, probably a semi-regular variable.02005-0240 BRG 8 The companion to 2MASS J02002975-0239579 has yet to be tested for common proper motion, but since its color and brightness are consistent with expectation and its separation is small (~0.32"), it is counted as a physical companion here. Jnn201202005-6246 HJ 3479 B is CPD-63@142.02006+2753 J 3257 A is an Algol-type binary, X Tri, P = 0.97d.02011+3518 STF 197 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200802011-1741 LDS5362 NLTT 6759/6757 Chm200402012-0729 GWP 250 ABL 1. Tob2012b02012-3000 CUS 1 Assuming a primary mass of 1.02 +/- 0.19 Msun, the derived flux ratio (~0.028 in H and K) gives a mass of ~0.5 Msun for the secondary. Cus201202013+1227 BPM 45 [PM2000] 74159 + [PM2000] 74128. Gvr201002013-0752 GWP 251 ABL 2. Tob2012b02015+1830 BPM 46 [PM2000] 74328 + [PM2000] 74271. Gvr201002019+7332 JNN 252 GJ 3125. Estimated age 30-300 Myr; masses 0.12 +/- 0.07 and 0.06 +/- 0.04 Msun; a ~5.0 au. Jnn201402019+2415 POU 157 ID uncertain. Nothing at Pourteau's coordinates. Pou193302020+7054 BU 513 48 Cas. A is a spectroscopic binary, same period as the visual pair. Suspected sub-periods of 39 yr (Baize) and 26 yr (Muller) are not Baz1941b confirmed by later measures. The radial velocities of the primary may Mlr1949c show a trace of a period of about 4 yr (Heintz). Hei1981e See Baize & Petit catalog of doubles with variable component. Baz1989d Masses and bolometric magnitudes are derived for the two components based on assumed spectral types and available parallaxes. 1980.7205: This measure was incorrectly attributed to ADS 1958 in McAlister et al. (1983). McA1983 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 2.96 +/- 0.42, 3.07, and 2.00 Msun, respectively. Mlk201202020+0246 STF 202 alp Psc = Alrescha. Both components are listed as Alpha CVn variables of small amplitude, and both may have variable RV. Sca1983f See Baize & Petit catalog of doubles with variable component. Baz1989d Absolute quadrant for 1998.657 determined by triple-correlation techniques Pru2002b Chevalier identified this star as alp Psc, but gave an incorrect Che1911 declination, leading to its initial designation as 02020+0320 CHE 32. Hrt2012b PWL 1 AC: SHY 132. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical. STF 202 AB: H 2 12. MEv201002021+0355 OSV 1 LDS5363.02021-1321 GAL 317 Object #59 in Gallo's original list. Gal1912b02022+7530 STF 185 Primary is V779 Cas, an Algol type eclipsing binary, P = 6.35340d. Zas201202022-1441 GWP 253 ABL 4. Tob2012b02022-1808 GWP 252 ABL 3. Tob2012b02022-4550 SHY 410 HIP 9495 + HIP 9672.02022-6236 TOK 70 HIP 9499. A is SB, no orbit, dRV=70.7 (Nordstrom et al. 2004). Nrd200402023-2634 LDS 65 NLTT 6825/6826 Chm200402025-1410 GWP 254 ABL 5. Tob2012b02026-1719 GWP 255 ABL 6. Tob2012b02027-3019 HJ 3478 B is CD-30@717.02030+3317 STF 201 eps Tri = 3 Tri02031-0725 STF 209 B is BD-08@371.02031-1229 GWP 256 ABL 7. Tob2012b02032+5514 BLL 4 A is a semi-regular variable, XX Per. B is BD+54@445.02034+3919 MLB 10 AB: Also known as SMA 27.02035+6408 HJ 1101 STI 337 (three Vat1926 measures from STI 337 merged 2008/06/25)02035+1744 BPM 47 [PM2000] 75525 + [PM2000] 75508. Gvr201002037+2556 STF 208 10 Ari. Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 2.94 +/- 0.84, 2.35, and 1.29 Msun, respectively. Mlk201202038+7013 MLR 375 1983.0663: This autocorrelogram was remeasured; the new results are listed in the catalog. McA1987b02038-0020 H 5 102 H V 102. 61 Cet. Spectrum composite; G5II-III+G5V.02039+8221 HJ 2090 The measure in BDS by Cogshall belongs to some other pair. Bu_1906 1904.69, 243.9@, 3.52" (Van Biesbroeck). VBs191402039+4220 STF 205 H III 5, SHJ 26. gam And = Almach. A quadruple system. Star A (mag 2.3, K3II) forms with BC the pair STF 205, separation 10". Star B is SB, P = 2.67 d (Maestre & Wright, ApJ 131, 119, 1960). See discussion by Morgan et al. (1978). BLM1978 A,BC: H 3 5. MEv2010 STT 38 BC: See discussion by Morgan et al. BLM1978 BC: Poor agreement between two theta measures. Mlr1956d BC: Additional notes may be found in Muller (1954). Mlr1954a02039+1231 BPM 48 [PM2000] 75778 + [PM2000] 75779. Gvr201002039-4525 RST2272 Primary is SB2, P=0.851 y. Aa,Ab UR in speckle. Koen et al. (2002 MNRAS 331, 45) find 311d photometric period. Tok2014d02042+5257 HJ 2104 B is BD+52@501.02042+4641 ADM 1 HTP 32. HAT-P-32. Primary is exoplanet host star. Adm201302042-1039 GAL 318 Object #62 in Gallo's original list. Gal1912b02044+1230 CHE 36 CHE 37.02046+2525 LTT 17328 Combined solution, based on reduction of Hipparcos intermediate astrometric data together with spectroscopic elements from the Geneva Extrasolar Planet Search Programs home page. HaI200102046+1757 GWP 257 XMI 235. Tob2012b02051+7717 SHJ 22 47 Cas. Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 47 Cas Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d02051-1737 BEU 3 PM = +1318-174.02053+2906 CHE 38 CD: Originally 02053+2907 CHE 38AB, until C component of 02053+2906 found to be prmary of 02053+2907. WAK 14 CE: Originally 02053+2907 WAK 14AC.02053-2803 LDS 67 NLTT 6979/6980 Chm200402054-5910 HJ 3481 B is CPD-59@185.02055+7607 BU 785 49 Cas.02055+0056 LDS5365 Error in WDS designation - incorrect precession of Luyten coordinates? Luy198402056+1444 BPM 49 [PM2000] 76857 + [PM2000] 76899. Gvr201002057-2423 I 454 CPD-24@891. C is CPD-24@889. AB,C = LDS 68. AB,C: SHY 135. Bayesian analysis by Shaya & Olling (2011) indicates Shy2011 very high (near 100%) probability pair is physical. WSI 7 Aa,Ab: Tokovinin et al. (2014) derive a combined spectroscopic/ interferometric orbit of the Aa,Ab pair, as well as a new orbit of the AB pair. Resulting component masses for Aa, Ab, B, and C are 0.74, 0.72, 0.57, and 0.78 Msun, respectively. Tok2014b02058+1241 CHE 42 There are no obvious errors in applying the offset from Chevalier's Che1910 plate center, but there are no appropriate pairs near his coordinates, nor at coordinates found by reversing the sign of either or both offsets. The pair is likely lost. Hrt2012b02062-1808 GWP 258 ABL 8. Tob2012b02065+5703 BAR 23 J 880.02068+2542 HO 312 11 Ari.02069-1126 SLW 99 Aka ABL 9.02070-1017 GAL 319 Object #63 in Gallo's original list. Gal1912b02070-4406 JNN 149 2MASS J02070176-4406380 and J02070198-4406444 are separated by only 7" and have similar estimated spectroscopic distances (13 and 21 pc, respectively) in Riaz et al. (2006), hence it is likely that they form Ria2006 a physical pair. Jnn201202074-5941 HJ 3484 B is CPD-60@183.02076+1355 ZHN 2 BDK 4. G 73-26 + SDSS J020735.60+135556.3. Distance 26 +/- 10 pc for primary, 35 +/- 5 pc for secondary. Estimated age of system 3-4 Gyr. Mass of secondary estimated at 0.079-0.081 Msun. Fah201002076-0037 LDS3346 NLTT 7066/7064 Chm2004 HJL 29. HJL198602079+1343 GWP 259 XMI 236. Tob2012b02080+2814 CHE 55 MLB 452.02080-0951 GAL 320 Object #64 in Gallo's original list. Gal1912b02081+1336 FAR 27 SKF 23. Primary is white dwarf WD 0205+133. Far200602082+1509 LDS5183 old LDS6131.02083+2543 ALP 6 2MASSW J0208183+254253 Further observations are required to determine the physical/optical nature of this triple. AlP200702084+2819 KUI 118 G072-058. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. NLTT 7087/7088 Chm200402085-0641 HDS 285 Possible sub-diffraction-limited component, but the astrometry is not consistent between the two observations. Hor2011b02087-0026 STF 218 Same as STF 220.02089+4927 BWL 9 Colors and/or astrometry are inconsistent with a late-type common proper motion companion based on visual inspection of the field from 2MASS, SDSS, DSS1, and/or DSS2. Primary is GJ 3136. Bwl201502090+5745 STI1791 AB. WDS designation changed from 02099+5744 when it was determined that TDS2135 comprised the primary of this wider pair.02091+5104 STF 213 C easily seen 8" north following. Magnitude about 10.5, not 12.5. B__1963b02091+4341 LDS3349 NLTT 7117/7118 Chm200402091+4048 STF 215 A is an eclipsing binary, BX And.02091+1511 GWP 260 XMI 237. Tob2012b02093-1958 GWP 261 ABL 10. Tob2012b02094+2556 H 6 69 H VI 69. 14 Ari. STTA 23. AC: HJL1012. HJL198602094-1011 HJ 2116 Richard Jaworski, in analysis of SuperCOSMOS data, has determined that Jaw2005 component C is the galaxy NGC 833, D is the galaxy NGC 835, E is the galaxy NGC 838 and F is the galaxy NGC 839. Thus, in the pairing "CD" both components are galaxies and not stars.02095+3459 MKT 4 bet Tri. Hummel et al. (1995) visual orbit based on astrometry from Mark III MkT1995 interferometer. Additional spectroscopic data yield component masses, luminosities, radii, effective temperatures, and distance. Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Hummel et al. (1995). MkT1995 Pourbaix gives combined solution for this resolved SB2, yielding orbital parallaxes and component masses. Pbx2000b Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 4.11 +/- 0.18, 5.26, and 1.82 Msun, respectively. Mlk201202096+4251 ES 48 Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200802097+2021 STF 221 AB: H 3 68. MEv201002097+0857 GWP 262 XMI 238. Tob2012b02098-4052 TOK 427 HIP 10096 is SB2 according to GCS. The separation corresponds to a period of ~5yr. Tok2015c02099+3449 HU 1034 Not seen 1948, 1951. No observations since that time.02103+3322 STF 219 SEI 24. Nsn2017a02104+3911 HJ 1109 C is a nebula.02104-5049 ESG 1 Gl 86. Magnitudes are K magnitudes of Lagrange et al. (2006). Lagrange et al. (2006) give two possible orbital solutions, based on Lgr2006 different assumed masses (70 Mjup and 0.5 Msun) for the secondary. Semi-major axes converted from au (47.58 and 18.42 au, respectively) to arcseconds assuming an Hipparcos-based distance of 10.9 pc. JHK photometry of primary from 2MASS, that of secondary transformed from NACO to 2MASS filters. 2001.7454: PA is measured in zenith mode. If data collected in equatorial mode, PA = 112.1. Rbr2011d Farihi et al. (2013) derive a mass of 0.59 +/- 0.01 Msun and Teff = 8180 +/- 120K for the white dwarf companion to GJ 86. Monte Carlo simulations yield the following orbital constraints: P = 120-481y, T0 = 1933-2067, e = 0.00-0.61, i = 114.7-122.6deg, a = 2.57-6.47" (27.8-69.8 au) Omega = 63.7-76.1deg, omega=0-358deg. The upper ranges of P and a are considered less likely. Far2013 GJ 86 A: Combined solution, based on reduction of Hipparcos intermediate astrometric data together with spectroscopic elements from Queloz Que2000 et al. (2000). HaI200102106+1027 GWP 263 XMI 239. Tob2012b02107-1507 FAR 28 Primary is white dwarf WD 0208-153. Far200602109+3902 STF 222 59 And. H 4 129. MEv201002109+1341 STF 224 H N 105; BDS 1146 is identical.02110+0317 GWP 264 XMI 240. Tob2012b02112+2604 BRT3260 Originally published as BRT 127. Brt192802114+1848 GWP 265 XMI 241. Tob2012b02115+5739 BU 874 5 Per.02117-0531 GWP 266 ABL 11. Tob2012b02117-1927 GWP 267 ABL 12. Tob2012b02122+4440 RUC 2 Aa,Ab. GZ And. Spectral type of Ab component estimated at M3-4V. Ruc2007 HJ 2117 A is a W UMa-type binary, GZ And.02123-0908 GWP 268 ABL 13. Tob2012b02124+3018 STF 227 iot Tri = 6 Tri. A is a spectroscopic binary, P = 14.73d. B is also an SB, P = 2.24d. One component is variable: TZ Tri. TZ Tri Koresko et al. (1998) PTI solution has period fixed at spectroscopic Krs1998 value of Kaye et al. (1995). Eat1995b STF 227 H 2 34. MEv201002124+1249 LDS1126 NLTT 7300/7301 Chm200402124-0223 HDO 56 Not found. There must be a large error in the Hd place. Burnham Bu_1909 could not find it anywhere in the vicinity.02124-0455 GWP 269 ABL 14. Tob2012b02124-7023 R 15 HLN 3. B is CPD-70@131.02125-0804 BRT 357 Also known as LDS3357.02127+1614 GWP 270 XMI 242. SLW 100. Tob2012b02128+7941 S 405 STTA 22. A is a Delta Scuti-type variable and spectroscopic binary, P = 4.12d. B is BD+78@71. AB: H 5 84. MEv201002128+0309 GWP 271 XMI 243. Tob2012b02128-0224 STF 231 66 Cet. B is BD-03@335. Aka SHJ 29 = H 4 25. AB: NLTT 7323/7321 Chm2004 HIP 10305. A is SB2, period 94.788d, resolved by speckle (TOK 39). A is evolved. B = HIP 10303. Tok2011a02129+5712 STTA 24 AB and AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200802129-0349 GWP 272 ABL 15. Tob2012b02130+0851 MCA 5 xi 1 Cet = 65 Cet. Also a spectroscopic binary. A 1985.8375 measure attributed to this pair by Mcalister actually actually belonged to 02157+2503COU 79. McA1987b Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Griffin & Herbig (1981). Grf1981b 5 1985.8375: A measure at this date, belonging to 02157+2503 = COU 79, was erroneously attributed to MCA 5 in McAlister et al. (1987). This McA1987b measure has been moved to COU 79 and averaged with a re-reduced measure from these data published by Hartkopf et al. (1996). Hrt1996a02131+5805 SHY 145 AC: HIP 10332 + HIP 12685.02132+4414 CHR 5 60 And. A spectroscopic binary. The negative results obtained during 1976 - 1980 are apparently due to a large magnitude difference. Hrt1984 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013 Intermediate Astrometric Data with spectroscopic elements by Griffin & Herbig (1981). Grf1981b02132+4030 SHY 136 AB: HIP 10339 + HIP 10321. B component is V450 And. HEL 5 Ba,Bb: V450 And. Helminiak et al. (2016) resolve this SB and BY Dra type variable, and derive a combined astrometric/spectroscopic orbit. The secondary is shown to be an M-type star, rather than brown dwarf. Resulting best-fit masses are 1.141 and 0.279 Msun (median values 1.113 +/- 0.065 and 0.277 +/- 0.021 Msun), respectively. Best-fit parallax is 37.24 mas (median 37.34 +/- 0.55 mas). Hel201602133+3649 JNN 18 Estimated age 30-300 Myr; masses 0.26 +/- 0.06 and 0.09 +/- 0.03 Msun; a ~2.8 au. Jnn201402135+5926 STI 351 STI180702135-0502 GWP 273 ABL 16. Tob2012b02135-2546 HJ 2120 B is CD-26@800.02136+5104 BAG 1 Aa,Ab: 6 Per. A is a long-period spectroscopic binary, now resolved by speckle interferometry. SB1, P = 4.5 yr. Halbwachs (1981) predicts maximum separation 0".047. HJL1981 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Christie (1936). Crs1936 STT 555 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200802136-0945 GWP 274 ABL 17. Tob2012b02137-0302 H 6 110 H VI 110. B is BD-03@341.02138-1933 RSS 54 CPD-20@24802140+4729 STF 228 Spectral types and masses of components assigned by ten Brummelaar et al., based on adaptive optics observations. TtB2000 Scardia says the quadrant unambiguous for their 2004 theta values of 105.8; this does not agree with other determinations of magnitude difference, however. Sca2005a Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 2.34 +/- 0.36, 2.52, and 2.47 Msun, respectively. Mlk201202140+1652 GWP 275 XMI 244. Tob2012b02142+0555 GWP 276 XMI 245. Tob2012b02142-1811 GWP 277 ABL 18. Tob2012b02144+3454 HU 807 Motion in separation, with little angular change. Close 1950-1960.02144-1441 GWP 278 ABL 19. Tob2012b02145+6631 MCA 6 55 Cas. Composite spectrum star: B9V + G0II-III, delta m = 0.2 mag Bnu1984 (Markowitz 1969) Mrz1969 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 3.70 +/- 1.31, 6.94, and 2.57 Msun, respectively. Mlk201202145+5912 STI1812 SMA 31.02145-1103 LDS5373 SLW 102.02146-0142 GWP 279 ABL 20. Tob2012b02147+3024 STF 232 H 2 35. MEv201002147+1657 GWP 280 XMI 246. Tob2012b02149+5829 STF 230 B spectrum B9IV.02149+1353 GWP 281 XMI 247. Tob2012b02150+5903 MLR 447 Also known as TDS2174.02152-3507 SHY 415 HIP 10483 + HIP 10385.02154+1126 GWP 282 XMI 248. Tob2012b02155+5231 GC 2695 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Griffin & Radford (1977). Grf1977c02155+1220 GWP 283 XMI 249. Tob2012b02156+4223 GIC 29 G133-079/G134-019. NLTT 7438/7440 Chm200402157+6740 ENG 10 B is BD+66@193. Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 SHY 10 BC: HIP 10529 + HIP 11167.02157+2503 COU 79 21 Ari. Couteau & Morel (1982) computed masses disagree with spectral Cou1982d type. Authors suggest 3rd component (mass ~1 Msun) as possible explanation. 1985.8375: This measure was erroneously attributed to 02130+0851 = MCA 5 by McAlister et al. (1987). The data were re-reduced McA1987b by Hartkopf et al., giving similar results. The measure has now been Hrt1996a replaced by the mean of the two separate reduction results. 1986.567: The separation of this partially resolved pair was calculated under the assumption of zero or otherwise known magnitude difference. Pair passed periastron earlier than predicted; now the orbit is definitive Tok1985 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 3.09 +/- 0.30, 3.04, and 1.17 Msun, respectively. Mlk201202157+1046 STF 237 AB: HJL 30. HJL198602157-0217 GWP 285 ABL 21. Tob2012b02157+1657 GWP 284 XMI 250. Tob2012b02158-1814 HTG 1 Orbit poorly covered, period rather indeterminate. Hei1978c Additional notes may be found in Burnham (1894). Bu_189402159+1416 GWP 286 XMI 251. Tob2012b02159+0638 A 2013 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.60 +/- 0.37, 1.51, and 0.79 Msun, respectively. Mlk201202160-0929 BRG 10 This likely triple system has only been observed in one epoch, hence it remains unconfirmed. The brightnesses and colors of all components are however consistent with expectation for a physical triple. Jnn201202160-1626 GWP 287 ABL 22. Tob2012b02161+1651 GWP 288 XMI 252. Tob2012b02161+1630 BPM 50 [PM2000] 83035 + [PM2000] 83004. Gvr201002162-2302 I 457 ADS 1744a.02163-0949 STF 242 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200802164-0731 SLW 106 = GWP 289 = ABL 23.02164-1233 SLW 105 = ABL 24.02164-1632 GWP 290 ABL 25. Tob2012b02165-2227 LDS3364 NLTT 7520/7519 Chm200402165-5131 DUN 6 phi Eri. B is CPD-52@284. SHY 137 AC: HIP 10602 + HIP 9685. SHY 137 AD: HIP 10602 + HIP 7699. SHY 133 CD: HIP 9685 + HIP 7699. SHY 143 CE: HIP 9685 + HIP 12225. SHY 130 DF: HIP 7699 + HIP 6485.02167-0430 GWP 291 ABL 26. Tob2012b02167-3100 LDS 71 NLTT 7535/7528 Chm200402167-6324 TOK 71 HIP 10621. NOMAD: PM(B)=(0,-30), PM(A)=(18,60). D is HIP 10754. Tok2011a02168+4346 GNS 1 Based on 2MASS and AstraLux images, Ginski et al. (2012) conclude the companion is a background object. Gns201202169+5703 STTA 25 B is BD+56@470.02169+0448 GWP 292 XMI 253. Tob2012b02169-2322 BRG 11 The companion to 2MASS J02165488-2322133 has not yet been confirmed to share a common proper motion, but the color and brightness of it are well consistent with a physical companion, hence it is counted as such in the statistics. Jnn201202171+3413 DOR 66 del Tri = 8 Tri. A is a double-lined spectroscopic binary, P = 10.02d. Proper motion +1154 -245. MKT 5 Aa,Ab: PM = +1154 -245. del Tri. Hummel et al. 1995) visual orbit based on astrometry from Mark III MkT1995 interferometer. Additional spectroscopic data yield component masses, luminosities, radii, effective temperatures, and distance. Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Hummel et al. (1995). MkT1995 Pourbaix gives combined solution for this resolved SB2, yielding orbital parallaxes and component masses. Pbx2000b Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 1.57 +/- 3.14, 1.92, and 1.05 Msun, respectively. Mlk201202172+5838 YSC 87 Ba,Bb: Originally 02171+5839 YSC 87, but found to correspond to B component of 02172+5838.02172-2849 LDS3365 NLTT 7557/7558 Chm200402173+3351 VIG 1 Primary is gam Tri. The B and C components are background stars, the D component ambiguous. Vig201202174+2845 STF 239 HJL 32. HJL1986 Aka H 4 40 = SHJ 31.02174+2708 GIC 30 AC: G035-037/G036-007.02176+2214 STF 244 HJL 33. HJL198602176-5400 RSS 55 CD-54@48702178+5638 A 1272 V438 Per, a W UMa type eclipsing binary, P = 3.50939d. Zas201202179+1941 TOK 72 HIP 10710. Primary is astrometric binary (Makarov & Kaplan 2005) Mkr200502179+1614 GWP 293 XMI 254. Tob2012b02180+5616 UC 29 Primary appears to be a close pair. Cbl2010c02180+3116 A 959 Primary is eclipsing binary of W UMa type, period 0.31069d. Zas2017b02180+1958 GWP 294 XMI 255. Tob2012b02180+0145 GC 2770 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Harper (1935). Hrp1935 Combined astrometric/spectroscopic orbit by Fekel et al. (2007). For Fek2007 primary, derive mass = 1.15 Msun, radius = 1.64 +/- 0.07 Rsun, Luminosity = 3.0 +/- 0.1 Lsun. Spectral types are G0IV and ~M0V. SB1. Combined orbit including RV data and Hipparcos Intermediate Astrometric data. Semimajor axis derived from photocentric a0 plus stellar evolutionary model. Derived properties for A and B: M/Msun = 1.20 + 0.53, L/Lsun = 2.76 + 0.04, dm = 4.60 mag, log age = 9.65. WaX2015b02180-1229 LDS 73 NLTT 7592/7593 Chm200402181+5731 BU 1170 7 Per = chi Per S 409 = H 6 19.02182+5715 STI1836 BKO 165.02182+3920 A 207 Scardia et al. (2001) orbit preliminary as all the orbital elements Sca2001d are still rather uncertain. Hipparcos parallax (0".01200 +/- 0.00311) seems to be overestimated and leads to a mass sum 0f 0.46 Msun, unacceptable for a system of type F5. Scardia (1982) classified the Sca1982a star as type F9. Dynamical parallax is 0".0065; the corresponding mass sum is 2.87 Msun.02184+5758 STI1839 STI1844.02184-0636 GWP 295 ABL 27. Tob2012b02186+4017 STF 245 ALI1193. EGG 2 Aa,Ab: This system has spectral type F2 from SIMBAD and parallax of 10.26 +/- 2.92 mas from van Leeuwen (2007). A previous orbit was VlF2007 calculated by Cvetkovic (2008) with period of 109 years and semimajor Cve2008c axis of 0.344 arcsec. However, our new observation shows that the system has a much shorter period and smaller semimajor axis. However, our orbit yields roughly the same total mass, with large uncertainty. The system appears to have executed nearly a full orbit since the first speckle observations taken of it in 1985 by McAlister et al. (1987). More data will be needed to confirm this orbital trajectory, but if correct, the smaller period makes the system much more attractive for future study. Hor2015b02186-2940 B 34 AV For, Algol (EA) type eclipsing binary, P = 1.8797 d. Zas201102187+3429 STF 246 H III 42, BDS 1165. HJL 34. HJL1986 H 3 42. MEv201002187+0412 BU 437 Some observations erroneously ascribed to STF 247, even Struve's discovery, seems to belong to this pair, whose delta-m = 2 is less than Burnham's estimate. Hei1992a02188+0840 GWP 296 XMI 256. Tob2012b02188+1440 GWP 297 XMI 257. Tob2012b02190+2839 HJ 1115 10 Tri.02191-0651 HJ 327 AC: The C component is the galaxy NGC 883.02193-0259 JOY 1 Aa,Ab: The primary is omi Cet = VZ Cet = 68 Cet = Mira, prototype of the Mira-type variables. "Orbits" have been computed for the visual pair, but are most likely false. B has in the past been identified as a Cepheid, VZ Cet; however, it appears that the component seen as variable is the Joy component, recently determined to be a White Dwarf. Skl2010 Recent papers (in particular 1995 PhD thesis by Harold L. Chambers II) suggest that the visible companion is not the star itself, but the accretion disc around it (material captured from Mira's stellar wind). Rapid fluctuations of brightness are described by Warner (1972 MNRAS 159, 95). See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Aa,Ab: Pair seen but not measured. Cou1958c Aa,Ab: Additional notes may be found in Couteau (1963). Cou1963a H 6 1 H VI 1. C is BD-03@355.02198-2352 HJ 2130 B is CD-24@1022.02200-2213 BRT1373 CD-22@784.02201-1703 GWP 298 ABL 28. Tob2012b02204+2456 POU 175 Also known as KU 9.02204+1617 BPM 51 [PM2000] 85486 + [PM2000] 85504. Gvr201002204+0135 GWP 299 XMI 258. Tob2012b02205+1733 BPM 52 [PM2000] 85552 + [PM2000] 85616. Gvr201002209-0954 GWP 300 ABL 29. Tob2012b02209-5632 RST 51 CD-57@470.02210-1650 GWP 301 ABL 30. Tob2012b02211+4246 STF 248 Pourbaix gives combined solution for this resolved SB2, yielding orbital parallaxes and component masses. Pbx2000b Combined spectroscopic/visual solution, yielding masses, etc. Trr1995a Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.39 +/- 0.49, 1.78, and 0.85 Msun, respectively. Mlk201202212+5651 BU 1171 Not seen in 1951 with 82-inch (Van Biesbroeck). VBs999902212+3653 GIC 31 AB,C: NLTT 7710/7708 Chm200402213-1057 HJ 3495 B is BD-11@445.02215-1251 GWP 302 ABL 31. Tob2012b02215-1354 GWP 303 ABL 32. Tob2012b02216+2338 STF 254 POU 178.02219+0824 GWP 304 XMI 259. Tob2012b02220+0445 TOK 231 Primary is SB1, P= 79.700 d. Companion at 53" is possibly a white Tok2012c dwarf (Tokovinin & Lepine 2012) Tok2014d02220-0034 GWP 305 ABL 33. Tob2012b02222-0348 GWP 306 ABL 34. Tob2012b02224+5551 BU 875 9 Per. Variable, V474 Per.02225+2830 FAR 29 Primary is white dwarf WD 0219+282. Far200602225-0536 GWP 307 ABL 35. Tob2012b02225-2349 LAF 27 TOK 40. Astrometric binary with 26.5 yr orbit has massive secondary with q~1. Tok2012a Tokovinin (2013) derived a combined spectroscopic/interferometric solution, including echelle spectroscopy and speckle interferometry. The B component is a close binary (tentative period 3.7d); masses of A and Ba+Bb are nearly equal. Tok2013a Astrometric binary with large acceleration, where the massive companion B is in fact a close pair of M dwarfs. Tok2013b kap For Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit based on Gon2002a combination of ground-based catalogs with Hipparcos.02226+1531 LDS3375 G004-016. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. NLTT 7795/7794 Chm200402229+5835 BLL 7 A is the semi-regular variable, S Per.02229+4129 TRN 10 The image rotator was in an unknown state, so two possible theta values are listed for the 2001.7451 observation - one for zenith up and one for north up. Trn2008 HD 14633 Rodgers (1974 M.S. Thesis, Univ. Toronto) made a preliminary orbital analysis (P =15.3 d) but the variations appear to be more complicated than originally claimed (Bolton & Rodgers 1978 ApJ 222, 234). Msn1998a02229-1718 GWP 308 ABL 36. Tob2012b02229-5106 EHR 1 CPM pair. Ehr201002230+0443 GWP 309 XMI 260. Tob2012b02231+7021 MLR 377 A premature orbit has been published. Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995) Ruy199502231+0246 GWP 310 XMI 261. Tob2012b02232-2952 BU 738 T incorrectly listed as 1953.489 by Scardia et al. (1990); should be Sca1990a 1953.849 (erratum noted in Inf. Circ. 112, 1990) Sca1990b Parabolic orbit. Fin1969b sigma = areal constant in the true orbit = 0.0199 arcsec^2/yr q = periastron distance in the true orbit = 0".499102233+2230 LDS3378 NLTT 7840/7842 Chm200402233+1525 AG 38 LDS 879. B is BD+14@387. AB: NLTT 7845/7843 Chm2004 AB: SHY 417. Bayesian analysis by Shaya & Olling (2011) indicates Shy2011 very high (near 100%) probability pair is physical. . HIP 11137. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc. AB: HJL 35. HJL198602233+1452 GWP 311 XMI 262. Tob2012b02236-1056 RST4203 Also known as OL 111.02238+4920 STF 256 Also known as STF 243.02239+5751 MLR 656 Also known as HDS 311.02239+5522 BU 1373 The primary is the Cepheid variable V440 Per. Evs2016a02239+3330 STF 258 Also known as STF 253.02242+1016 CHR 199 First detected as an occultation binary by Evans. Evn198002244-2253 LDS3382 NLTT 7922/7928 Chm200402245-0145 STF 265 HJL 36. HJL198602246+5959 STF 255 STI 360.02246+2537 ALP 7 2MASSI J0224367+253704 Further observations are required to determine the physical/optical nature of this pair. AlP2007