09001-1228 HU 225 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 2.38 +/- 1.07, 2.57, and 1.13 Msun, respectively. Mlk2012 WOR 36 A faint companion (mag. about 14, 5") found by Worley may be physical.09002+4258 LDS3840 NLTT 20703/20706 Chm200409003+0332 HJ 2479 The proper motion study was: A component: mu(RA) = -0.006+-0.002 mu(DEC) = -0.005+-0.001, B component: mu(RA) = 0.000+-0.006 mu(DEC) = -0.005+-0.001 FMR1999h09005+7526 HJ 1162 Also a spectroscopic binary with P = 1324d which cannot be the visual Grf2016a pair.09005+3225 HU 718 A premature orbit has been computed.09005+0617 RAB 1 Rabe identifies this as BDS 4887? Looks like another pair. Rab192309006+4147 KUI 37 10 UMa. Hyad. Well observed RV variation in agreement with the visual orbit. Spectral types and masses of components assigned by ten Brummelaar et al., based on adaptive optics observations. TtB2000 Calculated mass sum is 2.44 +/- 0.12 Msun, consistent with spectral types F5V. Mut2010b AB: Additional notes may be found in Duruy (1941), Dur1941 Duruy (1942), and Dur1942b Baize (1943). Baz1943a AB: Martin et al. (1998) derive component masses 1.525 +/- 0.104 and 0.920 +/- 0.080 Msun. Mig1998 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 2.37 +/- 0.33, 2.39, and 2.14 Msun, respectively. Mlk2012 AB: A typographical error in the Muterspaugh et al. (2010) orbit has Mut2010b been corrected; period is 7961.0d, not 7691.0d. Noticed by Rick Wasson (2016, private comm.) STT 566 AB,C: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200809008+0516 OSV 2 Ross 686,7.09013+1516 STF1300 NLTT 20763/20764 Chm200409013-3855 I 1513 CPD-38@2898.09014+3215 STF1298 66 Cnc.09015+3604 ALI 354 Bogus binary.09018+2754 SHJ 101 67 Cnc. A is a spectroscopic binary. B is BD+28@1673. H 6 41. MEv201009024-6547 WFC 78 SWR 62. CPM pair Skf200409024-6801 SWR 63 CPM pair Skf200409026-5956 HJ 4170 SWR 61.09032+4232 LDS3848 SLW 323.09032-1740 S 588 B is BD-17@2726.09032-6221 HJ 4175 Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200809035+3750 MUG 1 Metchev & Hillenbrand say pair probably physical, based on proximity. Met2004b Metchev & Hillenbrand (2009) estimate companion mass 0.49 Msun, Met2009 dK=2.10. Estimated V(B)=11.2, dV=4.0. Tok2014d09036+4709 A 1585 Elongations and quadrant doubtful. B__1963b See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d 1975.950: This observation was made under very poor conditions and yielded a poor set of fringes. BLM1978 1981.350: This observation was incorrectly attributed to Fin 347 by Tok1982a Tokovinin (1982a) (noted in Tokovinin 1982b) Tok1982b Calculated mass sum is 6.30 +/- 0.98 Msun, not well-constrained. Mut2010b Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 6.63 +/- 1.41, 9.53, and 2.19 Msun, respectively. Mlk201209036-2619 HJ 2482 SWR 60. CPM pair Skf200409037+4531 COU2686 Also known as HDS1312. While the HDS measure predates that of Couteau, Cou1994 the Couteau publication predates that of Hipparcos. HIP1997a09040+1349 FAR 7 SKF 29. Primary is white dwarf WD 0901+140. Far2005b09040+0259 GRV1017 SLW 327.09040-3204 PRO 80 SWR 64.09042+6446 LDS2301 LDS5201.09042+0301 GRV 775 HJL 103. HJL1986 SHY 536. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical.09045-5740 RST 375 Spectral type G2?09048+3759 LDS3851 NLTT 20894/20892 Chm200409050+2250 HDS1318 A is SB2, P=893.5d. B not seen in 2MASS K,J-band images, likely bogus. Tok2014d09050+1134 TOK 125 HIP 44579.09050+1058 BPM 554 [PM2000] 925928 + [PM2000] 925978. Gvr201009053+3848 OSO 24 G115-049. Not a common proper motion pair, based on comparison with POSS2 red plates. Oso200409055+0020 RST5313 Appears to be 5' error in 1855 declination of BD coordinates. Appears to be same as TDS6306; pairs merged.09055-4919 JNN 65 This star has a probably brown dwarf companion, but since only one epoch of data exists, this is still unconfirmed. Jnn201209056+5018 ES 2631 B is BD+50@1606.09056-7433 SWR 66 CPM pair Skf200409057-0816 FAL 26 A = RX Hya, eclipsing binary of Algol type, period 2.28165 days. Zas201509061+3537 WLY 4 The pair ALI 355 is bogus and was a measure of a plate flaw. The WLY 4 pair was found while searching for the ALI pair.09063-5904 LTT 3359 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d09066+0249 STF1309 HJL 104. HJL198609067+2031 OSO 25 G009-047. Common proper motion pair Oso200409067-3334 EGN 10 Pair bound. B component colors consistent with it being an M1-M4 dwarf with mass 0.30 +/- 0.01 Msun. Egn200709071+3037 AG 162 BDS 4940, H N 30 is the same star.09074+2259 HO 644 AC: Physical pair according to Daley. Dal2006a STF1311 AB: HJL 105. HJL1986 AB: H 3 92. MEv201009075-3445 HJ 4179 SWR 65. CPM pair Skf200409076+0004 TOK 126 HIP 44777. X-ray source 1RXS J090732.0+000352.09077+1040 CHR 257 kap Cnc = 76 Cnc. Hipparcos suspected non-single.09077-4438 I 492 A Beta Cephei-type variable.09079-0708 TOK 64 Aa,Ab: Estimated masses 0.95 and 0.61 Msun; sep 29.3 au, period 130 y. Tok2010c STF1316 HIP 44804. Close triple. Observed with NICI (Tokovinin et al. 2010). Tok2010c09080-2552 I 491 kap Pyx09080-4326 SEE 109 lam Vel = Suhail. A is an irregular variable.09080-5808 RST9001 Previously known as RST3624a.09080-6402 HJ 4185 B is CPD-63@1097. SWR 67. Probably dwarfs, not giants (as per Houk). CPM pair Skf200409081+4510 HJ 1164 Noted as not having been observed in a long time, but this is an error. WSI2008 That "105" note should have gone with 09147-0212BAL 517. Dam201109081-2204 HDO 121 Separation for 1870.18 >15" Win188209083+3641 BRT2220 ALI 591.09083-3707 TOK 127 HIP 44851. NOMAD: PM(B)=(+102,+500) V=16.37 (??). B is physical, despite crowded field with N*=98. PM(A)=(-59,-3). PMS star, X-ray source RXS J090817.3-370649, variable CY Pyx. Tok2011a09084+2732 STTA 97 B is BD+28@1698. HJL 106. HJL1986 SHY 207. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical.09085+2141 A 2134 Appears to be same pair as 09085+2142 TDS6348; systems merged.09086-2550 RST2610 Possibly triple: the known companion RST 2610 at 1".7 with estimated period 500 yr is unlikely to cause the RV variability and dmu. Tok2012a AB: A is suspected SB, no orbit. Tok2014d09086-3843 RST1416 CPD-38@3012.09086-4841 LDS 251 B is CD-48@4456.09087-0835 KUI 38 19 Hya. A is a spectroscopic binary.09087-2159 RSS 191 CPD-21@411309088+2638 STT 567 AB: 75 Cnc. A is a spectroscopic binary. B is BD+27@1716. AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 75 Cnc Combined spectroscopic/astrometric solution, based on high-resolution echelle spectra plus archival PTI visibility measurements. Derived masses 1.173 +/- 0.024 and 1.011 +/- 0.021 Msun, distance 31.246 +/- 0.051 pc. Knc2010 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 2.13 +/- 4.27, 1.98, and 1.07 Msun, respectively. Mlk201209090+1728 ONL 1 OCC 238.09091-1820 VIG 12 Optical/physical nature of the faint companion is undefined. Vig201209094+2203 WRH 16 xi Cnc = 77 Cnc. Uncertain binary, unresolved by speckle interferometry. A long-period spectroscopic binary.09095+3854 OSO 26 G116-009. Common proper motion pair Oso200409097-4207 CPO 40 LDS 253.09098+1134 CHR 131 Suspected occultation binary.09099-3022 H N 96 eps Pyx. A is a spectroscopic binary.09103+2200 WRH 17 79 Cnc. Less than 0.1" 1954 (Finsen); not resolved by speckle despite Fin1954c numerous attempts 1976-1983. Binary nature uncertain.09104+6708 STF1306 sig 2 UMa = 13 UMa. See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d AB: H 3 54. MEv201009109+6331 H 5 73 H V 73. tau UMa = 14 UMa. A is metallic-line star and long-period SB. A: Ren & Fu (2013) calculated an astrometric orbit, combining Ren2013 Hipparcos Intermediate Astrometric Data with spectroscopic elements by Bretz (1961). Brz1961 AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200809109-4519 HJ 4186 LDS 255.09110+6331 tau UMa Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Bretz (1961). Brz196109110-1929 I 824 Spectrum: Fm delta Del.09111+1757 BPM 555 [PM2000] 930950 + [PM2000] 930951. Gvr201009112+0128 GIC 83 G046-026/G046-027.09115+2801 HJ 805 AB: HJL 107. HJL198609117-4653 SEE 110 Algol (EA) type eclipsing binary, P = 2.61362 d. Zas201109118+1617 BPM 556 [PM2000] 931498 + [PM2000] 931492. Gvr201009119+1803 STT 568 AB: 80 Cnc. BUP 124 BC: C is +18@2136.09122-2555 JNN 150 2MASS J09121259-2555025 has the alternative identifier CD-25 6962B in SIMBAD, implicitly implying companionship with the G2-type star CD-25 6962 at 14" separation. However, given the apparently very different proper motions of the components (e.g. Roser et al. 2010), Rsr2010 we consider such a companionship questionable. Jnn201209123+1500 FIN 347 Aa,Ab: pi 1 Cnc = 81 Cnc. 1981.358: This observation was incorrectly attributed to ADS 7158 by Tok1982a Tokovinin (1982a) (noted in Tokovinin 1982b) Tok1982b 1983.9371, 1983.9372: Interferometric observations indicate that Wor1983 Finsen's 1965 orbit (see Worley & Heintz, 1983) must be revised. Bnu1984 1990.9166: Residuals (4.0 deg in theta, 0".007 in rho) to the orbit of Hartkopf (1989) are only fair, due to a combination of large zenith Hrt1989 distance and close angular separation at the time of this observation. A combined astrometric/spectroscopic orbital solution is given by Mason et al (1996). Msn1996a Reversed Delta m and slightly larger parallax/smaller masses than in Msn1996a the speckle-spectroscopic study by Mason et al.(1996). Pourbaix gives combined solution for this resolved SB2, yielding orbital parallaxes and component masses. Pbx2000b Aa,Ab: Combined solution orbit. Mass_a = 0.983 +- 0.045 Msun, Mass_b = 0.903 +- 0.049 Msun, orbital parallax = 48.78 +- 2.36 mas. Msn2012a Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 1.80 +/- 0.25, 1.86, and 0.91 Msun, respectively. Mlk2012 BUP 125 AB: Due to the high proper motion of the A component, a later observation of this pair by Soulie was incorrectly entered as a new Sle1986a component, SLE 478AD. STT 569 AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 WIL 1 AE: CPM pair. Using data from 2MASS, Wilson et al. (2001) derive a Wil2001 spectral type of L8V and mass 40-74Mjup for the companion (called Gl 337C in that paper). They also note that the C and D components for the system appear to be background objects without CPM to the AB pair. BUG 16 Ea,Eb: Burgasser et al (2005) resolved the E component (called Gl 337C in the paper) into a 0.53" pair of near-equal magnitude. At a distance to the system of 20.5 +/- 0.4pc, the close pair has a physical separation of 10.9 +/- 0.6 au. Period of the pair is estimated at 140-180y. Primary is L8; secondary is possibly early- or mid-T dwarf. Bug200509124+2653 A 1977 1921-1922 elongation uncertain. Less than 0.1" in 1956.09125+4912 MET 54 This cannot be the close 20.0-d spectroscopic binary. Grf2013f09125-4337 FIN 317 Aa,Ab: FIN 317 is a close subsystem in the 2.9" AB pair HJ 4188. After discovery of Aa,Ab in 1951 at 0.116", Finsen (1951) was unable to Fin1951b resolve the star again on twelve occasions till 1968, except one other tentative measure in 1962. Yet the object was resolved by speckle in Fin1964a 1989.94 at 0.144" and in 2006.18 at 0.123". Despite orbital period of ∼50 yr estimated from projected separation, the sub-system was not . detected in 3 runs at SOAR (2009-2012), while the wider pair AB was measured. This may be yet another case of erratic measures and non-resolutions. Tok2012b09126+0915 HEI 483 This is apparently the same pair as HJ 121.09128+6141 STF1315 B is BD+62@1055. H N 79. MEv201009128-4329 HU 1456 Primary is GG Vel, Algol-type eclipsing binary, period 1.475216d. Zas201309128-6055 HDO 207 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 34.09 +/- 12.51, 5.38, 2.57 Msun, respectively. Mlk201209131+3633 ES 2106 BRT3251. Brt195109131-4128 CPO 41 LDS 258. A is CPD-40@3274, B is CPD-40@3273.09133+0540 WFC 81 HJL 108. HJL198609136+4659 STF1318 A is SB2, P = 2536d. B is SB? Tok2014d09138+4313 BAG 45 Primary is the rotationally variable star EI Lyn.09139+0252 H 6 108 B is BD+03 2171.09142-5021 HJ 4192 B is CD-49@4232.09143+6125 16 UMa SB2. 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 = 1.12 + 0.61, L/Lsun = 2.71 + 0.09, dm = 3.70 mag, log age = 9.78. WaX2015b Fekel et al. (2015) derive an astrometric orbit, with values of P, T, e, and omega adopted from their spectroscopic solution. The secondary is thought to be a mid- to late-K dwarf. Fek201509143-0817 BU 908 B is BD-07@2762.09144+5241 STF1321 Proper motion of A = -2530,-563; PM of B = -2559,-656 (UCAC2). B is BD+53@1321. A premature orbit has been computed. Both components are suspected spectroscopic binaries (Abt & Levy 1973). AbH1973 AB: NLTT 21249/21251 Chm2004 Epoch-2000 coordinates of C component 0914355+524209; current AC separation ~2'.2 at 64deg. PM of D +035-003.09144+0219 HJ 2489 the Hya = 22 Hya. A is a SB. AB: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy2008 AB: H 5 54. MEv2010 B and C optical. No earlier measures of D. B__1963b09149+0427 HEI 350 A long-period astrometric binary, now resolved.09150+1253 HJ 2490 BDS 4982, HJ 2487 same star.09151-0825 GCB 22 BRT 427. J 3248.09152+2323 BUP 127 AB: A is exoplanet host. Tok2014d STT 570 AC: Optical pair, based on study of relative motion of the components using the method of apparent motion parameters. Kiy200809152+1643 BPM 557 [PM2000] 934187 + [PM2000] 934230. Gvr201009156+0422 RED 17 2MASS J09153413+0422045. Confirmed as binary by Liu (private comm. to Reid et al). Spectral types L7 and L7 Red2006b09156-1036 MTG 2 LHS 6167. Estimated age 30-300 Myr; masses 0.15 +/- 0.04 and 0.09 +/- 0.03 Msun; a ~1.0 au. Jnn201409157-0114 STF1329 B is BD-00@2163.09158-3725 SEE 111 A is a spectroscopic binary.09161-4454 DON 329 Variable.09163+2730 SLE 484 No sign of Soulie (1986) pair. Measured pair is obvious double; error in Soulie (1986) coordinates? Sle1986a09167+1955 LDS5162 LDS5202. NLTT 21351/21352 Chm200409167-0621 KUI 40 23 Hya. A is a long-period spectroscopic binary. Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d Jones (1928). Jon1928c09167-2448 JNN 67 We resolve this star into a close binary (as yet unconfirmed through common proper motion). It was recently classified as a classical Cepheid based on light curve analysis (Christiansen et al. 2008 MNRAS 385, 1749). We assume that this is a mis-classification, given that the unresolved spectral type is M0.5V. Jnn201209167-5501 BRT3291 CD-54@2689.09168-2157 I 493 Too close, position angle uncertain.09169-0524 OSO 27 G161-009. Neither is a common proper motion pair, based on comparison with POSS2 red plates. Oso200409171+0717 STTA 98 AB: Pair appears in an appendix list, not part of discoverer's regular numbering sequence.09172-2249 J 1543 CD-22@7068.09173-6841 FIN 363 Speckle observations needed to refine relative orbit. AB: Hipparcos parallax 30.64 +/- 0.70 mas. Dynamical parallax 27.2 mas, masses 1.63 and 1.37 Msun. FIN 363 has an unusually short period of only 3.44 yr. The Hipparcos photometry is doubtful because of close 0.1" separation. Tok2012b AB: Martin et al. (1998) derive component masses 3.661 +/- 0.338 and 3.661 +/- 0.338 Msun. Mig1998 AB: Docobo & Andrade (2013) derive a dynamical parallax of 29.71 +/- 1.33 mas and component masses 1.43 +/- 0.25 and 1.06 +/- 0.20 Msun. See paper for extensive notes on this system. Doc2013d09175+7715 KUI 39 Proper motion of A -1059 -020. Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 0.66 +/- 0.23, 1.17, and 0.65 Msun, respectively. Mlk201209176+3641 ES 1734 OL 109 is the same star, according to Barton.09179+2834 STF3121 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 1.39 +/- 0.75, 1.57, and 0.85 Msun, respectively. Mlk201209179+1130 HJ 128 A is a spectroscopic binary.09180-5453 JNN 69 2MASS J09180165-5452332 has a close (~0.49") companion to which it is probably physically bound, although this still needs to be confirmed through common proper motion. Jnn201209182-0036 HJ 126 STF1337. Pettit refers to his 1915 observation as of HJ 126, but Ptt1917 gives the cryptic note "Hard to identify with H star 1820. P.A. too small, distance too great." It appears to be a measure of the HJ pair, but typographically mangled. Earlier catalogued as PTT 25.09184+3522 STF1333 Aka H 1 31. Bu_1906 Additional notes may be found in Fatou (1941). Fat194109184-2022 S 595 B is BD-19@2673.09186+5231 HJ 2492 AB: B is the faint nebula NGC 2800.09186+2134 ALP 15 2MASSW J0918382+213406 Physical companionship of C component to this ultracool dwarf ruled out based on i-z and z-J colors, using photometry from SDSS. The B component was not detected by SDSS; followup observations are needed to determine its nature. AlP200709186+1953 SKF 31 FAR 55.09188+3648 STF1334 38 Lyn. A is a spectroscopic binary. CHR 173 Ba. Abt & Biggs (1972) note variable RV. AbH1972 STF1334 AB: H 1 9. MEv201009188+2647 LDS6226 NLTT 21428/21426 Chm200409188-2250 DON1080 J 1544. ARA1764.09190+1742 83 Cnc Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based Gon2002a on a combination of ground-based catalogs with Hipparcos.09191-4128 CHR 239 Astrometric binary; dm 2.4 mag, period ~ 10y? Accelerated pm Tok2012b Omega for Tokovinin et al. (2014) orbit flipped by 180deg, at request of author. Tok2014a09192+5824 LDS1226 NLTT 21416/21397 Chm200409193+5230 VBS 15 Identified as BDS 5000, HJ 2492 (Van Biesbroeck). May be another pair. VBs999909193+3831 GIC 84 G115-068/G115-069 = Melotte 25 EGG 33AB = GJ 1122AB.09194-7739 KOH 83 Aa,Ab: Estimated masses 0.88 and 0.81 Msun; sep 6.8 au, period 14 y. Tok2010c HJ 4214 HIP 45734. Aa,Ab is a 0.1" pair KOH 83, also observed with NICI. B is SB2 without orbit. This is a PMS quadruple, both components are slightly above the MS. Tok2011a AB: B is X-ray source, SB2 (Desidera et al 2006 A&A 454,553) Tok2014d09196-3513 SWR 70 Giants, not dwarfs Skf200409197+0444 LDS3876 SLW 348.09198-1158 B 2529 26 Hya. 1936, 1938 position angles 139@-122@. Distance 3.0". Invisible 1948 B__1951a09200+0500 STF1343 HJL 109. HJL198609200+0103 J 2501 Radio galaxy UGC 4956. J__1962a09202+3518 RED 11 2MASSW J0920122+351742 2000.107: HST WFPC2 observations by Reid et al. (2001). Paper includes Red2001 mass and age estimates, as well as discussion of L dwarf binary frequency and semimajor axis distribution. Assuming a spectrophotometric distance of 24.3 +/- 5.0 pc, Konopacky et al. (2010) derive a system mass of 0.11 +/- 0.11 Msun. Kon201009203-0817 GCB 24 J 2898.09205+0752 BRT2148 OL 172.09205-0933 SHJ 105 27 Hya. A is a spectroscopic binary. Spectrum composite: G8III-IV+F5V. AB: SHY 540. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical. AB: H 6 85. MEv2010 Toyota et al. (2009) monitored the RV of the A component every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion echelle (precision ~10 m/s). The star exhibits a linear trend in RV, with a slope -30 m/s/y. Toyota et al. assert that these variations are due to an unseen companion. Assuming a circular orbit, period is estimated at 3400d; if the mass of A is 2.32 Msun, the minimum mass ~10 Mjup. Toy200909207+5116 ARN 71 AD: HJL1055. HJL1986 AD: SHY 208. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical.09210+3811 STF1338 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 2.01 +/- 0.61, 2.59, and 2.58 Msun, respectively. Mlk201209210+3643 STF1339 H 1 31. MEv201009210+3223 GIC 81 G047-035/G047-034. Typographical error led to this pair being originally entered in the WDS as 08211+3226.09210-0100 FOX 161 J 1546. Bal 859.09211+4155 LDS3878 NLTT 21509/21510 Chm200409213+3426 STT 571 40 Lyn STF1342 BC: H 4 55 = SHJ 369. MEv201009214+8123 STF1304 B is BD+81@288.09214+0248 BAL2361 J 2497.09215-4528 HJ 9003 Previously known as HJ 5452a.09216-0243 FIL 21 BAL 202.09218+4330 LAW 17 LSPM J0921+4330 = GJ 3554. Law et al (2008) derive a distance of Law2008 11.8 +5.6/-2.2 pc and a projected separation of 7.1 +3.7/-1.2 au. Estimated spectral types are M4.5 and M4.5. GJ 3554. Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.21 +/- 0.04 Msun; a ~14.8 au. Jnn201409219+1156 BPM 558 [PM2000] 939493 + [PM2000] 939496. Gvr201009223-3209 RSS 199 Primary is 12.9d SB1, Period of AB pair ~4700y. Tok200609223-5428 SHY 541 AC: HIP 45952 + HIP 45937.09223-5558 EVS 14 Primary is the Cepheid V Vel. Evs2016a09226+6251 MLB 203 HJL 110. HJL198609228-0950 A 1342 A magnetic and variable star, KU Hya, , 3.41d, 0.05V, is in the system. Mlr1956a See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Combined analysis using speckle, radial velocity, various magnetic field and polarization measurements. Wad2000 AB: Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses 5.13 +/- 1.94, 4.25, and 2.00 Msun, respectively. Mlk201209233+0330 STF1347 HJL 111. HJL198609234-0503 GIC 85 G161-019/G161-020. NLTT 21625/21628 Chm200409234-7753 HJ 4217 Agrees with Herschel's place but not his description. Daw1922 High proper motion of A accounts for the discrepancy. The companion is clearly UCAC4 061-008434 and not UCAC2 497073 (UCAC4 Whi2013 061-008429) as suggested by SIMBAD.09236-5454 HJ 4207 B is CPD-54@2239.09243-1601 LDS6227 NLTT 21682/21683 Chm200409243-3926 FIN 348 Hipparcos detects a magnitude difference, which reverses the quadrant of the prior measures, and indicates that nearly a revolution has been completed. Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 4.29 +/- 0.76, 5.18, and 1.66 Msun, respectively. Mlk201209247+2611 BU 105 kap Leo = 1 Leo kap Leo. Engelmann speaks of a 10" star in the direction 65deg. There is certainly no companion in this place, and no third star near in any direction. Bu_189409249+5134 STT 200 A is a spectroscopic binary.09251+2933 BU 1423 AC. Burnham's measure, X coded now, was actually a measure from NGC Dam2013 2893 to BD+30 1873.09252+4606 HDS1353 Cvetkovic et al. (2016) estimate spectral types K4 and M1, masses 0.72 and 0.43 Msun. Dynamical parallax is 25.49 +/- 2.78 mas. Cve2016b09252+1602 FAR 8 SKF 32. Primary is white dwarf WD 0922+162. Far2005b09253-4816 HJ 4209 B is CD-47@4921.09254+1137 BPM 559 [PM2000] 942111 + [PM2000] 942115. Gvr201009255+0009 LDS5703 LDS6228. LHS 2140.09256+6329 JNN 275 G 235-25. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13 +/- 0.02 Msun; a ~2.4 au. Jnn201409256+5401 STF1346 AB: H 2 73. MEv201009257+4626 LDS3889 NLTT 21701/21699 Chm200409257+3837 ES 298 Four-component system. The question of whether the CDB system is a hierarchical triple remains open. Kiy201209257-6958 HJ 4216 B is CPD-69@1061.09260+2839 A 222 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.59 +/- 0.66, 2.49, and 1.10 Msun, respectively. Mlk201209260-1535 CLZ 15 GWP1172. Tob2012b09263+5847 BUG 9 SDSS J092615.38+584720.9 Estimated spectral types are T4: + T4:, effective temperatures ~1330 and ~1330 K. Masses are estimated at 0.029-0.073 and 0.029-0.073 Msun, and the orbital period (assuming the semi-major axis = 1.26 * rho) is ~18yr. Bug2006a09265+7826 STF1326 SHY 542. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical. AB: CfA: A=SB? Tok2014d09265-6618 RST 404 CD-65@769.09266-3047 SWR 71 CPM pair Skf200409272-0913 A 1588 29 Hya.09275+5338 LDS3893 SLW 356.09275+1054 J 388 STF1354.09275-5806 CHR 240 Astrometric binary; dm 0.3 mag, period ~ 4y? Accelerated pm. Tok2012b09276-0840 H 6 111 AB: H VI 111. alp Hya = 30 Hya = Alphard. B is BD-08@2681. Primary unresolved in H alpha. Bla1977a09276-3500 B 2215 Last position angle uncertain. Needs speckle. Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d Astrometric binary; dm 1.5 mag, period ~ 1.97y Tok2012b09276-4311 SWR 73 A component is 0".6 CPM pair Skf200409278-0604 B 2530 There may have been a quadrant reversal about 1951. The 3-year spectroscopic motion does not seem to relate to the visual pair. Giant primary according to isochrone fit. Sod1999 Single line SB, P = 2.5 y, also a known visual binary. Primary is G2V, so companion should likely be a cooler dwarf; this seems to be confirmed from magnitude differences observed at 750, 550, and 450nm. Bag1984b 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 2.06 +/- 0.31, 2.44, and 1.00 Msun, respectively. Mlk201209281+1150 BPM 560 [PM2000] 944081 + [PM2000] 944114. Gvr201009283-7815 HJ 4226 B is CPD-77@520.09285+0903 STF1356 ome Leo = 2 Leo. Mlr1956a Chevalier identified this star as ome Leo, but gave incorrect Che1911 coordinates, leading to its initial designation as 09283+0903 CHE 137. Hrt2012b Giant primary according to isochrone fit. 1980.019: This observation of omega Leo by Weigelt (1983) was Wgt1983 incorrectly attributed to 09412+0954 = omi Leo in earlier editions of both the interferometric catalog and the WDS. As a result, omi Leo was incorrectly assigned the discoverer designation WGT 1. H 1 26. MEv2010 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 1.67 +/- 0.24, 2.14, and 1.27 Msun, respectively. Mlk201209285+0811 H 4 47 H IV 47. 3 Leo.09285-2426 B 181 Not seen 1959-1962. May exhibit rapid retrograde motion.09286+1721 BPM 561 [PM2000] 944368 + [PM2000] 944357. Gvr201009287+7834 LDS1696 MLR 524.09287+4536 S 598 41 Lyn = Intercrus. STTA 99. B is BD+46@1510.09288-0722 GIC 87 G161-033/G161-034. NLTT 21868/21870 Chm200409291-0246 HJ 1167 tau 1 Hya = 31 Hya. B is BD-02@2902. HJL 112. HJL1986 H 6 71. MEv2010 GJ 348. A is an X-ray source; also SB1, P=2815d=7.685y (Halbwachs et HJL2012b al. 2012) Tok2014d09292+0024 BAL1151 J 3292.09293-0409 GIC 88 G161-036/G161-037. NLTT 21891/21892 Chm200409293-4432 DUN 77 B is CD-43@5332. AB: SHY 210. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011 high (near 100%) probability pair is physical. EGN 11 Ba,Bb: Single epoch, but likely bound. If so, colors indicate Bb component is M0-M3 dwarf with mass 0.43 +/- 0.01 Msun. Egn2007 DUN 77 sp, dDEC 24.65". Dun182909297+0433 HJ 137 Also known as STF1361.09299-3629 HDS1364 AB + TOK 440BC: HIP 46572 is called a "high proper motion star" in SIMBAD, although its PM and RV are actually quite moderate. The binary AB has moved little in the 24 years since its resolution by Hipparcos. We discover the subsystem BC with an estimated period of ~100yr. Tok2015c09302+5339 TDS 538 Both A and B are eclipsing binaries. Lhr201509304-5822 RST 408 A is an irregular variable.09305+3822 LDS3899 NLTT 21915/21914 Chm200409306+1036 STF1360 AB: HJL 113. HJL198609307+4502 FLA 1 Also known as ES 2632.09307+3339 HJ 1166 7 LMi. STTA100 = H 5 69.09307-2724 SWR 75 CPM pair Skf200409307-4028 COP 1 psi Vel. Identification of ascending node not quite certain. See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 3.70 +/- 0.50, 2.42, and 3.00 Msun, respectively. Mlk201209308-1623 LDS 272 GWP1189. Tob2012b09308-3153 DUN 78 zet 1 Ant09309+4441 STF1358 B is BD+45@1729.09309+2658 LDS 909 AB: NLTT 21938/21941 Chm200409312+1407 BPMA 37 [PM2000] 946218 + [PM2000] 946038. Gvr201009313-1329 KUI 41 Ross 440. The primary is probably a flare star. Pair often unresolved, so orbit probably eccentric with P<10y. Kui1943 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 0.74 +/- 0.21, 0.80, and 0.30 Msun, respectively. Mlk201209314-0012 BVD 77 GWP1190.09315+6304 STF1351 23 Uma. The primary is a Delta Scuti-type variable. AB: H 4 29. MEv201009317+3830 AG 168 BD+39@2255a.09320+0943 SHJ 107 6 Leo. STTA101 = H 5 26. A is spectroscopic binary. B is BD+10@2015.09320-0111 CHR 174 tau 2 Hya = 32 Hya. A spectroscopic binary, now probably resolved. Abt & Biggs (1972) note variable RV. AbH197209320-6720 RSS 12 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. Rss199609321+3531 KU 97 AB: Same as KU 144.09322-6247 FIN 140 A is a Mira-type variable, R Car.09327+3458 ES 299 Erroneously identified as +35 2017. Dam2013 BC also known as POP 56.09327+2659 LDS3903 NLTT 22012/22015 Chm2004 LAF 38 Heinze et al. (2010) determine the C component is a background object. Hze201009327+0152 FIN 349 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic masses of 3.59 +/- 1.32, 3.23, and 1.22 Msun, respectively. Mlk2012 Omega for Tokovinin et al. (2015) orbit flipped by 180deg, at request of author. Tok2015c09327-2826 I 1616 B is CD-27@6693. B is variable.09328+0249 J 2498 Not found by Heintz at IDS position. Hei1985a09328-5706 SYO 1 Spectral type B6/7II/III.09329+5141 BU 1071 the UMa = 25 UMa. A is a spectroscopic binary. HIP 46853. See Allen et al. (2000) for information on metallicity, AlC2000 age, galactic orbital parameters, etc.09331-3908 JC 21 B is CD-38@5675.09333-3838 GLI 292 Also known as RSS 206. #110 in the original list of Gilliss.09334-0711 CBL 131 A: HR 3805. Ren & Fu (2013) calculated an astrometric orbit, combining Ren2013 Hipparcos Intermediate Astrometric Data with spectroscopic elements by Griffin (1981). Grf1981c A: 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 = 1.51 + 0.50, L/Lsun = 63.57 + 0.04, dm = 8.00 mag, log age = 9.45. WaX2015b