01000+5702 MLR 626 Also known as TDS1710.
01000-7234 OGL 123 SMC105.4.9983 + SMC105.4.11297 Pli2012
01001+4443 STF 79 164 And. Both A and B are spectroscopic binaries.
H N 45. MEv2010
01001+1246 GWP 113 XMI 164. Tob2012b
01001-7135 OGL 124 SMC109.2.10029 + SMC109.2.10470 Pli2012
01002+5809 SKF 56BC Aka MRI 25.
01005-1923 SHY 392 HIP 4702 + HIP 4833.
01006+6027 BAG 36 Primary is the alpha2 CVn type variable V551 Cas.
01006-7343 OGL 125 SMC107.4.12713 + SMC107.3.646 Pli2012
01007-7250 OGL 126 SMC105.2.10999 + SMC105.2.12098 Pli2012
01007-7328 OGL 127 SMC106.2.10337 + SMC106.2.11173 Pli2012
01008-7400 OGL 128 SMC107.2.7090 + SMC107.2.7244 Pli2012
01010-7154 OGL 129 SMC108.4.34907 + SMC108.4.34906 Pli2012
01011-7119 OGL 130 SMC114.5.140 + SMC114.5.363 Pli2012
01012+3704 BRT2585 ALI 254. Also known as TDS1720.
01012-5610 HJ 3412 B is CPD-56@199.
01013+1745 GWP 116 XMI 165. Tob2012b
01014+3535 COU 854 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.42 +/- 1.13, 2.60, and 1.10 Msun, respectively. Mlk2012
01014+1155 BU 867 Misidentified in BDS and ADS. Corrections by Baize and Couteau.
A premature orbit has been calculated.
01014-7120 OGL 131 SMC114.5.22 + SMC114.5.226 Pli2012
01014-7210 OGL 132 SMC113.7.22785 + SMC113.7.22807 Pli2012
01015+6922 A 2901 1984.9965: This autocorrelogram was remeasured; the new results are
listed in catalog.
01015+1024 GWP 117 XMI 166. Tob2012b
01016+5339 HJ 2008 01015+5339SMA 11
01016-1630 LDS9107 Old LDS6107.
01017+4635 A 927 BRT 75
01017+2518 HDS 134 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.80 +/- 0.47, 2.33, and 2.40 Msun, respectively. Mlk2012
A: Teff = 5625+/-75 K, log g = 3.75+/-0.25, R = 2.75+/-0.30 \rsun, AlW2014
Mv = 2.99+/-0.30, M = 1.60+/-0.20 \msun, L = 15.84+/-1.60 \lsun
B: Teff = 5575+/-75 K, log g = 3.75+/-0.25, R = 2.65+/-0.30 \rsun,
Mv = 3.12+/-0.30, M = 1.46+/-0.20 \msun, L = 15.83+/-1.60 \lsun
01018-0652 LDS 33 NLTT 3377/3378 Chm2004
01019+1405 GRV 984 Typo in original WDS designation - entered as 01010+1405.
01020+0214 LDS3221 LDS5310.
01020-7201 OGL 133 SMC113.6.22750 + SMC108.3.39755 Pli2012
01020-7304 OGL 134 SMC106.4.40341 + SMC111.5.15843 Pli2012
01021-1516 LDS9108 Old LDS6108.
01023+8153 KNT 1 A is an Algol-type eclipsing binary, U Cep, P =19.3d. There is
circumstellar matter.
01023+1131 PLQ 11 LDS1085.
01023+0552 A 2003 Close, 0.2" or under. Position angles show large changes. A premature
orbit has been computed.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.79 +/- 1.16, 2.45, and 1.05 Msun, respectively. Mlk2012
01024+0504 HDS 135 Mean motion indicates P ~ 80 yr, rho decreasing. Msn1999b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.13 +/- 0.11, 1.39, and 1.35 Msun, respectively. Mlk2012
WNO 50 AC: GJ 3071 + GJ 1027. CPM pair. Mkr2008
01025+0933 GWP 119 XMI 167. Tob2012b
01025-7353 OGL 135 SMC107.3.8839 + SMC112.6.180 Pli2012
01026+6221 WNO 51 GJ 49 + GJ 51. CPM pair. Mkr2008
01027+0908 RAO 39 RoboAO finds 2 companions - Optical? 2MASS: B at 32.4" 145.3d, below RAO2015
the MS, optical? Tokovinin & Lepine (2012) miss AB but list an optical Tok2012c
companion at 1733". Tok2014d
AB: A is SB2 with P = 26.2 days (Griffin & Suchkov 2003). The tertiary Grf2003
companion B at 2".8 did not move substantially in a year since its
discovery by Riddle et al. (2015), but the PM of the main component A RAO2015
is small and the astrometry is not conclusive. B is located below the
MS on the CMD, although still within the errors of its photometry.
Considering the small field crowding, we count B as likely physical. Rbr2015d
01028+3148 sig Psc Combined spectroscopic/interferometric solution (Palomar Testbed Knc2004
Interferometer) by Konacki & Lane (2004), yielding distance = 112.9
+/- 0.9 pc, masses 2.65 +/- 0.27 and 2.36 +/- 0.24 Msun, spectral
types B9.5V, diameters 0.16 and 0.15 mas.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 8.19 +/- 0.87, 5.71, and 2.40 Msun, respectively. Mlk2012
01028+0049 LDS5311 Error in WDS designation - incorrect precession of Luyten coordinates? Luy1984
01029+5148 BU 1161 Rectilinear solution by Rica & Zirm (2012). FMR2012i
01029+4702 GIC 17 G172-034/G172-035. The A component is the variable star V359 And.
NLTT 3437/3438 Chm2004
01029+4121 HJ 1064 39 And.
01029+0753 OCC 480 eps Psc
NPOI Limb-darkened diameter 1.74 +/- 0.10 mas, NOI1999
R = 10.9 +/- 0.8 \rsun.
01030+4723 STT 21 A may be a spectroscopic binary.
01030-0450 BUP 13 25 Cet.
01031-7358 OGL 136 SMC112.7.5 + SMC112.7.92 Pli2012
01032+7113 JNN 250 LHS 1182. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13
+/- 0.02 Msun; a ~2.7 au. Jnn2014
01032+6032 MLB 43 This is a physical pair, with relative motion much smaller than the
proper motions. Relative motion may be affected by a perturbation in
the radial direction with a period of 25y. Kiy2012
01032+2006 LDS 873 NLTT 3462/3463 Chm2004
01033-6006 HJ 3416 Spectrum F6/8III/IV.
01033-7123 OGL 137 SMC114.5.6465 + SMC114.6.10201 Pli2012
01035+5019 STF 83 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). USN2013a
01035-0535 RST4162 J 1442.
01036-5516 DLR 1 AB is a low-mass binary with masses 0.19 +/- 0.02 and 0.17 +/- 0.02
Msun. At a distance of 47.2 +/- 3.1 pc the projected distance between
the stars is 12au. They are orbited by an L-type companion at 84au,
which shares common proper motion. The companion is either a 12-13
Mjup planet (assuming an age of 20 Myr) or a 14-15 Mjup brown dwarf
(for an age of 50 Myr). Dlr2013
01036-7138 OGL 138 SMC114.7.13732 + SMC114.8.18665 Pli2012
01037+4051 LDS3225 AB: Also known as GIC 18.
BC: NLTT 3481/3482 Chm2004
BC: Aside from the companion seen in the AstraLux images, there is an
additional possible wide companion at 26" separation, as noted in the
WDS. The wide components have very similar proper motions (e.g. Roser XXX2010
et al. 2010), so actual companionship seems probable. Jnn2012
BWL 5 AD: Colors and/or astrometry are inconsistent with a late-type common
proper motion companion based on visual inspection of the field from
2MASS, SDSS, DSS1, and/or DSS2. Primary is G 132-50. Bwl2015
01037-3024 B 649 CI Scl, Algol-type eclipsing binary, P = 14.7104 d. Zas2011
B is a close 14.7-d spectroscopic pair. Tok2019a
01037-7138 OGL 139 SMC114.7.13496 + SMC114.7.13580 Pli2012
01037-7158 OGL 140 SMC113.5.9293 + SMC113.5.9288 Pli2012
01038+2232 J 874 J measures a pair 1912 - 1917: 345@, 3".
Measures and magnitude differences discordant. J__1949a
Companion has variable magnitude. Cou1952a
01038+0122 STF 84 26 Cet.
STF 84 AB: H 4 83. MEv2010
BU 1355 AC: 1909 and 1921 measures disagree. BDS 494 same star.
01039-7255 SKF1068 OGL 141. SMC110.8.23710 + SMC110.8.23860 Pli2012
01040+3528 HO 213 A premature orbit has been calculated.
01040-6409 B 1913 Spectrum composite: K0III/IV+A/F.
01040-7134 OGL 142 SMC114.7.14379 + SMC114.6.11666 Pli2012
01040-7401 OGL 143 SMC112.7.11 + SMC112.7.755 Pli2012
01041+4408 UC 493 Not a CPM pair. The A component is a close double, leading to a
spurious proper motion (Skiff, private comm.).
01042+2256 GIC 19 G069-044/G069-043.
NLTT 3529/3528 Chm2004
01044-0518 STF 85 Probably the same as STF 211 with a 1 hr error in RA.
01044-4703 UC 495 AB and BC are probably not CPM pairs. The proper motion of the B
component was effected by a nearby bright star (Skiff, private comm.).
01047+0401 GWP 126 XMI 168. Tob2012b
01047-3929 GJ 9037 Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from the Geneva
Extrasolar Planet Search Programs home page. HaI2001
01048+0135 A 2310 Position angles vary widely. A premature orbit has been calculated.
01048-0528 STF 86 AB: H 3 73. MEv2010
01049+3649 A 1515 Periods from 86 to 419yr have been calculated. Possibly ambiguous case
01050+2119 LDS3228 NLTT 3570. White dwarf pair = WD 0102+21 = EGGR 462/463 Grn1986
01050-7132 OGL 144 SMC114.3.186 + SMC114.3.569 Pli2012
01051+3814 J 1804 ALI 488.
01051+1457 HJ 1068 72 Psc. A is a spectroscopic binary.
01052+1250 HJ 10 Primary is eclipsing binary of Algol-type, period 1.62785 d. Zas2012
01053-7331 OGL 145 SMC111.8.20419 + SMC111.8.20441 Pli2012
01055+8315 MLR 482 Also known as TDS 39.
01055+4928 ES 1206 1deg error in IDS led to similar error in WDS designation.
01055+1523 STF 87 NLTT 3597/3598 Chm2004
The B component may be a spectroscopic pair. Tok2019b
01055-7215 OGL 146 SMC113.2.30 + SMC113.2.126 Pli2012
01056+4927 OSO 12 G172-038. Neither is a common proper motion pair, based on color and
comparison with POSS2 red plates Oso2004
01056-7342 OGL 147 SMC112.5.12714 + SMC112.5.12879 Pli2012
01057+3304 MLB 444 Rectilinear solution by Cvetkovic et al. (2017). Cve2017
01057+2128 STF 88 psi 1 Psc
AB: HJL 12. HJL1986
AB: SHY 395. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
AB: H 4 9. MEv2010
YR 6 Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 4.29 +/- 0.78, 4.29, and 2.19 Msun, respectively. Mlk2012
01058+0455 STF 90 77 Psc. STTA 10. B is BD+04@176.
AB: HJL 13. HJL1986
AB: H 4 68. MEv2010
01058-2618 HJ 2014 LDS 34. HIP 5140. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
01058-5959 R 5 B is CPD-60@75.
01058-7150 OGL 148 SMC114.1.170 + SMC114.1.1973 Pli2012
01060+6120 LDS3230 Old LDS6109. Due probably to a typo in the epoch-1900 IDS coordinates,
LDS3230 was originally listed in the WDS as 00055+6119.
01060+2456 BRT 122 J 2708. J__1955
01060+1111 BPM 21 [PM2000] 41785 + [PM2000] 41845. Gvr2010
01061-4643 SLR 1 bet Phe. Variable?
Quoted errors in P and a are +/- 5.0y and +/- 0.016", respectively. Ary2015b
01062+4508 BRT 76 Algol-type eclipsing binary, period 5.613460 d. Zas2019
01062+3211 S 393 sig 2 Psc
AB: H 5 16. MEv2010
01065+5325 ES 616 One degree error in WDS designation - should be +5425.
01065+0154 HDO 42 Doolittle may have measured a different pair (see ADS). A__1932a
01065-3055 LDS2167 NLTT 3662/3663 Chm2004
01065-3441 LDS9110 Old LDS6110.
01066+1353 SHY 396 HIP 5207 + HIP 4387.
01069-1408 GAL 306 Object #34 in Gallo's original list. Gal1912a
01071+1740 BPM 22 [PM2000] 42380 + [PM2000] 42414. Gvr2010
01072+5752 STI1537 Rectilinear solution by Hurowitz et al. (2013). USN2013a
01072+5330 H 4 66 H IV 66.
01072+3839 A 1516 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.62 +/- 0.59, 2.89, and 1.10 Msun, respectively. Mlk2012
01072-0144 STF 91 B is 2mag above the MS in (K,V-K), on MS in (J,J-K). Wrong 2MASS ptm.
The B component is possibly a SB. Tok2014d
01072-7121 OGL 149 SMC114.4.6097 + SMC114.4.6144 Pli2012
01073+0537 GWP 130 XMI 169. Tob2012b
01073-3452 COO 6 Rectilinear solution by Friedman et al. (2012). USN2012a
01073-7201 OGL 150 SMC113.3.21615 + SMC113.3.21614 Pli2012
01074+0101 LDS5315 Error in WDS designation - incorrect precession of Luyten coordinates? Luy1984
01075+4116 RAO 40 Primary is SB, P=49.480d. Estim. mass of B 0.26 Msun. Tok2014d
Triple system with inner 74.1 day spectroscopic pair (Gorynya &
Tokovinin 2014 MNRAS 441, 2316) and tertiary from Riddle et al. (2015) RAO2015
confirmed as physical by our photometry and astrometry. Observations
demonstrate that photometry of B given in 2MASS is biased by proximity
of bright primary, as in many other similar pairs. Their "unusual"
colors derived from the 2MASS photometry are thus wrong. Rbr2015d
01075+0244 GWP 131 XMI 170. Tob2012b
01075-4145 LDS9111 Old LDS6111.
01076+2257 LDS9112 AB: Old LDS6112.
NLTT 3723/3725 Chm2004
01078-4129 RST3352 ups Phe. Variable RV suspected. The lines are poor and show a scatter
of 40km/s without apparent relation to the visual motion.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.16 +/- 0.34, 2.78, and 2.09 Msun, respectively. Mlk2012
01079-7311 OGL 151 SMC111.3.12611 + SMC111.3.12798 Pli2012
01080+3915 RAO 41 Primary is SB, P=1713d. Tok2014d
01083+5455 WCK 1 Aa,Ab: mu Cas = 30 Cas. Proper motion of A +3424 -1596 (FK5).
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 0.01 +/- 0.01, 1.22, and 0.95 Msun, respectively. Mlk2012
mu Cas Aa,Ab: Astrometric orbit. Spectroscopic elements are somewhat
different from those of Lippincott: P = 23.0, T = 1954.0, e = 0.30, Lip1981
omega = 178.0 (Worek & Beardsley 1977). Bey1977
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
The pair has now been resolved by infrared speckle interferometry. Mcy1983
Pierce & Lavery (1985), Karovska et al. (1986), Haywood et al. (1992), Pie1985
and McCarthy et al. (1993) all compare their observations with Kar1986b
published orbits and discuss luminosities and masses of components, Hay1992
helium abundances, etc.
Hipparcos astrometric solution adopts some elements from the orbit HIP1997d
of Heintz & Cantor (1994). Hei1994b
CHARA Array Limb-darkened diameter 0.973 +/- 0.009 mas, CIA2008d
R = 0.791 +/- 0.008 \rsun, Teff = 5297 +/- 32,
L = 0.442 +/- 0.014 \lsun.
CHARA Array Limb-darkened diameter 0.972 +/- 0.009 mas, CIA2012e
R = 0.790 +/- 0.009 \rsun, L = 0.428 +/-0.007 \lsun,
Teff = 5264 +/- 32 K.
STT 551 AB: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
01083-3535 FAR 2 SKF 328. Primary is white dwarf WD 0106-358 = GD 683. Far2005b
01084+0539 BUP 15 80 Psc. B is BD+04@192.
STT 552 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01084-5515 RST1205 zet Phe. Also known as Wurren. Mam2017b
A is an Algol-type system, spectrum composite, P = 1.67d.
Both B and C are probably physical.
Ling (2004) gives a derived orbital parallax 0".01176 and a mass sum Lin2004a
of 7.41 +/- 5.85 Msun
01085+6331 OSO 13 G243-062. Not a common proper motion pair, based on comparison with
POSS2 red plates. PM of A = +1047 -91. Oso2004
01086+1652 GWP 135 XMI 171. Tob2012b
01086+1917 GWP 136 XMI 172. Tob2012b
01086-1011 BUP 16 eta Cet = 31 Cet. B is BD-10@239.
01088+6145 ES 1945 Aka OL 113.
01088-7119 OGL 152 SMC119.5.5 + SMC119.6.162 Pli2012
01089+4512 HJ 2018 AB,C : Same as STF 92.
01091-7225 OGL 153 SMC118.8.502 + SMC113.1.14118 Pli2012
01092-7127 OGL 154 SMC119.6.1012 + SMC119.6.1006 Pli2012
01093+6234 LDS5179 old LDS6113.
01094+3543 BUP9005 A component is NGC 404. Skf2013
01094+2949 ALP 4 2MASSW J0109216+294925
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in August 2002. AlP2007
01094+0457 GWP 138 XMI 173. Tob2012b
01094-5636 HU 1342 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.71 +/- 0.86, 2.48, and 1.27 Msun, respectively. Mlk2012
01095+4715 STT 515 phi And = 42 And. Measure of 1985.830 made by MAPPIT. Han1987
Scardia et al. (2001) orbit considered preliminary. The real period Sca2001d
is probably long (>400 yr). The Hipparcos parallax is 0".00443 +/-
0.00080, giving a mass sum of 6.9 Msun, slightly in excess for a
binary of spectral type B7Ve. The dynamical parallax is 0".0033, in
reasonable agreement with the measured one but not acceptable as it
leads to an exaggerated mass sum (16.8 Msun).
Calculated mass sum is 6.5 +/- 2.8 Msun, in reasonable agreement with
spectral types B6IV and B9V, although mass is not well-constrained. Mut2010b
01096+4635 ES 1300 Due to a typographical error in the ADS, the AE, AF, AG, AH, and AI A__1932a
components of 01097+3537 were added as additional components to this
pair (the AE and AI pairs as BAR 66, the others as ES 1300).
01096+2802 BRT 123 OL 149.
01096-0507 LDS9114 Old LDS6114. LIT 3.
NLTT 3847/3849 Chm2004
01096-0711 HDS 151 This binary displays clear common proper motion, but the residual
astrometry does not seem to follow a simple trajectory consistent with
only orbital motion of the two visible components. In addition, the
brightness difference is larger than the spectral type difference
would imply at a common distance. This could indicate that the A
component is itself an unresolved binary. Jnn2012
01096-4616 GAA 5 AI Phe.
Ma,Mb = 1.1941 +/- 0.0007, 1.2438 +/- 0.0007 \msun, GaA2019
orbital parallax = 5.905 +/- 0.024 mas.
01097+3537 BAR 1 bet And = 43 And = Mirach
Also, see note to 01096+4635.
01097+0856 GWP 139 XMI 174. Tob2012b
01098-2013 HJ 2023 Primary is CT Cet, a W UMa type eclipsing binary, P = 0.25649d. Zas2012
01099+1352 BPM 23 [PM2000] 44058 + [PM2000] 44035. Gvr2010
01100-7327 OGL 155 SMC111.2.5925 + SMC111.2.6033 Pli2012
01101+5145 STT 23 AB: HJL 14. HJL1986
01102+2447 POU 107 J 1805.
01104-7352 OGL 156 SMC112.3.6394 + SMC117.6.1318 Pli2012
01105+1326 BPM 24 [PM2000] 44379 + [PM2000] 44460. Gvr2010
01105+1019 GWP 143 XMI 175. Tob2012b
01107+8021 STF 89 B is BD+79@32.
01107-2800 SWR 1 CPM pair Skf2004
01108+6747 HDS 155 A spectroscopic double lined orbit has been determined as well. Grf2012d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.02 +/- 0.23, 2.18, and 2.52 Msun, respectively. Mlk2012
01108+5141 DOO 3 BDS 631.
01109+0934 HJ 634 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01111+5509 STT 553 the Cas = 33 Cas. A is a spectroscopic binary,
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01111+3125 STT 25 82 Psc = g Psc
01111-7228 SKF1069 OGL 157. SMC115.5.12 + SMC115.5.319 Pli2012
01112+4113 A 655 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.59 +/- 0.83, 2.76, and 0.95 Msun, respectively. Mlk2012
01112+3743 HO 215 45 And. Also single 1903, 1906 (Doolittle), 1907 (Aitken).
A measure by Schembor (1925.60, 117.8@, 155.5", 6 - 6) belonged to Sch1927a
01107+4256 ENG 4AB instead.
Duplicity of A is questionable.
01112+1634 GWP 144 XMI 176. Tob2012b
01114+1526 BEU 2 GJ 3076. WDS designation incorrected entered as 01224+1526.
Estimated age 10-20 Myr; masses 0.10 +/- 0.03 and 0.04 +/- 0.01 Msun;
a ~5.6 au. Jnn2014
01114-7225 OGL 158 SMC118.8.10104 + SMC118.8.10016 Pli2012
01114-7323 OGL 159 SMC116.7.144 + SMC116.7.143 Pli2012
01116+0446 GWP 146 XMI 178. Tob2012b
01116+1404 GWP 145 XMI 177. Tob2012b
01117+1205 LDS3242 NLTT 3967/3952 Chm2004
01119+0455 GIC 20 G002-027/G070-044 = GJ 3077A+3078B.
01120+0642 GWP 149 XMI 180. Tob2012b
01120+0955 GWP 148 XMI 179. Tob2012b
01120-7231 OGL 160 SMC115.5.9132 + SMC115.5.9369 Pli2012
01121+6111 KR 10 AC: Doolittle's published position angle was 91.9deg, which does not Doo1901
match anything in the field. However, an obvious star is visible at
the same separation but 90deg off his theta measure. It is assumed he
made an error when rotating his micrometer.
SMA9001 AD: Doolittle noted "a 13.5 mag. companion about 7" from A was Doo1901
suspected on two nights". It is assumed he saw the Smart companion. Sma1932
01121+4700 BU 236 Aka HJ 2024.
01121-7400 OGL 161 SMC117.7.58 + SMC117.3.98 Pli2012
01125+0228 STT 27 35 Cet
01126+1704 NAU 1 The primary is GU Psc, a likely member of the young AB Doradus Moving
Group. Spectral types are M3 +/- 0.5 and T3.5 +/- 1. Age of the system
is 100 +/- 30 Myr, distance 48 +/- 5 pc. Nau2014
01129+3205 STF 98 B is BD+31@196a. The primary is a double-lined spectroscopic binary,
P = 2.21d. B may also be an SB (Hube, PASP 93, 490; 1981).
AB: H 4 120. MEv2010
SEI 13. Nsn2017a
01130+3004 STT 26 A is a spectroscopic binary.
01131+2942 A 1260 Angle increasing, with a probable close approach about 1950.
01131+1141 HD 7275 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
01131-7215 OGL 162 SMC118.2.51 + SMC118.2.127 Pli2012
01132-7400 OGL 163 SMC117.7.3315 + SMC117.7.3338 Pli2012
01133-0152 HIP 5697 The SB1 orbit suggests mass ratio q > 0.2 and axis 0".21. The companion
is probably just a bit too faint or too close to be resolved with NICI. Tok2012a
01134-3932 SHY 397 HIP 5709 + HIP 5490.
01134-7251 OGL 164 SMC115.2.45 + SMC115.2.260 Pli2012
01135-3821 BRG 4 The primary star in the system is a known eclipsing binary with a
period of 0.4455 days (Parihar et al. 2009 MNRAS 395, 593). Since the
angular separation is inside of our inner cut-off, we count the system
as a binary here for the purpose of multiplicity statistics, although
it is really a triple system. To estimate the mass of the primary for
the purpose of deriving the mass ratio to the tertiary component
detected in our images, we use the sum of the masses corresponding to
individual spectral types M1 and M3 derived for the eclipsing binary. Jnn2012
ASAS J011328-3821.1, eclipsing binary of Algol-type, period 0.44559d. Zas2016
01136+2825 HJ 635 Previously erroneously listed as 01126+2825. Also known as GRV 73.
01137+2435 STF 99 phi Psc = 85 Psc. A is a spectroscopic binary.
01137+0735 STF 100 zet Psc = Revati.
Both A and B are spectroscopic and occultation binaries, B has P=9.08d.
AB: HJL 15. HJL1986
AB: H 4 8. MEv2010
BU 1029 BC: Delta m given in ADS is greatly overestimated. Wor1967b
BC: Rectilinear solution by Rica & Zirm (2012). FMR2012i
01137-5040 HJ 3421 B is CD-51@312.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01139+1004 GWP 154 XMI 181. Tob2012b
01141+1698 87 Psc Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Stickland & Weatherby (1984). Stc1984
01141+0634 LDS3248 LDS5323.
01142-4041 B 2554 Hipparcos suspected non-single.
01144-0755 STFA 3 37 Cet = LDS3250. B is BD-08@215.
NLTT 4123/4121 Chm2004
AB: GJ 9045 A+B. CPM pair. Mkr2008
AB: H 5 24. MEv2010
01144-7319 OGL 165 SMC116.3.3 + SMC116.3.954 + SMC116.6.11112 Pli2012
01145-0503 ROL 1 Primary is exoplanet host, periods 1275d, 4046d. Tok2014d
RGS 1 Aa,Ab: HD 7449 has a close massive planet (P = 1270.5 +5.92/-12.1d,
a = 2.33 +0.01/-0.02 au, mass >1.09 +0.52/-0.19 Mjup) as well as a
more distant stellar companion. The Ab component is likely an M4-M5
dwarf. Rodigas et al. (2016) estimate P = 65.7 +227/-56y, a = 17.9
+32/-12.9 au, i = 59.7 +20.1/-25.8 deg, mass = 0.23 +0.22/-0.05 Msun. Rgs2016
01146-7402 OGL 166 SMC117.7.3320 + SMC117.7.3907 Pli2012
01148+6056 BU 1100 The quadrant interpretation by Zulevic is less likely. Zul1972a
Muller corrected an error in his elements (Ephem. Cat. 1964). Mlr1955b
One component is a SB, P = 5.33d.
Only elements P, T, and a have been amended by Starikova (1977) from Sta1977a
the orbit of Zulevic (1972). Zul1972a
01148+4309 LDS3251 NLTT 4129/4124 Chm2004
01148-0058 BUP 18 38 Cet.
A is a blue supergiant with multiple pulsation periods. IAU2014e
AC: C component is galaxy NGC 442.
01149+3236 SEI 14 None of the components seen on POSS plate; may be flaws on AC Potsdam
plate. The current WDS companion at the position of Scheiner's triple
is probably unrelated to anything seen on the plates.
AC: SEI 15. Nsn2017a
01152-3419 LDS 837 LDS5325.
01153+6040 LDS5180 old LDS6115.
01153+2234 J 3226 BRT2304. Barton lists theta as 226.9; probably typo for 266.9. Brt1939b
01155+3745 SHY 121 HIP 5881 + HIP 6278.
A: Ren & Fu (2013) calculated an astrometric orbit, combining
Hipparcos Intermediate Astrometric Data with spectroscopic elements by
Nidever et al. (2002). They derived component masses 0.95 and 0.28 Nid2002
Msun and an estimated semimajor axis of 30.68 mas. Ren2013
01155+0216 CHR 195 First detected as an occultation binary by Evn1983a.
01157+0241 GWP 157 XMI 182. Tob2012b
01157+0032 LDS5326 Error in WDS designation - incorrect precession of Luyten coordinates? Luy1984
01158+4702 LAW 9 LSPM J0115+4702S. Law et al (2008) derive a distance of 18.7 +9.3/-3.6 Law2008
pc and a projected separation of 5.2 +2.9/-0.9 au. Estimated spectral
types are M4.5 and M5.
In addition to the companion detected with AstraLux, it can be noted
that 2MASS J01154885+4702259 has a very similar proper motion to the
star J01155017+4702023 at just 27" separation (Roser et al. 2010), XXX2010
which is itself a close binary (Law et al. 2008). Thus, this is a very Law2008
likely quadruple system. Jnn2012
01158+0947 A 2102 Quadrant change. Not seen 1948 - 1954.
01158-6853 HJ 3423 kap Tuc = LDS 42.
I 27 HJ 3423 and I 27, separated by 320", form the quadruple system
kap Tuc. The position of I 27 is 011501.0-684908 (2000). Sca1981a
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
01158-7224 OGL 167 SMC118.1.5565 + SMC118.1.6020 Pli2012
01160+5849 STI1550BC Aka MRI 29.
01160+1534 GRV 986 SLW 58.
01162-7246 OGL 168 SMC115.2.6083 + SMC115.2.6082 Pli2012
01163+1243 BPM 25 [PM2000] 47807 + [PM2000] 47744. Gvr2010
01163-2056 LDS 41 NLTT 4238/4239 Chm2004
01163-3217 LDS1091 LDS5327.
01166+7402 HJ 2028 STTA 13.
01166+1831 HDS 169 A: 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 0.28 Msun Lat2002
and an estimated semimajor axis of 14.81 mas. Ren2013
01166+1507 GWP 161 XMI 183. Tob2012b
01166-0230 BU 1358 39 Cet. A semiregular variable, AY Cet, and spectroscopic binary, P =
56.8d. Radio flares and soft X-rays are observed, and a white-dwarf
companion is revealed by IUE observations.
01167-7142 OGL 169 SMC124.7.387 + SMC124.7.163 Pli2012
01168+2643 BRT3257 Originally published as BRT 124. Brt1928
01170-7311 OGL 170 SMC116.3.7036 + SMC116.3.7122 Pli2012
01171+1739 BPM 26 [PM2000] 48328 + [PM2000] 48320. Gvr2010
01171-7355 OGL 171 SMC117.3.682 + SMC117.3.1102 Pli2012
01172+0930 GWP 164 XMI 184. Tob2012b
01172+0201 HDO 45 Rectilinear solution by Mason et al. (2012). WSI2012
01175+0131 GWP 165 XMI 185. Tob2012b
01176+4018 A 1521 Rapid change, but the measures are inadequate to define the motion.
01177+2647 BRT3258 Originally published as BRT 125. Brt1928
01177-7150 OGL 172 SMC124.8.4147 + SMC124.8.4560 + SMC124.8.4191 Pli2012
01178+4945 HU 520 Quadrant indeterminate.
01178+4901 HJ 2033 Ea : Also known as STF 102 ET.
01179-7314 OGL 173 SMC116.3.7181 + SMC116.3.7479 Pli2012
01180+0037 GWP 167 XMI 186. Tob2012b
01181+4707 A 937 North preceding and slightly brighter of a finder pair. Narrow
apparent orbit. B__1963b
01182+5742 STI1556 Rectilinear solution by Hurowitz et al. (2013). USN2013a
01182+1409 BPM 27 [PM2000] 48977 + [PM2000] 49004. Gvr2010