00000-1930 LTT 9831 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
00002+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__1950c
00003+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" FMR1999c
00006-5238 FIN 294 Spectrum: K1/2III+A/F.
00008+0630 GWP 2 XMI 101. Tob2012b
00011+6935 STTA253 B is BD+68 1417.
00011-2326 LDS2070 B is CD-24 17944.
00012-0005 TOK 359 Long-period SB. Tok2013b
00012-0312 LDS9082 Old LDS6082.
00013+6021 STTA254 A is the semiregular variable WZ Cas.
00013+0742 DU 4 HJL 325. HJL1986
00013-7012 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. Mlk2012
00016+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 Chm2004
00020+4530 J 864 BRT 1164.
-22s and +2.4' from BD+44 4541. J__1955
AC: CPM pair. J__1955
00022+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). USN2011a
00023+1609 BPM 1 [PM2000] 1692 + [PM2000] 1685. Gvr2010
00023+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. Tob2012b
00024+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 Chm2004
00026+6606 STF3053 B is BD+65@1988.
00026+1841 SHY 378 AB: HIP 201 + HIP 206.
00028+1647 BPM 2 [PM2000] 2010 + [PM2000] 1993. Gvr2010
00028+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). USN2012a
00031+0816 STF3054 B component is eclipsing binary of Algol-type, period 2.2604 d. Zas2012
00032+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__1963b
00032+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. Tob2012b
00034-2430 LDS2076 NLTT 53/54 Chm2004
00037+1851 GWP 7 XMI 104. Tob2012b
00037+1134 BPM 3 [PM2000] 2710 + [PM2000] 2680. Gvr2010
00037-2824 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. Fah2010
00038-1317 XMI 1 Rectilinear solution by Hurowitz et al. (2013). USN2013a
00042+6217 H 5 79 9 Cas.
00042-1008 LDS3116 NLTT 86/84 Chm2004
00044+5804 OSO 1 G217-030. No common proper motion pairs, based on comparison with
POSS2 red plates Oso2004
00045+0045 GWP 10 XMI 106. Tob2012b
00045+1851 GWP 9 XMI 105. Tob2012b
00046+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 Red2006b
00046-7745 LDS 832 Aka TVB 18.
00047+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. MEv2010
00049-1320 GAL 295 Object #1 in Gallo's original list. Gal1912a
00050+0835 GWP 11 XMI 107. Tob2012b
00051+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). Hrp1926
00054+1620 STTA255 B is BD+15@4934.
00054-2559 LDS3119 NLTT 158/159 Chm2004
00055+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. Mlk2012
00056-0141 LDS3012 NLTT 176/175 Chm2004
00057+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). Pal2013
00057+4549 POP 217 AP: Rectilinear solution by Cvetkovic (2011). Cve2011d
00057+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. BFr2015
00059+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. Tok2012a
00063+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 Tok2014d
00063-4905 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. Egn2007
00064+4501 UC 320 Aka BVD 170. Skf2013
00066+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. Jnn2014
00068-2106 RSS 41 CPD-21@1
00068-0853 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. BFr2015
00070+0303 GWP 14 XMI 109. Tob2012b
00071+6309 MLR 105 No significant movement since first resolution. Drd2009
00073+2058 HDS 12 Rectilinear solution by Hartkopf & Mason (2013). Hrt2013b
00074-2936 LDS2088 NLTT 296/295 Chm2004
00076+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). USN2013a
00076-2718 LDS2089 NLTT 307/308 Chm2004
00077+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. Jnn2014
00078+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 Chm2004
00080+3123 STTA256 B is BD+30@3.
00081+3240 HJ 610 SEI 2. Nsn2017a
00082+6217 HJ 1936 Optical pair, since relative motion reflects the proper motion of
component A relative to B to high accuracy. Kiy2012
00082+5933 STI 8 AB: 00083+5934SMA 3
00082+0937 LDS9085 Old LDS6085.
00083+1329 GWP 17 XMI 110. Tob2012b
00084+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. Doc2014h
00085+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. Ren2013
00088+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). USN2012a
00089+3257 SEI 1 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
00089+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. Jnn2014
00090+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. Ary2002b
00092+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 Chm2004
00093+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. Mlk2012
00093+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 Chm2004
00094+1415 CHE 1 Due to poor published coordinates, identification with the coordinates
in the WDS is uncertain. Chevalier's measure does not agree well with Che1910
others for this pair. Hrt2012b
00094-2759 BU 391 kap 1 Scl
00096+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. Tob2012b
00096+1047 GWP 21 XMI 112. Tob2012b
00096+1052 GWP 20 XMI 111. Tob2012b
00097+3107 GIC 3 G130-050/G130-049.
NLTT 433/431 Chm2004
00100+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. Zas2012
00100+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. Cve2014
00103+7231 HJ 1941 See note to 00138+7233BUP 2.
00104+5831 BU 253 Ba,Bb: Rectilinear solution by Rica & Zirm (2012). FMR2012i
00104+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. AlP2007
00106-7313 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). FMR2012i
00108-5729 HJ 3350 Primary is BL Phe, a Beta Lyr type eclipsing binary, P = 0.81035d. Zas2012
00109+4807 LEP 2 NI 1.
00109+1705 GWP 24 XMI 114. Tob2012b
00110+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 Chm2004
00113+0625 GWP 27 XMI 115. Tob2012b
00113-2045 LDS 1 G266-060. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 525/526 Chm2004
00114+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. MEv2010
00116-2748 LDS2099 kap 2 Scl
00117+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) HIP1997d
00126+2143 LDS 861 NLTT 589/592 Chm2004
00126+1118 BPM 4 [PM2000] 8713 + [PM2000] 8668. Gvr2010
00130+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. Jnn2014
00134+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. LBu1990c
00135-0009 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. Gvr2010
00138+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. Tok2014d
00138-7442 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). USN2013a
00139+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 Chm2004
00139-0429 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. BFr2015
00141+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. Msh2015
00143-0535 OSO 2 G031-036. Not a common proper motion pair, based on comparison with
POSS2 red plates Oso2004
00144+3609 LDS3140 NLTT 703/704 Chm2004
00144+1643 BPM 6 [PM2000] 9941 + [PM2000] 9955. Gvr2010
00144-1424 GAL 296 Object #7 in Gallo's original list. Gal1912a
00145-0747 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. Rss1996
00150+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. MEv2010
00150-7251 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). Jnn2012
00152+5947 FYM 153 Purported AJ pair removed on request of author. FyM2014b
00152+3642 LDS3144 pa error = 359 deg. RAO2020b
00152+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. FMR2014d
00152+2454 GIC 4 G130-059/G130-060.
00153+5304 GIC 5 G217-041/G217-040.
NLTT 739/738 Chm2004
00153+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. Gvr2010
00153+0936 GWP 30 XMI 116. Tob2012b
00153-4006 WG 2 B is CPD-40@14.
00154-1134 GAL 297 00153-1133SLE 251. Object #9 in Gallo's original list. Gal1912a
00155-1608 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. Mlk2012
00157+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. AlP2007
00159-0853 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. Nls2012
00161+0902 GWP 32 XMI 117. Tob2012b
00162+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). VBs1954
00162-7951 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. Shy2011
00164+5722 TDS1375 Aa,Ab: formerly 00165+5722, WDS designation changed when merged with
HJ 1011 into triple
00164+1950 LDS 863 AB: NLTT 803/804 Chm2004
00165-2805 LDS2107 NLTT 834/835 Chm2004
00167+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. Mlk2012
00169-5239 GC 333 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Bopp et al. (1970). Evn1970
00171+3841 CHR 123 theta And = 24 And
00171-1205 CBL 202 GWP 34. Tob2012b
00171-1406 GAL 298 Object #12 in Gallo's original list. Gal1912a
00172-1921 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. MEv2010
00174+0221 STF 21 HJL 3. HJL1986
00176+1300 HJ 3 HJL 4. HJL1986
00176-1113 GAL 299 Object #13 in Gallo's original list. Gal1912a
00177+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. Trn2008
00178+1620 TOK 646 Primary is 39 Psc. B is likely physical, as it moves in the same
direction as A in DSS2 image. Tok2014d
00180+2057 LDS 864 NLTT 912/910 Chm2004
00180+0931 AG 1 HJL 5. HJL1986
00182+7257 A 803 Quadrant uncertain. Wor1967b
00182+1209 GWP 38 XMI 118. Tob2012b
00183+1646 BPM 8 [PM2000] 12613 + [PM2000] 12602. Gvr2010
00184+4401 GRB 34 AB: Proper motion of A +2892 +412. Proper motion of B +2863 +336.
Premature orbits have been calculated. RV of star A possibly variable.
A component is eruptive variable GX And and B component is the
eruptive variable GQ 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. Kiy2008
00184+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 422
00190+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. Dju1954c
00192+0827 GWP 39 XMI 119. Tob2012b
00194-0849 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. Jnn2012
00197+0624 ZUC 5 Primary is white dwarf PG 0017+061 = PHL 790. Zuc1992
00199+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 360-154.62 = 205.38 deg instead. Hrt2012b
00200+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. MEv2010
00201+4244 OSO 3 G171-050. AB is not a common proper motion pair, based on astrometry
and color. Oso2004
LDS3151 AC: NLTT 1038/1036 Chm2004
00203-3246 B 1025 Considerable motion, but no measures for more than 30 years.
00204+1757 OSO 4 G032-012. Not a common proper motion pair. Oso2004
00206-2356 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 EvD2016
00206+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. Mlk2012
00207+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. CCA2007
00207+0738 GWP 41 AB: XMI 121AB. Tob2012b
GWP 42 AC: XMI 121AC. Tob2012b
00208+2737 CHE 7 MLB 674. Also known as ROE 116.
00210+6740 HJ 1018 STF 18. Mlr1955c
00210+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. Hrt2012b
00210-3219 BRT1578 A likely plate flaw. Grv2021b
00210-7429 OGL 1 SMC139.6.72 + SMC139.6.636 Pli2012
00211+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. Cab2007b
00214+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. Sca2000b
00214+2744 CHE 10 MLB 675.
00214-7355 OGL 2 SMC138.6.56 + SMC138.6.104 Pli2012
00215-6744 HJ 3361 CD-68@10.
00215-7407 OGL 3 SMC138.8.18 + SMC138.6.78 Pli2012
00216-7442 OGL 4 SMC139.8.20 + SMC139.8.81 Pli2012
00217+1301 BPM 9 [PM2000] 14913 + [PM2000] 14833. Gvr2010
00218+6628 STT 7 CD: Previously listed incorrectly as AB,E, with quadrants flipped to
275 deg.
00219+1706 BPM 10 [PM2000] 15011 + [PM2000] 15046. Gvr2010
00219-2300 HJ 1957 Designated as HJ 3429 in BDS. Bu_1906
00220+4913 BWL 3 AC and 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 GJ 3030. Bwl2015
00220+4231 RAS 16 Poorly-studied silicon star with weak magnetic field. Ras2014
00221+4822 J 9001 Was a measure of a new pair designated as J 2384.
00222-7439 OGL 5 SMC139.7.1570 + SMC139.7.1569 Pli2012
00224+1329 STF 27 42 Psc.
00224+0640 FR 2 V Psc.
00225+4456 A 648 Measure very doubtful. Not seen double on two later nights. B__1963b
00226+5033 KU 67 B is BD+49@62.
00226-3111 LDS 14 NLTT 1165/1164 Chm2004
00229+6214 ES 115 Primary is V745 Cas, a W UMa type eclipsing binary, P = 1.41057d. Zas2012
00229+5420 ES 42 ES 154.
00229-1213 BUP 6 9 Cet.
00230+6112 STI 43 HJ 1023.
00234+2624 CHE 17 AC: 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 should be -0'.2783. Hrt2012b
00234-0121 HJ 1961 J 1433.
00235-0343 LDS3160 AB: NLTT 1213/1214 Chm2004
00236+0947 KUI 3 LDS3162
00239+2930 STF 28 B is BD+28@55. The variable, double-lined spectroscopic binary
BD+28@54 may belong to the system. This was previously reported as
BD+28@49, but was corrected by Weis{2002, "F.G.W. Struve's StF2002
Double Stars (STF2000.0)"}
SHY 383. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
00240+3835 BUP 7 A is a Mira-type variable, R And.
00240-0329 BU 488 Due to poor published coordinates, Chevalier's measure of this pair Che1910
was originally added to the WDS as a new discovery: 00245-0327 CHE 23 Hrt2012b
00240-7300 OGL 6 SMC136.8.38 + SMC136.8.178 Pli2012
00241-7300 OGL 7 SMC136.8.41 + SMC136.8.408 Pli2012
00242+1505 GWP 44 XMI 122. Tob2012b
00242-1305 VOU 83 Also single in 1958. Star confused with HU 4 (00246). VBs9999
00242-7349 OGL 8 SMC138.6.4018 + SMC138.6.246 Pli2012
00243+5201 HU 506 Aka V746 Cas.
A premature orbit has been computed.
Single 1934, 1953. A is SB, P = 28d:.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Additional notes may be found in van den Bos (1963). B__1963b
Also provide a solution to the usresolved ~25d companion. Hmn2018
00244+1322 BPM 11 [PM2000] 16681 + [PM2000] 16731. Gvr2010
00245-1217 GIC 7 LDS 3163 = G158-073/G158-074.
NLTT 1262/1265 Chm2004
00247-2653 LEI 1 Paper includes orbit of BC pair and estimate of mass sum. Lei2001a
HST WFPC2 photometry was also transformed to standard Johnson B and V
and Cousins R and I filters, yielding the following magnitudes for the
A, B, and C components: Lei2000
------ A ----- ------ B ----- ------ C ----- filt
17.17 +/- 0.05 20.57 +/- 0.07 21.48 +/- 0.11 B
15.35 0.04 18.68 0.06 19.07 0.07 V
13.63 0.04 16.30 0.05 16.65 0.05 R
11.66 0.04 14.01 0.05 14.43 0.05 I
Seifahrt et al. (2008) determine mass sum of BC pair to be 0.157 +/- Sef2008
0.009 Msun; mass of A 0.115 +/- 0.010 Msun. They find no sign of the
fourth component reported by Henry et al. (1999). Hen1999
Rajpurohit et al. (2012) derive Teff, log g, radius, luminosity, and Raj2012
spectral type for the components of LHS 1070 using various models.
Mean values (assuming distance = 8.8pc) are:
Teff (K) log g radius (Rsun) log(L/Lsun) spec
A: 2950 5.3 0.136 -2.92 M5.5
B: 2400 5.5 0.102 -3.44 M9.5
C: 2300 5.5 0.099 -3.55 L0
Koehler et al. (2012) derive masses for the A, B, and C components of
0.172+/-0.010, 0.077+/-0.005, and 0.071+/-0.004 Msun, respectively. Koh2012
VLTI Limb-darkened diameter 1.149 +/- 0.11 mas, LTI2003a
M = 0.631 +/- 0.031 \msun, R = 0.702 +/- 0.063 \rsun,
T = 3520 +/- 170 K.
00247-5359 HJ 3364 B is CPD-54@89.
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). USN2012a
00247-7240 OGL 9 SMC136.6.12 + SMC136.6.115 Pli2012
00248+1925 BRT2296 J 2586.
00249+1355 GWP 45 XMI 123. SLW 18. Tob2012b
00250+2726 CHE 24 There was a 1' error in Chevalier's determination of declination. Che1908
In addition, there was a trigonometric error in deriving theta; the
correct value is 180deg - theta. Hrt2012b
00250+0600 GWP 46 XMI 124. Tob2012b
00250-7244 OGL 10 SMC136.7.2977 + SMC136.7.2975 Pli2012
00251+4803 CRZ 2 BDK 2. G 171-58 + 2MASS J00250365+4759191. Distance 42.2 +2.0/-1.8
pc for primary, 31 +/- 6 pc for secondary. Estimated ages of
components are discrepant: 1.8-3.5 Gyr for primary, versus 0.1-0.5 Gyr
for secondary. The primary is a spectroscopic binary resolved by Hip1997a
Hipparcos, the secondary a close (~10au) L4+L4 pair, resolved by Reid Red2006b
(2006). Fah2010
HDS 56 Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.30 +/- 0.21, 1.85, and 1.10 Msun, respectively. Mlk2012
RED 14 Ba,Bb: 2MASS J00250365+4759191. Spectral types L4 and L4 Red2006b
00251+1824 HJ 621 Rectilinear solution by Cvetkovic (2011). Cve2011c
00251-3646 BRG 2 Like BRG 1, this stellar binary also had an asymmetric PSF, and we
therefore calculated the photometry in the same way as for that case.
Note that the photometry values presented here should replace those in Brg2010
Bergfors et al. (2010). Jnn2012
00251-7432 OGL 11 SMC139.2.27 + SMC139.3.744 Pli2012
00253+3230 STF 29 SEI 4. Nsn2017a
00253-7446 OGL 12 SMC139.1.28 + SMC139.1.120 Pli2012
00254+2036 A 2301 J 219.
00254+0156 STT 8 44 Psc
00254-7404 OGL 13 SMC138.2.19 + SMC138.7.4092 Pli2012
00255-7334 OGL 14 SMC135.8.3096 + SMC135.8.3687 Pli2012
00256+1536 LDS9089 Old LDS6089.
00256-1849 HJ 1964 SEE 8.
00257-5050 HJ 3365 B is CD-51@102.
00259-0748 RIA 1 LHS 1074.
00260+0027 GRV 974 Aka SLW 21.
00260-0542 LDS3168 NLTT 1360/1359 Chm2004
00261-1037 GIC 8 LDS5273 = G158-077/G158-078.
NLTT 1370/1374 Chm2004
00261-7057 OGL 15 SMC137.5.17 + SMC137.5.19 Pli2012
00262-4217 alp Phe Alden's astrometric solution uses values of P, T, e adopted from the Ald1938a
spectroscopic orbit (Lunt 1924). Lun1924b
00263-4218 CRU9004 alp Phe = Ankaa.
00266-1924 ARA 515 Aka ITF 33.
00267-7220 OGL 16 SMC140.1.3576 + SMC140.1.3730 Pli2012
00268+0722 DOO 23 Doolittle calls this HDO 21, BDS 210. However, this seems to be a Doo1915b
different pair.
00268-3220 LDS2121 LDS5274
NLTT 1416/1412 Chm2004
00269-0531 SCJ 1 B is BD-06@72.
00269-7123 OGL 17 SMC137.8.790 + SMC137.8.846 + SMC137.8.1090 Pli2012
00269-8308 I 177 Spectrum of B is F.
00270+1705 BFR 3 HD 2292 + 2MASS J00265989+1704463. Baron et al. (2015) estimate
spectral types G5 and M9 +/- 1, distances 42 +28/-14 and 65 +4/-20 pc,
masses 1.05 -1.12 and 0.108-0.118 Msun. BFr2015
00270-7237 OGL 18 SMC136.3.1 + SMC136.6.2735 Pli2012
00271-0628 LDS3169 NLTT 1426/1425 Chm2004
00272+4959 STF 30 B is BD+49@89.
00274+3054 HDS 62 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Griffin (1979). Grf1979c
00274+0124 GWP 51 XMI 125. Tob2012b
00276+5120 COU2252 Transcription error resulted in 10' error in WDS designation.
00274+5130TDS1470
00276+1616 GWP 52 XMI 126. Tob2012b
00276-3157 I 438 BC: Rectilinear solution by Friedman et al. (2011). USN2011a
00276-7221 OGL 19 SMC140.1.4858 + SMC140.1.4878 Pli2012
00277+0936 GIC 9 G001-005/G032-021.
00277-1625 YR 1 Ma,Mb = 1.362 +/- 0.033, 1.073 +/- 0.024 \msun. GmJ2022
00277-7228 OGL 20 SMC136.4.4 + SMC136.4.17 + SMC136.4.36 Pli2012
00277-7300 OGL 21 SMC136.1.16 + SMC136.1.168 Pli2012
00278+1803 BPM 12 [PM2000] 18879 + [PM2000] 18873. Gvr2010
00278-7251 OGL 22 SMC136.2.4 + SMC136.2.19 + SMC136.2.207 Pli2012
00279+2220 FRV 1 LP 345-25. Assuming a parallactic distance of 13.19 +/- 0.28 pc
(Gatewood & Coban 2009), Konopacky et al. (2010) derive a system mass Gat2009
of 0.121 +/- 0.009 Msun. Kon2010
Dupuy et al. (2010) determine system mass 0.120 +0.008/-0.007 Msun;
spectral types are M7.5 +/- 1.0 and M8.0 +1.5/-1.0. LiM2010
00280-2654 LDS2123 DEA 22.
00281-0001 HJ 1970 Designated as HJ 1972 in BDS. Bu_1906
00281-2512 B 5 AC = LDS2124
00281-7329 OGL 23 SMC135.1.4464 + SMC138.3.12 Pli2012
00282-1030 GAL 300 Object #18 in Gallo's original list. Gal1912a
00283+6344 HU 1007 A premature orbit has been calculated. Motion direct. B__1963b
00283+1131 BPM 13 [PM2000] 19197 + [PM2000] 19238. Gvr2010
00283-7339 OGL 24 SMC138.4.5573 + SMC138.4.5757 Pli2012
00283-7427 OGL 25 SMC139.3.2443 + SMC139.3.2445 Pli2012
00284-2020 B 1909 Difficult visual system, with two components remaining within 0".2
of each other throughout the orbit.
Two orbit solutions (van den Bos 1956, Soedehjelm 1999). High- B__1956b
eccentricity, half-period solution fits equally well but gives Sod1999
too high mass-sum (with no third component allowed by q).
1982.7657 autocorrelogram remeasured; new results listed in catalog. McA1987b
Martin et al. (1998) derive component masses 1.563 +/- 0.177 and
1.238 +/- 0.151 Msun. Mig1998
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.14 +/- 0.32, 2.15, and 1.05 Msun, respectively. Mlk2012
00287+5801 MLB 107 WDS changed from 00293+5800, BC pair merged with STI1355
00287+1502 ALP 3 2MASSI J0028394+150141
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in August 2002. AlP2007
00288+5756 OSO 5 G217-052. No common proper motion pairs, based on comparison with
POSS2 red plates. Oso2004
00288+0251 HJ 623 C component is galaxy NGC 125.
00289+5023 DAE 1 GJ 3036 = G172-001
Daemgen et al. derive a distance of 17.4 +/- 4.5 pc, a separation of Dae2007
7.4 +/- 2.2 au, and a predicted orbital period of 40 +19/-18 yr.
Spectral types are M4.0 +/- 0.5 and M4.5 +/- 0.5; masses are 0.24
+0.11/-0.07 and 0.19 +0.07/-0.05 Msub.
00289+1835 BPM 14 [PM2000] 19589 + [PM2000] 19539. Gvr2010
00290-0933 GIC 10 G158-086/G158-087.
NLTT 1529/1530 Chm2004
00291+5752 MLB 39 STI 1359.
00291-0742 MLR 2 Speckle measures show rapid motion.
00292+7646 HJ 1967 Aka PKO 19.
00293-0555 SHY 384 AB: HIP 2292 + HIP 2350.
RAO 1 BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral
types of B and C as G8V and M1V. Rbr2015a
BC: The B component is of type G5V, with mass 0.87 +/- 0.03 Msun.
Based on isochrone fitting, Wittrock et al. (2016) estimate the mass
of the C component at 0.48 +/- 0.03 Msun, and type likely an M dwarf. Wtt2016
00293-7244 OGL 26 SMC136.2.2867 + SMC136.2.2890 Pli2012
00295+1413 BPM 15 [PM2000] 20020 + [PM2000] 19943. Gvr2010
00296-2845 LDS2130 NLTT 1581/1580 Chm2004
00297+5548 MLB 150 STI1361.
00300-0357 HJ 322 12 Cet.
00300-1058 GAL 301 Object #19 in Gallo's original list. Gal1912a
00300-1657 CHM 2 NLTT 1595 + 1598.
00300-6023 JSP 855 00301-6027TDS1494
00300-7257 OGL 27 SMC136.1.2934 + SMC136.1.3498 Pli2012
00301+2945 BU 1095 28 And. A is a Delta Scuti-type variable, GN And.
00301-3740 DAY 1 2MASS J0030-3739 + 2MASS J0030-3740. Dwarf / white dwarf binary.
Spectral types M9+/-1 + DA, Teff 2000-2400 + 7600+/-175K, masses
0.07-0.08 + 0.48-0.65 Msun. Minimum age of the system > 1.94 Gyr. Day2008
00302+5929 STI 79 Historical measures of STI1363 match STI 79 and have been included.
00304-0947 CHE 27 This pair has opened considerably since its discovery (from 9".6 to Che1910
19"), due to the considerable proper motion of the primary. AC2000
coordinates of both components from ~1901 are in good agreement with
Chevalier measure, so identification with this pair appears probable. Hrt2012b
00305-7237 OGL 28 SMC136.3.2481 + SMC136.3.2710 Pli2012
00306+4919 OL 86 Aka TDS1492.
00306+1442 OSO 6 G032-026. Not a common proper motion pair, based on comparison with
POSS2 red plates Oso2004
00306-7358 OGL 29 SMC133.7.1599 + SMC138.1.5656 Pli2012
00306-7242 OGL 30 SMC136.3.2599 + SMC136.2.3059 Pli2012
00307+3208 STT 11 B is BD+31@66.
00307-1545 HJ 1979 J 1435.
00310+3817 ALI 480 Also known as ES 2447.
00311+5648 ES 2 BDS 269 same star.
00311-7239 OGL 31 SMC131.6.14 + SMC131.6.859 + SMC136.4.2269 Pli2012
00312+0631 GWP 57 XMI 127. Tob2012b
00312-3041 LDS2132 NLTT 1669/1668 Chm2004
00312-6102 HJ 3372 CD-61@81.
00313-7311 OGL 32 SMC130.6.354 + SMC130.5.916 Pli2012
00314+3335 HJ 5451 STTA 2. A is a spectroscopic binary. B is BD+32@81.
HJL1004. HJL1986
00314+0158 LDS 865 Also known as GWP 59 or XMI 128. Tob2012b
00314-1113 GAL 302 Object #21 in Gallo's original list. Gal1912a
00314-4848 RST 11 lam 1 Phe. A is a spectroscopic binary.
00315-6257 B 7 A: bet 1 Tuc. A is a spectroscopic binary.
I 260 C: bet 2 Tuc
bet 1,2,3 Tuc form a sextuple system with cpm.
bet 3 Tuc (mag. 5.14, A2) is the close binary B 8.
SHY 114 AE: HIP 2484 + HIP 2578.
SHY 114 AF: HIP 2484 + HIP 2729.
SHY 114 AG: HIP 2484 + HIP 1481.
SHY 113 FG: HIP 2729 + HIP 1481.
SHY 117 FH: HIP 2729 + HIP 1993.
SHY 117 FI: HIP 2729 + HIP 1910.
SHY 113 GH: HIP 1481 + HIP 1993.
00316+1344 LDS9091 Old LDS6091.
00317+5057 LDS3175 Coordinate correction and estimate of secondary's proper motion by
Caballero (2013, private comm.)
00318+5431 STT 12 lam Cas = 14 Cas. A premature orbit has been computed.
Spectral types of primary and secondary assigned by ten Brummelaar et
al., based on adaptive optics observations. TtB2000
Corrections to Drummond et al. (2014) orbit: P=245.70 +/- 35.96y,
T0=2025.54 +/- 4.65 (Drummond, private comm.)
Uniform disk diameter 0.224 +/- 0.017 mas,
Limb darkened diameter 0.230 +/- 0.017 mas,
Teff = 12000+/-500 K based on LD although SED result (12800 +/- 500)
thought to be more accurate due to poor binary flux correction.
Radius is 2.31 +/- 0.20 \rsun. CIA2019a
00319+3705 BRT2584 ALI 248.
00319-2750 LDS2134 NLTT 1711/1713 Chm2004
00319-7318 OGL 33 SMC130.6.16 + SMC130.6.13 Pli2012
00320+1426 GRV 975 Aka SLW 29.
00321+6715 MCY 1 Aa,Ab: Discovery designation is per Todd Henry 03/02/98.
K-band magnitudes of components 6.42 and 8.44, derived masses are
0.377 +/= 0.030 and 0.138 +/- 0.007 Msun. Doc2008d
VYS 2 AB: ADS 433, MLB 377. The primary is an astrometric binary, P=16y.
Proper motion +1.723 -0.242. A premature orbit has been computed for
the visible pair.
Also a flare star, V547 Cas.
Woitas et al. (2003) give orbital solution and determination of Woi2003
dynamical masses for this low-mass M dwarf triple.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Solution includes mass determination. Woi2003
In the orbit catalog figure illustrating the Docobo et al. (2006) Doc2006g
orbital solution, B is plotted relative to the center of mass. These
adjusted measures were provided by Docobo (2007, private comm.) See
also further analysis by Docobo et al. (2008), who derive a mass for Doc2008d
the B component (K-band mag 7.88) of 0.177 +/- 0.014 Msun (see note to
MCY 1 pair above for masses of Aa and Ab components.)
GL 22 Ba,Bb: Andrade & Docobo detect a sinusoidal pattern in the motion of
the B component, which they attribute to a possible 4th component of
the system in a 15y orbit. Masses under this scenerio are 0.162 +/-
0.014 Msun for Ba and 0.0152 +/- 0.0053 Msun (16.0 +/- 5.6 Mjup) for
Bb (assuming a circular solution) or 0.0147 +/- 0.0027 Msun (15.4 +/- Ana2009
2.8 Mjup) for Bb (assuming an elliptical solution). The Bb component
may be either a giant planet or a brown dwarf. Ana2011
00321+0155 GWP 60 XMI 129. Tob2012b
00321-0511 A 111 Elongations and quadrant of AB doubtful. B__1963b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.48 +/- 0.34, 1.75, and 0.85 Msun, respectively. Mlk2012
00321-1218 HDS 71 Cvetkovic et al. (2014) derive spectral types G2 and G5, masses 1.11
and 1.05 Msun. Dynamical parallax is 14.06 +/- 0.62 mas. Cve2014
00322-1050 LDS3176 NLTT 1727/1715 Chm2004
00322-7515 HJ 3374 B is CPD-75@48.
00323-6304 LDS9092 Old LDS6092.
00324+7335 LDS1509 NLTT 1681/1680.
00324+0657 MCA 1 51 Psc. A is a triple occultation system, and a resolved
interferometric pair. B is BD+06@65.
First detected as an occultation binary by Africano. Afr1976
Mason et al. give Aa,Ab,B triple solution (double (Aa)-B in HIP). Msn1997a
Orbit mostly dependent on Hershey pc obs; more IR speckle needed. Hry1973
The Aa,Ab components of ADS 449 apparently went through periastron
some time during 1987-1990. Hrt1992b
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.08 +/- 0.46, 3.66, and 2.40 Msun, respectively. Mlk2012
STF 36 AB: H 4 70. MEv2010
00325+0101 GWP 61 XMI 130. GRV1160. Tob2012b
00326+5513 RAS 17 SrCrEu star at about 36 pc. Secondary likely close to solar (G2-G5). Ras2014
00326+2018 HJ 1982 52 Psc.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00327+7807 STF 34 HJL 6. HJL1986
00327+2312 BU 1310 AC: Rectilinear solution by Friedman et al. (2012). USN2012a
00327+0732 GWP 62 XMI 131. Tob2012b
00327-6302 B 8 Aa,Ab: bet 3 Tuc. CPM with bet 1 and bet 2 Tuc = B 7.
SHY 116 AB: HIP 2578 + HIP 2729. B component = F component of 00315-6257.
SHY 116 AC: HIP 2578 + HIP 1993. C component = H component of 00315-6257.
00328+2817 STT 14 A is a spectroscopic binary. Aka H N 76.
00329-7445 OGL 34 SMC134.1.90 + SMC134.8.2266 Pli2012
00330+4442 LDS9093 Old LDS6093.
NLTT 1759/1762 Chm2004
00330+0850 J 2710 -9s, -5' from BD+08 69. Declinaison augmentee de 2'. J__1955
00330-7335 OGL 35 SMC130.8.5777 + SMC130.8.5810 Pli2012
00331-7446 OGL 36 SMC134.1.223 + SMC134.1.542 Pli2012
00332+1902 GWP 63 XMI 132. Tob2012b
00332-7114 OGL 37 SMC132.7.12 + SMC132.7.25 Pli2012
00334+1418 LDS9094 Old LDS6094.
00334-7104 OGL 38 SMC132.6.11 + SMC132.6.191 Pli2012
00334-7407 OGL 39 SMC133.8.4148 + SMC133.1.95 Pli2012
00335+4006 HO 3 A premature orbit has been computed.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.60 +/- 0.55, 2.07, and 1.10 Msun, respectively. Mlk2012
00336+1712 GWP 64 XMI 133. Tob2012b
00336-0811 LDS 5280 B component of 00339-0813 LDS5281 found to be the A component of
LDS5280; pairs merged, with LDS5281 made AC pair (with quadrant flip).
00337-3500 HJ 3375 HIP 2663. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
00339+1748 GWP 65 XMI 134. Tob2012b
00340-7056 OGL 40 SMC132.5.883 + SMC132.5.916 Pli2012
00344-7252 OGL 41 SMC131.7.3527 + SMC131.7.4371 Pli2012
00346+6254 BU 108 AB: B component is SB, P=156.430d Tok2014d
00345-0433 STF 39 AB,C: H 4 76. MEv2010
00346-7105 OGL 42 SMC132.6.1065 + SMC132.6.1159 Pli2012
00349+2627 COU 548 Originally entered as AG 4.
00350+5636 ES 3 BDS 326 identical.
00351+8337 MLR 481 00356+8338HDS 80
00351+0209 RST5182 J 3281.
00352-0336 HO 212 13 Cet.
Visual primary is 2.1d SB1 (#27 in Batten et al., 1989) and may be a Bte1989
Delta Scuti-type variable.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
1979.5326: This measure was incorrectly attributed to ADS 2200 McA1982d
BU 490 AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
00353-0942 CHE 28 J 1437 = 00358-0942CHE 28
00356-7342 OGL 43 SMC133.4.124 + SMC133.4.3322 Pli2012
00357+0233 LAW 7 LSPM J0035+0233 = NLTT 1930. Law et al (2008) derive a distance of Law2008
14.5 +6.3/-2.4 pc and a projected separation of 6.8 +3.1/-1.0 au.
Estimated spectral types are M5 and M6.0.
00357-7055 OGL 44 SMC132.5.871 + SMC132.5.912 + SMC132.5.1085 Pli2012
00358+5241 GIC 11 G172-011/G217-059.
NLTT 1920/1921 Chm2004
00359-7429 OGL 45 SMC134.3.2988 + SMC134.3.3515 Pli2012
00360+2959 STF 42 Hyperbolic orbit by Hopmann. Hop1967
sigma = areal constant in the true orbit = 0.1432 arcsec^2/yr
q = periastron distance in the true orbit = 6".123
Hopmann made small but unspecified corrections to the node and
inclination before computing residuals and ephemeris. Fin1970b
All hyperbolic orbits rejected from Fourth Orbit Catalog Wor1983
A is a spectroscopic binary.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00360+0514 GWP 66 XMI 135. Tob2012b
00360+1040 GWP 67 XMI 136. Tob2012b
00361+3858 J 2711 ALI 723.
00363-3818 RST5183 A is a close 4.8-d spectroscopic pair. Tok2019a
00364-7313 OGL 46 SMC130.3.8754 + SMC130.3.8886 Pli2012
00365-0639 LDS3183 NLTT 1976/1977 Chm2004
00365-7246 OGL 47 SMC131.2.1420 + SMC126.6.896 Pli2012
00366-4908 LDS 21 A is a spectroscopic binary, P = 3.74d. B is CD-49@138.
SHY 118. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
B component is SB, P=22d Tok2006
00366-7435 OGL 48 SMC134.2.2429 + SMC134.2.2618 Pli2012
00367+1542 GWP 68 XMI 137. Tob2012b
00368+1605 KU 69 HJL 7. HJL1986
00369+3343 H 5 17 pi And = 29 And. H V 17. STTA 4. BDS 263, HJ 1030 identical.
A is a spectroscopic binary, P = 143.6d. B is BD +32@102.
MKT 1 Aa,Ab: Hummel et al. (1995) visual orbit is based on astrometry from MkT1995
the Mark III interferometer. Additional spectroscopic data yield
masses, luminosities, radii, effective temperatures, and distance.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Hummel et al. (1995). MkT1995
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 11.98 +/- 2.06, 11.18, 4.79 Msun, respectively. Mlk2012
RBR 3 Aa,Ac: PA for 2001.7424 observation is measured in zenith mode. If
data collected in equatorial mode, PA = 97.6. Confirmation of the pair
should establish the proper value for theta. Rbr2007
00372+7149 HDS 86 1997.7289: Large change in separation seen since Hipparcos epoch. Msn1999b
00373+5801 BU 1097 Spectrum composite; A2+K.
00373-2446 BU 395 Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
HIP 2941. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.79 +/- 0.29, 1.92, and 0.91 Msun, respectively. Mlk2012
YSC 170.
00374-2054 FAR 23 GJ 2010 = NLTT 2019. Primary is white dwarf WD 0034-211. Far2006
00374-3717 I 705 Many attempts, but only a few positive observations.
00374-3904 WHI 1 Other IDs uncertain; based on Simbad search using epoch-1950
coordinates 003456-392028 from White et al. (1991). Whi1991
00374-7243 OGL 49 SMC131.3.3943 + SMC131.3.4041 Pli2012
00376+1257 GWP 69 XMI 138. Tob2012b
00376+1547 GWP 70 XMI 139. Tob2012b
00378-7246 OGL 50 SMC131.2.5591 + SMC131.2.6860 Pli2012
00378-7413 OGL 51 SMC128.8.65 + SMC128.8.358 Pli2012
00379+1404 GWP 71 XMI 140. GRV1161. Tob2012b
00379-7256 OGL 52 SMC131.1.6657 + SMC126.7.785 Pli2012
00381-7127 OGL 53 SMC132.1.1336 + SMC132.1.1337 Pli2012
00381-7345 OGL 54 SMC128.5.115 + SMC128.5.276 + SMC128.7.9551 Pli2012
00382+0322 J 1042 BAL 1609.
00383-7124 OGL 55 SMC132.1.1263 + SMC132.1.1284 Pli2012
00384+0130 BAL 947 Probably ARG 47, BD+00@93.
00385+4300 LDS5176 old LDS6095.
NLTT 2053/2057 Chm2004
00386+4738 OSO 7 G172-016. Common proper motion pair Oso2004
00386+1420 GWP 72 XMI 141. Tob2012b
00386-2118 LDS2140 NLTT 2075/2062 Chm2004
00386-3903 WHI 2 Other IDs uncertain; based on Simbad search using epoch-1950
coordinates 003609-391934 from White et al. (1991), where pair is Whi1991
listed as possibly resolved.
00387-7431 OGL 56 SMC129.7.14 + SMC129.7.603 Pli2012
00388+3101 AG 430 B is BD+30@90.
Not confirmed using images from the Digitized Sky Surveys Oso2004
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00388-2506 HJ 1991 B is CD-25@235.
00389-2536 HJ 1992 B is CD-26@195.
00389-7248 OGL 57 SMC126.7.3 + SMC126.7.86 Pli2012
00391-7313 OGL 58 SMC125.6.23680 + SMC125.6.24279 Pli2012
00392+1329 GWP 73 XMI 142. Tob2012b
00393+3052 BU 491 del And = 31 And
A is a long-period spectroscopic binary, P = 15000d (?).
BTM 1 Aa,Ab: Bottom et al. (2015) resolve the spectroscopic binary del And
using the Palomar 5m and Stellar Double Coronograph. The physical
separation is 11.55 +/- 0.13 au; the spectral type of the companion is
estimated at K4 +/- 2. Btm2015
Aa,Ab: Gontcharov & Kiyaeva (2002) orbit based on combination of Gon2002b
ground-based catalogs with Hipparcos. They quote masses of 1.3+/-0.4
and 1.3 Msun for the two components, and estimate their spectral types
as K3III and white dwarf.
Mk III Limb-darkened diameter 4.12 mas. MkT1991
Mk III Limb darkened diameter 4.17 +/- 0.06 mas MkT2001
Mk III Limb-darkened diameter 4.136 +/- 0.041 mas MkT2003
NPOI Limb-darkened diameter 4.24 +/- 0.06 mas NOI2001b
00394+2115 STT 550 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
LUH 3 54 Psc. AC: Common proper motion for both components was determined
through comparison of relative location with that obtained by 2MASS.
The B component is determined to be a possible T dwarf (T7.5 +/- 0.5)
based on mid-IR colors and magnitudes. Age is determined to be 7 +/-
3 Gyr and mass of C component 0.051 +/- 0.014 Msun. Luh2007
The T dwarf is referred to by Luhman et al. as the "B" component,
either because the non-physical STT 550 was not considered, or the WDS
was not consulted. In any event, this component referred to in the WDS
hierarchy as "C" is sometimes called "B" in the literature.
CHARA Array Limb-darkened diameter 0.790 +/- 0.027 mas, CIA2008c
R = 0.947 +/- 0.032 \rsun.
00395+6151 STI 110 00394+6158MLB 378
00395+6002 HJ 1042 STI 111.
00395+1454 GIC 12 AB: LDS 868 = G032-037/G032-038.
NLTT 2126/2125 Chm2004
JNN 249 Ba,Bb: G 32-37B. Estimated age 300-1000 Myr; masses 0.33 +/- 0.03 and
0.19 +/- 0.01 Msun; a ~4.3 au. Jnn2014
00396+8445 HJ 1986 STTA 3. B is BD+83@11.
00398+6157 LAM 1 MLB 379. STI 114AC.
BDS notes AB measure 357deg, 69".87 - Burnham was unable to find any
pair that matched this separation - perhaps typo for 6".98?
STI 113 BD: Previously 00399+6158STI 113AB.
00398-1418 GAL 303 Object #23 in Gallo's original list. Gal1912a
00399+2126 STF 46 55 Psc.
00400+7652 STTA 5 B is BD+76@16.
00400+1336 BPM 16 [PM2000] 26418 + [PM2000] 26431. Gvr2010
00400+1016 PLQ 7 The A component has been resolved as a close spectroscopic binary. Tok2020h
00400+0106 GWP 74 XMI 143. Tob2012b
00401+5014 V523 Cas Multiple system including contact binary. Pribulla & Rucinski (2006) Pbl2006
estimate the mass of the contact pair at 1.130 Msun and the minimum
mass of the wider component at 0.31 Msun.
00403+2403 BU 1348 AC : Carries BU 1348 from ADS (562), despite earlier discovery by STF.
BC : AD equated with this component.
BC: Rectilinear solution by Mason et al. (2012). WSI2012
00403-0855 GAL 304 Object #24 in Gallo's original list. Gal1912a
Also known as FAB 3.
00403-7241 OGL 59 SMC126.6.564 + SMC126.6.565 Pli2012
00404+0722 OSO 8 G001-012. Not a common proper motion pair, based on comparison with
POSS2 red plates Oso2004
00405+5632 BU 1349 alp Cas = 18 Cas = Schedar
Mk III Limb-darkened diameter 5.4 +/- 0.4 mas. MkT1989
Mk III Limb-darkened diameter 5.64 mas. MkT1991
Mk III Limb-darkened diameter 5.72 +/- 0.08 mas
Mk III Limb-darkened diameter 5.608 +/- 0.056 mas. MkT2003
NPOI Limb-darkened diameter 5.60 +/- 0.06 mas, NOI1999
R = 42.1 +/- 1.7 \rsun.
NPOI Limb-darkened diameter 5.65 +/- 0.08 mas. NOI2001b
NPOI Limb-darkened diameter 5.903 +/- 0.036 mas,
R = 45.03 (+1.57- 1.68) \rsun, Teff = 4476 +/- 15 K,
L = 734.2 +/- 42.2 \lsun. NOI2023
H 5 18 AD: H V 18. Also HJ 1993.
AD: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AD: Rectilinear solution by Hurowitz et al. (2013). USN2013a
00405-1631 BU 109 B is BD-17@108.
00405-4829 LDS9096 Old LDS6096.
00405-7321 OGL 60 SMC125.7.29221 + SMC125.7.29234 Pli2012
00406-0023 ARG 48 BAL 646.
00406-1502 GAL 305 Object #26 in Gallo's original list. Gal1912a
00407-0421 HJ 323 B is BD-05@100.
00408+1618 GWP 76 XMI 144. Tob2012b
00408-7125 OGL 61 SMC127.8.10 + SMC127.8.21 Pli2012
00409+0810 GWP 77 XMI 145. Tob2012b
00409-7320 OGL 62 SMC125.7.29414 + SMC125.7.30547 Pli2012
00410+3257 SEI 8 Listed in ADS as both #565 and #580 (00420+3304POT 8)
00414-7124 OGL 63 SMC127.8.1547 + SMC127.8.2057 + SMC127.8.2076 Pli2012
00415+5550 GIC 13 G218-007/G218-008 = GJ 1015AB.
00416+2438 WRH 28 Hynek 1. Not certainly resolved by Wilson in 1949, but successfully
resolved by McAlister in 1980.
1983.9362: this (and presumably other) negative results may be due
to a delta m between 1.5 and 3. Bnu1984
00416-0934 GRV1162 SLW 36.
00416-5621 RNR 1 2MASS J0041353-562112. Spectral types M6.5 +/- 1 and M9.0 +/- 1.
Assuming age of ~10 Myr, component masses are ~30 and ~15 Mjup;
distance 50 +21/-10 pc, orbital period 126 +86/-37y. Rnr2010
00417-4729 LDS9097 Old LDS6097.
00417-7102 OGL 64 SMC127.6.1579 + SMC127.6.1681 Pli2012
00418-5630 HJ 3387 xi Phe. Variable.
00419+1751 A 2303 J 585.
00419+1341 JMS 1 BDK 3. NLTT 2274 + 2MASS J00415453+1341351. Distance 21 +/- 8 pc for
the primary, 31 +/- 6 pc for the secondary. Estimated age of system
4.5-8 Gyr. Mass of secondary estimated at 0.081-0.083 Msun. Fah2010
NLTT 2274 + 2MASS J00415453+1341351. Baron et al. (2015) estimate
spectral types M4.0 +/- 0.5 and M9.5 +/- 0.5, distances 23 +14/-9 and
40 +6/-12 pc, masses 0.207-0.272 and 0.076-0.083 Msun. BFr2015
00420-7306 OGL 65 SMC125.5.32790 + SMC125.5.33233 Pli2012
00422-7435 OGL 66 SMC129.2.448 + SMC129.2.992 Pli2012
00424+1721 BPM 17 [PM2000] 27917 + [PM2000] 27832. Gvr2010
00424+0410 STT 18 AB: Visual orbit (Grade 4) gives too large mass sum of 52 Msun. Tok2014d
00426-5407 HJ 3388 B is CPD-54@159.
00427-3828 HDO 182 lam 1 Scl
00427-6537 I 440 Probable rapid motion, as yet undefined by the measures.
Derived orbital parallax 0".00685, mass sum 4.91 +/- 2.94 Msun Lin2004a
00427-7409 OGL 67 SMC128.1.11 + SMC128.1.217 Pli2012
00428+3533 TOK 10 FF And. Primary is 2.2d SB2. Estimated period of visual pair 4400y.
G-solution in HIPPARCOS. Tok2006
This system is noted as being triple in Tokovinin et al. (2006), Tok2006
including a close spectroscopic binary pair with approximately 1.3 mas
separation and a likely wider companion at 11" separation. Due to
these separations however, it is counted as single for our purposes. Jnn2012
00429+2047 A 2205 A premature orbit has been calculated.
00431+3913 MLB1054 ALI 727.
00431+0707 OSO 9 G001-013. Not a common proper motion pair, based on comparison with
POSS2 red plates Oso2004
00432+0128 GWP 80 XMI 146. Tob2012b
00432-2146 LDS1078 SLW 39.
00432-3759 UC 427 CPM candidate confirmed physical by photometry (2MASS and V mags). Tok2013c
Spectral type of comoving secondary estimated as M0-1, mass 0.56 Msun. Mug2014
00434-0054 STF 53 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00434-5728 HJ 3391 eta Phe.
MRN 1 Aa,Ab: Marion et al. (2014) estimate the companion as K1V, at about
6.8au separation from the A0IV primary. They derive a minimum orbital
period of ~9.5y, consistent with an astrometric companion reported by
Makarov & Kaplan (2005). A followup K-band observation suggests Mkr2005
spectral type for the secondary of ~G5V. Mrn2014
00435+3351 BUP 241 AB: B is BD+32@120.
WEI 46 AC: Distances are 1321" and 1310".
00436-2354 LDS2147 NLTT 2383/2381 Chm2004
00437+7211 OSO 10 G242-065. Neither is a common proper motion pair, based on comparison
with POSS2 red plates Oso2004
00439+0946 J 2712 Not found by Heintz at IDS position. Hei1990b
00441+5655 MLR 625 Also known as TDS1589.
00441-7238 OGL 68 SMC126.3.2852 + SMC126.3.910 Pli2012
00442+3122 GRV 40 Aka HJL1007
00442+4614 STF 52 Primary is eclipsing binary V355 And (period 4.7184 day). Zas2010
00443-7439 OGL 69 SMC129.2.3173 + SMC129.1.2349 Pli2012
00444+3332 STF 54 STF 56.
SEI 9. Nsn2017a
00444+1235 HJ 6 AG 7.
00445-1715 B 2513 Probably BD-18@118.
00445-3607 B 640 Primary is CR Scl, eclipsing binary of W UMa-type, period 0.246537d. Zas2013
00446+4341 LDS5177 old LDS6098.
00446+2007 GWP 84 XMI 147. Tob2012b
00446-1856 LDS3195 AC: NLTT 2439/2437 Chm2004
00447+4817 BU 231 omi Cas = 22 Cas
Primary is a spectroscopic binary, P = 1033:d.
NOI 3 Aa,Ab: Hipparcos astrometric solution adopted some elements from the HIP1997d
orbit of Abt & Levy (1978). AbH1978
Koubsky et al. (2010) combined solution uses NPOI astrometric data NOI2010
together with radial velocities from the Dominion Astrophysical and
Ondrejov Observatories. The secondary appears to be of similar mass to
the primary, although the magnitude difference is nearly 3 magnitudes.
One possible explanation might be that the secondary is comprised of a
close pair of similar stars, possible early A dwarfs.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 6.12 +/- 2.94, 7.39, and 5.62 Msun, respectively. Mlk2012
00448+4202 LDS5178 old LDS6099.
00448+3940 ALI1011 MLB 810.
00450-7234 OGL 70 SMC126.4.9807 + SMC126.4.10299 + SMC126.4.10283 Pli2012
00451+0533 PLQ 8 BAL2993.
HJL 8. HJL1986
00451-7310 OGL 71 SMC125.4.14538 + SMC125.4.14830 Pli2012
00452+0015 LDS 836 AB: Primary is SB1, P=11.439d (Griffin 2002 Obs 121, 221). Tok2014d
00453+1019 STF 58 B is BD+09@85.
00454+1422 LDS1079 G032-046. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
00454-7413 OGL 72 SMC128.1.8607 + SMC128.1.10178 Pli2012
00455+1232 HJ 7 Rectilinear solution by Mason et al. (2012). WSI2012
00455-1253 BUP 8 18 Cet.
00456+3628 ALI 21 Astrographic Catalogue plate defect. Grv2023b
00456-7115 OGL 73 SMC127.2.1735 + SMC127.1.582 Pli2012
00456-7331 OGL 74 SMC125.1.37411 + SMC125.1.37410 Pli2012
00457+7459 H N 122 A: 21 Cas = YZ Cas
A is an Algol-type eclipsing and spectroscopic binary, P = 4.47d.
00457-1625 MLF 1 aka HO 624
00457-3510 LDS3191 LDS5294
00457-7401 OGL 75 SMC128.2.9138 + SMC128.2.10100 Pli2012
00458+5459 ARG 2 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00458-4733 HDO 183 AB: PMS star, X-ray source, rapid rotation, debris disk. Tok2014d
00458-7242 OGL 76 SMC126.3.12924 + SMC126.3.13758 Pli2012
00459+3347 LAW 8 LSPM J0045+3347 = NLTT 2511. Law et al (2008) derive a distance of Law2008
14.9 +7.0/-2.6 pc and a projected separation of 4.0 +2.1/-0.6 au.
Estimated spectral types are M4.5 and M5.5.
00459-7359 OGL 77 SMC128.2.9204 + SMC128.2.11627 Pli2012
00460+3626 HJ 627 ALI 22.
00460-7108 OGL 78 SMC127.3.1324 + SMC127.2.2113 Pli2012
00461-0539 LDS3199 NLTT 2540/2538 Chm2004
00462-2214 RST4155 Ma,Mb = 1.043 +/- 0.026, 0.990 +/- 0.024 \msun. GmJ2022
00462-7250 OGL 79 SMC126.2.15522 + SMC126.2.15521 Pli2012
00463+6517 HJ 1052 STI 124.
00463-0634 HDS 101 Cvetkovic et al. (2016) estimate spectral types F2 and F9, masses 1.56
and 1.20 Msun. Dynamical parallax is 9.22 +/- 1.22 mas. Cve2016b
00464+3057 STFA 1 STTA 6. B is BD+30@114.
H 5 123. MEv2010
00464-7332 OGL 80 SMC103.5.132 + SMC103.5.864 Pli2012
00466-7334 OGL 81 SMC103.5.4 + SMC103.5.25 Pli2012
00467+1335 BPM 18 [PM2000] 30523 + [PM2000] 30577. Gvr2010
00467-0426 LDS9100 Old LDS6100.
NLTT 2582/2586 Chm2004
00467-7228 OGL 82 SMC101.6.16943 + SMC101.6.16996 Pli2012
00468-5200 HJ 3398 B is CPD-52@91.
00469+0533 GWP 86 XMI 148. Tob2012b
00470+3848 ES 223 00471+3848ALI 729
00470-1152 CUD 1 AB: Component A is the central star of the planetary nebula NGC 246. Skf2013
Adam & Mugrauer (2014) estimate spectral type of B component as K2-K5,
mass 0.85 Msun. Ada2014
ADA 1 AC: Adam & Mugrauer (2014) detect an additional companion to the white
dwarf primary. Estimated spectral type is M5-M6, mass 0.1 Msun. All
components share common proper motion. Ada2014
00471+3800 J 2713 ALI 485.
00471-7304 OGL 83 SMC100.6.7164 + SMC100.6.7261 Pli2012
00473+2416 BUP 9 AB: zet And. A is an eclipsing and spectroscopic binary, P = 17.8d.
Mk III Limb-darkened diameter 4.4 +/- 0.5 mas. MkT1989
AC is probably optical.
Proper motion +758 -1146.
00474+5106 H 5 82 H V 82. STTA 7. B is BD+50@142.
00474+3314 BOW 1 Not found by Heintz at IDS position. Hei1990b
00474+1730 BPM 20 [PM2000] 30911 + [PM2000] 30961. Gvr2010
00474+1726 BPM 19 [PM2000] 30878 + [PM2000] 30861. Gvr2010
00474-7345 OGL 84 SMC103.7.16909 + SMC128.5.14891 Pli2012
00476+5533 TDS1614 WDS designation changed slightly when merged with STI1428 into triple
00476-1812 LDS9101 Old LDS6101.
00477+1253 STTA 8 LDS2796. B is BD+12@90.
AB: HJL 9. HJL1986
00479-2921 I 261 Rapid, but as yet undefined, motion.
1989.9437: Having had only one other measure in the last 35 years,
this pair needs further observation, especially since we appear to be
near periastron at this epoch.
00480+5127 STF 59 AB: H 1 40. MEv2010
00481-7234 OGL 85 SMC101.7.31055 + SMC101.5.77 Pli2012
00481-7348 OGL 86 SMC103.7.20241 + SMC103.7.6961 + SMC103.7.7536 Pli2012
00482+1737 GWP 87 XMI 149. Tob2012b
00482+1055 DAM 864 CD: GII 108.
00484+0517 HEI 202 The AB pair was seen on two photographic plates by Heintz, but the
companion was not visible on 164 other plates, nor was it seen on
repeated checks with a micrometer. The parallax plates also yield
large residuals, leading Heintz to suspect variability. Hei1984i
CHARA Array Limb-darkened diameter of A : CIA2012f
R = 0.6954 +/- 0.0041 \rsun, L = 0.26073 +/-0.00263 \lsun,
Teff = 4950 +/- 14 K, M = 0.753 \msun.
00486-2357 LDS 27 NLTT 2704/2705 Chm2004
00487+4619 SMA 10 A 1-deg error in WDS designation, apparently a typo in transcribing
coordinates from the original source.
00487+1841 BU 495 Hipparcos parallax of 0".01628 yields a mass sum of 2.14 Msun
with an uncertainty of 28%, agreeing well for a double star of
spectral type G0. The dynamical parallax is 0".0149, in reasonable
agreement with the measured one. Semi-major axis erroneously given
as 0.317; a = 0.617 matches Scardia's figure, so is assumed to be
the intended value. Sca2000b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.00 +/- 0.67, 2.30, and 1.05 Msun, respectively. Mlk2012
Quadruple system. The inner AB pair, BU 495, has an orbit with a 143.6
+/- 4.0 yr period (Scardia et al. 2000). The CPM component C at 152" Sca2000b
from AB was found by Tokovinin & Lepine (2012), who estimate the Tok2012c
probability of it being physical as 0.99. The component C was resolved
by Riddle et al. (2015) into a 0".67 pair Ca,Cb. The PM is too small RAO2015
to determine if the Ca and Cb share common PM, but the low density of
background stars and the small separation imply that the pair Ca,Cb is
physical. Rbr2015d
00487+0735 BUP 11 del Psc = 63 Psc
00489-7434 OGL 87 SMC104.8.5148 + SMC129.2.824 Pli2012
00490+4435 MCT 2 Initially entered into WDS incorrectly as 00490+5535.
GJ 3058. Estimated age 50-150 Myr; masses 0.22 +/- 0.10 and 0.18 +/-
0.08 Msun; a ~19.0 au. Jnn2014
00490+1656 BUP 12 64 Psc. A is a spectroscopic binary.
64 Psc Combined spectroscopic/interferometric solution by Boden et al. (1999) Bod1999b
yields P=13.824621 days, T=JD 2450905.984.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.51 +/- 5.01, 2.80, and 1.10 Msun, respectively. Mlk2012
00491+5749 STF 60 eta Cas = 24 Cas = Achird.
Proper motion of A +1141 -572. PM of B = +1105 -493.
A has been reported to be a Dob1927
spectroscopic binary, but this is not confirmed. Doberck, Pavel, and Pav1914
Harshaw measure attributed to BC, then later to BE, was actually to Hsw2004
another faint star; confusion was due to the high proper motion of the
B component and the long time span since the previous measurement.
Proper Motion of E -003-001, F -010+000, G +009-005, H -006-001
System has been discussed by van de Kamp & Flather. Kam1955
AB: H 3 3. MEv2010
AB: Additional notes may be found in Simonov (1937). Smw1937
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.58 +/- 0.85, 1.71, and 1.60 Msun, respectively. Mlk2012
AB: Raghavan et al. (2010) do not accept the astrometric sub-system as Rag2010
real. Tok2014d
CHARA Array Limb-darkened diameter 1.623 +/- 0.004 mas, CIA2012e
R = 1.039 +/- 0.004 \rsun, L = 1.252 +/-0.019 \lsun,
Teff = 6003 +/- 24 K, M = 0.972 +/- 0.012 \msun,
Age = 5.4 +/- 0.9 Gyr.
AD: Rectilinear solution by Hurowitz et al. (2013). USN2013a
00492+5720 A 921 Star C (mag. 14, 4.5") is probably physical.
00494-2313 PES 1 A : Teff = 5400 +/- 60 K, Age = 2.3 +/- 1.4 GYr, M = 0.856 +/- 0.014 Pes2019
\msun, R = 0.769 +/- 0.016 \rsun.
B : Teff = 1300 +/- 100K, R = 0.91 +/- 0.16 \rjup, M = 70.2 +/- 1.6
\mjup.
00494-7401 OGL 88 SMC103.8.8139 + SMC103.8.8451 Pli2012
00496-5410 HJ 3402 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00497-1841 B 2067 Primary is Hipparcos acceleration solution (G-code) binary. Is the
acceleration caused by the companion, or is it a triple? Companion
not measured by HIP, could cause false acceleration? 2MASS: another
companion at 6.6", 276.2deg is listed, likely bogus. Tok2014d
00497-7336 OGL 89 SMC103.6.31460 + SMC103.6.31513 Pli2012
00498+7027 ENG 2 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00499+3027 STTA 9 B is BD+29@139.
00499+2743 STF 61 65 Psc = i Psc
H 2 84. MEv2010
00500-0401 RST4158 J 1440. J__1941a
00501+1606 GWP 88 XMI 150. Tob2012b
00502+1604 GWP 89 XMI 151. Tob2012b
00502-7147 OGL 90 SMC102.4.11 + SMC102.4.92 Pli2012
00503+6235 MRI 32 FMR 35.
00503-7217 OGL 91 SMC101.4.18707 + SMC101.4.18866 Pli2012
00504+5038 BU 232 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.83 +/- 2.67, 2.70, and 1.20 Msun, respectively. Mlk2012
00505+7538 HJ 1997 B is BD+74@31.
00505+5930 LDS9102 Old LDS6102.
00505+2450 LDS3203 NLTT 2805/2804 Chm2004
00506-7328 RSS 2 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. Rss1996
00507+6415 MCA 2 A spectroscopic binary and resolved interferometric pair. Composite
spectrum: B9.5V+G0III-IV.
Combined spectroscopic/visual solution by Mason et al. (1997). Msn1997b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 9.12 +/- 1.74, 8.22, and 2.40 Msun, respectively. Mlk2012
00508+5123 OSO 11 G172-024. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
00508+3203 A 922 No observations 1932-69. Apparently has completed nearly a revolution.
00509+1215 GWP 91 XMI 152. Tob2012b
00511+2231 AZC 7 BC measure of 00511+2236LDS3204 now with this pair and decoupled with
the former LDS3204AB.
00511-7204 OGL 92 SMC102.2.129 + SMC102.2.1604 Pli2012
00511-7226 DBR 213 DBR 214.
00512+2211 KU 70 motion direct.
00513+5840 GIC 14 G218-015/G218-016.
00513-7413 OGL 93 SMC104.3.46 + SMC104.3.1506 Pli2012
00515+5630 DAL 11 RoboAO: 2 faint companions near B at 16.7" and 15.0", likely optical. RAO2015
Star in cluster IC 1590 (NGC 281 nebula) Tok2014d
Significantly different proper motion and parallax for components, so Jao2017
non physical.
00515-7225 OGL 94 SMC101.3.29657 + SMC101.4.5258 + SMC101.3.30856 Pli2012
00516+4412 YR 19 Aa,B: These observations were previously presented in Horch et al Hor2009
(2009, 2010). The data presented here are the result of a reanalysis Hor2010
using a trinary fit to include the close component YR 123Aa,Ab,
although the Aa,Ab component was not always of high enough quality to
include. In the course of reanalyzing these observations, it was also
noticed that the magnitude differences appearing in Horch et al (2011)
for the two filters shown were reversed. The values here correct that
error. Hor2011b
00516+2237 A 1808 Orbits with periods around 110y and a ~0.13" have been computed.
Motion direct.
Omega for Docobo (1988) solution corrected from 322.8 to 332.8 Doc1988b
degrees. Ruy1995
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.31 +/- 1.64, 5.27, and 2.88 Msun, respectively. Mlk2012
00516+0735 GWP 93 XMI 153. Tob2012b
00516-7354 OGL 95 SMC103.1.11891 + SMC103.1.11996 Pli2012
00517-1600 GWP 94 ABL 82. Tob2012b
00519+3750 GIC 15 G132-035/G132-036.
00519-1553 GWP 95 ABL 83. Tob2012b
00519-5921 HJ 3404 LDS 28.
00520+3353 HJ 628 Possibly the same a STF 66 with an error of 2 deg in dec.
00520+2035 GIC 16 G069-027/G069-029.
00521-1925 RSS 44 CPD-20@105
00522-2237 STN 3 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
00522-3534 BRT3373 A likely plate flaw. Grv2021b
00523-7224 DBR 236 DBR 237.
00523-7252 OGL 96 SMC100.4.53934 + SMC100.4.11604 Pli2012
00523-7350 OGL 97 SMC103.2.6804 + SMC103.2.6864 Pli2012
00524-6930 DUN 2 lam 1 Tuc. B is CPD-70@38.
SHY 390. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
Both A and B are above MS by 2 mag! The parallax can't be wrong. Tok2014d
RMK 1. Rectilinear solution by Letchford et al. (2018). LRR2018a
00527-2400 BU 734 A is a spectroscopic binary.
00528+5638 BU 1 This is a trapezium system (Abt 1986) which lies at the center of the AbH1986
ABH 5 cluster IC 1590 at a distance of 2.94 +/- 0.15 kpc (Guetter & Turner
1997 AJ 113, 2116). All four components were observed and appeared to
be single. Msn1998a
BU 1 AD: HJL 10. HJL1986
00528+0111 LDS9104 Old LDS6104.
00528-7308 OGL 98 SMC100.3.19805 + SMC100.3.19803 Pli2012
00529-0038 LDS 29 NLTT 2925/2926 Chm2004
00529-0856 LDS3208 NLTT 2931/2928 Chm2004
00531+6107 BU 497 A is a spectroscopic binary.
00533+0405 A 2307 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 7.12 +/- 2.18, 3.24, and 1.40 Msun, respectively. Mlk2012
00534-4114 CPO 24 LDS 30.
00535+2536 BRT 119 00535+2537POU 73
Primary an eclipsing binary of W UMa-type, period 0.345575 day. Zas2013
00535-0041 TOB 359 Pair found when 00536-0039HDO 38 misidentified. Dam2015c
00536-0039 HDO 38 Primary is galaxy LEDA 1137438.
00537+1758 GWP 97 XMI 154. Tob2012b
00537-3722 BRT1581 A likely plate flaw. Grv2021b
00537-7236 OGL 99 SMC101.2.48111 + SMC105.6.27571 Pli2012
00540-2503 HJ 3407 B is CD-25@344, spectrum F2V.
00541+2615 LDS3210 NLTT 2989/2990 Chm2004
00542+5108 HU 1018 Rectilinear solution by Scardia et al. (2017). Sca2017c
00543-7358 OGL 100 SMC107.7.2 + SMC107.7.62 Pli2012
00545+5619 CTT 2 B component is BD+55@196.
00545-7230 OGL 101 SMC105.5.24224 + SMC105.5.24308 + SMC105.5.25393 Pli2012
00546+3910 STF 72 B is BD+38@139.
00546+1911 STT 20 66 Psc. Wor1956b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.70 +/- 1.01, 4.39, and 2.57 Msun, respectively. Mlk2012
00547-6558 LDS9105 Old LDS6105.
00547-7129 OGL 102 SMC109.6.11 + SMC109.6.145 Pli2012
00547-7229 OGL 103 SMC105.5.24345 + SMC105.5.160 Pli2012
00548+0857 GWP 100 XMI 155. Tob2012b
00548-6727 GLI 7 B is CPD-68@33.
00548-7303 OGL 104 SMC106.5.28410 + SMC106.5.28476 Pli2012
00548-7358 OGL 105 SMC107.7.205 + SMC107.7.460 Pli2012
00549-3615 BRT1582 A likely plate flaw. Grv2021b
00550+5858 BU 1098 ups 1 Cas = 26 Cas
00550+2406 ENG 3 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
00550+2338 STF 73 36 And. One component is
variable. A combined photometric/polarimetric/speckle spectroscopic
analysis of this system was made by Tamazian et al. Tam2000
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Subgiant stars, spectral types G6 and K6. Calculated mass sum is 1.86
+/- 0.15 Msun, in reasonably agreement with these classifications. Mut2010b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.86 +/- 0.14, 2.29, and 1.35 Msun, respectively. Mlk2012
FOX 115 AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
00552-4724 CD-48 216 HD 5388 was known to have a companion thought to be a planet candidate
of minimium mass M sin i = 1.96 Mjup. Sahlmann et al. (2011) derive a
combined astrometric/spectroscopic orbit, using values of P,e,T, and
omega from the spectroscopic orbit of Santos et al. (2010 A&A 512,
A47). They determine the orbit is nearly face-on, yielding an
estimated mass for the companion of 69 +/- 20 Mjup. Thus it can no
longer be considered a planet. SaJ2011b
00552-7401 OGL 106 SMC107.7.14 + SMC107.7.241 Pli2012
00553-7318 OGL 107 SMC106.6.7246 + SMC106.6.7641 Pli2012
00554+4611 ES 1298 The angle for 1914 has been increased 100 degrees.
The 1914 Espin measure is probably in error by 100deg. Cou1955c
00554+1545 LDS2801 LDS3212.
00554+1253 GWP 103 XMI 156. Tob2012b
00556-4316 CBL 115 May be the omitted CPO 25.
00557+5748 ES 405 Motion for component B relative to A reflects the proper motion of A
to within the errors. Therefore, in spite of the fact the small proper
motions of these two components are similar, we consider their
physical relationship to be in doubt. Kiy2012
00557-7145 OGL 108 SMC109.8.11703 + SMC109.8.11918 Pli2012
00558-1832 B 645 Probable rapid motion, but little observed.
00559+5937 STI 146 Rectilinear solution by Hurowitz et al. (2013). USN2013a
00560-7155 OGL 109 SMC108.5.26777 + SMC108.5.26787 Pli2012
00561+5406 A 1259 Rectilinear solution by Rica & Zirm (2012). FMR2012i
00561-8237 WHI 3 Possibly resolved Whi1991
00564+0548 GWP 105 XMI 157. Tob2012b
00565+5928 ES 1709 STI 95 is identical Hei1983a
00566+1040 STF 76 ET Psc, W Uma (EW) type eclipsing binary, P = 0.439298 d. Zas2011
00566-1614 HJ 2002 Evidently a mistake in position angle by Herschel (HJ).
00566-5633 LPO 1 Spectral type G5?
00567+6043 BU 1028 gam Cas = 27 Cas
A is nova-like variable. Photocentric motion of (probably) the Aa pair
detected by Gontcharov et al. Gon2001
1975.636: Disk unresolved in H alpha emission and H beta. Bla1977a
Very small relative motion of B despite the high proper motion of A
reveals this as a common proper motion companion.
AD: The D component is the A component of 00568+6022. Mam2017
00568+6022 BU 1099 Theta for 1979.7703 incorrectly given as 308.6 in McAlister & Hendry McA1982d
(1982). Also, the measure for 1979.7730 was a spurious preliminary
measure of the observation on 1979.7703, and has been deleted.
The A component is the D component of 00567+6043. Mam2017
BAG 10 Aa,Ab: The primary is 4.24d SB2 (Young, Pub DAO Victoria 1, 287, 1921;
F.C. Fekel, personal comm.). HR 266.
Astrometric binary (P=4.85yr) discovered in residuals to speckle
data for 83-year AB pair (Cole et al. 1992), as well as in residuals CWA1992
to SB orbit.
The Ab component is a 4.2d pair consisting of a B9V and A7V. Tok2021b
00568+3830 HJ 1057 mu And = 37 And
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
00568+1525 GWP 106 XMI 158. Tob2012b
00568-7210 OGL 110 SMC108.7.49889 + SMC108.7.49890 Pli2012
00569+6152 HJ 1056 Aka STI 149.
00570+5729 ES 44 Not the same as 00591+5729STI1500
00570-7315 OGL 111 SMC106.6.41340 + SMC106.6.16701 + SMC106.6.15030 Pli2012
00572+2325 FOX 116 eta And = 38 And. A is a spectroscopic binary, P = 115.7d.
MKT 2 Hummel et al. (1993) orbital elements were derived from Mark III MkT1993b
interferometer astrometry. Combined with spectroscopy by Gordon (1946
ApJ, 103, 13) to yield masses and distance.
Errors are given as "error ellipses"; these values are tabulated
below. Columns include date (BY), major and minor axes of the ellipse
(mas), and ellipse orientation (deg):
1990.5359 0.57 0.04 107.1
1990.5687 0.12 0.02 105.8
1990.5742 0.17 0.02 105.2
1990.6125 0.43 0.05 102.7
1990.6262 0.12 0.03 98.5
1990.6426 0.09 0.02 96.9
1990.6563 0.08 0.02 93.3
1990.6591 0.06 0.01 85.7
1990.6646 0.24 0.02 81.0
1990.6673 0.06 0.02 82.2
1990.6728 0.09 0.03 100.6
1990.6837 0.61 0.09 78.9
1990.7056 0.08 0.02 92.4
1990.8233 0.08 0.02 98.0
1991.6037 0.22 0.04 105.1
1991.6557 0.10 0.02 88.5
1991.6584 0.12 0.03 98.1
1991.7077 0.10 0.03 96.5
1991.7104 0.08 0.02 99.7
1991.7132 0.05 0.01 84.4
1991.7460 0.08 0.02 84.3
1992.6413 0.19 0.03 85.5
1992.6441 0.56 0.05 96.3
Pourbaix gives combined solution for this resolved SB2, yielding Pbx2000b
orbital parallaxes and component masses.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.88 +/- 0.22, 5.02, and 2.63 Msun, respectively. Mlk2012
00573+6020 ARG 3 B is BD+59@149.
00573+2518 POU 79 LDS 871.
00573+1100 ITF 49 Aka ITF 94.
00574+2053 J 2587 BRT2300.
00576-7131 OGL 112 SMC109.3.163 + SMC109.3.288 Pli2012
00577+0441 GWP 107 AB: XMI 159AB. Tob2012b
GWP 108 AC: XMI 159AC. Tob2012b
00577-7326 OGL 113 SMC106.7.19223 + SMC106.7.12940 Pli2012
00578-7346 OGL 114 SMC107.5.14324 + SMC107.5.14471 Pli2012
00580-7306 OGL 115 SMC106.5.52673 + SMC106.5.51760 Pli2012
00586+4709 BRT 73 The 1893 observation differs substantially from modern observations.
Either the 1893 observation is erroneous (which we consider the most
probable), or there exist perturbations in the system. The question of
the physical relationship of this system remains open. Kiy2012
00587-7144 OGL 116 SMC109.1.23 + SMC109.1.460 Pli2012
00587-7207 OGL 117 SMC108.3.6583 + SMC108.3.6695 Pli2012
00588+1044 GWP 109 XMI 160. Tob2012b
00588-7149 OGL 118 SMC109.1.85 + SMC109.1.231 Pli2012
00589+3230 SEI 10 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
00589+0339 GWP 110 XMI 161. Tob2012b
00591+5824 STI1501 Rectilinear solution by Hurowitz et al. (2013). USN2013a
00591+5729 STI1500 Not the same as 00570+5729ES 44.
00592-1211 LDS3217 NLTT 3252/3253 Chm2004
00593+0706 GWP 111 XMI 162. Tob2012b
00593-0040 A 1902 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.23 +/- 0.70, 2.54, and 1.20 Msun, respectively. Mlk2012
00593-7142 OGL 119 SMC109.2.9765 + SMC109.1.13352 Pli2012
00594+0047 STF 80 B is BD+00@158.
AB: Additional notes may be found in Holden (1972). Hln1972
A: In addition to the linear solution for the resolved pair,
astrometric orbits have been computed for an unseen close companion to
A. Dommanget give two orbits calculated from perturbations seen to the
rectilinear motion. Dom1969
00595+3202 SEI 11 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
00596-0111 A 1903 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.31 +/- 0.60, 2.11, and 0.95 Msun, respectively. Mlk2012
00596-7549 GLI 8 B is CPD-76@82, spectrum G0/2V.
00598+0629 KUI 4 The primary is variable, WW Psc.
00599-7146 OGL 120 SMC109.1.13337 + SMC113.6.34323 Pli2012
00599-7208 OGL 121 SMC108.3.14363 + SMC108.3.15476 Pli2012
00599-7410 OGL 122 SMC107.1.178 + SMC107.1.218 Pli2012
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
T0 converted from negative to positive by subtracting from P. FMR2020c
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.
Measures attributed to this pair are actually of 01006+4719 = MAD 1. Mad1856
Error identified by Wilfried Knapp. Bu_1883
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
01064+3230 LDS3231 Aka RAO 184.
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
Aa,Ab : 0.7400 +/- 0.0122, 0.1728 +/- 0.0035 \msun, respectively. BdH2020
Age estimated as 12.7 +/- 2.7 Gyr.
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" are kap Tuc. Sca1981a
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Mass = 1.35, 0.88, 0.86, 0.80 \msun for A, B, C, D, respectively. Tok2020d
Teff = 6513, 5145, 5062, 4850 K for A, B, C, D, respectively.
Physical quintuple the period of A,CD is suggested to be ~270 kyr.
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
01182-7136 OGL 174 SMC124.7.4469 + SMC124.7.4898 Pli2012
01184-2332 LDS2182 Appears to be same as SKF1373. Primary is B component of 01183-2330
SKF1372; pair moved to become AC pair (with quadrant flip).
01185+7323 A 814 Not separated about 1951 (Van Biesbroeck). Possible quadrant change. VBs9999
01186+3855 GIC 21 G132-069/G132-068.
NLTT 4342/4337 Chm2004
01186-2255 FAR 24 Primary is white dwarf WD 0116-231. Far2006
01187-0052 HJ 5453 LDS 43. HIP 6130. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
AB: NLTT 4362/4361 Chm2004
EGN 1 Aa,Ab pair bound. Colors of Ab component consistent with M2-M5 dwarf,
with mass 0.24 +/- 0.01 Msun. B component is K7 dwarf and shares
CPM with A. C component is likely a background star. Egn2007
01187-2249 HDO 47 Probably = HDO 48.
01188+3724 STF 108 The A component is a spectroscopic binary.
01188-5637 RST 29 Spectral type G5?
01191-7215 OGL 175 SMC123.7.2850 + SMC123.7.2849 Pli2012
01192+5821 STI1560 B is BD+57@248. FMR9999
01192-4338 B 1423 Zurlo et al. (2013) estimate the period of this system at ~300y, in an
eccentric orbit with a semi-major axis of ~50au. The companion is
likely a white dwarf. Zur2013
01194+6418 MLB 186 TDS1841.
01194+1158 BPM 28 [PM2000] 49715 + [PM2000] 49656. Gvr2010
01194-7129 OGL 176 SMC124.3.274 + SMC124.3.22 Pli2012
01194-7246 OGL 177 SMC120.7.5025 + SMC120.8.5604 Pli2012
01194-7359 OGL 178 SMC122.7.221 + SMC122.7.232 Pli2012
01195+5816 ES 408 CD component also known as STI1562
01195+1850 GWP 169 XMI 187. Tob2012b
01195-7205 OGL 179 SMC123.6.2701 + SMC123.6.3359 Pli2012
01196-0520 A 313 Only elements P and T have been amended by Starikova (1977) from the Sta1977a
orbit of Heintz (1968). Hei1968a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.39 +/- 1.07, 2.59, and 1.10 Msun, respectively. Mlk2012
01197+1209 CHR 196 First detected as an occultation binary by Africano. Afr1975
01197-7203 OGL 180 SMC123.6.2671 + SMC123.6.3140 Pli2012
01198-0031 STF 113 42 Cet.
AB: Absolute quadrant for 1998.657 determined by triple-correlation
techniques. Pru2002b
A,BC. 1985.8430: This autocorrelogram was remeasured; the new results
are listed in catalog.
Star A (mag. 6.3, G8III) is in slow direct motion at 1.6" separation.
T incorrectly given as 1992.52 by Baize (1990); should be 1993.02 Baz1990a
(erratum noted in Inf. Circ. 111, 1990)
FIN 337 BC: 1982.7629, 1982.7657, 1983.7106: A mistake in reduction resulted in
90 degree errors for these three measures. McA1987b
BC: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.79 +/- 0.56, 3.32, and 1.20 Msun, respectively. Mlk2012
01198-7157 OGL 181 SMC123.5.2462 + SMC123.5.2499 Pli2012
01199+0350 CHE 29 BAL2084. Hln1972
01200+5747 STI1571 Aka LYS 5. Identity not recognized due to large pm affecting pa.
Rectilinear solution by Hurowitz et al. (2013). USN2013a
01200-1549 HJ 2036 A is an SB. Binary or triple? Tok2014d
01201+5814 H 3 23 H III 23. phi Cas = 34 Cas. A is a spectroscopic binary.
A quintuple system. C has spectral type B5/6Ia/be.
01201+3900 GIC 22 G132-071/G132-072.
NLTT 4410/4412 Chm2004
01203-0933 LDS9116 Old LDS6116.
01203-4841 HJ 3428 B is CD-49@378.
01204+0937 GWP 171 XMI 188. BVD 15. Tob2012b
01205+0418 J 1807 BAL 2085.
01205-1957 TOK 203 Two astrometric orbits are derived by Goldin & Makarov (2006), the Gln2006
longest one has P = 8.93 yr, axis 55 mas, and e = 0.84. Tok2012a
Retrograde motion by 4deg since first resolution in 2011. Goldin &
Makarov (2006) propose two orbits with periods ~9yr; semi-major axis Gln2006
should then be 0".15, so the system is near apastron. Tok2013b
01207+0333 GWP 172 XMI 189. Tob2012b
01207-7145 OGL 182 SMC124.1.101 + SMC124.1.545 Pli2012
01208+1127 AG 17 LDS 878. B is BD+10@167.
HJL 17. HJL1986
01208+1035 PLQ 13 B is BD+09@153.
HJL 16. HJL1986
01211+6439 S 397 35 Cas. STTA 15 = H 5 81. B is BD+63@175.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01211+1540 J 227 B is variable Cou1952a
01211+0736 SLE 257 The primary is a W UMa system, AQ Psc.
01211-0403 LDS3267 G 271-42.
01211-3508 LDS5330 Aka LDS9117 the old LDS6117.
01211-7251 OGL 183 SMC120.2.15 + SMC120.2.163 Pli2012
01211-7305 OGL 184 SMC121.5.2620 + SMC121.5.3200 Pli2012
01212+5159 NLTT 4450 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos
Intermediate Astrometric Data with spectroscopic elements by Latham et
al. (2002). They derived component masses 1.21 and 0.26 Msun and an Lat2002
estimated semimajor axis of 35.17 mas. Ren2013
01212+4108 LDS3266 NLTT 4468/4469 Chm2004
01213+1132 BU 4 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
The Hipparcos parallax (0".00616 +/- 0.00141) yields a mass sum of Sca2001d
4.7 Msun, in excess for a binary of type F1III.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 9.73 +/- 6.50, 3.62, and 1.64 Msun, respectively. Mlk2012
01215-2908 RUC 1 BE Scl. Spectral type of resolved companion estimated at G5-8V. Ruc2007
01218-2408 SEE 13 Motion direct. A premature orbit has been computed.
01219-4003 WG 8 BRT 643. Brt1933
01220+1848 GWP 175 XMI 190. Tob2012b
01220-6943 I 263 A premature orbit has been computed. Motion direct.
01221-2654 LDS2189 NLTT 4564/4566 Chm2004
01223+0331 DEA 38 NLTT 4558 + 2MASS J01221697+0331235. Baron et al. (2015) estimate
spectral types G5 and L2 +/- 1, distances 58 +/-3 and 43 +13/-40 pc,
masses 1.05 -1.12 and 0.071-0.076 Msun. BFr2015
01223-7332 OGL 185 SMC121.1.5 + SMC121.1.187 Pli2012
01226+1200 GWP 178 XMI 191. Tob2012b
01227+1410 GWP 179 XMI 192. Tob2012b
01227+0032 LDS3270 Aka WNO 42. G 70-55.
01227-7258 OGL 186 SMC120.1.13 + SMC120.1.32 Pli2012
01228-2440 BWL 63 Bowler et al (2013) derive the following properties: age 120+/-10 Myr,
distance 36+/-4 pc, masses 0.40+/-0.05 Msun and 12-14 or 23-27 Mjup. Bwl2013
01230-1258 GAL 307 LDS 46. Object #40 in Gallo's original list. Gal1912a
KUI 6 BC: BC shares CPM with A. B__1963b
01230-3035 LDS2190 According to Richard Jaworski the precise position he determine may be Jaw2006
correct if Luyten's original separation is off by an order of
magnitude (i.e., 11.8" rather than 118").
01232+4905 KU 8 HU 524.
01233+0152 LDS5332 CVR 26.
01233-0209 LDS3271 NLTT 4616/4615 Chm2004
01233-2105 LDS2191 NLTT 4626/4625 Chm2004
01233-7256 OGL 187 SMC120.1.3850 + SMC120.1.4139 Pli2012
01234+5809 STF 115 First measured by F.W. Struve in 1836 at an angular separation of Hrt1989
0".68, this system had opened to 1".2 by 1910, then steadily closed
to 0".35 at the time of the first speckle measurement in 1978.
The pair reached an apparent minimum separation of 0".01 in the
spring of 1984.
1983.7107 This autocorrelogram was remeasured; the new results are
listed in the catalog.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.36 +/- 0.67, 2.80, and 1.20 Msun, respectively. Mlk2012
01235-7356 OGL 188 SMC122.3.2 + SMC122.3.173 + SMC122.5.71 Pli2012
01236+3415 CRJ 4 NLTT 4619. The A component is SB, P=83.9d. Primary is G8IV. The 0.3"
companion is physically associated with primary, based on multi-epoch
astrometry. The estimated spectral type of the companion ~M1V, its
mass > 0.297 Msun. CrJ2013
01236+0753 GWP 180 XMI 193. Tob2012b
01237+3743 CIA 15 47 And.
Mass = 1.636 +/- 0.050, 1.587 +/- 0.049 \msun for A and B. CIA2020a
Radius = 1.84 +/- 0.05, 1.66 +/- 0.12 \rsun for A and B.
Teff = 7280 +/- 110, 7280 +/- 120 deg K for A and B.
Age = 1.0 Gyr, distance = 61.7 +/- 0.7 pc.
01237-6217 RST 31 Spectral type G0?
01239+0050 GWP 182 XMI 194. Tob2012b
01239-7228 OGL 189 SMC120.4.3345 + SMC120.4.3627 Pli2012
01240-0800 HJ 1079 44 Cet. A is a Delta Scuti-type variable, AV Cet.
01240-0811 BU 505 the Cet = 45 Cet.
01240-2933 LDS2192 NLTT 4676/4656 Chm2004
01241-1244 GAL 308 Object #42 in Gallo's original list. Gal1912a
01242+1254 HJ 13 C component is galaxy NGC 514.
01243+0426 GWP 183 XMI 195. Tob2012b
01243-0655 BU 1163 The system is also detected as a spectroscopic binary. B__1951a
Only elements P, T, and a have been amended by Starikova (1978) from Sta1978c
the orbit of van den Bos (1961). B__1961e
This system underwent periastron in late 1988, an event now covered by
speckle observations. Hrt1992b
A combined visual-spectroscopic orbit by Morbey (1975) gives almost Mrb1975
the same elements, but in the representation of position angles Sod1999
Soderhjelm's elements are preferable.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.59 +/- 0.41, 2.74, and 1.30 Msun, respectively. Mlk2012
01245+3902 STTA 17 B is BD+38@256.
D is BD+38@253.
01245+1740 BPM 29 [PM2000] 52622 + [PM2000] 52637. Gvr2010
01245-2839 LDS2194 NLTT 4694/4695 Chm2004
01245-3356 JAO 1 Aa,Ab: GJ 2022 = G274-024
Daemgen et al. derive a distance of 12.6 +/- 2.3 pc, a separation for
the AC pair of 26.0 +/- 4.8 au, and a predicted orbital period of 330
+95/-93 yr. Spectral types for both components are M5.0 +/- 0.5;
masses are 0.14 +0.03/-0.02 and 0.13 +0.03/-0.02 Msun. Dae2007
01246+5311 ES 2583 B is BD+52@332.
01247-7402 OGL 190 SMC122.2.45 + SMC122.2.104 Pli2012
01248-2614 RST1218 LDS 3277.
NLTT 4714/4713 Chm2004
01250+1424 GWP 185 XMI 196. Tob2012b
01251+4537 A 939 Recent observations seem to rule out Muller's short-period Mlr1955a
alternative.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.54 +/- 1.99, 3.23, and 1.45 Msun, respectively. Mlk2012
01252-0412 HJ 638 01252-0409BU 1361
J 1445. Nsn2016
01252-7954 HJ 3443 B is CPD-80@23.
01253-5930 HJ 3435 B is CPD-60@111.
01254+0227 GWP 186 XMI 197. Tob2012b
01256+3133 STT 30 AC: HJL 18. Aka MAD 9. HJL1986
AC: SHY 402. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
STTA 18.
B is above MS (wrong ptm), while A and C are on it. C is SB2, HJL2012b
P=14.908d (Halbwachs et al. 2012) Tok2014d
01256+2331 TOK 11 Primary is 5.4d SB1. Estimated period of visual pair 880y. Tok2006
01257+0258 J 1899 BC: Error in coordinates listed in Jonckheere (1941), star is at J__1941a
1h 23.2m, not 0h 23.2m. Star of mag 7.3 at 131" is BD+02 207. J__1952
01257+0107 GWP 188 XMI 199. Tob2012b
01257+0611 GWP 187 XMI 198. Tob2012b
01258+6014 BUP 19 del Cas = 37 Cas = Ruchbah. A spectroscopic and (perhaps) eclipsing
binary.
01259+6808 BU 1101 psi Cas = 36 Cas.
H 5 83 H V 83, SHJ 18, STF 117. C is BD+67@124.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01260+1450 BPM 30 [PM2000] 53515 + [PM2000] 53480. Gvr2010
01261+0925 GWP 189 XMI 200. Tob2012b
01261-2618 SWR 2 CPM pair Skf2004
01262+3435 WSI 96 Provisionally designated WSI9101. Tok2010
The initial observations of WSI 96 by Mason et al. (2011) are Msn2011d
considered spurous. The pair resolved by Roberts et al. (2015) using
AO is believed to be a different pair, whose magnitude difference
would have been beyond the dm limit of speckle. The original WSI 96
designation was retained, however. Spectral types of the components
are estimated as F7V and M2V, masses as 1.4 and 0.4 Msun. Rbr2015b
01263+0711 LDS9118 Old LDS6118.
01263-0440 TOK 204 Possible physical companion at 24".4, 227deg in 2MASS. Tok2012a
Direct motion by 20deg since first resolution in 2011, at constant
separation. Estimated period ~10yr. The small RV amplitude suggests an
orbit in the plane of the sky. Tok2013b
01264+5929 STI 213 STI1607.
01265+1812 HDS 187 Also a spectroscopic binary with P = 3087d which cannot be the visual Grf2015b
pair.
01267-7408 OGL 191 SMC122.1.1145 + SMC122.1.1144 Pli2012
01269-5023 ART 1 Low-mass wide double, discovered on 2MASS and Digital Sky Survey
frames. Artigau et al. determine sectral types M6.5V +/- 0.5 and M8V Art2007
+/- 0.5, distances 63 +/- 5 and 61 +/- 6 pc. Based on evolutionary
models, the masses are 0.095 +/- 0.005 and 0.092 +/- 0.005 Msun for an
age > 1Gyr, or 0.020 +/- 0.003 and 0.019 +/- 0.003 Msun for and age
~30Myr. The projected separation is ~5100 au.
01270+1500 GWP 190 XMI 201. Tob2012b
01270+1200 LDS3282 G002-038. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc. Also known as LIT 5.
NLTT 4817/4814 Chm2004
01270-0009 STF 125 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01270-3058 RSS 3 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. Rss1996
SHY 403. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
01270-3233 LDS2199 Some unconfirmed early observations. A is the semiregular variable
R Scl.
01270-7405 OGL 192 SMC122.2.1199 + SMC122.2.1250 Pli2012
01271-5158 SHY 404 HIP 6772 + HIP 6804.
01274-0204 J 1446 BAL 6.
01274-2220 RST2261 CD-22@503.
01275+1546 BPM 31 [PM2000] 54366 + [PM2000] 54359. Gvr2010
01276+6429 TDS1882 CD: Originally 01276+6430 TDS1882; primary found to be C component of
01276+6429.
01276+0402 GWP 192 XMI 202. Tob2012b
01277+6321 STI 215 MLB 382.
01277+4524 BU 999 ome And = 48 And
This cannot be the close 254.9-d spectroscopic binary. Grf2011b
Although the pair has been repeatedly resolved with the CHARA Array
with the Separated Fringe Packet technique, a full solution is not CIA2010
yet complete.
CIA 4 Aa,Ab: Combined solution by Farrington et al. (2014) yields masses
0.993 +/- 0.056 and 0.888 +/- 0.058 Msun, as well as an orbital
parallax 39.12 +/- 1.97 mas (compared with the Hipparcos parallax of
34.94 +/- 3.1 mas). CIA2014a
BU 82 CD: There is a faint star between the AB and CD pairs. The change in
AC is due to the proper motion of A. This is common to AB. Bu_1894
01277+1620 BPM 32 [PM2000] 54497 + [PM2000] 54549. Gvr2010
01277+0521 BU 1164 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.51 +/- 0.76, 2.67, and 1.05 Msun, respectively. Mlk2012
01278+5928 STI1618 STI 217.
01281-5238 CVN 2 Both the B and C companions are probably background objects. Cvn2005a
01282+1244 GWP 193 XMI 203. Tob2012b
01283+5329 STF 123 AB: Also known as HU 1651, but the 1911 Hussey measure has a quadrant
flip and a large sep error. Hu_1911
01283+1731 GWP 194 XMI 204. Tob2012b
01283+1429 AG 18 B is BD+13@217.
01283-1615 LDS3284 NLTT 4889/4888 Chm2004
01284+0758 S 398 STTA 19. B is BD+07@214.
HJL 19. HJL1986
01284+0758 A hierarchical quadruple. AB is a wide binary with an estimated period Tok2020h
of 300k years; the Ba,Bb pair has an estimated period of about 200
years and the close Ba1,2 pair has a spectroscopic orbit of 116d.
01284-4319 gam Phe Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Luyten (1936). Luy1936
01287-4710 LDS 48 Aka UC 562.
01289+0633 PLQ 16 LDS3285.
01290+7412 HJ 2045 LDS1529.
A is above MS, B on the MS. A component possibly a close double Mkr2005
(Makarov & Kaplan 2005) but nothing on the close sub-system in SIMBAD. Tok2014d
01291+2143 HO 9 BC: According to Griffin, the radial velocities of B and C differ by Grf1987c
30km/sec. Either the pair is optical, or one component is a
spectroscopic binary.
AB and AD: Optical pairs, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
AD: Rectilinear solution by Hurowitz et al. (2013). USN2013a
01291+1040 GWP 195 XMI 205. Tob2012b
01292+4820 BWL 6 AC: Source appears spatially extended; probably a background galaxy.
Primary is G 172-56. Bwl2015
01295+6319 MLB 330 This pair was purged from an earlier edition of the WDS as it was not
found by Heintz. It has apparently been located. It and the nearby
MLB 329 are in NGC 559. Hei1985a
01295+3054 BUP 20 B is BD+30@229.
01296-2138 SEE 14 48 Cet.
01297+4228 ZUC 6 SKF 314.
Primary is white dwarf WD 0126+422 = GD 13. Zuc1992
01297+2250 A 1910 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 6.11 +/- 1.86, 4.31, and 2.09 Msun, respectively. Mlk2012
01298+1014 CHR 197 First detected as an occultation binary by Africano. Afr1977b
01299+3100 ENG 6 B is BD+30@232.
01300-2231 I 445 A,BC = LDS 51.
01302+0609 STH 6 A: mu Psc = 98 Psc
01305-4242 I 1609 SY Phe, an Algol-type eclipsing binary, P = 5.27095d. Zas2012
01306-4446 DHI 1 At a distance of 40 +/- 14pc, the projected physical separation is 130
+/- 50au. Spectral types are M9.0 +/- 0.5 and L6 +/- 1. Dhital et al.
conclude the pair is physical. Dhi2011
01307-1227 GAL 309 Object #45 in Gallo's original list. Gal1912a
01309+5244 GIC 23 G173-002/G173-003.
NLTT 4991/4993 Chm2004
01312+7016 38 Cas Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Wright & Pugh (1954). Wri1954
01315+1521 BU 506 eta Psc = 99 Psc. A is a Beta CMi-type variable. Baz1964
NPOI Limb-darkened diameter 2.64 +/- 0.11 mas, NOI1999
R = 26. +/- 2. \rsun.
01316-1901 HJ 2052 B is BD-19@263. BDS 796, HJ 3373 same star.
01317+6103 STF 128 STI 227.
01317+1506 CHR 198 First detected as an occultation binary by Beavers. Bvr1977
01319+1603 BF Psc Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Griffin (1975). Grf1975a
01319+1026 GWP 196 XMI 206. Tob2012b
01320-1604 GAL 310 Object #46 in Gallo's original list. Gal1912a
01321+1657 STF 132 A is a spectroscopic binary, P = 36.6d.
A: 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 = 1.14 + 1.02, L/Lsun = 5.40 + 1.41, dm = 1.46 mag,
log age = 9.86. WaX2015b
Improved SB2 orbit for the unresolved pair. Kie2018
A: Teff = 5367 +/- 166 K, B: Teff = 5150 +/- 228.
AB: H 4 130. MEv2010
AB, AC, and AD: Optical pairs, based on study of relative motion of
the components using the method of apparent motion parameters. Kiy2008
AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
01321+1434 BPM 33 [PM2000] 57016 + [PM2000] 57059. Gvr2010
01323-2633 ARG 4 B is CD-27@523.
01325+1645 BPMA 1 [PM2000] 57224 + [PM2000] 57397. Gvr2010
01325+1417 LDS1102 NLTT 5103/5102 Chm2004
01326-2745 LDS2206 NLTT 5136/5135 Chm2004
01326-4944 SHY 405 HIP 7189 + HIP 7086.
01327+6336 EVS 9 Primary is the Cepheid V636 Cas. Evs2016a
01327-0139 FIL 2 B is BD-02@235.
01328+3551 STF 133 Confusion between C and D in ADS. With quadrant for CD north preceding,
AC obviously has greater separation than AD. B__1962d
Identifications of several later AC and AD measures were switched to
give motion consistent with earliest measures. Quadrants were flipped
for CD measures, which now agree with AC and AD measures. AC has
smaller separation than AD, and C is slightly brighter than D.
A 1911 Ea,Eb: Originally 01238+3553; found to be E component of 01328+3551.
01329+1954 LDS3289 NLTT 5133/5127 Chm2004
01329+1200 GWP 197 XMI 207. Tob2012b
01329-3652 GC 1881 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
01330+1027 GWP 198 XMI 208. Tob2012b
01331-0602 LDS3290 NLTT 5155/5154 Chm2004
01331-1951 LDS1103 NLTT 5163/5169 Chm2004
01332+6041 STF 131 Spectrum of B: B3IV.
01332+3231 SEI 17 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
01333-0014 UC 582 aka ITF 47.
01333-2411 LDS2209 NLTT 5178/5160 Chm2004
01335+6039 BUP 22 B is BD+59@273.
01337-1213 HWE 4 The linear formula by Job & Tamburini seems ruled out, as it makes Job1969b
the current quadrant opposite to what is observed.
01338+0346 RBR 32 Suspected non-single. Hor2002b
01343-0827 A 314 Derived orbital parallax 0".00978, mass sum 4.14 +/- 2.34 Msun Lin2004a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.85 +/- 0.99, 2.60, and 1.20 Msun, respectively. Mlk2012
01344+4844 ES 2587 G172-061. Not a common proper motion companion after comparison with
POSS2 red plates Oso2004
01344-1607 FAR 25 Primary is white dwarf WD 0131-163. Far2006
01345+1448 LDS9119 Old LDS6119.
01347+0720 GWP 199 XMI 209. Tob2012b
01348+2935 BRT 5 An Algol-type system, RS Tri.
01349+1234 STF 136 AB: H 4 131. MEv2010
01349-6909 GLI 12 B is CPD-69@74.
01350-2955 BU 1000 AB,C triple+var solution (AB in HIP). Sod1999
B is 0.47d eclipsing binary (= BB Scl).
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
01352-1829 RSS 49 CPD-19@169
01354+6305 MLB 280 Also classified K1V.
01354+4123 ES 1494 Probably identical with ADS 1241 ( = ALD).
01356+6117 STI 237 This and STI 239 are members of the multiple system HJ 1083.
01360+2646 BU 507 Morlet et al. note that this has similar position angle, separation,
and delta-m as HDS 212. HDS 212 removed. Mor2000
01360+0739 STF 138 D is BD+06@245.
AB: H N 92. MEv2010
01361-2954 HJ 3447 tau Scl. Arend orbit rejected from Fourth Orbit Catalog Ard1968
("orbit completely faulty and irreparable") Wor1983
01361-3718 HJ 3448 Spectral type of A may be K. B is CD-37@605.
01364+7909 STF 127 B is BD+78@50.
01364+3209 SEI 18 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
The faint pair now measured for the lost SEI 18 may be this new pair. Dam2017a
01368+4124 BUP 23 ups And = 50 And = Titawin. A is a spectroscopic binary.
AB: exoplanets with P=4.61d, 237.7d, 1302d, 3848d Tok2014d
LWR 1 AD. Determined to be CPM pair from examination of POSS I and II plates
(epochs 1953 and 1995), plus 2MASS. Conclude spectral type of
companion M4.5V. Lwr2002
AD: Raghavan et al. (2010) consider D physical, high PM (no PM given). Rag2010
CHARA Array Limb-darkened diameter 1.114 +/- 0.009 mas, CIA2008c
R = 1.631 +/- 0.014 \rsun.
ups And A: Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from Butler CPS1999b
et al. (1999). HaI2001
BUP 23 AB: Rectilinear solution by Rica et al. (2017). FMR2017b
01368+4124 STT 554 AC: Rectilinear solution by Rica et al. (2017). FMR2017b
01371+1209 VSC 1 = pi Psc = 102 Psc.
01372+1147 TOB9002 Measured as HJ 16 but actually an anonymous pair added here. Tob2012b
01373+1828 GWP 204 XMI 210. Tob2012b
01374+2510 G034-039 Boden et al. (2006) give combined spectroscopic/interferometric Bod2006
solution, including PTI observations. Derive distance of 42.23 +/-
0.21 pc (pi = 23.68 +/- 0.12 mas), age 9.12 +/- 0.25 Gyr, with
abundances near solar. The K0IV primary appears to have evolved off
the MS and is traversing the Hertzsprung gap toward red giant phase.
Masses are 1.072 +/- 0.014 and 0.8383 +/- 0.0081 Msun, luminosities
2.451 +/- 0.041 and 0.424 +/- 0.023 Lsun, radii 2.048 +/- 0.081 and
0.887 +/- 0.071 Rsun.
01374-8217 GLI 14 Spectrum G5III:+K1/2.
01375-1135 LDS9120 Old LDS6120.
01376+2233 STTA 20 B is BD+21@218.
Pair appears in an appendix list, not part of discoverer's regular
numbering sequence.
01376+1727 GWP 205 XMI 211. Tob2012b
01376+0709 PLQ 19 HJL 21. HJL1986
01376-0645 BRG 5 BC: Initially entered as WDS 01369-0648, the primary of BRG 5 was
later found to be the B component of 01376-0645 CAB 3.
01376-0924 KUI 7 1982.7657: This autocorrelogram was remeasured; the new results are
listed here. McA1987b
Combined spectroscopic/visual orbit, also yielding orbital parallax
and component masses and absolute magnitudes. Tok1993
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
Martin et al. (1998) derive component masses 1.712 +/- 0.296 and
1.140 +/- 0.226 Msun. Mig1998
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.51 +/- 0.43, 2.49, and 1.13 Msun, respectively. Mlk2012
01377+4825 HDS 215 Rectilinear solution by Hartkopf & Mason (2013). Hrt2013b
01377-5714 KRV 54 alp Eri = Achernar
Ma = 6.0 +/- 0.6, Mb = 2.0 +/- 0.1 \Msun, Ra = 8.14 +/- 0.26, Rb = 1.70
+/- 0.08 \Rsun, Teff_a = 15539 +/- 438, Teff_b = 9064 +/- 624 K, La =
3493 +/- 429, Lb = 17.5 +/- 5.1 \Lsun. Krv2022
01379-8259 TOK 426 HIP 7601 is a nearby (27pc) dwarf also known as GJ 67.1 or HR 512.
According to Wichman et al. (2003 A&A, 400, 293), it is a young
spectroscopic triple detected in X-rays (1RXS J013755.4-825838). GCS
also recognized the star as SB2. Spectroscopic monitoring (Tokovinin,
in preparation) shows that all three components are similar stars of
approximately one solar mass. Here we resolved the outer subsystem AB
and observed its fast motion. In fact it was already resolved at SOAR
on 2011.036 at 221.0deg and 0".044, but this low-quality observation
has not been published. The available data indicate that the period
of AB is 1.35years; the pair completed nearly two revolutions since
its first resolution in 2011. Tok2015c
01380+4600 HJ 2063 Aka A 944AB,C.
01385+7302 HJ 2054 40 Cas.
01386-4113 CPO 110 B is CD-41@445.
01387+0359 GWP 208 XMI 212. Tob2012b
01387-4515 HJ 3451 LDS 55.
01388-1758 LDS 838 LUY 726-8. L 726-8 = UV Cet. Both components are active flare stars
According to Harrington & Behall the mass ratio is 0.487 +/- 0.011 and
the individual masses are 0.115 (0.008) 0.109 (0.008) Msun for A & B,
respectively. Hrr1973
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
This pm star with flare characteristics is a difficult object. VBs1954
Magnitude uncertain due to flares. USN1988b
AB: Kervella et al. (2016) derive a new orbit for GJ 65 and determine
the following physical parameters:
masses (Msun): A = 0.1225 +- 0.0043 B = 0.1195 +- 0.0043
radii (Rsun): 0.165 +- 0.006 0.159 +- 0.006
[Fe/H] (dex): -0.03 +- 0.20 -0.12 +- 0.20
log (cgs): 5.092 +- 0.015 5.113 +- 0.015 Krv2016
Using the parallax from Gaia DR3 and the mass ratio from Worley, Gai2018
individual masses of Ma = 0.1191 +/- 0.0018 \msun and Mb = 0.1144 +/- Wor1973b
0.0017 \msun are determined for these components. Msn2023
01388-5327 DUN 4 While this pair appears to have common proper motion and parallax, a
linear solution has been performed and identified therein as optical. LRR2022c
01393+5257 STF 139 Neither AB, AC or BC are physically associated. Kiy2015c
01393+1638 BU 5 103 Psc.
01394-1748 HJ 2067 HJ 3380.
01397+4602 EGB 1 ES 553.
01397-3728 HJ 3452 B is CD-38@572.
01398+1704 BPM 34 [PM2000] 61379 + [PM2000] 61385. Gvr2010
01398-5612 DUN 5 Some measures have been corrected by Andrew James (personal
correspondance). Note that this is p Eri, not rho Eri
(03027-0741BU 11).
Measures of 1947.60 and 1947.84 made by triangulation of multiple Der9999
measures.
01399+1515 STF 142 B is BD+14@@251.
01400+2702 ALP 5 2MASSW J0140026+270150
Companion seen as elongated in I-band image taken at WIYN in August
2002. Physical companionship to this ultracool dwarf ruled out. AlP2007
01400-1348 GAL 311 Object #48 in Gallo's original list. Gal1912a
01402+7303 HJ 2055 AB: Rectilinear solution by Hurowitz et al. (2013). USN2013a
01404+3420 STF 143 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01405-0917 LDS9121 Old LDS6121.
01406+4035 BU 1362 tau And = 53 And. A is a spectroscopic binary. Variable?
01409+6410 RAO 32 AC: C component = A component of WDS 01409+6409 TDS1951.
01409+6409 TDS1951 Primary = C component of WDS 01409+6410.
01409+1117 A 2320 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.33 +/- 0.76, 2.02, and 0.95 Msun, respectively. Mlk2012
01409+4952 HU 531 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.66 +/- 0.98, 2.11, and 0.79 Msun, respectively. Mlk2012
01409+0138 A 2404 Quadrant uncertain.
01410-0524 TOK 228 Primary is EY Cet, variable of BY Dra type, X-ray source Tok2014d
01412-6741 LDS 56 HIP 7869. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
01413+2545 STF 145 Period of AB estimated at 7300y. Tok2006
Primary is SB2, P=4.435d. Aa,Ab has suspected close tertiary because
K1,K2 are var, e>0. B is SB1, P=1.435d. RoboAO find a companion to B
(98deg, 4.80", dI=7.2mag), but it is considered optical. Tok2014d
01413+1246 GWP 214 XMI 213. Tob2012b
01413+1007 STF 146 B is BD+09@203.
HJL 22. HJL1986
01414+3704 LDS3300 NLTT 5619/5621 Chm2004
01414-7909 HJ 3467 tau 1 Hyi
01417+0712 GWP 215 XMI 214. Tob2012b
01417-7616 JSP 25 Aka TDS1958.
01418+4237 MCY 2 An astrometric binary now resolved by infrared speckle interferometry.
Discovery designation per Todd Henry 03/02/98.
Improved pc (Delta m > 6) orbit combining pg (Lippincott 1983) and Lip1983
Hipparcos obs. Scaling by the speckle IR (Henry 1993) gives orbit size Hen1993
and mass ratio.
Martin et al. (1998) derive component masses 0.795 +/- 0.159 and
0.136 +/- 0.053 Msun. Mig1998
The estimated magnitude difference in V (~6 mag) is too large for the
companion to have been detected. Hrt2009
Mass of A(B) determined to be 0.95+/-0.11(0.254+/-0.019) \msun. Orbital
parallax 79.08 +/- 0.63 mas. Trr2022
01419-0907 GRV1170 Aka SLW 81.
01420+4252 ROE 64 HJL 23. HJL1986
01423+5134 CUD 2 Component A is the central star of the planetary nebula NGC 650/1 Skf2013
= Messier 76.
01424+2609 BRT3259 Originally published as BRT 126. Brt1928
01424-0645 A 1 A premature orbit has been computed.
Omega corrected from 24.0 to 58.9, omega from 58.9 to 24.0 Ruy1995
01425+5000 B 2550 BD+49 440 (8.5) and 441 (9.0) are together in a high power field. Both
are close pairs; brighter star is deep orange, the fainter (ADS 1341,
HU 1210) is white. At present the brighter star is the easier pair,
but as its duplicity was missed by Hussey, Aitken, and van Biesbroeck,
then they measured CD, it must have opened out more recently. B__1963b
01425+2016 HJ 2071 A: 107 Psc.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
107 Psc Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
01426+6033 BU 1363 A 3588-d spectroscopic orbit has been found for the A component. Grf2012d
The primary is the E component of 01426+6033.
01427+0637 J 1808 HJL 24. HJL1986
01430+6402 STI 264 Component A is a pulsating star in the open cluster NGC 637. Since
relative motions of all three components are small and in agreement
with each other, we believe all three stars are members of the same
cluster. It is not currently possible to determine whether of not they
form a closed triple system. Kiy2012
01431+3426 COU 668 Aa,Ab: TDS1964.
01431+2101 JNN 251 Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.15 +/- 0.03
Msun; a ~4.8 au. Jnn2014
01432+6056 MLR 106 AC: STI 271.
01433+6033 BU 1103 44 Cas. A is a spectroscopic binary.
FYM 160 AH: Fay (2013) notes an H component in their Figure 1, but does not FyM2013d
include a measurement.
ARN 32 AE: E component is primary of 01426+6033 BU 1363
01433-1736 HJ 3455 B is BD-18@292.
01434-0705 STF 150 B is BD-07@283.
01434-1127 GAL 312 Object #50 in Gallo's original list. Gal1912a
01435+5318 HJ 2069 B is BD+52@417.
01435-1038 GAL 313 Object #51 in Gallo's original list. Gal1912a
01436+2802 GIC 24 G072-028/G072-029.
NLTT 5738/5740 Chm2004
01437+5014 CIA 6 Phi Per. Be+sdO binary, resolved by the CHARA Array. The hot subdwarf
companion is detected in near-IR; flux contribution 1.5% in H (dH=4.6)
and restricted fits indicate flux contribution rises to 3.3% (dV~3.7)
in visible. Combined interferometric/spectroscopic orbital solution
yields masses 9.6+/-0.3 and 1.2+/-0.2 Msun for the Be primary and
subdwarf secondary, respectvely. The inferred distance (186+/-3pc),
kinematical properties, and evolutionary state are consistent with
membership of phi Per in the alpha Per cluster. CIA2015a
01437+0934 BU 509 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.69 +/- 0.64, 1.83, and 0.85 Msun, respectively. Mlk2012
01438+1954 GWP 216 XMI 215. Tob2012b
01438+1206 HJ 18 Possibly BD+11@225. BDS 899, HJ 18. HJ position angle in 1820: 220@.
Disagrees with 1912 - 1922: 143@.
01441-1556 BUP 25 tau Cet = 52 Cet. Optical. Proper motion of A -1718 +856.
01442-0813 LDS9122 Old LDS6122. Primary is QSO, Z=0.239.
01443+6652 HAU 10 HJL 25. HJL1986
01443+5732 BU 870 A premature orbit has been computed.
Primary is eclipsing binary V773 Cas (period 2.58734 day). Zas2010
Light curve and radial velocity combined solution determined. Zas2017
ARN 55 AD: HJL1011. HJL1986
01443+0929 KPR 1 AC: Separation may be a factor of 10 too small.
STF 155 AB: H 2 49. MEv2010
01448+5708 B 2548 Rapid motion.
This close pair precedes BD+56 338 (ADS 1371, BU 453) by 12 sec of
time and is 0.6' north of it. All measures given in Pub Yerkes O. IX,
pt 1 and 2, by van Biesbroeck and myself, assigned to BU 453, are
obviously of the new pair. My estimates of the difference in magnitude
vary between 0.4 sf and 0.7 np, which seems rather large to be error
of estimation, even in so close a pair. B__1963b
01449+2005 109 Psc Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from Vogt et al. CPS2000c
(2000). HaI2001
01449+1951 A 2322 EU Psc, Algol-type eclipsing binary, per 1.69261 d. Zas2011
Observed wrong star? van den Bos has 4 measures in 1962, and I have B__1963b
positive measure in 1964. Wor1967b
01450+6032 STI 281 AB: BKO1073AC.
MRI 27 AC: BKO1073AB.
01450+5707 BU 453 Premature orbits have been calculated. Motion direct. Baz1972
01450+2703 COU 750 Rapid motion.
01450-0104 LDS9123 Old LDS6123.
NLTT 5822/5818 Chm2004
01452+2317 GIC 25 G034-048/G034-049.
01454+0909 OCC9041 110 omi Psc = Torcular.
01454-3957 BRG 6 2MASS J01452133-3957204 has only been observed in one epoch, but the
color and brightness of the detected companion are consistent with
expectation, hence we count it as an unconfirmed binary. Jnn2012
01455-6035 JSP9001 Previously known as JSP 13a.
01456+1148 GWP 217 XMI 216. Tob2012b
01456-0224 J 1448 BC. Gauchet (1926) measure originally listed as CD pair, with theta Gau1926a
flipped by 180deg.
01456-2503 HJ 3461 eps Scl. A premature orbit has been computed.
01457+0834 BAG 38 Primary is the alpha2 CVn type variable UZ Psc.
01458+1200 BPM 35 [PM2000] 64864 + [PM2000] 64876. Gvr2010
01458+0043 GWP 219 XMI 217. Tob2012b
01459+7142 HJ 1090 01459+7142FOX 119CD. WDS designation for HJ 1090 changed from
01461+7143 due to inclusion in multiple.
HJ 1089 AB: Rectilinear solution by Mason et al. (2012). WSI2012
01459-4357 HJ 3463 B is CD-44@509.
01460+8005 GW Cep Multiple system including contact binary. Pbl2006
01460+6113 STF 151 STF 151rej and Duner 1 are identical.
01462+5326 HJ 2079 Confused with nearby 01463+5328 HJ 2080, as pairs are also of similar
separation and position angle.
01462+3343 HU 804 A premature orbit has been computed.
01463+5328 HJ 2080 Confused with nearby 01462+5326 HJ 2079, as pairs are also of similar
separation and position angle.
01466+1639 GWP 221 XMI 218. Tob2012b
01467+0214 GWP 222 XMI 219. Tob2012b
01469+4234 DUP 1 Dupuy et al. (2015) resolved a low-luminosity T9/Y0 binary, using Keck
laser guide star imaging. Masses are estimated as 4.6 +1.0/-1.1 and
4.3 +1/0/-1.2 Mjup (for age of 1Gyr) or 16.9 +3.8/-4.0 and
15.9 +3.5/-4.4 Mjup (for age of 10Gyr). Dup2015
01474+0355 HJ 2084 Aka STT 36.
01474-2157 GD 1400 Song et al. (2006) confirm common proper motion of this brown dwarf Son2006
and its planetary mass companion.
01475-4955 RED 15 2MASS J01473282-4954478. Spectral types M8: and L2: Red2006b
01476+3453 CSW 1 AB: This star has a possible wide brown dwarf companion at 43" Csw2008
separation, according to Casewell et al. (2008). Jnn2012
KIR 6 BC: B component is an L0.5V brown dwarf. The spectrum of the secondary
shows it to be a background M star. Kir1999
01477+6351 ENG 7 A is GJ 75 = V987 Cas. B is BD+63@241.
AB: Rectilinear solution by Friedman et al. (2011). USN2011a
01477+1643 BPMA 2 [PM2000] 65958 + [PM2000] 65844. Gvr2010
01477-4358 I 52 Gomez et al. (2016) derive dynamical parallax and component masses:
7.50 +/- 0.33 mas, 1.310 +/- 0.032 Msun, 1.128 +/- 0.027 Msun. Doc2016i
A is a close 5.3-d spectroscopic pair. Tok2019a
01478-8011 HJ 3474 tau 2 Hyi
01479+4440 A 949 BJN 26.
This measure was published as BRT 346. Note to BRT 346: This seems to
be ADS 1412, although the magnitude difference is discordant.
BD+44 369, with which ADS 1412 is identified, was not seen as double. Brt1939a
01480+4353 ES 1498 BRT 325. Brt1930
01481-2533 FAR 26 Primary is white dwarf WD 0145-257. Far2006
01482+1657 TOK 945 4 Ari.
01483+1203 LDS1116 LDS3311.
NLTT 6012/6013 Chm2004
01483-4130 RGS 2 GJ 77. Rodigas et al. (2016) detect a companion to the old solar-type
star HD 11112, and determine it is likely a gravitationally bound cool
white dwarf. SED fits (pure-H and pure-He models) suggest a mass for
the companion in the range 0.90-1.08 Msun, Teff 7300-9800K,
log (L/Lsun) -3.69 - -3.36, and age 2.43-3.92 Gyr. Rgs2016b
01486+1618 BU 510 AC: H 5 92. MEv2010
01486-0955 JNN 17 LP 708-465.
01487+7528 HJ 2075 LDS1540.
01487+3306 GIC 26 G072-038/G072-037.
NLTT 6030/6027 Chm2004
01487-2916 HJ 3466 B is CD-29@590.
01488-0125 STF 171 B is BD-02@300.
01489+1411 GWP 223 XMI 220. Tob2012b
01489-2053 ARA1256 Primary is TW Cet, a W UMa type eclipsing binary, P = 0.31685d. Zas2012
01489-3153 LDS3316 NLTT 6087/6088 Chm2004
01491+2956 2M 0149+29 2MASSW J0149090+295613. Astrometric orbit by Harris et al. (2015)
yielded the following properties: spectral types M9.5+L4, absolute J
mags 11.74+13.40, masses 0.084 +/- 0.008 and 0.069 +/- 0.010 Msun. USN2015
01491+0236 GWP 224 XMI 221. Tob2012b
01493+4754 CHR 4 Aa,Ab: Although this new component is indicated as Aa,Ab we have not
firmly established whether it is associated with the A or B component
of the wide pair. McA1987b
B is a spectroscopic binary. The system appears to be quintuple.
STF 162 AB: Rectilinear solutions by Zirm & Rica (2014) Zir2014b
and Genet et al. (2015). GnR2015a
Despite the linear solution, proper motion and parallax favor a Grv2020a
physical connection. Long period and/or high eccentricity possible.
01493+1808 GWP 225 XMI 222. Tob2012b
01496+1741 GWP 226 XMI 223. Tob2012b
01496-1041 ENG 8 53 Cet = chi Cet. LDS2222.
SHY 8. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
01497-1414 HU 422 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.42 +/- 0.46, 2.45, and 1.20 Msun, respectively. Mlk2012
01498-3824 GC 2219 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
HDO 186 Additional notes may be found in Herschel (1847). HJ_1847b
01499+8053 STT 34 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 14.28 +/- 6.95, 4.72, and 2.24 Msun, respectively. Mlk2012
01499+1324 LDS1118 Also known as LDS6124 and LDS9124. Richard Jaworski first Jaw2006
recognized that these systems were the same.
01500-0408 A 2602 Gomez et al. (2016) derive dynamical parallax and component masses:
15.65 +/- 1.62 mas, 0.748 +/- 0.037 Msun, 0.748 +/- 0.037 Msun. Doc2016i
01501+3538 ALI 28 No stars seen at AC catalog locations - probably plate flaws.
01501+2217 STF 174 1 Ari. Spectrum composite; K1III+A6V. Spectroscopic binary?
H 1 73. MEv2010
01502+1600 BPM 36 [PM2000] 67462 + [PM2000] 67449. Gvr2010
01503+1146 GWP 227 XMI 224. Tob2012b
01504+2942 MLB1059 Aka MLB 448.
01505-2042 ARA1257 A likely plate flaw. Grv2021a
01509+1626 BPM 37 [PM2000] 67854 + [PM2000] 67921. Gvr2010
01509+1031 GWP 228 XMI 225. Tob2012b
01510+2107 STF 175 AB: H 2 56. MEv2010
01511+1135 BPM 38 [PM2000] 68017 + [PM2000] 67969. Gvr2010
01512+2439 HO 311 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 4.19 +/- 1.30, 3.38, and 1.40 Msun, respectively. Mlk2012
01513+6451 STF 163 B is BD+64@244.
01513-3800 LDS9125 Old LDS6125.
01514+4329 HJ 2089 B is BD+42@388.
01515+0457 STF 177 Formerly, BD+04@320. Corrected by Weis. StF2002
01515-0744 HIP 8653 Small acceleration of 2 mas yr-2, possibly single. Tok2012a
01515-1020 BNU 1 Aa,Ab: zet Cet = 55 Cet = Baten Kaitos. A is a long-period
spectroscopic binary, P = 1652d, and has been resolved by speckle
interferometry. B is BD-11@360.
01515-1858 LDS9126 Old LDS6126.
01516+1618 BPM 39 [PM2000] 68302 + [PM2000] 68249. Gvr2010
01518-5458 SHY 128 AC: HIP 8687 + HIP 7387.
01519+6426 GIC 27 G244-037/G244-036 = GJ 3117A/3118B.
01520+1049 STF 178 H 1 56. MEv2010
Additional notes may be found in Couteau (1952). Cou1952a
01521+5430 SMA 24 Also known as STI1703.
01522+6627 STF 167 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01522-5220 CVN 3 CPM pair. The spectral type of the B component is M9.5 +/- 1,
Teff = 2100 +/- 200K; age ~30 Myr, mass 25 +/- 10 Mjup. Cvn2005a
01523-0620 LDS9127 Old LDS6127.
01525+1710 GWP 232 XMI 226. Tob2012b
01526+3127 HJ 645 SEI 20. Nsn2017a
01528+4016 MLB 999 BRT 2198.
01528+1544 BPM 40 [PM2000] 69032 + [PM2000] 69018. Gvr2010
01528+0117 GWP 233 XMI 227. Tob2012b
01530-2805 HJ 3472 SWR 3. CPM pair Skf2004
01531+2935 BUP 27 alp Tri = 2 Tri = Mothallah. A is a spectroscopic binary, P = 1.77d.
01532+3719 STF 179 H 1 89. MEv2010
01533+4044 HJ 1094 55 And.
01534+7003 STF 169 Primary is V776 Cas, a W UMa type eclipsing binary, P = 0.44042d. Zas2012
01535+1918 STF 180 gam Ari = 5 Ari = Mesarthim. According to R.G. Aitken, Robert Hooke A__1935f
noted this as a double in 1664. Hooke wrote: "I took notice that it Hoo1665
consisted of two small stars very near together; a like instance to
which I have not else met in all the heavens." HFC1928
A is a variable of the Alpha CVn type.
AB: H 3 9. MEv2010
Uniform disk diameter 0.336 +/- 0.019 mas,
Limb darkened diameter 0.346 +/- 0.019 mas,
Teff = 11000 +/- 1100 K based on LDD.
Radius is 1.97 +/- 0.12 \rsun. CIA2019a
BU 512 Primary is C component of STF 180. WDS designation changed from
01538+1918 and components labelled CD.
01536+6324 PTT 3 OL 114, STI 317 are identical.
01536+0311 xi Psc Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin & Herbig (1981). Grf1981b
01539+5611 RBR 33 Suspected non-single. Hor2002b
01541-7729 JSP 31 Apparent rapid retrograde motion, but measures sparse.
01543+6542 GIC 28 G244-042/G244-041.
01543-1543 GAL 314 Also known as LDS1120.
Object #55 in Gallo's original list. Gal1912a
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
CHM 3 AC. NLTT 6398 + 6395.
01544-2250 LDS3322 NLTT 6400/6399 Chm2004
01544-4230 phi Phe Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
Chemically peculiar late-B star, initially thought to be a triple,
with spectroscopic period 41.4d and astrometric period 878d. Using
Coralie spectra from 2000-2010, Korhonen et al. (2013 A&A 553, A27)
find a spectroscopic period of 1126d. Spectroscopic data by Pourbaix
et al. (2013) exclude the 40d period, but are insufficient to refine
the Korhonen solution. Their spectroscopic elements are combined
with the Hipparcos astrometry to refine the initial astrometic orbit. Pbx2013
01546+2049 MKT 3 bet Ari = Sheratan. Astrometry from Mark III interferometer is combined
with spectroscopy (Tomkin & Tran 1987) by Pan et al. (1990) to Tom1987b
determine orbital elements, masses, and distance. Masses agree well MkT1990
with empirical mass-luminosity relation.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Pan et al. (1990). MkT1990
Martin et al. (1998) derive component masses 2.067 +/- 0.203 and
1.281 +/- 0.178 Msun. Mig1998
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 3.19 +/- 0.13, 3.51, and 1.82 Msun, respectively. Mlk2012
01549+1124 BPM 41 [PM2000] 70299 + [PM2000] 70233. Gvr2010
01551+2847 STF 183 According to Scardia et al. (2001), orbital elements are well defined; Sca2001d
only the period is still rather uncertain. The Hipparcos parallax
(0".00727 +/- 0.00189) gives a mass sum of 3.8 Msun +/- 82%, in excess
for a binary of type F2. The dynamical parallax (0".0074) agrees well
with the observed one.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 4.82 +/- 2.85, 3.45, and 1.35 Msun, respectively. Mlk2012
01551-1204 LDS9128 Old LDS6128.
01553-2134 DON 26 CD-22@641.
01554+0257 A 2407 A premature orbit has been computed.
01555+7637 LDS1545 Aka LOC 67.
01556+0146 BU 1367 A 2408.
Rectilinear solution by Rica & Zirm (2012). FMR2012i
01559+0151 STF 186 Spectroscopic binary? Spectrum composite; F7V+G0V.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.22 +/- 1.22, 2.56, and 1.07 Msun, respectively. Mlk2012
01560+5728 STI1717 Apparently the same as MRI 41.
01560+0529 GWP 236 XMI 228. Tob2012b
01560+0046 RST5186 BD+00@311a.
01560-5137 HJ 3473 chi Eri
01561+6035 AG 301 HJL 26. HJL1986
01561+3745 HJ 1097 ALI 494.
01562+3715 BU 1368 Bb: b is BD+36@349.
STFA 4 56 And. B is BD+36@354.
01563+0829 GWP 237 AB: XMI 229AB. Tob2012b
GWP 238 AC: XMI 229AC. Tob2012b
01564+3650 J 2719 ALI 259.
01568+3931 ALI1022 Not found by Heintz at IDS position. Hei1990b
01568+3802 TOB9001 BC: A measure by Espin incorrectly attributed to this pair led to its
earlier designation as 01569+3759ES 228CD.
01568+2303 BVD 21 RoboAO resolved the B component (201.1deg, 0.199", dI=1.61 mag) but
the pair was not accepted as real. Tok2014d
01570+3101 A 819 A premature orbit has been computed.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.97 +/- 1.00, 2.49, and 1.20 Msun, respectively. Mlk2012
AB,C: HJL 27. HJL1986
01571+1517 BPM 43 [PM2000] 71640 + [PM2000] 71653. Gvr2010
01571+1414 BPM 42 [PM2000] 71596 + [PM2000] 71608. Gvr2010
01572+1644 GWP 241 XMI 230. Tob2012b
01572-1015 GAL 315 LDS 60. Object #56 in Gallo's original list. Gal1912a
HIP 9094. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 6529/6530 Chm2004
CHARA Array Limb-darkened diameter 0.611 +/- 0.081 mas, CIA2008c
R = 2.18 +/- 0.29 \rsun.
CHARA Array Limb-darkened diameter of A : CIA2013c
R = 2.1425 +/- 0.0687 \rsun, L = 2.6056 +/-0.1041 \lsun,
Teff = 5013 +/- 62 K, M = 1.133 \msun, Age = 7.8 Gyr.
01575+5558 ES 1811 STI1732.
Vatican zone coordinates yield 1911.9, 295.2, 5.61, showing Espin's
distance is too small and that there is no change so far. VBs1954
01576+4205 YSC 125 There is some evidence of a very faint third component in this system
with separation of 0.45 arcsec. Hor2011b
Improved SB2 orbit. A: Teff = 5789 +/- 21 K, B: Teff = 4544 +/- 164. Kie2018
NLTT 6522 Orbit determined by fitting revised Hipparcos intermediate astrometric
data. Derived component masses 0.99 +/- 0.11 and 0.75 +/- 0.05 Msun. Ren2010
01577-3625 LDS 62 LDS5359. TSN 72.
01579+2336 H 5 12 H V 12. STTA 21. 9 Ari = lam Ari. A is a Beta Lyrae-type and
spectroscopic binary. B is BD+22@289.
AB: HJL 28. HJL1986
01579+0924 GWP 243 XMI 231. Tob2012b
01579-2851 LDS 61 NLTT 6581/6583 Chm2004
01581+4123 S 404 Same as STF 190 rej, SHJ 404, H IV 104, H 4 104, H IV 128, H 4 128.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
01583+0250 GWP 245 XMI 232. Tob2012b
01583-8218 I 311 Composite spectrum: G8/K0(V)+(G).
01584+2547 A 2011 B is strongly above MS, very red in V-K (wrong 2MASS ptm?). Hipparcos
does not resolve AB, but has X-solution and suspected non-single. Tok2014d
01584-2304 LDS3330 NLTT 6605/6606 Chm2004
01585+3643 J 1809 ALI 262.
01586+3834 LPL 1 La Palombara et al. (2012) detect a companion to the hot subdwarf
BD+37 442, using the XMM Newton satellite. The companion is thought to
be a white dwarf or neutron star, likely powered by accretion from the
wind of the primary. LPl2012
01586-5332 HU 1557 Primary is CI Eri, an Algol-type eclipsing binary, P = 1.23819d. Zas2012
01588+1702 GWP 247 XMI 233. Tob2012b
01588-0949 J 1449 BD-10 410. Previously published declination corrected by +4'. J__1949a
GAL 316. Object #57 in Gallo's original list. Gal1912a
01588-2212 HJ 2103 B is BD-22@329.
01588-6134 alf Hyi Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
01589-5652 LDS 63 LDS6106 = LDS9106 (incorrectly listed in the WDS as 00593-5652).
B is CPD-57@385 = CD-57@396.
01590-1640 LDS9129 Old LDS6129.
01590-2255 H 2 58 H II 58. A is a W UMa-type system, AA Cet.
01591+3313 ENG 9 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: Rectilinear solution by Friedman et al. (2011). USN2011a
01591+1523 GWP 248 XMI 234. Tob2012b
01598+1543 BPM 44 [PM2000] 73241 + [PM2000] 73209. Gvr2010
02000+1334 LDS5181 old LDS6130.
02003-0138 BAL 9 J 3333. Nsn2016
02004-0831 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. Jnn2012
02005-6246 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. Kiy2008
02011-1741 LDS5362 NLTT 6759/6757 Chm2004
02012-0729 GWP 250 ABL 1. Tob2012b
02012-3000 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. Cus2012
02013+1227 BPM 45 [PM2000] 74159 + [PM2000] 74128. Gvr2010
02013-0752 GWP 251 ABL 2. Tob2012b
02015+1830 BPM 46 [PM2000] 74328 + [PM2000] 74271. Gvr2010
02019+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. Jnn2014
02019+2415 POU 157 ID uncertain. Nothing at Pourteau's coordinates. Pou1933
02020+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. Mlk2012
02020+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. MEv2010
02021+0355 OSV 1 LDS5363.
02021-1321 GAL 317 Object #59 in Gallo's original list. Gal1912b
02022+7530 STF 185 Primary is V779 Cas, an Algol-type eclipsing binary, P = 6.35340d. Zas2012
02022-1441 GWP 253 ABL 4. Tob2012b
02022-1808 GWP 252 ABL 3. Tob2012b
02022-4550 SHY 410 HIP 9495 + HIP 9672.
02022-6236 TOK 70 HIP 9499. A is SB, no orbit, dRV=70.7 (Nordstrom et al. 2004). Nrd2004
02023-2634 LDS 65 NLTT 6825/6826 Chm2004
02025-1410 GWP 254 ABL 5. Tob2012b
02026+5941 CIA 53 V780 Cas.
02026-1719 GWP 255 ABL 6. Tob2012b
02027-3019 HJ 3478 B is CD-30@717.
02030+3317 STF 201 eps Tri = 3 Tri
02031-0725 STF 209 B is BD-08@371.
02031-1229 GWP 256 ABL 7. Tob2012b
02032+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. Gvr2010
02035-0455 TOK 873 also known as VSC 2. Hor2024
02037+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. Mlk2012
02038+7013 MLR 375 1983.0663: This autocorrelogram was remeasured; the new results are
listed in the catalog. McA1987b
02038-0020 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). VBs1914
02039+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
Mk III Limb-darkened diameter 7.84 mas. MkT1991
Mk III Limb-darkened diameter 7.814 +/- 0.078 mas. MkT2003
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). Mlr1954a
02039+1231 BPM 48 [PM2000] 75778 + [PM2000] 75779. Gvr2010
02039-4525 RST2272 Primary is SB2, P=0.851 y. Aa,Ab UR in speckle. Koen et al. (2002
MNRAS 331, 45) find 311d photometric period. Tok2014d
02042+5257 HJ 2104 B is BD+52@501.
02042+4641 ADM 1 HTP 32. HAT-P-32. Primary is exoplanet host star. Adm2013
02042-1039 GAL 318 Object #62 in Gallo's original list. Gal1912b
02044+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. HaI2001
02046+1757 GWP 257 XMI 235. Tob2012b
02051+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) HIP1997d
02051-1737 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 Chm2004
02054-5910 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? Luy1984
02056+1444 BPM 49 [PM2000] 76857 + [PM2000] 76899. Gvr2010
02057-2423 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. Tok2014b
02058+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. Hrt2012b
02062-1808 GWP 258 ABL 8. Tob2012b
02065+5703 BAR 23 J 880.
02068+2542 HO 312 11 Ari.
02069-1126 SLW 99 Aka ABL 9.
02070+4512 WOR 1 AB: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
BKO 12 AC: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
LMP 27 AD: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
There is an unresolved (P=897d) spectroscopic companion to A. Tok2019b
02070-1017 GAL 319 Object #63 in Gallo's original list. Gal1912b
02070-4406 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. Jnn2012
02074-5941 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. Fah2010
02076-0037 LDS3346 NLTT 7066/7064 Chm2004
HJL 29. HJL1986
02079+1343 GWP 259 XMI 236. Tob2012b
02080+2814 CHE 55 MLB 452.
02080-0951 GAL 320 Object #64 in Gallo's original list. Gal1912b
Rectilinear solution by Hurowitz et al. (2013). USN2013a
02081+1336 FAR 27 SKF 23. Primary is white dwarf WD 0205+133. Far2006
02082+1509 LDS5183 old LDS6131.
02083+2543 ALP 6 2MASSW J0208183+254253
Further observations are required to determine the physical/optical
nature of this triple. AlP2007
02084+2819 KUI 118 G072-058. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 7087/7088 Chm2004
02085-0641 HDS 285 Possible sub-diffraction-limited component, but the astrometry is not
consistent between the two observations. Hor2011b
02087-0026 STF 218 Same as STF 220.
02087-1005 HU 16 HD 13191, W UMa-type eclipsing binary, period 0.31542 d. Zas2018
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. Bwl2015
02090+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__1963b
02091+4341 LDS3349 NLTT 7117/7118 Chm2004
02091+4048 STF 215 A is an eclipsing binary, BX And.
02091+1511 GWP 260 XMI 237. Tob2012b
02093-1958 GWP 261 ABL 10. Tob2012b
02094+2556 H 6 69 H VI 69. 14 Ari. STTA 23.
AC: HJL1012. HJL1986
02094-1011 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. Mlk2012
02096+4251 ES 48 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: Rectilinear solution by Hurowitz et al. (2013). USN2013a
02097+2021 STF 221 AB: H 3 68. MEv2010
02097+0857 GWP 262 XMI 238. Tob2012b
02098-4052 TOK 427 HIP 10096 is SB2 according to GCS. The separation corresponds to a
period of ~5yr. Tok2015c
02099+3449 HU 1034 Not seen 1948, 1951. No observations since that time.
02103+3322 STF 219 SEI 24. Nsn2017a
02104+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). HaI2001
02106+1027 GWP 263 XMI 239. Tob2012b
02107-1507 FAR 28 Primary is white dwarf WD 0208-153. Far2006
02109+3902 STF 222 59 And.
H 4 129. MEv2010
02109+1341 STF 224 H N 105; BDS 1146 is identical.
02110+0317 GWP 264 XMI 240. Tob2012b
02112+2604 BRT3260 Originally published as BRT 127. Brt1928
02113+4407 ES 2590 Rectilinear solution by Hartkopf & Mason (2015). WSI2015
02114+1848 GWP 265 XMI 241. Tob2012b
02115+5739 BU 874 5 Per.
02117-0531 GWP 266 ABL 11. Tob2012b
02117-1927 GWP 267 ABL 12. Tob2012b
02120+0422 SKF1518 A is also a double-lined binary (5.9d) so this is a physical triple. Tok2019b
02122+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.
Neither AC, BC or CD are physically associated. Kiy2015c
02123-0908 GWP 268 ABL 13. Tob2012b
02124+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. MEv2010
T0 converted from negative to positive by subtracting from P. FMR2020c
02124+1249 LDS1126 NLTT 7300/7301 Chm2004
02124-0223 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. Tob2012b
02124-7023 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. Tob2012b
02128+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. MEv2010
02128+0309 GWP 271 XMI 243. Tob2012b
02128-0224 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. Tok2011a
02129+5712 STTA 24 AB and AC: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
02129-0349 GWP 272 ABL 15. Tob2012b
02130+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). Hrt1996a
02131+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). Grf1981b
Mk III Limb-darkened diameter 2.907 +/- 0.048 mas. MkT2003
02132+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). Hel2016
02133+3649 JNN 18 Estimated age 30-300 Myr; masses 0.26 +/- 0.06 and 0.09 +/- 0.03 Msun;
a ~2.8 au. Jnn2014
02135+5926 STI 351 STI1807
02135-0502 GWP 273 ABL 16. Tob2012b
02135-2546 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. Kiy2008
AB: Rectilinear solution by Hurowitz et al. (2013). USN2013a
02136-0945 GWP 274 ABL 17. Tob2012b
02137-0302 H 6 110 H VI 110. B is BD-03@341.
02138-1933 RSS 54 CPD-20@248
02140+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. Mlk2012
02140+1652 GWP 275 XMI 244. Tob2012b
02142+0555 GWP 276 XMI 245. Tob2012b
02142-1811 GWP 277 ABL 18. Tob2012b
02144+3454 HU 807 Motion in separation, with little angular change. Close 1950-1960.
02144-1441 GWP 278 ABL 19. Tob2012b
02145+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. Mlk2012
02145+5912 STI1812 SMA 31.
02145-1103 LDS5373 SLW 102.
02146-0142 GWP 279 ABL 20. Tob2012b
02147+3024 STF 232 H 2 35. MEv2010
02147+1657 GWP 280 XMI 246. Tob2012b
02149+5829 STF 230 B spectrum B9IV.
02149+1353 GWP 281 XMI 247. Tob2012b
02150+5903 MLR 447 Also known as TDS2174.
02152-3507 SHY 415 HIP 10483 + HIP 10385.
02154+1126 GWP 282 XMI 248. Tob2012b
02155+5231 GC 2695 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin & Radford (1977). Grf1977c
02155+1220 GWP 283 XMI 249. Tob2012b
02156+4223 GIC 29 G133-079/G134-019.
NLTT 7438/7440 Chm2004
02157+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. Mlk2012
02157+1046 STF 237 AB: HJL 30. HJL1986
02157-0217 GWP 285 ABL 21. Tob2012b
02157+1657 GWP 284 XMI 250. Tob2012b
02158-1814 HTG 1 Orbit poorly covered, period rather indeterminate. Hei1978c
Additional notes may be found in Burnham (1894). Bu_1894
02159+1416 GWP 286 XMI 251. Tob2012b
02159+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. Mlk2012
02160-0929 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. Jnn2012
02160-1626 GWP 287 ABL 22. Tob2012b
02161+1651 GWP 288 XMI 252. Tob2012b
02161+1630 BPM 50 [PM2000] 83035 + [PM2000] 83004. Gvr2010
02162-2302 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. Kiy2008
02164-0731 SLW 106 = GWP 289 = ABL 23.
02164-1233 SLW 105 = ABL 24.
02164-1632 GWP 290 ABL 25. Tob2012b
02165-2227 LDS3364 NLTT 7520/7519 Chm2004
02165-5131 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. Tob2012b
02167-3100 LDS 71 NLTT 7535/7528 Chm2004
02167-6324 TOK 71 HIP 10621. NOMAD: PM(B)=(0,-30), PM(A)=(18,60).
D is HIP 10754. Tok2011a
02168+4346 GNS 1 Based on 2MASS and AstraLux images, Ginski et al. (2012) conclude the
companion is a background object. Gns2012
02169+5703 STTA 25 B is BD+56@470.
02169+0448 GWP 292 XMI 253. Tob2012b
02169-2322 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. Jnn2012
02171+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. Mlk2012
02172+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 Chm2004
02173+3351 VIG 1 Primary is gam Tri. The B and C components are background stars, the D
component ambiguous. Vig2012
02174+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. HJL1986
02176-5400 RSS 55 CD-54@487
02178+5638 A 1272 V438 Per, a W UMa type eclipsing binary, P = 3.50939d. Zas2012
02179+1941 TOK 72 HIP 10710. Primary is astrometric binary (Makarov & Kaplan 2005) Mkr2005
02179+1614 GWP 293 XMI 254. Tob2012b
02180+5616 UC 29 Primary appears to be a close pair. Cbl2010c
02180+3116 A 959 Primary is eclipsing binary of W UMa type, period 0.31069d. Zas2017b
02180+1958 GWP 294 XMI 255. Tob2012b
02180+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. WaX2015b
02180-1229 LDS 73 NLTT 7592/7593 Chm2004
02181+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. Tob2012b
02186+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. Hor2015b
02186-2940 B 34 AV For, Algol-type eclipsing binary, P = 1.8797 d. Zas2011
02187+3429 STF 246 H III 42, BDS 1165.
HJL 34. HJL1986
H 3 42. MEv2010
02187+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. Hei1992a
02188+5714 BKO 168 AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
02188+0840 GWP 296 XMI 256. Tob2012b
02188+1440 GWP 297 XMI 257. Tob2012b
02190+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. Tob2012b
02204+2456 POU 175 Also known as KU 9.
02204+1617 BPM 51 [PM2000] 85486 + [PM2000] 85504. Gvr2010
02204+0135 GWP 299 XMI 258. Tob2012b
02205+1733 BPM 52 [PM2000] 85552 + [PM2000] 85616. Gvr2010
02209-0954 GWP 300 ABL 29. Tob2012b
02209-5632 RST 51 CD-57@470.
02210-1650 GWP 301 ABL 30. Tob2012b
02211+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. Mlk2012
02212+5651 BU 1171 Not seen in 1951 with 82-inch (Van Biesbroeck). VBs9999
02212+3653 GIC 31 AB,C: NLTT 7710/7708 Chm2004
02213-1057 HJ 3495 B is BD-11@445.
02215-1251 GWP 302 ABL 31. Tob2012b
02215-1354 GWP 303 ABL 32. Tob2012b
02216+2338 STF 254 POU 178.
02219+0824 GWP 304 XMI 259. Tob2012b
02220+0445 TOK 231 Primary is SB1, P= 79.700 d. Companion at 53" is possibly a white Tok2012c
dwarf (Tokovinin & Lepine 2012) Tok2014d
02220-0034 GWP 305 ABL 33. Tob2012b
02222-0348 GWP 306 ABL 34. Tob2012b
02224+5551 BU 875 9 Per. Variable, V474 Per.
02225+2830 FAR 29 Primary is white dwarf WD 0219+282. Far2006
02225-0536 GWP 307 ABL 35. Tob2012b
02225-2349 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 Chm2004
02229+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). Msn1998a
02229-1718 GWP 308 ABL 36. Tob2012b
02229-5106 EHR 1 CPM pair. Ehr2010
02230+0443 GWP 309 XMI 260. Tob2012b
02231+7021 MLR 377 A premature orbit has been published.
Omega corrected from 0.0 to 180.0 by Ruymaekers & Nys (1995) Ruy1995
02231+0246 GWP 310 XMI 261. Tob2012b
02232+6050 MZA 42 DN Cas.
02232-2952 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".4991
02233+2230 LDS3378 NLTT 7840/7842 Chm2004
02233+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. HJL1986
02233+1452 GWP 311 XMI 262. Tob2012b
02236-1056 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. Evs2016a
02239+3330 STF 258 Also known as STF 253.
02242+1016 CHR 199 First detected as an occultation binary by Evans. Evn1980
02244-2253 LDS3382 NLTT 7922/7928 Chm2004
02245-0145 STF 265 HJL 36. HJL1986
02246+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
02246-4050 GC 2912 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Barker et al. (1967). Evn1967
02247+4008 LDS3381 NLTT 7887/7890 Chm2004
02249+5153 ES 764 B is BD+51@567.
02249+3039 UC 733 AC: Candidate on Tokovinin list, now reconfirmed as CPM. The primary
hosts an exoplanet. Tok2013c
02250-1501 GWP 312 ABL 37. Tob2012b
02252+1217 BRT1170 1deg error in WDS designation, apparently an error in transcribing
coordinates from the original source.
02253-0802 GWP 314 ABL 39. Tob2012b
02253-1242 GWP 313 ABL 38. Tob2012b
02255-1834 GWP 315 ABL 40. Tob2012b
02256+5017 BUP 31 65 And.
02257+6133 STF 257 The primary is SB1 V559 Cas, P = 1.58 d.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
02257+0846 GWP 316 XMI 263. Tob2012b
02257-2119 HJ 3500 HIP 11324. B = HIP 11323. Both components are below the MS, the true
parallax should be 12.6 mas (as for the B-component in Hipparcos). Tok2011a
02258-1038 HJ 2140 Identical with HJ 2134, 4 minutes west.
02259+1747 JNN 19 LP 410-22.
02260+4228 LDS3383 Aka SLN 57.
02260-1520 H 3 80 H III 80. A is a variable of the Alpha CVn type, AB Cet, and a
spectroscopic binary.
02262+3428 HDS 318 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.48 +/- 0.19, 1.81, and 1.80 Msun, respectively. Mlk2012
The spectroscopic orbit of this pair has been computed. Grf2018e
Orbital parallax 21.02 +/- 1.5 mas. Mass-A is 0.99 +/- 0.15 \msun. ATl2021
Mass-B is 0.95 +/- 0.13 \msun.
Mass-A is 1.08 +/- 0.07 and Mass-B is 0.96 +/- 0.06 \msun. EEA2021
02262-0833 GWP 318 ABL 42. Tob2012b
02262-1602 GWP 317 ABL 41. Tob2012b
02263+0618 VIG 2 The B component appears to be a faint background star. Vig2012
02265+5417 STF 260 HJL 37. HJL1986
02268+5853 HD 14947 Garmany & Stencel (1992 A&AS 94, 211) include this star in Per OB1. Msn1998a
02268+1034 STTA 27 B is BD+09@322. A is VW Ari, a Delta Scuti-type variable.
02269+3733 ADM 2 WSP 33. WASP-33. Primary is del Sct-type variable and exoplanet host. Adm2013
02270-0326 GWP 319 ABL 43. Tob2012b
02272+0309 GWP 320 XMI 264. Tob2012b
HIP 11417. SB, no orbit. NOMAD: PM(B)=(-12,-68), V=14.73. Nrd2004
Primary is SB2, P=5.997d, but the mass ratio is unknown. Tok2014d
02273+5433 LAW 10 LSPM J0227+5432. Law et al (2008) derive a distance of 18.6 +9.5/-3.4 Law2008
pc and a projected separation of 13.2 +7.2/-2.2 au. Estimated spectral
types are M4.5 and M5.
02273-0304 GWP 321 ABL 44. Tob2012b
02274+3059 INN 1 Rotation periods 12.1d (AG Tri, 13.7d wrong) and 4.7d. Skf2013
02274+1807 GWP 322 XMI 265. Tob2012b
02278+0426 A 2329 Using the Hipparcos parallax value of 60.22 +/- 1.75 mas, the orbital
elements of Andrade (2007) yield a mass sum of 1.25 +/- 0.14 Msun. Ana2007
Masses of the two K7V components are estimated at 0.63 +/- 0.01 and
0.62 +/- 0.01 Msun.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.37 +/- 0.12, 1.25, and 0.65 Msun, respectively. Mlk2012
02279+4710 BWL 10 AB: Primary is a probable member of the AB Dor moving group. Bwl2015
02280+0248 GWP 324 XMI 266. Tob2012b
02280-0520 GWP 323 ABL 45. Tob2012b
WDS designation corrupted at some point to 02280-0303. Corrected.
02280-3349 SHY 140 HIP 11477 + HIP 11448.
02281+3251 ES 2407 GCB 6.
02282+5423 STF 267 B is BD+53@530.
02282+2952 STF 269 STT 41. May also be H 1 21.
02284-0404 GWP 325 ABL 46. Tob2012b
02286+5521 ES 872 There is a difference of 18 degrees in the measured angles. The Espin
measure appears correct. Es_1910b
02286-0704 A 447 WSP 77.
02287+1850 GWP 326 XMI 267. Tob2012b
02287-3114 TOK 73 HIP 11537. The V-photometry is affected by small separation. B is red
in the V-K color, variable? Astrometric binary in HIPPARCOS (Makarov
and Kaplan), possibly new triple? Mkr2005
PMS star (Torres et al. 2006). TrC2006
SIMBAD: PMS star and X-ray source 1RXS J022843.6-311332. Tok2011a
Companion is partially resolved in 2MASS images, for that reason the
star is not found in the 2MASS point-source catalog. Pre-main-sequence
star according to SIMBAD. Tok2012a
A hierarchical quadruple. The resolved pair has an estimated period of Tok2020h
3000 years while their are two closer spectroscopic components, one
with a period of 22d while the other is 1146d.
02288+3215 WOR 2 Tamazian et al. derive a dynamical mass sum of 1.40 +/- 0.25 Msun Tam2005
and classify the stars as K6-7V and M0V. Absolute magnitudes of
the two components are estimated at +8.0 and +8.6, leading to
individual masses of 0.65 and 0.61 Msun, in good agreement with
the dynamical mass sum.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.46 +/- 0.20, 1.25, and 0.55 Msun, respectively. Mlk2012
02288-0826 GWP 327 ABL 47. Tob2012b
02290-0302 GWP 328 ABL 48. Tob2012b
02291+6724 STF 262 iot Cas. The primary is an unresolved binary, also an Alpha CVn
CHR 6 type variable, P = 1.74 d, and an astrometric, spectroscopic, and
spectrum variable (Rakos 1962; Klock, AJ 70, 176, 1965). The RV Rak1962
variation has not been confirmed.
Heintz (1962) also detected this pair as a submotion to the visual Hei1962
orbit of the AB pair with a period of 52 years and an amplitude of
0".11. Star C (mag. 8.4, dG4) is probably physical, but Hopmann Hop1960b
(1960) computed a hyperbolic orbit for it, as there is some RV
difference between C and A. q = periastron distance in the true
orbit = 6".7056. All hyperbolic orbits were rejected from the
Fourth and subsequent orbit catalogs. Wor1983
Soderhjelm gives Aa,Ab,B,C quadruple solution (AB in HIP). High Sod1999
mass-sum, strangely well-behaved speckle obs at Delta m=4?
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Drummond et al. (2003) give solution for Aa,Ab incorporating motion of Dru2003
the AB pair. The authors conclude that the motion of B relative to
the CHR pair appears to be rectilinear. Masses of the CHR components
are derived.
1985.8540: This autocorrelogram was remeasured; the new results are
listed in the catalog. McA1987b
STF 262 AB: H 1 34. AC: H 3 4. MEv2010
AC: Hyperbolic orbit. Hop1960b
02291+2331 VBS 6 The inclination must be high.
02294+5532 STF 268 A is a spectrum variable and shell star.
02296+6039 STF 263 A is a possible Beta Cep variable, V528 Cas.
02297-0030 GWP 329 ABL 49. Tob2012b
02297+0134 GWP 330 XMI 268. Tob2012b
02297-0955 GAL 321 Object #69 in Gallo's original list. Gal1912b
02305+2514 STF 271 AB: H N 12. MEv2010
02307-0407 GWP 331 ABL 50. Tob2012b
02308+5533 STF 270 AB: HJL 38. HJL1986
Is there a wobble in the PA of AB? Tok2014d
02309+0158 GWP 332 XMI 269. Tob2012b
02310+1358 GWP 333 XMI 270. Tob2012b
02310+0823 GIC 32 G004-024/G073-059.
02312+0811 LDS3396 Aka NSN 527.
02313-1310 GAL 322 Object #70 in Gallo's original list. Gal1912b
02315+0106 SHY 422 BC: HIP 11736 + HIP 12728.
02318+8916 STF 93 alp Umi = 1 UMi = Polaris. Cepheid variable and spectroscopic binary,
P = 30y. A close companion has been suspected. The close pair,
measured three time from 1937-1939 by R.H. Wilson using an eyepiece WRH1941b
interferometer, was not seen again until Evans et al. (2006) resolved Evs2006
it with HST. Wilson's measures agree with the combined astrometric/
spectroscopic solution by Gerasimovic (1936), although both orbit and Ger1936
measures are called into dispute by the more recent orbit of Wielan et Wln2000
al. (2000), whose solution includes mass estimates, etc.
NPOI Limb-darkened diameter 3.28 +/- 0.02 mas, NOI1999
R = 46. +/- 3. \rsun.
An earlier orbit by Wyller (1957) was rejected from Fourth Orbit Wye1957
Catalog ("amplitude below noise level") Wor1983
Component B = BD+88@@@7. See discussion of this system by Roemer. Re_1965
While Hipparcos parallax of A 7.56 +/- 0.48 from the original mission HIP1997a
and 7.54 +/- 0.011 mas from the re-reduction, the HST-FGS parallax of VlF2007
B = 6.26 +/- 0.24 mas implies that that A is high luminosity and BdH2018
pulsating in the second overtone if AB is physical, i.e., the distance
to B is the same as A.
The C component was observed by Burnham in the late 19th century, then Bu_1894
not seen again until the early 21st century by Daley and Ashcroft. Dal2006a
The extremely large magnitude makes the pair too close for most large
astrometric surveys.
The D component has also been recently recovered in 2MASS data. TMA2003
According to Jim Daley, the R-I color for C is 0.56 and for D it is
0.67. The V-I color for D is 1.08. Dal2006b
Published measures precessed to J2000 are here "X" coded. Measures CIA2024c
precessed back to date of observation to maintain consistency with
other cataloged measures.
Mean diameter of the primary is 3.143 +/- 0.027 mas. At the Gaia
distance of 136.90 +/- 0.34 pc this corresponds to 46.27 +/- 0.42 \rsun
and the mass of the Cepheid is 5.13 +/- 0.28 \msun.
AB: H 4 1. MEv2010
02318-0021 GWP 334 ABL 51. Tob2012b
02319+5742 BU 1314 V425 Per. Variable in light and radial velocity.
02319+0108 LDS9132 Old LDS6132. Primary is confirmed quasar: Z = 1.26.
02320+1822 STF 273 H N 106. MEv2010
02320-1955 BRT 297 LDS3400.
02321-1515 GWP 335 ABL 52. Tob2012b
sig Cet. B is BD-15@@447.
SHY 141. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
02322+5415 HJ 2142 Neither AB, AC or BC are physically associated. Kiy2015c
02323+4630 BRT 330 Since precise position has been corrected from previous precise WSI2002
position null detection not relevant.
02324-1849 GWP 336 ABL 53. Tob2012b
02327+6127 STI 368 Both visual components were observed and appeared to be single. Msn1998a
MZA 8 EL and EM pairs were originally 02326+6128 MZA 8AB and AC, until
match of E component of 02327+6127 to primary of 02326+6128 noticed.
02327+0704 GWP 337 XMI 271. Tob2012b
02328+0021 GRV1174 SLW 119.
02328-3421 LDS9133 Old LDS6133.
02329+3433 GC 3048 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
02329+1502 TOK 12 Estimated period of visual pair 160y. Tok2006
Primary is SB2, P=19.4161d (Katoh et al. 2013 AJ 145, 41) Tok2014d
02330+4852 HJ 2144 B is BD+48@694.
02331-7738 BVD 25 B is CPD-78@59.
02332+7013 RBR 34 Suspected non-single. Hor2002b
02332-2207 DON 35 CD-22@863.
02333+5219 STT 42 Distance small, measures often discordant.
1982.7604: This autocorrelogram was remeasured; the new results are
listed in catalog. McA1987b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.00 +/- 1.28, 4.13, and 2.19 Msun, respectively. Mlk2012
02333-1933 GWP 338 ABL 54. Tob2012b
02333-7554 HJ 3522 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
02335+5732 HJ 2143 B is BD+56@657.
02338-2814 HJ 3506 ome For.
02340-1812 BRG 13 There is insufficient motion between the two epochs of observation of
2MASS J02335984-1811525 to establish common proper motion of the
binary, but the components are nearly equal brightness and color, and
reside at a relatively small separation of ~0.85" hence it is almost
certainly a physical pair. Jnn2012
02342+0916 GWP 339 XMI 272. Tob2012b
02342+0139 LDS9134 Old LDS6134.
02343+4017 AG 42 STF 275.
02344+3542 J 1810 ALI 35.
02344+2040 A 2218 Identification error in ADS. Pair is BD+20 426, not BD+19 375. Cou1970c
02344-4259 HJ 3510 Spectrum: G3/5III/IV.
02347-0752 BUP 32 77 Cet.
02350-1522 GWP 340 ABL 55. Tob2012b
02351-1046 GAL 323 Object #71 in Gallo's original list. Aka J 1452. Gal1912b
02352+0407 TOK 649 Resolved using ANDICAM2. Primary SB? Tok2014d
02353+4017 A 1818 Baize suspected another close pair in the region.
02353-0334 MUG 2 Followup spectroscopy confirmed the B component is a dwarf; estimated Mug2005
mass is 0.286 +- 0.017 Msun. Primary is planet host star. Colors of B Egn2007
component consistent with M1-M4 dwarf with mass 0.31 +/- 0.02 Msun. Met2009
HIP 12048. The B component estimated mass 0.29Msun.
2001.7454: PA is measured in zenith mode. If data collected in
equatorial mode, PA = 183.7. Rbr2011d
CHARA Array Limb-darkened diameter 0.490 +/- 0.049 mas. CIA2009a
R = 2.05 +/- 0.21 \rsun, L = 2.3 +/- 0.1 \lsun,
Teff = 4982 +/- 254 K.
79 Cet A: Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from Marcy et al. CPS2000b
02354-0228 GWP 341 ABL 56. Tob2012b
02355+5948 HIP 12062 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos
Intermediate Astrometric Data with spectroscopic elements by
Latham et al. (2002). They derived component masses 0.96 and 0.45 Msun Lat2002
and an estimated semimajor axis of 35.47 mas. Ren2013
02356+6106 RAO 7 Primary is close astrometric binary; also SB? Tok2014d
02356+3719 STF 279 AB: H N 47.
02358+3441 AG 304 15 Tri. B is BD+34@471.
02359+6338 CTT 3 The B component is BD+62@423.
02359+1515 GWP 342 XMI 273. Tob2012b
02359+0536 STF 281 nu Cet = 78 Cet
The A component is a 714d spectroscopic binary. B is not a binary, so
this is a physical triple. Grf2015a
02359-2830 SWR 4 CPM pair Skf2004
02360-0750 BUP 33 80 Cet.
02360-1312 GWP 343 ABL 57. Tob2012b
02360-2331 GIZ 1 GJ 1048. Discovered by Gizis et al. (2001) on 2MASS images. The A Giz2001
component is K2V; conclude secondary is L1, mass ~0.077 Msun.
Seifahrt et al. (2004) combine 2MASS measure with earlier UK Schmidt Sef2004
near-IR southern survey data to show stars have similar proper motion,
so are likely physical companions.
02361+0653 GKI 1 AB: This object was misidentified as HD 61660 by McAlister (1978). McA1978c
PTI Limb-darkened diameter = 0.941 +/- 0.07 mas, PTI2001
R = 0.729 +/- 0.064 \rsun.
VLTI Limb-darkened diameter 0.936 +/- 0.07 mas, LTI2003a
M = 0.790 +/- 0.039 \msun, R = 0.708 +/- 0.05 \rsun.
CHARA Array Limb-darkened diameter of A : CIA2012f
R = 0.7949 +/- 0.0062 \rsun, L = 0.26790 +/-0.00239 \lsun,
Teff = 4662 +/- 17 K, M = 0.767 \msun.
PLQ 32 AC: GJ 105. Proper motion of A +1811 +1451 (FK5). Spectroscopic binary
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
HIP 12114. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
02362-1656 GWP 344 ABL 58. Tob2012b
02363+4012 BAZ 2 V377 And, Algol-type eclipsing binary, period 4.0632 d. Zas2018
02363-0500 GWP 345 ABL 59. Tob2012b
02363-6329 B 1435 Spectral type F6?
02366+1231 GWP 346 XMI 274. Tob2012b
02366+1227 MCA 7 31 Ari. This system has a small Delta m (~0.1 in the blue, 0.3 in the
red) as determined from lunar occultation measures by Africano et al. Afr1978
Measures in 1982.7659, 1984.7046, and 1988.6544 were based on Hrt1994
reprocessing of archival video data. Hrt2000a
Martin et al. (1998) derive component masses 11.001 +/- 1.969 and
9.407 +/- 1.707 Msun. Mig1998
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 19.08 +/- 2.57, 2.95, and 1.13 Msun, respectively. Mlk2012
02368+1723 BPM 53 [PM2000] 95004 + [PM2000] 94927. Gvr2010
02368-1929 ARA 523 BRT1374. Brt1935b
02369+5953 STF 277 V791 Cas, a Beta Lyr type eclipsing binary, P = 2.88680d. Zas2012
02370+2439 STFA 5 30 Ari. STTA 29. A is 1.1d SB1; AB has estimated period of 34,000y. Tok2006
B is BD+24@375.
HJL 39. HJL1986
SHY 142. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
H 5 49. MEv2010
Primary is SB2, P=1.109d. B is exoplanet host, P=335d. A is F6III, but
on the MS. Tok2014d
RAO 8 BC: Exoplanet host star. Roberts et al. (2015) estimate the spectral
types of B and C as F8V and M1V. Rbr2015a
02370-3435 MUG 12 Primary is GJ 9088 = lam 2 For. Spectral type of comoving secondary
estimated as M5-6, confirmed by follow-up spectroscopy. Mass of
secondary ~0.11 Msun. Mug2014
02371+6232 MLR 31 No significant movement since first resolution. Drd2009
02371+1740 GWP 347 XMI 275. Tob2012b
02371-0926 ITF 62 BD: Originally 02368-0926ITF 62.
02371+0055 LDS5388 Error in WDS designation - incorrect precession of Luyten coordinates? Luy1984
02371-2951 LDS3405 NLTT 8520/8519 Chm2004
02374-5233 EHR 2 Primary is eta Hor. Physical/optical nature ambiguous. Ehr2010
TOK 186 Aa,Ab: The Marion et al. (2014) measure is in good agreement with the Mrn2014
Hartkopf et al. (2012) discovery observation, but hints at a Tok2014a
significantly eccentric and/or inclined orbit. A face-on, circular
orbit with a semimajor axis of 3.6au would have a period of ~3.7y,
which is in line with the 3.0y astrometric period found by Goldin &
Makarov (2007). Gln2007
02376+2250 LDS1132 NLTT 8503/8502 Chm2004
02378+1737 BPM 54 [PM2000] 95638 + [PM2000] 95705. Gvr2010
02380+1418 GWP 348 XMI 276. Tob2012b
02381-0541 SLW 126 Aka ABL 60.
02382+4604 A 1278 A premature orbit has been computed.
02382-1123 STF 288 H 3 79. MEv2010
02383-3012 UC 766 CPM candidate confirmed physical by photometry (2MASS and V mags). Tok2013c
02386+0327 KUI 9 HR 775 in Cetus. Some scatter in measured position angles.
02387-5257 COO 14 Spectrum: F8IV/V + G/K.
SHY 424 AC: HIP 12326 + HIP 12361.
02388+3325 STF 285 H 1 21. MEv2010
02389+1526 AG 43 HU 1043.
02389-5450 HJ 3520 B is CPD-55@444.
02390+6235 STTA 28 B is BD+61@445.
02390+1452 STF 287 H N 107. MEv2010
02392-0016 GWP 350 ABL 62. Tob2012b
02392-0933 GWP 349 ABL 61. Tob2012b
02394-0318 GWP 351 ABL 63. Tob2012b
02396-1152 FIN 312 eps Cet = 83 Cet. Pourbaix gives combined solution for this resolved
SB2, yielding orbital parallaxes and component masses. Pbx2000b
Arenou give combined solution of astrometric orbits and DSBs. Paper
includes masses and distances. Are2000
Systematic errors are clearly present and the period remains in doubt. Fin1954c
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.68 +/- 0.35, 2.39, and 2.40 Msun, respectively. Mlk2012
Docobo & Andrade (2013) derive a dynamical parallax of 41.43 +/- 0.68
mas and component masses 1.37 +/- 0.09 and 1.03 +/- 0.08 Msun. See
paper for extensive notes on this system. Doc2013d
CHARA Array Limb-darkened diameter of A : 2.126 +/- 0.014 mas, CIA2007
R = 0.735 +/- 0.005 \rsun.
02398-1522 GWP 352 ABL 64. Tob2012b
02398-3354 LDS3413 HIP 12411. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
02399+0009 A 1928 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.83 +/- 0.56, 2.33, and 1.05 Msun, respectively. Mlk2012
02399-2429 TOK 205 A faint companion near the detection limit is found, our measures are
uncertain. The estimated long period P ~ 100 yr suggests that the
Hipparcosacceleration of 17 mas yr-2 is spurious. Tok2012a
The tentative resolution on 2011.84 at 78deg, 0".34, dK=3.8 is not
confirmed here, with new good-quality images. The star has constant RV
so could be single. Tok2013b
02401+1148 FAR 30 Primary is white dwarf WD 0237+115. Far2006
02401+0255 UC 771 CPM candidate confirmed physical by photometry (2MASS and V mags). Tok2013c
02402+0436 HDS 347 Mean motion indicates P ~ 90 yr, rho increasing. Msn1999b
02404-1914 RST2285 Despite being nearby the WDSS pair 0240239-191332 appears unrelated.
02405-1341 GAL 324 Object #74 in Gallo's original list. Gal1912b
02406+3420 WNO 43 Aa,Ab: Identified as WNO 13 by Routley. USN1972
GIC 33 AB = G074-039/G074-040. AC = G074-039/G074-041.
AB: NLTT 8633/8634 Chm2004
02407+6117 STF 284 A is a Beta CMa-type variable, V482 Cas.
CHR 208 Both visual components were observed: A was resolved (CHR 208Aa,Ab),
B appeared to be single. Gies & Bolton (1986) found a large scatter Gie1986
in radial velocities (but could not find a suitable period), and this
suggests that at least one component may be a spectroscopic binary. Msn1998a
02407+2704 STF 289 33 Ari. A spectroscopic binary.
HJL 41. HJL1986
H 4 5. MEv2010
02407+2637 STT 43 Scardia et al. (2001) orbit considered preliminary because the arc of Sca2001d
the observed orbit is only 90 degrees and is placed completely around
aphelion. The Hipparcos parallax of 0".01385 +/- 0.00125 gives a mass
sum of 3.1 Msun, an overestimate for a star of type F7V. The dynamical
parallax of 0".0149 agrees well with the measured one.
02410+6539 STF 282 AB: HJL 40. HJL1986
02410+3905 A 1820 AB: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
02410-2506 LDS3414 NLTT 8688/8689 Chm2004
02412-0042 STF 295 84 Cet. A is a Delta Scuti-type variable.
CHARA Array Limb-darkened diameter of A : CIA2013c
R = 1.2080 +/- 0.0288 \rsun, L = 2.1332 +/-0.0825 \lsun,
Teff = 6356 +/- 46 K, M = 1.168 \msun, Age = 2.1 Gyr.
02413+2659 L 55 Since precise position has been corrected from previous precise WSI2013
position null detection not relevant.
02413-0432 BWL 12 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 75-35. Bwl2015
02413-5725 BRG 14 2MASS J02411909-5725185 is yet to be confirmed as a common proper
motion binary, but the color and brightness of the companion are well
consistent with it being bound. Jnn2012
02414+3629 HJ 328 Aka ALI 269.
02415+4053 COU1511 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.86 +/- 1.13, 2.54, and 1.05 Msun, respectively. Mlk2012
02415+1115 GWP 353 XMI 277. Tob2012b
02415-7128 B 1923 Actually a quadruple. Both A (1852d) and B (108d) are spectroscopic Tok2022e
binaries.
02418-5300 JFF 1 Aka CAB 6.
02420+4248 HJ 1123 B is BD+42@588, spectrum B9IVp(Hg,Mn,Eu).
02420-1824 GWP 354 ABL 65. Tob2012b
02421+1351 LDS3416 NLTT 8720/8721 Chm2004
02421-0134 OL 9 Since precise position has been corrected from previous precise WSI2004b
position null detection not relevant.
Aka RST4211.
02422+4242 HJ 1124 Aka BKO 172.
02422+4012 MCA 8 12 Per. SB2 resolved by speckle interferometry by McAlister (1977). McA1977
Elements P = 331.0d, T, e, and longitude of periastron for McAlister McA1978a
solution are from the spectroscopic orbit by Colacevich (1941). Cla1941
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Colacevich (1941).
Martin et al. (1998) derive component masses 1.125 +/- 0.169 and
1.389 +/- 0.193 Msun. Mig1998
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
Bagnuolo et al. (2006) solution combines speckle data with data from Bgn2006
the CHARA Array. Authors derive orbital parallax 41.19 +/- 0.21 mas,
masses 1.382 +- 0.019 and 1.240 +- 0.017 Msun, and a magnitude
difference 0.409 +/- 0.013 mags in K' (2136 nm). Values for omega and
Omega are switched in their Table 3.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.59 +/- 3.80, 2.58, and 1.07 Msun, respectively. Mlk2012
02422-2445 LDS3418 NLTT 8753/8759 Chm2004
02423+1639 BPM 55 [PM2000] 98625 + [PM2000] 98718. Gvr2010
02423+1415 GWP 355 XMI 278. Tob2012b
02424+3837 EVT 1 Aa,Ab: Exo-planet host Tok2014d
02424+2001 BLA 1 Aa,Ab: mu Ari = 34 Ari. Occultation binary, known to have variable
radial velocity. Bag1984b
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.64 +/- 0.47, 5.77, and 2.24 Msun, respectively. Mlk2012
02424+0247 GWP 356 XMI 279. Tob2012b
02424-0214 LDS9135 Old LDS6135.
02424-1358 LDS3419 NLTT 8758/8757 Chm2004
02425+4016 STF 292 B is BD+39@611.
H 4 64. MEv2010
02425+1045 CHR 200 First detected as an occultation binary by Blow et al. Blw1982a
02426-5048 iot Hor Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from Kurster CPS2000e
et al. (2000). HaI2001
HD 17051 No comoving objects found within separation/magnitude range listed.
However, Chauvin et al. (2006) note finding at least one faint Cvn2006
background object.
02426-7947 TOK 362 This 0.6" pair with dK=1.1 is obvious and should have been resolved
both by visual observers and by Hipparcos, yet there are no
indications of previous resolution in the literature. The declination
of -79deg may have something to do with the missed companion, as the
southern sky is less well surveyed for binaries. Tok2013b
02427+3932 J 2401 Jonckheere says is two faint condensations of a nebula. Galaxy .
UGC 2180. J__1962a
02427+1434 GWP 357 XMI 280. Tob2012b
02427-1513 GWP 358 ABL 67. Tob2012b
02428+4249 HJ 2155 B is BD+42@605.
02431+0330 GWP 359 AB: XMI 281AB. Tob2012b
GWP 360 AC: XMI 281AC. Tob2012b
02433+1926 BAG 20 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin et al. (1985). Grf1985b
Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
However, this is a Hyades non-member Grf1988
Grf2013c
02433+1718 BPM 56 [PM2000] 99282 + [PM2000] 99285. Gvr2010
02433+0314 STF 299 gam Cet = 86 Cet = Kaffaljidhma. AC is a CPM pair, according to Alden. Ald1924
AB: Additional notes may be found in Muller (1946). Mlr1946a
02434-3756 TOK 187 Triple. The A-component is 0.955d SB2; the tertiary is resolved with
speckle. As A is located some 1.7m above the main sequence, the object
can be closer than indicated by the Hipparcos parallax of 24.6 mas. Tok2012a
02434-6643 FIN 333 Probably an ambiguous case, although only one solution has been
tested.
More speckle obs needed to define orbit.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 14.55 +/- 4.04, 2.67, and 1.20 Msun, respectively. Mlk2012
02435+2742 35 Ari Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Abt & Levy (1978). AbH1978
02435+1611 BPM 57 [PM2000] 99396 + [PM2000] 99434. Gvr2010
02438-2754 BU 261 Aka HDO 59.
02440-0601 TOK 75 HIP 12764. A is SB, no orbit, dRV= 2.5). Contradictory photometry of Nrd2004
B, it is too close in 2MASS (5"). NOMAD: PM(B)=(-99,-71) V=7.79 (??)
Considering the brightness of B and N*=15, it is almost certainly Tok2011a
physical. A new triple system. See Bonavita & Desidera (2007). Bnv2007
02442+4914 STF 296 the Per = 13 Per. A premature orbit has been computed.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Data appear equally well fit by rectilinear solution - see catalog.
CHARA Array Limb-darkened diameter 1.103 +/- 0.009 mas, CIA2012e
R = 1.319 +/- 0.011 \rsun, L = 2.235 +/-0.040 \lsun,
Teff = 6157 +/- 37 K, M = 1.138 +/- 0.010 \msun,
Age = 4.0 +/- 0.4 Gyr.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: H 3 58. MEv2010
AC and BC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
02442-2530 FIN 379 Aa,Ab: More than one revolution apparently has occurred.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.55 +/- 0.22, 2.20, and 1.02 Msun, respectively. Mlk2012
BSO 1 HIP 12780. A is visual binary FIN 379, 0.1". B = HIP 12779. Tok2011a
02443+5704 STF 293 AB: Additional notes may be found in van den Bos. B__1963b
02443+1600 GWP 361 XMI 282. Tob2012b
02445-1859 GWP 362 ABL 68. Tob2012b
02446+7912 BVD 26 Primary is V405 Cep.
02446+2928 STF 300 H 1 74. MEv2010
02447+6128 KRV 3 Classical Cepheid DF Cas.
02448+4231 LDS3424 NLTT 8830/8829 Chm2004
02448+1536 KIR 7 A close double dwarf pair,spectral types M5V and M5.5V. Kir1999
02449+5456 ES 50 Initially assigned as TDS 94. Corrected 11/27/01.
02449+1007 TOK 1 Aa,Ab: mu Cet = 87 Cet. Considered somewhat uncertain by Tokovinin.
Not resolved by McAlister on several occasions.
A preliminary spectroscopic orbit with a period of 1202 days has been
published by Abt (1965). AbH1965
02449-1336 GWP 363 ABL 69. Tob2012b
02451-1834 tau 1 Eri Despite a large acceleration of 26 mas yr-2, no RV variability was
found in the GCS from two measures. Tok2012a
02452-4344 CPO 29 LDS 78.
BRG 15 Aa,Ab: 2MASS J02451431-4344102 is a member of an approximately equal-
brightness binary with ~50" separation, in addition to being a close
binary discovered with AstraLux. Jnn2012
02452-6700 GLI 18 Spectrum: F5/6III/IV.
02455-6342 HDO 306 gam Hor. A spectroscopic binary.
02456-7114 HDS 357 Primary is CN Hyi, a W Uma type eclipsing binary, period 0.45611d. Zas2012
02457+4456 LDS5393 old LDS6136.
AB: NLTT 8869/8870 Chm2004
GIC 34 AC = G078-004/G078-003 = GJ 3178A+3179B.
02457-3943 B 2077 Astrometric orbit for primary, P=2.303y (Golden & Makarov 2007). PM(A) Gln2007
moves almost towards B, so the increased separation is not reflex PM. Tok2014d
02460-0457 BU 83 A premature orbit has been calculated.
A: Dommanget (1972) astrometric orbit calculated from perturbations Dom1972a
seen to rectilinear motion.
02461+1250 GWP 364 XMI 283. Tob2012b
02462+0536 RAO 9 AB: Primary is HIP 12925. A 13.8m star at 221.7deg, 494.3" appears to
share common proper motion, but the probability of physicality is only
36%. It is likely this star is another member of the Tuc-Hor moving
group. HIP 12925 and 12862 also appear to be a co-moving pair. Tok2013c
AB: The primary is a spectroscopic binary. Tok2014d
Quadruple system with 3-tier hierarchy: a close spectroscopic pair
with yet unknown period, Robo-AO companion D at 1".89, and CPM
companion C at 494" (Tokovinin & Lepine 2012). Yet another star, Tok2012c
HIP 12862, at 0.9deg, also shares common PM and parallax. The stars
are young and belong to the Tucana–Horlogium moving group (Zuckerman .
et al. 2011 ApJ 732, 61). Our photometry places D slightly above the
MS. D was independently discovered by Brandt et al. (2014) by high- Bdt2014
contrast imaging at Subaru. They measured it on 2012.0 at 252.9 deg RAO2015
and 1".893, in excellent agreement with Riddle et al. (2015). Rbr2015d
TOK 651 AC: Tuc-Hor moving group? Additional CPM companions at 725" and 1536". Tok2014d
AD: Too wide to be a companion at 3271", but CPM, common parallax. F
is a rapid rotator (Vsini=109km/s), on main sequence.
02462-0619 GWP 365 ABL 70. Tob2012b
02463+1427 GWP 366 XMI 284. Tob2012b
02464+0301 GWP 367 XMI 285. Tob2012b
02470-0952 A 2608 The northern pair, CD, is slightly fainter Hei1985a
02470-1320 RST3371 Variable: CU Eri.
02472+3611 ALI 38 No star seen at AC catalog location of the purported secondary
- probably a plate flaw.
02473+1812 BPM 58 [PM2000] 102021 + [PM2000] 102010. Gvr2010
02473+1803 GWP 368 XMI 286. Tob2012b
02473+1717 A 2222 CD: Aitken gives the magnitude of B as 13.8. I could not see it at all
on the first two nights, glimpsed it on the fourth, and made a very
uncertain measure on the third. Variable? B__1962d
02474-1733 GWP 369 ABL 71. Tob2012b
02475+1922 STF 305 A premature orbit has been computed.
02476+5357 STF 301 A is a long-period spectroscopic binary, P = 675d.
02476+1014 HJ 655 Hipparcos identified the B component as a candidate for Hyades HIP1998
membership. However, re-reduction of the Hipparcos parallax places VlF2007
the B component elsewhere, so this is an optical pair. Grf2013c
02478-0411 GWP 370 ABL 72. Tob2012b
02479-0529 GWP 371 ABL 73. Tob2012b
02480-0108 GRV 993 SLW 134.
02480-0940 GAL 325 Object #76 in Gallo's original list. Gal1912b
02480-2836 RED 20 One companion is ~10" from CD-29 1020 = 2MASS J02481094-2835382. To
the SW at a milar distance is 2MASS J02480263-2835465. There are no
USNO-B1 proper motions for the fainter stars, but comparison of
Digitized Sky Survey UKST and 2MASS images show little evidence of
significant relative motion. IR colors are consistent with a K0/M3/M6
triple at 60pc. System appears non-hierarchical, with projected
separations of ~600au between each component. Red2007a
02481-1244 GAL 326 Object #77 in Gallo's original list. Gal1912b
02482+2704 LDS1138 HIP 13081. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
LDS1138 NLTT 8997/8996 Chm2004
02483+1532 BPM 59 [PM2000] 102707 + [PM2000] 102652. Gvr2010
02486+1344 GRV 146 NI 4.
Primary is BQ Ari, a W UMa type eclipsing binary, period 0.282335d. Zas2011
02487+3107 GJ 9102 1981.6875: HD 17433 was misidentified as Gliese 113 by Balega et al. Bag1984b
(1984). It is uncertain whether this observation is of HD 17433 or of
GJ 113 = HD 17382.
02488-0301 GWP 372 ABL 74. Tob2012b
02489+3823 ALD 10 First measure probably 90@ in error. Ali1955
02490-1029 BRG 16 The system is precisely at the 3 sigma threshold for statistically
significant exclusion of the background star hypothesis. By chance,
the AB astrometry is just below the criterion (2.7 sigma) and BC is
just above (3.1 sigma), so in principle the BC pair is inconsistent
with chance alignment, if the pair does share a common proper motion
with A. However, the proper motion of the system has of course been
determined based on A, so until the AB physical connection has been
demonstrated to the required accuracy, the 3.1 sigma confidence of the
BC pair is irrelevant. Hence, we label the entire system as
undetermined for now, although it is obviously very likely that the
whole system is indeed bound. Jnn2012
02490-1432 KPP2871 Aka TOI 1201.
02491-1712 GWP 373 ABL 75. Tob2012b
02491-3224 B 1031 bet For
02493+1728 STF 311 pi Ari = 42 Ari. A is a spectroscopic and occultation binary.
AB: H 1 64. MEv2010
02493-1033 STF 315 Rectilinear solution by Hartkopf & Mason (2013), however, the close Hrt2013b
parallax and proper motion argues for an orbital solution. Izm2019
02494+4336 LDS3429 LDS9137. LDS6137.
NLTT 9035/9037 Chm2004
02495+5705 MCA 9 V480 Per.
02496-0932 GWP 374 ABL 76. Tob2012b
02497+1209 CHR 201 First detected as an occultation binary by Evn1983a.
02498-0220 GWP 376 ABL 78. Tob2012b
02498-0346 GWP 375 ABL 77. Tob2012b
02498-2015 HJ 3533 B is BD-20@523.
02498-2434 BU 877 gam 1 For. AB =? LDS 80. Separation and position angle (sf)
agree, as does the DM number from LDS catalog. The quoted primary
magnitude of the LDS pair is much fainter, however - possibly a poor
measure of CB instead?
02499+0856 STF 313 B component is EE Cet, a W UMa type eclipsing binary, P = 0.37992d. Zas2012
02499-0206 GWP 377 ABL 79. Tob2012b
02500+2716 MCA 10 Aa,Ab: 41 Ari = Bharani. Aa is a spectroscopic binary and resolved
interferometer pair.
STT 47 AB: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
H 5 116 AC: H V 116.
AC: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
H 6 5 AD: H VI 5. D is BD+26@470.
02501+1646 GWP 378 XMI 287. Tob2012b
02502+7255 HJ 2157 Also known as STF 298.
Primary is V793 Cas, an Algol-type eclipsing binary, period 1.652303d. Zas2011
02502+1343 SHY 426 HIP 13223 + HIP 13122.
02502+0641 AG 55 AB,C: HJL 42. HJL1986
02502-3551 HJ 3536 eta 2 For
02504+3551 LDS3430 Old LDS6138. LDS9138.
NLTT 9076/9097 Chm2004
02505+1113 BPM 60 [PM2000] 104291 + [PM2000] 104261. Gvr2010
02505-0414 GWP 379 ABL 80. Tob2012b
02506+3819 BUP 34 16 Per.
02507+5554 STF 307 eta Per = 15 Per = Miram. A is a spectroscopic binary. B is BD+55@712.
Mk III Limb-darkened diameter 5.381 +/- 0.055 mas. MkT2003
NPOI Limb-darkened diameter 5.260 +/- 0.073 mas,
R = 173.10 (+9.69-10.80) \rsun, Teff = 4082 +/- 30 K,
L = 7508. +/- 864 \lsun. NOI2023
02507+1910 TOK 76 HIP 13269. The 2MASS PSC companion at 17.2" is likely an artifact (not
detected in J and H bands). A is an astrometric binary. Tok2011a
02507+1601 BPM 61 [PM2000] 104457 + [PM2000] 104476. Gvr2010
02508-3956 SHY 427 AB: HIP 13271 + HIP 13499.
02509+0331 PLQ 36 LDS3432.
02510+1317 GWP 381 XMI 289. Tob2012b
02510+1329 GWP 380 XMI 288. Tob2012b
02510-2100 SEE 20 tau 2 Eri = 2 Eri = Angetenar
02511+6025 STF 306 Spectroscopic binary, also classified Oe5V and O7.5.
AC: See BDS 1430.
AG: G component = A component of 02512+6023.
STI 398 EF: previously 02512+6025STI 298AB, merged with STF 206 system.
fh: previously 02512+6025STI 298bc, merged with STF 206 system.
02512+6023 D 9001 See BDS 1431.
02513+0303 HO 218 Position angle and distance changing rapidly but
period not established. Needs speckle.
02514-1526 GWP 382 ABL 81. Tob2012b
02514-2139 DON 43 Gomez et al. (2016) derive dynamical parallax and component masses:
8.24 +/- 0.22 mas, 1.110 +/- 0.014 Msun, 1.045 +/- 0.013 Msun. Doc2016i
02516+6033 BU 1374 B component spectral type B0III AbH2000
CD: Also known as STI 400.
02516+4803 HJ 2160 AB: Rectilinear solution by Cvetkovic et al. (2017). Cve2017
02517+5921 GIC 35 G246-014/G246-013.
02518+5819 BLL 8 A is a spectroscopic binary. B is BD+57@652.
02518-2117 SEE 21 This very close visual system was discovered at a separation of 0".36 See1898b
and has closed steadily for over 90 years. It is unknown at this
point whether the system is still approaching periastron or has
begun to widen. Hrt1993
02520-5347 BRT2020 CD-54@578.
02521+1536 GWP 383 XMI 290. Tob2012b
02521-6054 HJ 3540 CD-61@515.
02522+1520 BPM 62 [PM2000] 105424 + [PM2000] 105482. Gvr2010
02525+2505 LDS1140 NLTT 9175/9176 Chm2004
02525-1246 LWR 4 EP Eri
02527-1105 GWP 384 ABL 84. Tob2012b
02529+5300 STF 314 AB,C: H 1 38. MEv2010
02529+1040 AG 56 HD 17906, W UMa-type eclipsing binary, period 0.4238 d. Zas2018
02531-1212 GAL 327 Object #78 in Gallo's original list. Gal1912b
02532+4155 LDS9139 Old LDS6139.
02532-1007 GWP 385 ABL 85. Tob2012b
02533+2714 ALP 8 2MASSI J0253202+271333
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in August 2002. AlP2007
02536-0745 GWP 386 ABL 86. Tob2012b
02536-3826 TOK 652 Primary is psi For Tok2014d
02537+3820 BU 524 AB: 20 Per. Barnard gives this as 20 Per = BU 520. Bar1898b
Star A is a suspected variable of Delta Scuti type. A suspected
spectroscopic 3.5 yr period is not confirmed (Scarfe & Fekel 1978). Scf1978
A measure on 1979.5326 was incorrectly attributed to ADS 2200 by
McAlister & Hendry (1982); it actually belongs to ADS 490. McA1982d
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Aristidi et al. (1999) orbit includes mass determination. Ari1999
Docobo et al. (2001) orbit includes mass determination. Doc2001c
Calculated mass sum is 3.88 +/- 0.58 Msun, a bit high for a pair of
mid-F dwarfs. Mut2010b
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.88 +/- 0.60, 2.99, and 1.38 Msun, respectively. Mlk2012
STF 318 AB,C: HJL 43. HJL1986
AB,C: H 3 60. MEv2010
02542+3644 ES 2555 ALI 274.
02542-1225 GWP 387 ABL 87. Tob2012b
02543+5246 LAB 1 Aa,Ab: tau Per = 18 Per. Spectrum composite; G4III+A4V. A is a
long-period spectroscopic binary, resolved by speckle interferometry. Lab1974
Speckle observations have resolved the pair and invalidate an
astrometric solution by Kamper (1969). Kam1969a
van de Kamp & Andersen orbit rejected from Fourth Orbit Catalog Kam1969a
("amplitude below noise level") Wor1983
Time of 1989 mideclipse determined as JD = 2447542.31+/-0.01d. DSH1991
Eclipse duration is 2.09d. Inclination of orbit is 88.74deg.
Time of 1989 mideclipse determined as JD = 2447542.34d. Their model REG1992
results give 16 \rsun, 2.4 \msun, Sp G8IIIa and Teff = 5160+/-150 for
the primary and 2.2 \rsun, 1.8 \msun, Sp A3/4V and Teff = 8970+/-150
for the secondary. The mass ratio is 1.1+/-0.2.
Time of 1989 mideclipse determined as JD = 2447542.302/-0.007d. Smk1990
Eclipse duration is 1.936+/-0.029d. P = 1515.869+/-0.059d.
Time of 1984 mideclipse determined as JD = 2446026.48+/-0.05d. XXX1986
Eclipse duration is 2.3-3.1d.
Zeta Aurigae-type binary.
The elements P, T, e, and longitude of periastron for the McAlister McA1981c
(1981) orbit are from the orbit by Colacevich (1941). Cla1941
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Demircan & Selam (1992). Dmr1992
The 52" distant, visual double BC may be physical.
02544+0946 HJ 658 HIP 13543. B is a known close binary A 2341 of 1.3" separation,
partially resolved in the ANDICAM images in K and V bands. Tok2011a
02544-0030 GWP 390 AB: ABL 88AB. Tob2012b
GWP 391 AC: ABL 88AC. Tob2012b
02544+0635 GWP 388 XMI 291. Tob2012b
02544+1754 GWP 389 XMI 292. Tob2012b
02546+1306 BPM 63 [PM2000] 107057 + [PM2000] 107037. Gvr2010
02548+4332 HJ 2162 Star C is A of HJ 2163, BDS 1479.
02548+2916 BRT 130 1deg error in WDS designation, apparently an error in transcribing
coordinates from the original source. Appears to be the same as COU 677.
02548-0640 GWP 393 ABL 89. Tob2012b
02548+1401 GWP 392 XMI 293. Tob2012b
02548-2754 HDO 58 Aka HDO 61.
02549+1913 GWP 394 XMI 294. Tob2012b
02549-0709 JNN 21 The primary is an SB2 binary with an 11.8 day period (Torres et al.
2002 AJ, 123, 1701). Since the angular confirmed to share a common
proper motion) 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 adopt the mass ratio of 0.58 derived from the
spectroscopic orbit and use the mass corresponding to an M3 spectral
type for the primary. Jnn2012
02550-1402 GAL 328 Object #81 in Gallo's original list. Gal1912b
02552-0800 EGN 2 Pair likely unbound. Egn2007
02552-4549 CPO 113 This is ESO 247-11, B is an interacting galaxies. Dam2010
02553-0348 GWP 396 ABL 91. Tob2012b
02553-1209 GWP 395 ABL 90. Tob2012b
02555+0731 GWP 397 XMI 295. Tob2012b
02556+2652 STF 326 Parabolic orbit by Hopmann (1967). Hop1967
sigma = areal constant in the true orbit = 0.05215 arcsec^2/yr
q = periastron distance in the true orbit = 2".827
Data appear equally well fit by rectilinear solution - see catalog.
02556+1311 HU 1047 Close, position angles scattered. No positive observations since 1937.
02557-1223 GAL 329 Object #82 in Gallo's original list. Gal1912b
02558+3429 LDS9140 BC: Old LDS6140.
NLTT 9308/9312 Chm2004
02558+1909 A 2342 Closing in with little angular change.
02558-1606 GWP 398 ABL 92. Tob2012b
02559+1455 BPMA 3 [PM2000] 107836 + [PM2000] 107938. Gvr2010
02559-1521 LDS3441 NLTT 9361/9360 Chm2004
02560+1221 GWP 399 XMI 296. Tob2012b
02561+2003 HER 6 AC: Additional notes may be found in Herbig (1962). Her1962
CVN 6 Ca,Cb: COR 1Aa,Ab previously cataloged is actually this pair.
02562+2359 JNN 253 Estimated age 1000-10000 Myr; masses 0.07 +/- 0.02 and 0.07 +/- 0.01
Msun; a ~0.4 au. Jnn2014
02563+5852 STF 321 B is BD+58@531.
02563-1816 GWP 400 ABL 93. Tob2012b
02564+1534 BPM 64 [PM2000] 108162 + [PM2000] 108210. Gvr2010
02564-1722 LDS3442 NLTT 9390/9388 Chm2004
02565+6322 MLB 390 Also known as STI 405.
02565+5526 LDS5401 Duplicity first noted by Ross: Ross 364-5. Ros1926
02567+4248 LDS9141 old LDS6141. A is possibly the same as A of LDS2815.
AB: NLTT 9354/9355 Chm2004
02570+1244 BPM 65 [PM2000] 108547 + [PM2000] 108528. Gvr2010
02571-1244 GWP 401 MBL 1. Tob2012b
02572+1157 GWP 402 XMI 297. Tob2012b
02572+0153 A 2413 Component variable? Hln1963
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
According to Scardia et al. (2001), this orbit is now well defined and Sca2001d
will certainly change little in the future; only the period is still
slightly uncertain. The Hipparcos parallax is 0".02012 +/- 0.00150.
This gives a mass sum of 2.1 Msun +/- 29%, agreeing very well with
expected values for a system of type G0. Compared to the orbit
calculated by Scardia in 1980, the total mass of the system, whose Sca1980e
uncertainty was then 55%, is now much better defined. The dynamical
parallax is 0".0193, well in agreement with the measured parallax.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.64 +/- 0.52, 2.04, and 1.05 Msun, respectively. Mlk2012
02572-2458 BU 741 Rica (2012) derived a dynamical parallax of 45.0 mas (compared with FMR2012g
44.51 +/- 2.09 mas from Hipparcos) and a mass sum (using the Hipparcos
parallax) of 1.5 +/- 0.3 Msun.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.46 +/- 0.44, 1.66, and 0.79 Msun, respectively. Mlk2012
02573+3156 DCH 116 21 Per.
02578+4431 STF 328 Statistically the same parallax within the errors would indicate the
components are physical.
02579+6400 STI 409 PTT 7.
02579+0025 STF 332 HJL 44. HJL1986
02581+6912 STF 317 BDS mentions a third star 15 sec f at 102.4@.
02582+0310 GWP 403 XMI 298. Tob2012b
02583-0002 GWP 404 MBL 2. Tob2012b
02583-4018 PZ 2 the Eri = Acamar. A is a spectroscopic binary.
02584-0135 A 208 C is BD-02@528.
02585-1453 GWP 405 MBL 3. Tob2012b
02586+2408 BU 1173 Star C (mag. 13, 4.6") is probably physical.
02586+1741 HO 498 Last star in a row of four. STT 49 20' n, 1.9m f. Ho_1899a
02586+1302 GWP 406 XMI 299. Tob2012b
02586-1628 GWP 407 MBL 4. Tob2012b
02588+4322 LDS2816 B is BD+42@664.
02590-0746 GRV 996 SLW 141.
02592+2120 STF 333 eps Ari. Variable velocity suspected.
Rica (2012) derived a mass sum (using the Hipparcos parallax 9.81 +/- FMR2012g
0.79 mas) of 7.4 +/- 1.8 Msun.
02594+6034 TRN 14 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
Position angle ambiguity solved by Jesus Maiz Apellaniz.
02595+3916 BRT2202 ALI 763.
02596+3849 MLB1002 ALI 764.
02596+0508 BAL2603 J 1811.
02596-1436 LDS3445 NLTT 9570/9569 Chm2004
02596-2516 LDS3446 zet For
NLTT 9579/9563 Chm2004
02598+3856 LAW 11 LSPM J0259+3855 = NLTT 9527. Law et al (2008) derive a distance of Law2008
18.8 +9.3/-3.4 pc and a projected separation of 17.6 +9.4/-2.8 au.
Estimated spectral types are M4.5 and M5.5.
03001+6244 STI 417 MLB 391.
03001+3911 ALI 765 A is the eclipsing binary ST Per.
03001+1139 BPM 66 [PM2000] 110407 + [PM2000] 110416. Gvr2010
03002-1110 BRT2627 J 1454.
03006+4753 A 1529 Round 1951 - 1954.
03007+5700 KR 15 Heintz gives the correct identification and position. Hei1983a
03008+1527 BPM 67 [PM2000] 110893 + [PM2000] 110922. Gvr2010
03009+5940 STTA 31 B is BD+59@581.
03009+5221 STF 331 Both components are spectroscopic binaries.
H 3 36. MEv2010
03011+4453 HJ 2167 AB: HJL 45. HJL1986
03012-1816 GWP 408 ABL 94. Tob2012b
03013+6035 MLR 108 V1018 Cas, an Algol-type eclipsing binary, period 4.12781d. Zas2011
03013-0636 GWP 409 ABL 95. Tob2012b
03014+1607 BPM 68 [PM2000] 111250 + [PM2000] 111338. Gvr2010
03014+0615 HDS 385 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.20 +/- 0.32, 1.76, and 1.82 Msun, respectively. Mlk2012
Teff for A & B : 5670 +/- 100 and 5580 +/- 100 K Mda2018
R for A & B : 0.877+/-0.08 and 0.821+/-0.07 \rsun
L for A & B : 0.71 +/-0.06 and 0.59 +/-0.09 \lsun
M for A & B : 0.99 +/-0.19 and 0.96 +/-0.15 \msun
Age = 11.5 +/- 2 Gyr.
03014-1409 GWP 410 ABL 96. Tob2012b
03015+6029 ALV 1 RAFGL 4029 IRS 1. Massive YSO, member of cluster of IR sources. Alv2004
03015+3225 STF 336 SEI 26. Nsn2017a
03019-1633 RST2292 AB: LDS3448.
A : M = 0.257+/-0.014 \msun, R = 0.268+/-0.027 \rsun. WJG2019b
B : M = 0.215+/-0.014 \msun, R = 0.236+/-0.027 \rsun. WJG2019b
C : M = 0.161+/-0.014 \msun, R = 0.197 /-0.027 \rsun. WJG2019b
03021+0005 GAU 2 BAL 652.
03023+4124 STF 337 B is below MS in both (V,V-K) and (J,J-K) CMDs: wrong plx(B)=39.9mas!
Wrong PM(B) in HIP? Tok2014d
03023+1820 A 2414 A premature orbit has been computed.
03023+0405 alp Cet Menkar
1975.634: Disk possible marginally resolved (0".014 +/- 0".005) at 400
and 425 nm.
1975.639: Disk possible marginally resolved at 460 nm. Bla1977a
03023-7154 FIN 360 the Hyi. Not seen for certain 1962-1969, and not observed since.
Needs speckle.
03024+4204 BRT1135 LDS2824.
03025-1516 HJL1114 IR Eri. A combined interferometric/spectroscopic solution by
Halbwachs et al. (2016) yields masses 0.982 +/- 0.010 and 0.8819 +/-
0.0089 Msun. HJL2016
03027-0741 BU 11 rho 2 Eri = 9 Eri. Note: this is not p Eridani (= 01398-5612DUN 5).
03030-0205 STF 341 Primary is possible SB? On Keck RV program, but only small RV var. Tok2014d
A 1136d spectroscopic solution for the B component has been found Tok2019g
making this a triple system.
03031-0049 GWP 413 ABL 97. Tob2012b
03032-0215 J 1455 BAL 21.
03033-1848 GWP 414 ABL 98. Tob2012b
03034-0804 LDS5409 A possible wide companion to 2MASS J03032132-0805153 at 172" with
similar proper motion is noted in WDS. Jnn2012
03035+2304 HDS 389 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.50 +/- 0.27, 1.91, and 1.79 Msun, respectively. Mlk2012
Primary is SB, P(AB)=2152d=5.89y. Metchev & Hillenbrand (2009) Met2009
resolve AB and list two faint optical(?) companions at 4", dK~5. Tok2014d
Teff for A & B : 6140 +/- 100 and 5300 +/- 100 K Mda2018
R for A & B : 1.234+/-0.05 and 0.820+/-0.05 \rsun
L for A & B : 1.94 +/-0.08 and 0.48 +/-0.10 \lsun
M for A & B : 1.18 +/-0.22 and 0.84 +/-0.12 \msun
Age = 3.5 +/- 1.5 Gyr.
03036+3627 BUP 37 The COU 869Aa companion was suspected by Burnham. Bu_1913
03036-1001 GWP 415 ABL 99. Tob2012b
03036-2536 BRG 17 One or both of the stars in this system must be highly variable. The
magnitude differences between the primary and secondary vary from 5.14
mag to 1.72 mag between different observations in Bergfors et al. Brg2010
(2010) and here. In contrast to the individual note on this system in
Bergfors et al., we assume here that the designation LTT 1453 refers
to the primary star. Jnn2012
First noted as a likely binary by Makarov & Kaplan (2005), based on Mkr2005
significant differences between Hipparcos and Tycho proper motions,
then later resolved as part of the Astralux Lucky imaging survey by
Bergfors et al. (2010) and Janson et al. (2012). Their 2008 and 2010 Brg2010
measures, together with measures from 2011 reveal a constant Jnn2012
separation but a P.A. changing by ~3 deg/yr. Bwl2015
03038+0608 KPP3161 A : Teff = 6113 +/- 40 K, M = 1.06 +/- 0.06 \msun. XXX2020a
B : Teff = 18200 +/- 3000 K, M = 1.12 +/- 0.15 \msun.
03039+1514 BPM 69 [PM2000] 112964 + [PM2000] 112917. Gvr2010
03041+3509 POP 11 Popovic coordinate offset was apparently in error. Pop1969c
03042+6142 LDS9142 Old LDS6142.
03044+2118 JNN 23 The close (~0.40") companion to 2MASS J03042184+2118154 is counted as
an unconfirmed binary companion, since it has not yet been tested for
common proper motion. Jnn2012
03045+3844 SMA 33 ALI 766.
03046-5119 DUN 10 B is CD-51@706.
SHY 433. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
HIP 14307 and 14313 form a 38" pair belonging to the FG-67 sample.
TOK 428 AC: AC is not co-moving. C=HIP14257 has different parallax Tok2014d
TOK 428 Ba,Bb: The component B is resolved here at 0".19. The estimated
period of Ba,Bb is ~25yr. No motion is seen in 2 months. The subsystem
Ba,Bb is also manifested by asymmetric line profiles (Tokovinin, in
preparation). The A component has never been observed at high angular
resolution. Tok2015c
03047+6346 STF 335 B is BD+63@388.
03048+5330 WRH 29 Aa,Ab: gam Per = 23 Per. SB2. Spectrum composite: G8III+A2V. WRH1955
zeta Aurigae-type binary.
1975.781: Uncertain angle readout Bla1977a
Analyses of the spectroscopic/interferometric orbit are given by McA1982a
McAlister (1982) and Popper & McAlister (1987). Elements P, T, e for Ppp1987
the McAlister (1982) orbit are from the spectroscopic orbit by
McLaughlin (1948). MLa1948
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
McAlister (1982). McA1982a
Pourbaix gives combined solution for this resolved SB2, yielding Pbx2000b
orbital parallaxes and component masses.
1998.657: Absolute quadrant determined by triple-correlation technique Pru2002b
The physical nature of visual companion B (57", mag. 11) is uncertain.
Aa,Ab: Malkov et al. (2012) derive dynamical and spectroscopic masses
5.80 +/- 88.31 and 4.72 Msun, respectively. Mlk2012
NPOI Limb-darkened diameter 3.894 +/- 0.018 mas, Sp = G8III, NOI2018
R =31.21 +/- 1.195 \rsun, Teff = 4589 +/- 58 K, L =389.6 +/-35.5 \lsun,
M = 3.64 +/- 0.25 \msun, Age = 0.23 +/- 0.05 Gyr.
03048-0603 GWP 416 ABL 101. Tob2012b
03049+3446 HU 812 Hussey position angle 1902: 199.4@. Probably wrong quadrant. Hu_1905a
HIP 14342. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
03052-0156 GWP 417 ABL 102. Tob2012b
03052-3725 BRG 18 This target, like BRG 23, gives conflicting information about whether
the AB pair is physically bound. The brightness and color are fully
consistent with B being an M3.5 companion to the M2.0 primary.
Furthermore, the separation is only 0.2", and the whole field is
otherwise empty. This indicates physical companionship. However, the
deviation from the expectation of a background source is only 1.1
sigma, and the companion has moved 3.6 times closer to the background
expectation than its original position where the motion has a 14 sigma
confidence. This, by contrast, suggests a chance alignment. Since the
magnitude of motion is not inconsistent with what could be expected
for orbital motion of a real physical pair, we keep it as binary in
our analysis, but we note that further observations will be necessary
in order to resolve this issue satisfactorily. Jnn2012
03054+2515 STF 346 52 Ari. AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 9.10 +/- 6.84, 6.89, and 3.39 Msun, respectively. Mlk2012
03054-1432 GWP 418 ABL 103. Tob2012b
03055+0234 BAL1630 OL 183.
03056+1150 GIC 36 G005-013/G005-012.
03056-0238 GWP 419 ABL 104. Tob2012b
03058+3202 ES 326 BC: SEI 27. Nsn2017a
03059+1302 BPMA 4 [PM2000] 114294 + [PM2000] 114392. Gvr2010
03061+7925 STF 320 Spectroscopic binary? Spectrum composite; M1III+F7IV.
03063-1243 LDS3452 NLTT 9888/9881 Chm2004
03064+1545 ALP 9 2MASSW J0306268+154514
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in February 2003. AlP2007
03069+4022 A 1532 Also known as V568 Per.
A is a 1325d spectroscopic double which cannot be this pair. Tok2019b
03071+3757 BRT2203 ALI 513.
03072-0520 GWP 423 ABL 105. Tob2012b
03073-1346 CRJ 7 Crepp et al. (2015) determine effective temperatures for the A and B
components of 5680 +/- 40 and 978 +20/-43K. Spectral types are G3V and
T5.5 +/- 1, masses 0.95 +/- 0.02 and >51.9 +3.6/-4.3 Mjup,
ages 4.6-10 Gyr. CrJ2015
03074+5831 RAFGL 437 Shows subarcsecond monopolar nebula extending towards SE at PA
135 +/- 10deg. Alv2004
03075-7859 HJ 3568 A is a spectroscopic binary.
03076-4702 TOK 206 The companion with q = 0.29 is resolved with NICI but unresolved with
speckle, being too faint in the optical. Tok2012a
03077+3637 ENG 11 B is BD+36@631.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
03078+2533 TOK 234 The B component was suspected of duplicity (0".253, 240.5deg,
dI=2.7mag) by RoboAO, but the pair was not accepted as real Tok2014d
03078+1223 BPM 70 [PM2000] 115596 + [PM2000] 115589. Gvr2010
03078-2750 VIG 3 Optical/physical nature of the faint companion is undefined. Vig2012
03079-2813 LDS 86 AB: NLTT 9987/9985 Chm2004
03080-0135 GWP 425 ABL 107. Tob2012b
03080-0537 GWP 424 ABL 106. Tob2012b
03082+4057 LAB 2 Aa,Ab: bet Per = 26 Per = Algol , prototype of the Algol-type binaries.
The eclipse phenomena, known since historical times (although the time
of minimum brightness was first measured by Montanari on 8 Nov 1670)
was first explained as an eclipsing binary by Goodericke as early as
1782. According to R.G. Aitken, this was verified when it was noted as A__1935f
the second spectroscopic binary based on photographic spectra
obtained by Prof. H.C. Vogel at Potsdam in November, 1889. Belopolsky
discovered a variation in the radial velocity with a period of order
1.8 years, later resolved by Labeyrie and his speckle camera in 1973; Lab1974
the magnitude difference is about 2.5.
The binary, a radio and X-ray source, is triple (and possibly
quadruple, but the variation with the 32 yr period is more probably an
apsidal rotation of the eclipsing pair).
The spectroscopic data were discussed by Hill et al. (1970, 1971). HlG1970
ADS lists several distant, faint, and probably optical companions. HlG1971
Elements P, T, e, and omega for Labeyrie et al. (1974) orbit adopted Lab1974
from the spectroscopic orbit of Hill et al. (1971).
Analysis of the spectroscopic/interferometric orbit is given by
Bonneau (1979) Bnu1979
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Hipparcos astrometric solution adopts some elements from the orbits of HIP1997d
Pan et al. (1993) and MkT1993a
Gatewood et al. (1995). Gat1995
Peterson et al. (2011) orbits of both the outer (LAB 2Aa,Ab) and Ptn2011
inner (CSI 1Aa1,Aa2) are based on VLBI measures combined with
speckle and radial velocity data. Assuming masses of the primary and
secondary of 3.70 and 0.79 Msun, respectively, they derive a mass for
the tertiary of 1.51 +/- 0.02 Msun.
BU 526 AB: Additional notes may be found in Burnham (1894). Bu_1894
03084+4020 BRT2204 ALI 1031.
03084+2620 OSO 14 G037-026. Not a common proper motion pair, based on color Oso2004
03084-2410 LDS 87 NLTT 10008/10007 Chm2004
03084-7033 HLN 19 DAM 782.
03087+1736 COU2680 BD+17@499a.
03087-1432 GWP 426 ABL 108. Tob2012b
Not a double star, but an edge-on galaxy: USNO-B1.0 proper motion is Skf2012
spurious.
03088-0952 GWP 427 ABL 109. Tob2012b
03090+4415 STF 351 B is BD+43@637.
03090+1740 COU 358 BD+17 501a. Mistaken identification with BD+17 501 led to earlier
incorrect WDS designation as 03088+1801.
03091+4937 BUP 38 iot Per. Proper motion of A +1263 -091.
03092+0728 STFA 6 STTA 32. B is BD+06@487.
03094-3004 LDS3460 NLTT 10074/10076 Chm2004
03095+4544 HDS 404 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 0.90 +/- 0.09, 0.87, and 0.75 Msun, respectively. Mlk2012
03095+4451 ES 2596 kap Per = 27 Per = Misam. A is a spectroscopic binary.
03096+0512 A 2030 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.41 +/- 0.32, 2.11, and 1.05 Msun, respectively. Mlk2012
03096-0054 CHE 75 Aka BAL 281.
03098-1238 GWP 428 ABL 110. Tob2012b
03099-0654 UX Eri Multiple system including contact binary. Pribulla & Rucinski (2006) Pbl2006
estimate the mass of the contact pair at 1.901 Msun and the minimum
mass of the wider component at 0.59 Msun.
03099-8332 HJ 3582 Spectral type of A : F2IIISrEuSi: Estimated orbital period ~100,000y. Soz2017
03101+0210 RST5197 Aka TDS2463.
03101-6355 HJ 3559 B is CPD-64@231.
03104+0238 OL 177 Not found by Heintz at IDS position. Position corrected. Hei1990b
03104-0004 GWP 429 ABL 111. Tob2012b
03105+5040 LDS9143 Old LDS6143.
03107+2226 LDS3461 NLTT 10112/10110 Chm2004
03107-4023 LDS9144 Old LDS6144. Recognized to be the same as LDS5414 by John Greaves. Grv2006c
03108+3724 LDS9145 Old LDS6145.
NLTT 10082/10091 Chm2004
03110+1648 SPF 1 L dwarf 2MASS J03105986+1648155 resolved into close components at L/T
boundary. Approximate orbital period 72 +/- 4 years, distance 25 +/- 4
pc, system mass ~30-60 Mjup. Spectral types of both components are
estimated at L9 +/- 1. Spf2010
03112+2225 H 5 117 Also known as STF 359.
AC: Rectilinear solution by Friedman et al. (2011). USN2011a
03113+3937 BLL 10 ome Per = 28 Per
03117+8128 STF 327 A is a spectroscopic binary.
03118+3525 GIC 37 G095-014/G095-013.
03119+6131 HDS 407 A is also a 59d spectroscopic binary. Tok2019b
03121-2859 HJ 3555 alp For = 12 Eri = Dalim. The magnitude of B is uncertain and has been
suspected to vary. Another century is needed for apastron coverage.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
A is GJ 127. B is possible SB. Variability of RV(B) is based on
historic RV (Eggen, van den Bos) Tok2014d
03121-6420 HJ 3562 B is CPD -64@231.
03122+3713 STF 360 A premature orbit has been calculated. Data appear equally well fit by
rectilinear solution - see rectilinear elements catalog.
A is SB1, P=415d. B is possible long-period SB. Tok2014d
03123-2727 LDS 88 NLTT 10222/10227 Chm2004
03124-4425 JC 5 Ma,Mb = 1.365 +/- 0.031, 1.134 +/- 0.024 \msun. GmJ2022
03124-1157 GWP 432 AB: ABL 112AB. Tob2012b
GWP 433 AC: ABL 112AC. Tob2012b
03124-4425 JC 8 Variable RV of AB, not explained by the visual motion, has been
reported (Eggen 1965), but Heintz's mass ratio does not support Egg1965b
the presence of a fourth body. Hei1979a
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.59 +/- 0.73, 2.18, and 3.82 Msun, respectively. Mlk2012
HJ 3556 AB,C: Star C (mag. 9.2, 3.5") is in slow retrograde motion.
Heintz (1979) gives AB orbit, attempts AC orbit with P=987yr. Hei1979a
The motion of AC is not directed away from PM(A), hence physical. Tok2014d
03125-3449 LDS 89 LDS5418.
03127+7133 STT 50 A premature orbit has been calculated.
Bespalov (1961) has a = 1".618, Finsen & Worley (1970) assume this Bsp1961
is a misprint. Fin1970b
03128+3720 WZ 6 ES 2556.
03128-0112 HJ 663 94 Cet.
AB: B is PMS star and SB1 (P=2.026y). Planet (P= 1.2y=535.7d) around
A. Is this true planet or Ba,Bb effect? Tok2014d
CHARA Array Limb-darkened diameter 0.788 +/- 0.026 mas, CIA2008c
R = 1.930 +/- 0.067 \rsun.
TOK 654 AF: CPM companion HD 20619 = GJ 135: 7.03V, G1.5, HD 20169 at 133'
from AB (0.7 pc) Tok2014d
03130+3254 LDS9146 AB: Old LDS6146.
B is deeply below MS, blue in V-K and J-K. White dwarf? WDS: too fast
motion of AB, optical? Hyades cluster. CfA: RV var? Tok2014d
Hyades cluster. The 2MASS companion B can be physical. Tok2014d
Previous AD companion, TOK 655, is the same as the known AB pair. The Dam2015d
Luyten measure was poor.
03130-0343 GWP 434 ABL 113. Tob2012b
03132+1710 BPM 71 [PM2000] 119048 + [PM2000] 119061. Gvr2010
03134-0852 GWP 438 ABL 114. Tob2012b
03135+4417 ES 559 Also known as LDS9147, LDS6147, and LDS2836. These were all recognized
by John Greaves (personal corres.) to be the same pair.
NLTT 10231/10232 Chm2004
03136+3909 STF 364 HJL 46. HJL1986
03141+5934 TRN 15 CC Cas. Classification in Mason et al. (1998) is from the tomographic Msn1998a
analysis of Hill et al. (1994 A&A 282, 455).
The image rotator was in an unknown state, so two possible theta
values are listed for the 2001.7452 observation - one for zenith up
and one for north up. Trn2008
03141+0832 GIC 38 G079-015/G079-016.
03144-0227 GWP 440 ABL 115. Tob2012b
03146-0940 GWP 441 ABL 116. Tob2012b
03147-3533 GAA 4 TZ For, a detached eclipsing binary. A combined spectroscopic/
interferometric orbit by Gallenne et al. (2016) yields a semimajor
axis of 0.5564 +/- 0.0001 au, distance 185.9 +/- 1.9 pc, and the
following component parameters:
mass (Msun): 2.057 +/- 0.001 1.958 +/- 0.001
radius (Rsun): 8.28 +/- 0.22 3.94 +/- 0.17
luminosity (Lsun): 1.57 +/- 0.02 1.36 +/- 0.03 GaA2016
03149-1400 HJ 3558 HJ 3551 is identical.
03150+0101 GIC 39 G077-035/G077-034. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
03151+1618 HU 1055 The companions C, D, and E, given in the ADS, do not exist. They
should be under ADS 2426. B__1963b
03154-6930 R 22 Also appears to be R 27.
03158+5057 HU 544 A = V572 Per: eclipsing binary of Algol-type, period 1.21317 days. Zas2015
03158-0849 SHY 154 HIP 15197 + HIP 15244. Primary is zet Eri = Zibal.
03160+4853 LDS9148 Old LDS6148.
NLTT 10355/10353 Chm2004
03160+3441 HO 503 A spectroscopic binary and ellipsoidal variable, V423 Per.
03162+1302 BPMA 5 [PM2000] 120872 + [PM2000] 120882. Gvr2010
03165-0642 GWP 443 ABL 117. Tob2012b
03165-3541 SHY 439 AB: HIP 15239 + HIP 15432.
SHY 439 AC: HIP 15239 + HIP 15152.
SHY 439 AD: HIP 15239 + HIP 15933.
SHY 441 BC: HIP 15432 + HIP 15152.
03166+4943 ES 463 Aka OL 150.
03166+3238 STF 370 According to Burling, the long unconfirmed system, 03064+3153HJ 5456,
may also be this pair. Bur2005
SEI 29. Nsn2017a
03167+4237 LDS9149 Old LDS6149.
03167+2639 TOR 4 Formerly known as PAN 1.
03167-0332 TOK 78 HIP 15247. A is SB without orbit, dRV= 6.6. Nrd2004
03168+7830 STF 345 Also known as STF 340.
03168+0501 A 2032 HIP 15253. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
03172+4522 PRV 2 GJ 3213. Pravdo et al. (2006) derive masses 0.370 +/- 0.034 and
0.195 +/- 0.021 Msun. Prv2006
03174+0739 BU 1039 Hyades vB 1. BU 1039AB, with rho = 2".2 and Delta m = 6.0 is outside
the detection window. Msn1993a
AC: HJL 47. HJL1986
AC: SHY 155. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03175+6540 STT 52 A premature orbit has been calculated.
03175-0107 GWP 445 ABL 118. Tob2012b
03175-1222 J 1456 BRT2628. Brt1947
03176-1412 GWP 446 ABL 119. Tob2012b
03177+6108 STI 441 03175+6108SMA 36
03177+3838 STT 53 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.51 +/- 0.99, 2.40, and 1.05 Msun, respectively. Mlk2012
03178-7029 R 28 Aka RSS 62.
03180-6656 EHR 3 Physical/optical nature undefined. Ehr2010
03182-6230 BNU 2 Aa,Ab: zet 2 Ret. B has common proper motion, +1370 +660, and is
CPD-63@217 = zet 1 Ret.
Aa,Ab: Likely a spurious pair. Last measured 1978 and unresolved by
SOAR on 3 occasions 2008-2012. Tok2010
Tok2012d
Tok2014a
Aa,Ab is suspicious, 1 observation in WDS, not binary in Raghavan et Rag2010
al. (2010). Jones et al. (2002) do not detect SB with precise RV at CPS2002b
the AAT. Tok2014d
ALB 1 AB = LDS 92. HIP 15371. See Allen et al. (2000) for information AlC2000
on metallicity, age, galactic orbital parameters, etc.
AB: SHY 16. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03184-0056 AC 2 95 Cet. According to Eggen this pair shares common proper motion with Egg1960
BD -01 474 at 11'.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
03184-0708 LDS3473 HIP 15396. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 10536/10548 Chm2004
03184-2231 SEE 23 15 Eri. CD-22@1146. Motion direct.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.33 +/- 0.80, 3.35, and 1.20 Msun, respectively. Mlk2012
03185+4721 MET 1 V522 Per. Met2004a
03185+1511 LDS9150 Old LDS6150. HIP 15394. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
03186+0827 LUH 6 AC: LSPM J0318+0827S + 2MASS J03184214+0828002. Luh2012b
03187+1527 LDS9151 Old LDS6151. SLE 41.
03187-1834 HJ 3565 A is a spectroscopic binary.
03188-0028 ABT 3 BAL 656.
03188-0321 GWP 447 ABL 120. Tob2012b
03189-0101 BU 1177 Gomez et al. (2016) derive dynamical parallax and component masses:
10.03 +/- 0.77 mas, 0.906 +/- 0.033 Msun, 0.886 +/- 0.032 Msun. Doc2016i
03190-1549 GWP 448 ABL 121. Tob2012b
03192-5306 HJ 3571 CD-53@674.
03193-0232 GWP 449 ABL 122. Tob2012b
03194+6156 JNN 254 G 246-33. Estimated age 35-300 Myr; masses 0.29 +/- 0.11 and 0.17 +/-
0.07 Msun; a ~10.8 au. Jnn2014
03194+0322 STT 557 AB: kap 1 Cet = 96 Cet. Variable? A is a spectroscopic binary.
B is BD+02@521.
03195-2145 JC 1 tau 4 Eri = 16 Eri. A is an irregular variable.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
03199-0321 GWP 450 ABL 123. Tob2012b
03200+6539 BUP 43 Shell star. Light and spectrum variable, BK Cam. May also be a long-
period spectroscopic binary.
03200+3845 BRT2205 MLB 819. ALI 774.
03201-2851 LDS 93 van den Bergh reports a third star at 38@, 105.6". Bgh1958
A is exoplanet host, P=592d. B = HIP 15526 hosts exoplanets with
P=29.1d, 85.1d. Tok2014d
B is CD-29@1229.
NLTT 10636/10635 Chm2004
SHY 157. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03202-1457 LDS3479 NLTT 10629/10617 Chm2004
03202-1632 GWP 452 ABL 124. Tob2012b
03203+1944 STF 376 H 2 76. MEv2010
03203+1625 SLE 42 Hipparcos suspected non-single.
03206+0902 GIC 40 G079-029/G079-030 = GJ 9114AB.
HIP 15572. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
Primary is SB1, P=321.6d Tok2014d
03207+8459 STF 319 Schiller measures 1910.87,331.1@,42.32",7.7-9.2. Shr1913
03207+1736 HJ 3245 See BDS for components.
03210-0054 LDS5420 LDS5420A was B component of 03211-0054ITF 55AB, LDS5420B was ITF 55C
Pairs merged; ITF 55AB --> 03210-0054ITF 55AD (with quadrant flip),
ITF 55AC --> 03210-0054ITF 55BD (also with quadrant flip).
03211-2632 SWR 5 CPM pair Skf2004
03212+2109 COU 259 tau 1 Ari = 61 Ari. A is an irregular variable.
03213+4302 A 1706 LDS2842.
03214+4320 VIG 4 Optical/physical nature of the faint companion is undefined. Vig2012
03216-0841 GWP 454 ABL 126. Tob2012b
03217+0845 STF 380 A premature orbit has been calculated.
03219+4904 WEB 1 B is BD+48@892.
03220+1715 LDS3483 G006-003. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 10701/10698 Chm2004
03220-1636 LDS3485 NLTT 10725/10724 Chm2004
03226-0210 GWP 456 ABL 127. Tob2012b
03226-3011 LDS3487 LDS5422.
NLTT 10762/10761 Chm2004
03227+1717 BPM 72 [PM2000] 124803 + [PM2000] 124860. Gvr2010
03227+1037 GIC 41 BC: 03328+1040 UC 997.
03228-0042 GWP 457 ABL 128. Tob2012b
03229+2949 STF 379 H III 91, BDS 1688.
H 3 91. MEv2010
03230-0548 GWP 458 ABL 129. Tob2012b
03232+4554 LDS9152 Old LDS6152. HD 20835. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
03232-1404 GWP 459 ABL 130. Tob2012b
03233-0337 GWP 460 ABL 131. Tob2012b
03233-0748 BU 531 CHARA Array Limb-darkened diameter of A : CIA2013c
R = 2.4214 +/- 0.0764 \rsun, L = 4.0279 +/-0.1529 \lsun,
Teff = 5261 +/- 65 K, M = 1.056 \msun, Age = 7.2 Gyr.
03233-5000 HJ 3573 LDS 94. A is CD-50@1015, B is CD-50@1014 (Roman).
03234-0710 GWP 461 ABL 132. Tob2012b
03234-1015 HJ 2188 STF 387.
03236+0453 BU 1178 A is a spectroscopic binary.
Greenwich measure of 1921 erroneous. No certain change since 1890. B__1963b
03236-4005 I 468 glimpsed? I__1948a
Soderhjelm (1999) gives possible orbit from two widely spaced visual Sod1999
observations + Hipparcos data.
03236-8116 SHY 161 AC: HIP 15803 + HIP 17184.
03237-0609 GWP 462 ABL 133. Tob2012b
03238+2432 LDS1144 NLTT 10780/10781 Chm2004
03240-0007 GRV 997 = GWP 464 = ABL 135. Tob2012b
03240-2613 HJ 3572 B is CD-26@1270.
SWR 6. CPM pair Skf2004
03242+2347 LDS 884 AB,C: NLTT 10804/10808 Chm2004
03242-1048 GWP 463 ABL 134. Tob2012b
03243+4952 BUP 44 alp Per = 33 Per = Mirfak
03244-1539 A 2909 There are many negative observations. Needs speckle.
HIP 15868. A is the close pair A 2909, 0.1". The 2MASS PSC companion
at 17" is called C in the WDS. Tok2011a
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 0.62 +/- 0.11, 2.10, and 1.01 Msun, respectively. Mlk2012
CfA: SB? P=9115d? =25y? UR at SOAR from 2008.6 to 2012.9, in Mlr1955a
contradiction with orbit of Muller (1955). Tok2014d
A spurious orbit of this ghost pair has been computed which is Doc2016d
contradicted by the many non-resolutions. Tok2019d
03245+4626 LDS9153 Old LDS6153.
03248-1533 GWP 466 ABL 136. Tob2012b
03249+1552 BPM 73 [PM2000] 126226 + [PM2000] 126261. Gvr2010
03249-0356 GWP 467 ABL 137. Tob2012b
03253+1158 BPM 74 [PM2000] 126464 + [PM2000] 126473. Gvr2010
03256-1855 GWP 468 ABL 138. Tob2012b
03257+0551 JNN 255 AB: GJ 3224. Estimated age 300-1000 Myr; masses 0.25 +/- 0.06 and 0.14
+/- 0.01 Msun; a ~6.3 au. Jnn2014
AC: Estimated age 300-1000 Myr; masses 0.48 +/- 0.25 and 0.45 +/- 0.24
Msun; a ~48.1 au. Jnn2014
03259+4540 COU1682 TDS2544.
03261+1229 A 829 Probably ambiguous case, but only one solution has been tested.
03262+2950 ALP 10 2MASSW J0326137+295015
Further observations are required to determine the physical/optical
nature of this pair. AlP2007
Astrometric orbit by Harris et al. (2015) yielded the following
properties: spectral types L3.5+L7, absolute J mags 12.99+14.5,
masses 0.061 +/- 0.010 and 0.044 +/- 0.008 Msun. USN2015
03262-1817 GWP 469 ABL 139. Tob2012b
03263+1709 JNN 256 Estimated age 1000-10000 Myr; masses 0.24 +/- 0.03 and 0.16 +/- 0.03
Msun; a ~20.6 au. Jnn2014
03264+3520 HDS 430 Cvetkovic et al. (2016) estimate spectral types F7 and G8, masses 1.30
and 0.97 Msun. Dynamical parallax is 15.60 +/- 0.44 mas. Cve2016b
03265+5909 GIC 42 G246-036/G246-035.
03266+2843 CHR 9 Aa,Ab: This is UX Ari, an RS CVn type binary that is not eclipsing.
Peterson et al. (2011) orbits of both the outer (CHR 9Aa,Ab) and Ptn2011
inner (CIA 10Aa1,Aa2) are based on VLBI measures combined with
speckle and radial velocity data. Assuming masses of the primary and
secondary of 1.10 and 0.95 Msun, respectively, they derive a mass for
the tertiary of 0.75 +/- 0.01 Msun.
CIA 10 Aa1,Aa2: Orbit of Hummel et al. (2017) corrected for apparent 0.5d Hmm2017b
error in T0 (2456238.134d changed to 2456237.634d). Also, they were
unaware of the wide CPM companion, so erroneously refer to the close
pair as Aa,Ab and the CHR pair as AB.
Aa1,Aa2: Mass of Aa1 & Aa2 = 1.30(0.06) & 1.14(0.06) \msun. Hmm2017b
Teff = 4560(100) & 5670(100) for Aa1 & Aa2. Diameters = 0.97(0.02) &
0.35(0.02) mas. Orbital parallax = 19.20(0.28) mas.
TOK 13 AB: AB is CPM, estimated period 20,000y. Primary is 6.4d SB2.
The spectrum shows 3 components (Fekel, 1986 private communication),
two of which are identified with the 6.44-day system described by
Carlos & Popper (1971), while the third is possibly the component Ppp1971
listed here.
Evolved or bad 2MASS photometry. Tok2006
03266+1406 BPM 75 [PM2000] 127254 + [PM2000] 127284. Gvr2010
03269+1609 BPM 76 [PM2000] 127466 + [PM2000] 127423. Gvr2010
03269-2344 RSS 4 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. Rss1996
03271+1845 CHR 10 Resolution of an occultation binary.
03272+0944 HDS 433 1975.629: Marginally resolved at 450 nm? Bla1977a
Hierarchical quadruple, including 51y, 145d, and 7.14d pairs
(HDS 433AB; MKT 15Aa,Ab; and MKT 15Aa1,Aa2; respectively). The 7d pair
is eclipsing. Nemravova et al. (2016) combine spectroscopy, Nem2016
photometry, and interferometry to derive orbits of all three pairs,
yielding the following component parameters:
Parameter Aa1 Aa2 Ab
Mass (Msun) 2.252 +- 0.027 2.125 +- 0.027 3.89 +- 0.25
Radius (Rsun) 1.700 0.035 1.618 0.039 2.81 0.28
Teff (K) 10700 160 10480 130 14190 150
Mbol (mag) 0.923 0.079 1.120 0.075 -1.14 0.22
(Note: Nemravova et al. refer to the pairs as AC; AB; and Aa,Ab.
However, the HDS pair was assigned components A and B at discovery.) HIP1997a
03276+5847 RAFGL 490 Extended emission seen in H-band, no subarcsecond structure resolved. Alv2004
03276+0954 J 305 May be the same as GJ 3226, which is not in the WDS. At the SIMBAD Dam2017c
precise position of GJ 3226 a measure from Gaia-DR1 is 117.1 deg @
1.530", quite close to the measures of J 305.
03278+5627 STI1984 The relative motion is small but fairly certain; it is smaller than
the proper motions of both components. Therefore, although the
component proper motions are of the same order, we consider this to be
a physical pair. Kiy2012
03278-2352 LDS3496 NLTT 11000/10999 Chm2004
03279+5625 MLB 116 Triple star with weak hierarchy. Motions of all components relative to
each other are small. If we trust the relatively large pm for A from
the WDS, the system is physically bound; however there is an
appreciable discrepancy between this pm and the value given by
Kharhenko & Rezer (2001, Kinemat. Fiz. Nebesn. Tel 17, 409). Therefore
we are not yet able to determine with confidence whether or not the
components are physically bound. Kiy2012
03279-1948 GC 4128 Hipparcos astrometric solution assumed circular orbit (e = omega = 0); HIP1997d
Cluster Melotte 25 #EGG21.
03280+2631 LDS1146 NLTT 10977/10976 Chm2004
03280+2028 STF 394 AB: H 3 77. MEv2010
03282+5628 ES 1777 Relative and proper motions are of the same order, making it
impossible to judge whether the pair is physically bound. Kiy2012
03282+0409 A 2417 BC is also known as V1221 Tau.
03282-1335 GAL 330 Object #94 in Gallo's original list. Gal1912b
03282-3551 I 58 chi 3 For
03284+2248 BAG 2 Aa,Ab: 66 Ari. A is a spectroscopic and occultation binary.
Agreement is poor between this observation and the only other
measurement, by Balega (1988, private communication). Hrt1992b
03284-1425 GWP 470 ABL 140. Tob2012b
03286-1537 LDS3498 NLTT 11020/11021 Chm2004
Also known as GJ 3228A, this star has a wide binary companion at 16" VVO1991
separation (e.g., Weis 1991). Jnn2012
03289+4039 ES 2598 LDS6169.
03289-2723 LDS9154 Old LDS6154.
LHS1549-50.
03291+5956 STF 385 CS Cam.
03291+0118 MET 2 RX J0329.1+0118
03292-0226 GWP 471 ABL 141. Tob2012b
This is the galaxy LEDA 1092357. Dam2017c
03294+4931 BU 1179 34 Per.
Magnitude 11.6 of Burnham is underestimate; mine are similar to the
photometric values of Kuiper (1.93) Baz1954a
03294-2406 GAA 18 AK For
03294-6256 HJ 3580 kap Ret. LDS 100.
03295-1558 GWP 472 ABL 142. Tob2012b
03296+2431 SAR 1 HBC 347 = V1224 Tau.
03297+5955 HLM 2 Aka HLM 42.
03297-0850 GAL 331 Object #95 in Gallo's original list. Gal1912b
03298+8402 STF 343 STF 347.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
03300+5527 STF 390 Aka H N 66.
03301+1258 BPMA 6 [PM2000] 129571 + [PM2000] 129567. Gvr2010
03301-1019 GWP 473 ABL 143. Tob2012b
03302+7402 LDS1572 G221-010/G221-011.
NLTT 10954/10953 Chm2004
Aka GIC 43.
FAR 31 NLTT 10954. Primary is white dwarf WD 0324+738. Far2006
03304-1257 GWP 474 ABL 144. Tob2012b
03305+5418 LEP 15 NI 7.
03305+2006 STF 399 AB: H 4 89 (aka, H IV 89) MEv2010
A component SB1, P=32.5y. Is AB a real physical pair, or just two
members of Hyades? Tok2014d
03307-1926 HDS 441 Cvetkovic et al. (2016) estimate spectral types G2 and G5, masses 1.11
and 1.05 Msun. Dynamical parallax is 24.78 +/- 1.48 mas. Cve2016b
03309+7041 JNN 257 LHS 1553. Estimated age 1000-10000 Myr; masses 0.31 +/- 0.03 and 0.17
+/- 0.02 Msun; a ~7.9 au. Jnn2014
03309+1256 5 Tau Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Harper (1924). Hrp1924
03309-6200 TOK 190 The double-lined SB detected in GCS is resolved by speckle. Its
estimated orbital period of 4 yr explains the acceleration. Tok2012a
03311+2744 STFA 7 STTA 34. B is BD+27@513.
HJL 49. HJL1986
03311+1544 HDS 443 1997.7181 Large change in separation seen since Hipparcos epoch. Msn1999b
03312+1947 STF 403 AB: H 1 55. MEv2010
03313+6644 OSO 15 G246-038. Not a common proper motion pair, based on comparison with
POSS2 red plates. PM = +1193 -1066. Oso2004
03313+2734 SHY 445 BC: HIP 16410 + HIP 16742.
03313-5955 JSP 47 CD-60@724.
03314+5842 STI1991 STI1997.
03314+0131 HJ 2194 Rectilinear solution by Friedman et al. (2011). USN2011a
03316+4752 STT 56 Primary also is classified B8.5VeShell.
03317+1331 BPM 77 [PM2000] 130670 + [PM2000] 130734. Gvr2010
03318+3803 ES 2458 ALI 517 is the same pair. Hei1980a
03319+3536 ES 2559 BRT 3235.
03319-2537 VIG 5 The B component appears to be a faint background star. Vig2012
03320+6735 STT 54 B is BD+67@@274.
03320+1820 LDS3501 NLTT 11140/11139 Chm2004
03320-0223 BRT 363 A likely plate flaw. Grv2021b
03321+4801 BAG 40 Primary is the rotationally variable star V396 Per.
03321+4340 COU1688 AB: A premature orbit has been calculated with very sparse data, since
most of the observations are negative.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.58 +/- 1.35, 2.16, and 0.95 Msun, respectively. Mlk2012
LDS9155 AC: Old LDS6155. HIP 16467. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
NLTT 11124/11125 Chm2004
03322+1133 AG 68 H IV 44. Also known as STF 409.
H 4 44. MEv2010
03323-0705 STF 411 B is BD-07@619 (Roman).
B component spectral type F9IV AbH2000
03326+2844 JNN 24 This is a close triple system discovered with AstraLux, where in
particular the tertiary component is difficult to fit for. Since the
relative positions of the BC pair components are therefore clearly
dominated by noise scatter in both separation and position angle, we
set the error of each epoch to the scatter among the data points and
make no assessment of orbital motion for the BC pair (although by
contrast, clear orbital motion is seen of the pair with respect to the
A component). Jnn2012
Estimated age 10-20 Myr; masses 0.07 +/- 0.01 and 0.04 +/- 0.01 Msun;
a ~8.7 au. Jnn2014
03327+3540 CHR 261 This object is a new addition to older Hyades member lists added by
Schwan (1991 A&A, 243, 386), although Griffin (1992 private comm.)
doubts that this object is actually a cluster member. While its status
is not definitive, subsequent confirmation or suspected duplicity (by
another technique) makes the discovery measurement somewhat more
probable. Msn1993a
03327-0553 GWP 476 ABL 145. Tob2012b
03328-0247 GWP 477 ABL 146. Tob2012b
03329-0927 BLA 2 eps Eri = 18 Eri = Ran. Macintosh et al (2003) made a K-band search for MBA2003
MBA 1 extrasolar planets in the dust surrounding eps Eri, using Keck, NIRC2,
and AO. The relative motions for these 10 objects between 2001 Dec and
2002 Aug were all well below expected motions for true companions,
leading to conclusion all these faint companions are background stars.
03332+4615 ES 560 NLTT 11174/11176 Chm2004
03334+2322 STT 57 STTA 35 = S 429.
03335+5846 STF 396 B is BD+58@618. Spectrum of A: Am(A3/A7/F0).
03336-0735 GWP 478 ABL 147. Tob2012b
03336-1904 RSS 66 CPD-19@376
03337+5752 CHR 117 Cf orbit in McAlister et al. (1992). High-space-velocity binary. McA1992
See Balega et al. (2001) for further discussion of Li abundance. Bag2001
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.47 +/- 0.38, 3.40, and 1.13 Msun, respectively. Mlk2012
03339+3205 HJ 334 STT 540.
SEI 30. Nsn2017a
Rectilinear solution by Friedman et al. (2012). USN2012a
03339-3105 B 52 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.62 +/- 1.43, 2.46, and 1.20 Msun, respectively. Mlk2012
03342+4837 BU 787 Burnham notes: "Hussey measures a third star, 175.8deg, 12.70arcsec Hu_1903b
(1898.70) 1n. I could not see this on one night with the 40-inch, but
measured 11m star in nearly the same direction, 175.6deg, 36.78arcsec
(1899.13) 1n." Bu_1906
C does not exist. B__1960b
AB: Rectilinear solution by Cvetkovic (2011). Cve2011c
Despite having an orbit, an optical pair based on parallax an proper Izm2019
motion. Mlk2022
03342+4651 HDS 452 V578 Per, eclipsing binary of bet Lyr type, period 0.97077d. Zas2016
03343+6348 MLB 190 Also known as WFC 16.
03343+2625 OL 152 COU 687.
03344+2428 STF 412 7 Tau. Only P, T, and a were redetermined by Vlaicu & Vasile (1961); Vla1965
the remaining elements were from the orbit of Luyten (1934). Luy1934c
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.04 +/- 1.54, 4.91, and 2.09 Msun, respectively. Mlk2012
AB,C: H 4 88. MEv2010
03344-1940 GWP 480 ABL 148. Tob2012b
03345+1948 STF 414 H III 78. STT 58.
H 3 78. MEv2010
One or both components may be variable. SHS2023f
03346-1613 GAL 332 Object #96 in Gallo's original list. Gal1912b
03346-3104 LDS3508 NLTT 11300/11288 Chm2004
03348+2126 BRT3261 AB: Also known as TDS2588.
AB: Additional notes may be found in Couteau (1952). Cou1952a
J 932 AB,C: Additional notes may be found in Jonckheere (1949) and J__1949b
Couteau (1952). Cou1952a
03349-1604 GAL 353 Object #97 in Gallo's original list. ARA 17. Gal1912b
03350+6002 STF 400 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.96 +/- 1.62, 2.62, and 1.30 Msun, respectively. Mlk2012
03350+3201 STF 410 A is an ellipsoidal variable, IX Per.
03351-2309 ARA1976 Rectilinear solution by Mason & Hartkopf (2016). Msn2016a
03352+0543 TOK 657 CPM, common parallax, both on MS. Tok2014d
03353+1549 BPM 78 [PM2000] 133139 + [PM2000] 133157. Gvr2010
03354+3948 MLB1064 ALI 1035.
03355-3218 LDS3510 NLTT 11346/11349 Chm2004
03356+4253 LDS9156 Old LDS6156.
AD: NLTT 11280/11270 Chm2004
03357-1644 GWP 484 ABL 149. Tob2012b
03361-0320 J 1457 HD 22393. J__1941a
03362+4220 A 1535 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.99 +/- 0.69, 2.06, and 0.95 Msun, respectively. Mlk2012
03368+2106 LDS3511 NLTT 11370/11371 Chm2004
03368+0035 STF 422 A premature orbit has been computed. The primary is a variable of the
RS CVn type, V711 Tau., and also a spectroscopic binary, P = 2.8 d.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
H 3 45. MEv2010
03369-4957 SEE 29 The astrometric orbit of the stars comprising the A component was
generated by a fit to individual data points available in Hipparcos
Intermediate Astrometry Data. Mkr2007a
Primary is possible SB. Tok2014d
TOK 207 Likely triple. The inner pair produces RV variability and acceleration,
the outer companion at 2".7 is discovered with NICI. Tok2012a
03370-2808 LDS 840 NLTT 11423/11421 Chm2004
03372+3710 BRT3236 ALI 283.
03373-8517 R 39 Also appears to be R 48.
03374-8051 HJ 3607 B is CPD-81@89.
03375+3107 GC 4314 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
03376+1751 LDS3512 NLTT 11415/11416 Chm2004
03376-0103 GWP 486 ABL 150. Tob2012b
03377+7235 HJ 2190 C component is galaxy NGC 1343.
03377-0801 GWP 487 ABL 151. Tob2012b
03378+4046 COU1517 AB Per, an Algol-type eclipsing binary, P = 7.1601d. Zas2012
03378+1526 HD 22522 This star was misidentified as BD+17 0593 = SAO 93525 in the first
speckle catalog. McA1984b
03379+8017 MLR 456 Also known as TDS2606.
03379+1950 LDS3515 G006-022. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 11424/11425 Chm2004
03381-1133 OL 151 Aka HEI 315.
03382-5947 DUN 14 B is CPD-60@261.
SHY 448. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03383+4448 S 430 STTA 37. B is BD+44@759.
AB: HJL 50. HJL1986
03388+5055 ES 953 Appears to be the lost HJ 2197. Dam2015b
03388-1607 LDS3517 NLTT 11485/11486 Chm2004
03390+4232 RAO 47 Triple system consisting of an astrometric binary with period of 3 yr
(Goldin & Makarov 2007) and Robo-AO tertiary B at 1".76. Considering Gln2007
the fast PM(A), the fixed position of AB during 1 year would appear to
confirm it as a physical binary. B is located well below the MS,
although its photometry has a large uncertainty. If it is a physical
component with unusual colors, the system merits further study. Rbr2015d
03392+5632 JNN 258 G 175-2. Estimated age 1000-10000 Myr; masses 0.60 +/- 0.10 and 0.38
+/- 0.03 Msun; a ~24.7 au. Jnn2014
03393+5632 JNN 258 Aa,Ab: Originally 03392+5632; merged with 03393+5632.
03395-1017 GWP 494 ABL 153. Tob2012b
03396+3747 GRV 185 Primary is V736 Per, Algol-type eclipsing binary, period 3.76674d. Zas2013
03396+2530 LDS9158 old LDS6158. This is the common proper motion pair Wolf 204,5.
03396+1823 TOK 14 AB has estimated period 5000y; primary is 8.7d SB2. Tok2006
LDS9159 AC: Old LDS6159.
NLTT 11499/11500 Chm2004
JAO 9 Ba,Bb: Referred to as G 006-026BC by Jao et al. (2016), but the C Jao2016
component is the Luyten companion. Combined astrometric/spectroscopic
solution yields component masses 0.474 +/- 0.053 and 0.436 +/- 0.049
Msun, plus an orbital parallax of 26.34 +/- 0.2 mas. There is an
error in their Table 3: a" = 0.0225 +/- 0.0008" (Jao, private comm.)
03397-0331 GWP 495 ABL 155. Tob2012b
03397-1612 GWP 496 ABL 154. Tob2012b
03397-2727 LDS 841 NLTT 11538/11539 Chm2004
03398+3328 ES 327 Also known as GJ 9119 B, this star is a wide companion to GJ 9119 A at
about 14" as noted in e.g. the WDS catalog. It is however single in
the separation range covered by the AstraLux data. Jnn2012
A is also a 183d spectroscopic binary. Tok2019b
03398+0515 J 1812 BAL 2608.
03400+6352 STTA 36 A,BC: HJL 51. HJL1986
A,BC: SHY 160. Bayesian analysis by Shaya & Olling (2011) indicates Shy2011
very high (near 100%) probability pair is physical.
03401+3407 STF 425 H 2 52. MEv2010
The B component was resolved at Palomar (0.580"). Genet et al. (2013)
detect a wobble in the motion of AB, with P~107y, alpha~0.18"
suggesting M2~0.5 Msun Tok2014d
AB: known binary, which shows apparently a non-Keplerian motion. Rica
Romero & Zirm (2014) proposed that the motion was caused by an unseen FMR2014c
companion and calculated an astrometric orbit for it with P = 107 yr,
eccentricity 0.61, and photocenter semimajor axis 0".179. Our
observations were able to resolve the predicted subsystem Aa,Ab. For
the time of our observations the orbit predicts a companion position
angle of 43.3 deg, in excellent agreement with the position angle of
44 +/- 1.3 deg measured here. The ratio of the predicted displacement
to the measured separation of 0".50 is r = 0.32 = q/(1+q). Hence, the
mass ratio q = 0.47 (the contribution of the light from Ab to the
photo-center is neglected). The mass of Aa is estimated at 1.16 Msun
from its absolute magnitude, leading to 0.54 Msun for Ab. The absolute
magnitude of Ab corresponds to a smaller mass of 0.33 Msun. This
discrepancy, if confirmed, can be explained by Ab being a close pair
of M-dwarfs, as happens in other known multiple systems, e.g., in kap Tok2013a
For (Tokovinin 2013). Rbr2015d
AB: Rectilinear solutions by Rica & Zirm (2014) FMR2014c
and Genet et al. (2015). GnR2015a
03402-1936 GC 4392 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
03403-0805 STF 433 B is BD-08@698.
03404-1502 GWP 497 ABL 156. Tob2012b
03405-1925 GWP 498 ABL 157. Tob2012b
03406+2846 STF 427 H N 23. MEv2010
V1268 Tau, Algol-type eclipsing binary, P = 8.161235 d. Zas2011
03407+0643 A 1934 Companion not seen in 1934.
03409+1435 BPM 79 [PM2000] 137052 + [PM2000] 137046. Gvr2010
03409-1237 STF 436 B is BD-13@712.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
03413+4554 BU 1181 Motion in separation. The period may be fairly short. Needs speckle.
Additional notes may be found in van den Bos (1963). B__1963b
Known triple system. Inner binary has been known for over a century Bu_1894d
(Burnham 1894); its first orbit was computed by Riddle et al. (2015). RAO2015
They also detected a third component C which was confirmed by
examination of 2MASS images. The close binary is detectable in our Ks
images, but the PSFs of the stars are overlapping and we are unable to
make a consistent measurement with fitstars. We are able to extract
the astrometry of the AC pair and consider it as likely physical. Rbr2015d
03414-0934 GWP 501 ABL 159. Tob2012b
03414-1421 GWP 499 ABL 158. Tob2012b
03416+2655 LDS6095 Also known as GRV 187.
03418+6239 BLL 12 A is a semi-regular variable, U Cam. B is BD+62@594.
03418+5317 A 985 Primary is the eclipsing binary CV Cam, P = 0.97326 day. Zas2010
03419-5542 JNN 25 2MASS J03415581-5542287 and J03415608-5542408 are separated by only
12" and have similar estimated spectroscopic distances (14 and 20 pc,
respectively) in Riaz et al. (2006), hence it is likely that they form Ria2006
a physical pair. 2MASS J03415581-5542287 is a close (~0.61") binary in
our data, so the system is likely triple in reality, although common
proper motion of all components has yet to be proven. Jnn2012
03422+6313 BD Cam Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin (1984). Grf1984c
03422+5436 HJ 2198 B is BD+54@704.
03423+3141 COU 691 A premature orbit has been computed.
03424+3358 STF 431 40 Per = o Per. A spectroscopic binary. Spectrum of B: A1Vn.
H 3 39. MEv2010
03424-1200 GWP 503 ABL 160. Tob2012b
03424-8001 HJ 3612 Spectrum: G0/2III/IV. B is CPD-80@94.
03425+3256 HJ 336 Also known as STF 432.
Rectilinear solution by Friedman et al. (2012). USN2012a
03425+1416 BPM 80 [PM2000] 138169 + [PM2000] 138144. Gvr2010
03425+1216 JNN 26 Since the two epochs of observation were acquired over a baseline of
only a few months, there is not yet sufficient motion to confirm
common proper motion of the companion that was detected with AstraLux.
However, the separation between components is rather small (~0.86"),
and the fact that the companion is clearly detected in z' but too
faint in i' implies that it must be very red, as expected for a real
companion. Hence, we count it as a binary system for statistical
purposes. Jnn2012
Primary is an active M4.0Ve star, age 60-300 Myr. Bowler et al (2015)
confirm B is physically bound and detect slight orbital motion. The
projected separation is 19.8 +/- 0.9 au. Spectral type of B is
L0 +/- 1, mass 35 +/- 8 Mjup. Bwl2015
03425+0202 BAL1260 HJL 52. HJL1986
03426+1718 GC 4435 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
03426-2445 RST2317 TDS2636.
03427+1448 BPM 81 [PM2000] 138368 + [PM2000] 138396. Gvr2010
03427-2428 LDS3527 NLTT 11680/11682 Chm2004
03429+4747 BUP 46 del Per = 39 Per. A possible variable of the Alpha CVn type.
03430+4554 JNN 259 NLTT 11633. Estimated age 1000-10000 Myr; masses 0.28 +/- 0.03 and
0.20 +/- 0.04 Msun; a ~21.8 au. Jnn2014
03430+2515 LDS1148 NLTT 11651/11648.
03431+2541 STF 435 H 3 88. MEv2010
03435+7247 LDS1579 Rectilinear solution by Hurowitz et al. (2013). USN2013a
03435-4549 PRB 1 Primary is WD 0341-45 = VY Hor, secondary (not found in Aladin) is
BPM 31492. Possible CPM pair, according to Probst (1983). Prb1983
03438+4236 ENG 14 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
03439+1640 GIC 44 AB = G006-029/G006-028 = GJ 9122AB.
AB: NLTT 11693/11688 Chm2004
AB: SHY 17. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03439-7100 HJ 3603 B is CPD-71@@218.
03440+3822 STF 434 B is BD+37@@821.
03440-1836 GWP 505 ABL 161. Tob2012b
03441+3207 DCH 3 HMW 72. Monitored for photometric variability 1998-2003 by Cohen et
al. (2004). Range of variability dI = 0.527 mag, no periodicity found. CHW2004
03442+3207 STF 437 H 3 37. MEv2010
SEI 31. Nsn2017a
03442-6448 LDS 104 bet Ret. A is a spectroscopic binary. B has separation of 1480". B is
CPD-65@272.
bet Ret Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Jones (1928). Jon1928a
03443+3217 BU 535 38 Per = omi Per = Atik. Ellipsoidal and spectroscopic binary.
03443+3208 DCH 4 HMW 73. Monitored for photometric variability 1998-2003 by Cohen et
al. (2004). Range of variability dI = 1.271 mag; multiple periods,
average = 7.582d. Photometry may be contaminated by nearby star. CHW2004
03444+3210 DCH 5 HMW 10/78 = LLRL 10/45. Monitored for photometric variability
1998-2003 by Cohen et al. (2004). Range of variability dI = 0.030 mag
for A component, 4.816 mag for B. No periodicity found for either
component. Photometry of B may be contaminated by nearby companion. CHW2004
03444+3207 DCH 7 HMW 136. Monitored for photometric variability 1998-2003 by Cohen et
al. (2004). Range of variability dI = 0.789 mag, no periodicity found. CHW2004
03444+3206 DCH 6 HMW 39. Monitored for photometric variability 1998-2003 by Cohen et
al. (2004). Range of variability dI = 0.251 mag; multiple periods,
average = 9.667d. CHW2004
03444+2812 A 1826 Not seen on three nights 1964-1982.
03444+1637 BPM 82 [PM2000] 139475 + [PM2000] 139465. Gvr2010
03445+3212 DCH 8 HMW 13 = LLRL 12. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.048 mag, no
periodicity found. CHW2004
03445+3211 DCH 10 HMW 86. Monitored for photometric variability 1998-2003 by Cohen et
al. (2004). Range of variability dI = 0.318 mag, no periodicity found. CHW2004
03445+3210 DCH 9 HMW 75 = LRLL 40. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.337 mag, nonperiodic. CHW2004
03445+3209 DCH 12 HMW 12 = LLRL 29. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.181 mag; multiple
periods, average = 2.237d. CHW2004
03445+3208 DCH 13 HMW 42 = LRLL 86. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.097 mag; multiple
periods, average = 6.532d. CHW2004
03445-1322 GAL 354 Object #99 in Gallo's original list. Gal1912b
03446+3210 BU 880 AB: HMW 1 = LRLL 1. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.455 mag, no
periodicity found. CHW2004
SEI 32. Nsn2017a
STF 439 AB,C: H 3 38. MEv2010
03446+3209 DCH 11 AB: HMW 27/28 = LLRL 16/33. Monitored for photometric variability
1998-2003 by Cohen et al. (2004). Range of variability dI = 0.097 mag
for A, 1.462 mag for B. Multiple periods seen for A, average = 2.656d.
Photometry of B may be contaminated by nearby companion. CHW2004
03446+3209 HER 20 CD: HM 107 = LLRL 165. Monitored for photometric variability 1998-2003
by Cohen et al. (2004). Range of variability dI = 0.328 mag, no
periodicity found. Photometry may be contaminated by nearby star. CHW2004
03446+3208 HER 7 Additional notes may be found in Herbig (1962). Her1962
03446+3207 DCH 14 HMW 11 = LRLL 6. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.094 mag; multiple
periods, average = 1.687d. CHW2004
03446+2754 STTA 38 Optical with BU 1041BC, which is BD+27@558, at 03 44.7 +27 55.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
BU 1041BC The B component has both an astrometric and a spectroscopic orbit Gln2007
which are not associated with the optical BC pair. Grf2015c
03446-5416 HJ 3592 See claimed A was a close pair in 1897, but no trace of it was seen See1898c
subsequently by van den Bos, Dawson, and Innes. Daw1918a
03447+3211 HER 21 HM 98 = LRLL 166. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.960 mag, no
periodicity found. Photometry may be contaminated by nearby star. CHW2004
03447+3210 DCH 15 HMW 99 = LRLL 221. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 2.136 mag, no
periodicity found. CHW2004
03447+3209 DCH 16 HMW 14 = LRLL 9. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.109 mag; multiple
periods, average = 2.539d. CHW2004
03447+3208 DCH 17 HMW 111 = LLRL 52. Monitored for photometric variability 1998-2003 by
Cohen et al. (2004). Range of variability dI = 0.187 mag, no
periodicity found. Photometry may be contaminated by nearby star. CHW2004
03447+2449 ITO 7 Pleiades HII 405.
03447+2414 LDS6103 A component is Pleiades star Melotte 22 HII 430.
03448+4602 BAG 8 Combined astrometric/spectroscopic solution by Balega et al. (2002), Bag2002b
including determination of component masses.
The Balega (2002) orbit predicts a separation of 0.055" in mid-2006, Bag2002b
opening rapidly to 0".197 in late 2007. Perhaps T0 is not quite
correct? Hrt2009
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.54 +/- 0.13, 1.54, and 0.79 Msun, respectively. Mlk2012
A(B) Teff = 5350+/-50(4400+/-50) K, R = 0.95+/-0.06(0.58+/-0.06) \rsun, AlW2014c
L = 0.56+/-0.01(0.10+/-0.02) \lsun, M = 0.83+/-0.05(0.60+/-0.05) \msun.
03448+2417 HL 6 Primary is Pleiades star Celaeno = 16 Tau.
03448-7002 LFR 1 SHY 450. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
03449+2407 HL 7 Primary is Pleiades star Electra = 17 Tau.
Uniform disk diameter 0.472 +/- 0.025 mas,
Limb darkened diameter 0.478 +/- 0.025 mas,
Teff = 14700 +/- 800 K based on LDD.
Radius is 5.91 +/- 0.47 \rsun. CIA2019a
03452+4235 ES 2601 nu Per = 41 Per
03452+2450 HL 8 Primary is Pleiades star 18 Tau.
03452+2428 HJ 3251 Primary is Pleiades star Taygeta = 19 Tau = 19 Pleiadum.
A is a spectroscopic and occultation binary.
03454+2402 HL 10 Primary is Pleiades star.
03454-2752 BU 1003 A premature orbit has been computed. Motion direct and increasing as
the pair closes in. However, there are no measures in the last twenty
years.
03457+2438 YAM 1 Pleiades cluster member. Primary is the BY Dra type variable V855 Tau. Yam2013
03457+0603 HJ 2204 29 Tau. A is a spectroscopic binary.
03458+2422 HL 11 Primary is Pleiades star Maia = 20 Tau.
03458+2309 STF 444 Spectroscopic binary, P = 7.15d.
03459+2433 HL 12 Primary is Pleiades star Asterope = 21 Tau.
03459+2402 HL 13 Primary is Pleiades star.
03460+7302 MLR 457 Same as HDS 476.
03460+2734 CTI7214 V1274 Tau.
03460+2432 HL 14 Primary is Pleiades star 22 Tau.
03460+1721 BPM 83 [PM2000] 140561 + [PM2000] 140577. Gvr2010
03461-1522 GWP 508 ABL 163. Tob2012b
03461-1708 GWP 507 ABL 162. Tob2012b
03461-6405 HJ 3600 B is CPD-64@271.
03462+2434 POU 309 LDS6108.
Both components are Pleiades variables. A = Melotte 22 HII 879 = V813
Tau, while B = Melotte 22 HII 883 = V789 Tau.
03462+1710 HJ 3252 This star has a possible wide companion at about 8" as noted in the
WDS. It is however single in the separation range covered by the
AstraLux data. Jnn2012
03463+2411 BU 536 In the Pleiades. The motion so far is retrograde and rectilinear. Hzg1958
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Both elliptical orbit and rectilinear trajectory were calculated by
Popovic & Pavlovic (1995). See also rectilinear catalog. Pop1995d
03463+2357 HL 15 Primary is Pleiades star 23 Tau = Merope.
03463-1235 GAL 355 Object #103 in Gallo's original list. Gal1912b
03464+7523 STF 418 Same as PRZ 4. Coordinates of PRZ 4 correct and retained.
03464+2435 ITO 8 AB: Pleiades HII 996. Primary is the BY Dra-type variable V1045 Tau. Ito2011
LDS6110 AC: Possibly common with LDS6108.
03464+1143 LEP 119 LHS 1589 = NLTT 11793. Lepine et al. determine a photometric distance Lep2007b
of 81 +/- 18 pc; masses are estimated at 0.25 and 0.20 Msun.
03465+2508 ITO 9 Pleiades HII 1015.
03465+2426 ITO 10 Pleiades HII 1032. Primary is V1171 Tau. Both companions are
background stars. Yam2013
03465+2415 CHR 12 Pleiades cluster member.
1985.8488: This measure is from reanalysis of archival data. Not
listed as an SB by Abt et al. (1965), but it may show measurable AbH1965b
velocity variation at some phases of a possibly eccentric orbit. Msn1993b
Aa,Ab: Observed 20 times 1982-1998 and resolved 4 times 1983-1989,
with separations decreasing from 0.236" to 0.160". Motion indicates a
~40-year period orbit. Hrt2009
03466+2950 BRT 233 MLB 683.
03466+2458 MET 34 Pleiades cluster member. The companion is a background star. Yam2013
03466+2255 RDR 2 Primary is an F6 Pleiades member (HII 1132). Based on common motion
over 4 years, Rodriguez et al. (2012) conclude the B component is
either a companion to the primary or (less likely) a nearby comoving
Pleiades member. Assuming they comprise a physical pair, the companion
is a brown dwarf, with mass estimated at 0.06 +/- 0.01 Msun,
temperature 2600 +/- 100K. Rdr2012b
03467+2402 LDS6111 A component is a Pleiades variable = Melotte 22 HII 1124 = V814 Tau.
03467-1231 GAL 356 Object #104 in Gallo's original list. Gal1912b
03470+4126 STF 443 HIP 17666. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
AB: NLTT 11792/11791 Chm2004
Proper motion of A +596 -1249. Proper motion of B +594-1259. B is a
single-lined spectroscopic binary, P = 48.65d. A common proper motion
companion, G095-059, mag. 13.4, lies more than 2 degrees away.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: HJL 53. HJL1986
03470+2431 CHR 124 Occultation binary. Has variable radial velocity. Pleiad.
03471+2449 BU 537 Variable, V534 Tau.
03473+2424 BOV 18 Geissler et al (2012) conclude companion is an M8 brown dwarf, the
first substellar companion discovered around a Pleiades star. Mass
estimates range from 0.052 to 0.063 Msun, depending on distance, etc. Gei2012
Pleiades cluster member. The companion shares common proper motion. Yam2013
03473+2348 HL 18 Primary is Pleiades star.
03473+2344 HL 19 Primary is Pleiades star.
BOV 17 CF: 03471+2343BOV 17 = HL 19C, system merged.
03474+2435 HL 20 Primary is Pleiades star.
03474+2355 STF 450 POU 311. Primary is Pleiades star.
03474+2255 HD 23610 Hipparcos astrometric solution assumed circular orbit (e = omega = 0); HIP1997d
Cluster Melotte 22 #1407.
03475+2417 HL 22 Primary is Pleiades star.
03475+2406 STFA 8 Primary is Pleiades star Alcyone = 25 Tau = eta Tau = V647 Tau.
STTA 42.
A is an occultation and spectroscopic binary.
B, at 03 47.4 +24 07, is an occultation binary.
C is V647 Tau.
BC: HJL1029. HJL1986
BD: HJL1028. HJL1986
CD: HJL1027. HJL1986
03476+2337 HL 24 Primary is Pleiades star.
03478+3501 ES 235 Primary is eclipsing binary of Algol-type, period 1.92873d. Zas2014
03478+3212 HR 1164 Orbit determined by fitting revised Hipparcos intermediate astrometric
data. Derived component masses 1.44 +/- 0.09 and 1.15 +/- 0.08 Msun. Ren2010
03479+3336 STF 448 HJ 5457. A is a spectroscopic binary. Also, one component is variable.
03479+2555 BRT2520 Heintz finds no pair in the field, and believes identity with J 27 Hei1985a
(03470+2855) is possible.
03479+2407 BU 538 AB. Identification of a 2000.8 measure by Lampens et al. (2007) Lmp2007
originally attributed to 03481+2409 COU 80 was corrected by the
author; it actually was of this pair.
03480+6840 KUI 13 See discussion by van de Kamp & Chao-Yuan Yang. Kam1967
WNO 16 AD: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
BD: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
03480+4032 TOK 240 Primary is an exoplanet host, P=1565d Tok2014d
03480-7048 HJ 3606 B is CPD-71@223.
03481+2409 COU 80 Pleiad.
Identification of a 2000.8 measure by Lampens et al. (2007) originally Lmp2007
attributed to this pair was corrected by the author; it actually was
of 03479+2407 BU 538AB.
03482+2419 CHR 155 Included in the Pleiades cluster survey of Abt et al. (1965), who did AbH1965b
not detect variable RV. Pearce & Hill (1975 Pub DAO, 14, 319) did
notice velocity variation at the 1% level, and Liu et al. (1997) found Liu1997
the system to be a SB2, although large velocity difference may imply a
closer companion than this. Msn1993b
03482+2219 EQ Tau Multiple system including contact binary. Pribulla & Rucinski (2006) Pbl2006
estimate the mass of the contact pair at 1.752 Msun and the minimum
mass of the wider component at 0.49 Msun.
03483+2325 HL 25 Pleiades H 722. Primary was misidentified as SAO 76125 in the first
speckle catalogue. McA1984b
03483+1109 STF 452 30 Tau.
H 3 66. MEv2010
03483-0943 GWP 517 ABL 164. Tob2012b
03484+5202 HU 546 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.17 +/- 0.43, 1.53, and 1.20 Msun, respectively. Mlk2012
03486+3039 SHY 453 HIP 17796 + HIP 18204.
03486-3737 DUN 16 f Eri. One component is a possible Beta Lyrae-type system.
03489+6445 STT 62 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.82 +/- 0.52, 2.75, and 1.20 Msun, respectively. Mlk2012
03489+2351 HL 27 Primary is Pleiades star 26 Tau.
03490+5120 LDS9160 Old LDS6160. NLTT 11871/11873.
03491+4358 V376 Per Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
03491+2347 TRR 16 V1282 Tau.
Ma,Mb = 0.978 +/- 0.024, 0.897 +/- 0.022 \msun. Orbital parallax is
7.310 +/- 0.026 mas. Spectroscopic dm (518.7 nm) = 0.63. Trr2020b
03492+3651 J 2721 BRT 2586. ALI 288.
03492+2408 CHR 125 Aa,Ab: Pleione, 28 Tau = BU Tau. Shell star and suspected long-period
spectroscopic binary (Hoffleit 1982) . Pleiades cluster member. Hof1982
Frequently unresolved, probably due to large Delta m. Msn1993b
For their measure, Roberts et al. reports that the "The close
proximity of the two star's PSFs prevented accurate measurement of the
astrometry and photometry." Rbr2007
Aa,Ab: Observed 3 times 1987-1991 (all observations noted as weak), Rbr2007
then unresolved until a 2002 (0.24") measure at 900nm Hrt2009
RBR 4 AF: 2002.0924: PA is measured in zenith mode. If data collected in
equatorial mode, PA = 119. Confirmation of the pair should establish
the correct value for theta. Rbr2007
03492+2403 STF 453 Primary is Pleiades star Atlas = 27 Tau = Melotte 22 #2168
Position angles scattered. Distances range from "single" to 0.6". Some
question duplicity. A is a long-period spectroscopic binary.
MKT 12 Aa1,Aa2: Hipparcos astrometric solution assumed circular orbit (e =
omega = 0). HIP1997d
Pan et al. (2004) orbit is based on Mark III and PTI measures. A PTI2004
distance to the Pleiades of 135 +/- 2 pc is determined. Masses for the
components are calculated as 4.90 +/- 0.28 and 3.65 +/- 0.08 Msun.
Zwahlen et al. (2004) orbit is based on published Mark III and PTI Zwa2004
measures, plus additional Mark III and NPOI astrometric data and
ELODIE echelle spectra. This combined spectroscopic/interferometric
solution yields masses of 4.74 +/- 0.25 and 3.42 +/- 0.25 Msun; the
distance 132 +/- 4 pc found agrees with "traditional" Pleiades
distances obtained through MS fitting techniques.
Aa1,Aa2: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 5.68 +/- 0.79, 6.68, and 3.31 Msun, respectively. Mlk2012
Uniform disk diameter 0.464 +/- 0.043 mas,
Limb darkened diameter 0.469 +/- 0.043 mas,
Teff = 13500 +/- 300 K based on LDD.
Radius is 5.98 +/- 0.67 \rsun. CIA2019a
03493+5707 S 436 STTA 39. B is BD+56@847.
HJL1030. HJL1986
03493-1656 GWP 519 ABL 165. Tob2012b
03494+5214 ES 770 B is BD+51@781.
03494+2423 STTA 40 AB: LDS6116. B is BD+23@560. A is Pleiades star and occultation double
HL 30 BC: Primary is Pleiades star. Also known as STU 2BC.
HL 30 BD: Also known as STU 2BD.
03495+5239 STF 446 Also known as STF 454. Another classification: B0Ib. The primary is
slightly variable; the system is a member of the cluster NGC 1444.1
03495+1255 AG 74 Primary is V1128 Tau, a 10th magnitude W UMa type eclipsing binary,
with period 0.3053725d. Zas2011
03496+6318 CAR 1 Also known as MOAI 1.
1995.948: Theta corrected from published value of 213 deg (Aristidi,
private communication)
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.76 +/- 0.61, 3.36, and 1.82 Msun, respectively. Mlk2012
03496+3859 HU 1067 A RW Aur-type variable, XY Per. Both components may vary.
dm estimates on a number of nights. quadrant reversed on 1936 Jan 17,
indicating primary is responsible for variation. Beyer (AN 263, 71,
1937) established the irregular character of the variation. VBs1954
03496-0220 YR 23 Triple. The RV amplitude of 9.5 km s-1 and double lines seen in GCS
cannot be caused by the visual system YR 23 with estimated period of
~50 yr which could however be responsible for dmu. Tok2012a
The Hipparcos parallax, individual magnitudes and standard relations Tok2018a
for main-sequence stars leads to masses of 1.14, 0.96 and 0.80 \msun
for A and the unresolved Ba and Bb pair.
Ba,Bb is estimated to have a dM in V band of 1.2 and a maximum
separation of 26 mas.
03497+2343 HL 32 Primary is Pleiades star.
03497+2320 YAM 2 BC: Pleiades cluster member. The companion is a background star. Yam2013
Pair initially 03495+2323 YAM 2; merged with 03497+2320 LDS6118.
03498+2421 HL 33 Primary is Pleiades star.
03498+2342 ITO 11 Pleiades HII 2462.
03499+2313 ITO 12 Pleiades HII 2506.
YAM 3 Pleiades cluster member. The companion is probably a background star. Yam2013
03500+2351 STT 64 A is a spectroscopic binary, P = 16.72d, spectrum B9.5VpSiSrCr. Pleiad
03501+4458 CHR 126 A spectroscopic binary.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
P'edoussaut et al. (1987). Ped1987
Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Pedoussaut et al. (1987). Ped1987
03501+0637 TOK 80 HIP 17936. The magnitude difference in the 2MASS PSC dK=1.8 is
suspect (5" separation), dK=3.4 is measured with ANDICAM. Tok2011a
03502+3449 ES 277 AB: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
03502-1335 FAR 32 NLTT 11972. Primary is white dwarf WD 0347-137. Far2006
03503+2535 STT 65 One star variable? Wor1967b
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 4.15 +/- 0.39, 3.39, and 3.91 Msun, respectively. Mlk2012
03503-0131 SHY 164 AE: HIP 17950 + HIP 16933. E component = A component of 03379-0231.
AB: Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
However, radial velocity classifies this as not a Hyades member. Grf2013c
03504+7120 HJ 2200 gam Cam
03505-1219 GAL 357 Object #105 in Gallo's original list. Gal1912b
03506+2431 YAM 4 Pleiades cluster member. Primary is V1174 Tau. Yam2013
03506-4234 EGN 3 Pair bound, with projected separation 73au. Mass of secondary
0.15 +/- 0.01 Msun; spectral type M4-M6. Egn2007
03507-1206 GAL 358 Object #106 in Gallo's original list. Gal1912b
03508+4546 FMR 63 Typographical error in initial WDS designation (03508+4946)
03510+1414 JLM 1 Erroneously labelled as JML 1; changed upon request of discoverer.
03511+3548 BRT3238 ALI 51.
03511+1551 BPM 84 [PM2000] 144054 + [PM2000] 144088. Gvr2010
03513+2621 A 1830 The few observations do not define the nature of the motion.
03514+2538 HEI 9 Primary is eclipsing binary of Algol-type, period 1.26292 d. Zas2012
03514-1610 GWP 523 ABL 166. Tob2012b
03517+7030 HJ 1139 B is BD+70@263.
03517+2433 LDS5437 A component is a Pleiades variable = Melotte 22 HII 3096 = V1054 Tau.
B component is flare star V383 Tau.
03518+3453 ARN 58 Also known as GRV 196.
03518-0306 GWP 524 ABL 167. Tob2012b
03520+2440 BOV 27 AB: Assuming a Pleiades parallax of 7.43 +/- 0.17 mas (distance 134.6
pc; Soderblom et al. 2005, AJ 129, 161), Schaefer et al. (2014) find a
total mass of 1.42 +/- 0.10 Msun. The revised Hipparcos parallax of
8.32 +/- 0.13 (120.2 pc; van Leeuwen 2009, A&A 497, 209) gives a total
mass of 1.01 +/- 0.05 Msun, which is not consistent with the
corresponding photometric masses of the components. Sfr2014
03520+0632 KUI 15 31 Tau.
AB: Additional notes may be found in Van Biesbroeck (1954) and VBs1954
Couteau (1955). Cou1955c
03525+3546 ES 2334 BRT 3239. ALI 52.
03525-0403 GWP 525 ABL 168. Tob2012b
03526-0829 RST4762 The few measures do not define the motion.
03527-0522 HJ 338 30 Eri.
03529+3532 ES 2459 BRT 3240.
03529-0633 GWP 528 ABL 169. Tob2012b
03530+1158 BPM 85 [PM2000] 145369 + [PM2000] 145423. Gvr2010
03530-1332 GWP 529 ABL 170. Tob2012b
03534+1743 BPM 86 [PM2000] 145657 + [PM2000] 145663. Gvr2010
03535+3538 ES 2460 Identical to ALI 54 and BRT 3237 Hei1983a
03535+3307 RBR 36 Suspected non-single. Hor2002b
03535-1229 GAL 359 Object #107 in Gallo's original list. Gal1912b
03535-1440 GWP 531 ABL 171. Tob2012b
03536+2718 OCC9003 The OCC2010 solution is ambiguous and one is arbitrarily "T" coded
until the true solution is determined.
03536+2146 OL 184 TDS2678. Appears to be the same as 03549+2148 OL 200. IDS notes that
OL 200 is possibly identical to 03559+2146 HU 815, but they appear
to be different pairs.
03537+5316 A 1293 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.00 +/- 0.24, 1.94, and 1.05 Msun, respectively. Mlk2012
03539-1751 GWP 532 ABL 172. Tob2012b
03541+3153 STF 464 zet Per = 44 Per. A is a spectroscopic binary.
AD: H 6 96. MEv2010
03543-0257 STF 470 32 Eri. A is a spectroscopic binary.
AB: H 2 36. MEv2010
03544+0116 TOK 81 RoboAO finds a companion to B (233deg, 3.05", dI=5.88mag), but it is
thought to be optical. Tok2014d
03544-0649 A 461 Less than 0.1" in 1954 - 1961. It appears that a revolution has been
completed.
03544-4021 FIN 344 Spectroscopic binary.
1989.9438: This is the first observation of this system since those of
Finsen in the 1960's, and is considerably closer than any of his
results. It is known that in some instances Finsen's rho values
appeared systematically larger than those of speckle; further
observations of this system will determine whether such is again the
case. Hrt1993
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 4.24 +/- 0.59, 4.58, and 4.88 Msun, respectively. Mlk2012
03545+3203 LEI 6 Member of Taurus-Auriga molecular cloud. Dae2015
03545+0510 STTA 41 A is a Delta Scuti-type variable, V479 Tau. B is BD+04@@600.
A,BC(60") is probably physical.
A 1831 BC: Less than 0.1" in 1954 - 1955 with 82-inch.
A premature orbit has been computed. Motion direct.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
03546+3519 HJ 669 AC: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
03546+2507 HAT 1 30' error in WDS designation.
Member of Taurus-Auriga molecular cloud. Dae2015
03546+2131 LDS1149 Old LDS6161. LDS9161.
03547+5200 TOR 5 Formerly known as PAN 2.
03547+1529 BPM 87 [PM2000] 146665 + [PM2000] 146678. Gvr2010
03547-1811 GWP 533 ABL 173. Tob2012b
03548-3542 TOK 82 HIP 18305. NOMAD: PM(B)=(-89,+19), V=11.48(??).
PM(A)=(+108,+218). Tok2011a
03549-1426 GAL 360 Object #109 in Gallo's original list. Gal1912b
03553-0237 BRT1928 BAL 25.
03553-1921 GWP 534 ABL 174. Tob2012b
03554+3103 HO 325 A is a RW Aur-type variable, X Per, and also a long-period
spectroscopic binary.
03557-2236 I 722 CD-22@1398.
03558+5225 TOR 6 Formerly known as PAN 3.
03558+5224 STF 462 HJ 2206.
03561-4509 CPO 121 LDS 108.
03561-4746 HU 1361 HIP 18402. B is definitely physical, but it is too red in the
(Kabs,V-K) CMD. Infrared companion? Nothing on B in SIMBAD. Tok2011a
03562+5939 ENG 16 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
HDS 497 AD: CfA: P=12625d=34.6y? Abt & Willmarth (2006): RV=-22.18 const. AbH2006
03563-1935 GWP 535 ABL 175. Tob2012b
03564+4404 LDS5186 NLTT 12174/12173 Chm2004
03565-3642 BAS 2 This is the X Ray source EUVE J0356-36.6.
03566+6951 LDS1583 A is also a 1539d spectroscopic binary. Tok2019b
03566+5042 S 440 43 Per. A is a spectroscopic binary. B is BD+50@861.
CIA 16 Aa,Ab
Mass = 1.434 +/- 0.014, 1.409 +/- 0.014 \msun for A and B. CIA2020a
Radius = 1.67 +/- 0.06, 1.60 +/- 0.10 \rsun for A and B.
Teff = 6790 +/- 120, 6770 +/- 90 deg K for A and B.
Age = 1.4 Gyr, distance = 38.7 +/- 0.2 pc.
AB: H 5 41. MEv2010
03569+2005 OCC1090 OCC9087.
03571-0828 RST4764 Rapid retrograde motion.
03572-0706 OSW 7 Typographical error in WDS - initially entered as 03572-0025, with dec
portion copied from OSW 8.
03573-1054 GWP 536 ABL 176. Tob2012b
03575-0110 BU 543 A premature orbit has been computed. A is a flare suspect.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
NLTT 12237/12236 Chm2004
03576+5712 ES 1820 Doubtful this system is physically bound, since relative motion is
larger than pm of A. Kiy2012
03578+4932 KU 82 B is BD+49@1068.
03579+5142 SCA 176 Scardia (2017) measured an 8" pair located near the close (0".4) pair Sca2017b
COU2358 COU2358. Proper motions for the COU pair and the primary of the SCA Cou1988b
pair were similar, so they were merged into one multiple system, with
an 18" pair added to link them. This wide pair was given the same SCA
176 discoverer designation and assigned components AB. The components
for the COU pair were changed to Aa,Ab, those of the 8" pair to BC.
03579+4001 STF 471 eps Per = 45 Per. A is a Beta Lyrae-type binary.
AB: H 2 22. MEv2010
03580-1331 HJ 3608 gam Eri = 34 Eri = Zaurak. Variable?
The faint pair, presumeably the original system, was recovered in Dal2009
2009, which appears to have common proper motion. All subsequent
measures of the HJ 3608 were of a more distant pair with linear
motion relative to the primary, presumeably optical.
Mk III Limb-darkened diameter 9.332 +/- 0.173 mas. MkT2003
03583+2757 ARG 58 AG 75.
03583-1659 GWP 537 ABL 177. Tob2012b
03584+2538 LDS5459 Also known as LDS9162.
NLTT 12251/12250 Chm2004
03586-0239 BU 1042 B is BD-03@651.
03587+1646 LDS5462 GWP 538. Luyten's original 1960 measure listed theta = 144deg, 90deg Luy1984
different from the angle found by Bernal. Agreement on coordinates, ABl2012a
separation, and magnitude difference led to the conclusion Luyten made
a trigonometry error in his reduction.
03590+3547 TRN 16 = ksi Per = Menkib.
The image rotator was in an unknown state, so two possible theta
values are listed for the 2001.7342 observation - one for zenith up
and one for north up. Trn2008
Uniform disk diameter 0.216 +/- 0.016 mas,
Limb darkened diameter 0.245 +/- 0.010 mas,
Radius is 10.1 +/- 1.3 \rsun. CIA2018e
03590+0947 HU 27 The value of omega for Ling's (2001) orbit was incorrectly given as Lin2001b
263.1 in IAU Inf. Circ. 144.
Ling (2004) derived an orbital parallax 0".01239 and a mass sum of Lin2004a
1.94 +/- 0.82 Msun.
03590-0056 HEI 215 Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
However, radial velocity classifies this as not a Hyades member. Grf2013c
03591-0656 LDS3545 NLTT 12296/12294 Chm2004
03591-2312 FAR 3 FAR 33. Primary is white dwarf WD 0357-233. Far2005b
03592+8020 JNN 27 A companion to 2MASS J03591438+8020019 was detected on two separate
occasions with AstraLux, in both cases the detection is rather
tentative, but since it is detected twice with consistent properties
we count it as a genuine detection. However, due to the poor quality
of the fit and the fact that the two epochs of observation are only
separated by 3 months, we do not try to acquire two epochs of
astrometry, but merely quote the astrometry as the mean (and standard
deviation) of the two epochs. Jnn2012
03593+5714 MZA 43 MY Cam.
03596-1019 HU 29 Motion in a highly-inclined orbit.
03597+4809 STT 68 A is an Algol-type binary, IQ Per. B is BD+47@921.
03597-1147 GWP 540 ABL 178. Tob2012b
03597-1301 GAL 361 Object #110 in Gallo's original list. Gal1912b
03598+1133 STF 478 LDS5464.
03599+1325 LDS1150 Aka LDS5465.
04005+1935 KOH 1 Metchev & Hillenbrand say pair probably physical, based on proximity. Met2004b
Member of Taurus-Auriga molecular cloud. Dae2015
04005-4145 DON 58 B is above the MS in (V,V-K). Tuc-Hor moving group? (Kiss et al., 2011
MNRAS 411, 117) Tok2014d
04005-5120 TOK 83 HIP 18713. NOMAD: PM(B)=(+44,+43). PM(A)=(+162,-39). Tok2011a
04007+2023 BD+19 641 Hyades vB 9
SB with P > 7 yr according to Griffin et al. (1988). Grf1988
04008+1812 BUP 49 A is a spectroscopic binary. B is BD+17@664.
04008+0505 A 1937 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.32 +/- 1.76, 2.84, and 2.00 Msun, respectively. Mlk2012
04009+2312 STF 479 H N 93.
04009-1027 STF 487 B is BD-10@814.
04018+2303 LDS5476 Aka RAO 114.
04021-3429 BU 1004 HIP 18824. See Allen et al. (2000) for information on metallicity, AlC2000
LDS3551 age, galactic orbital parameters, etc.
BU 1004 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
LDS3551 AD: Holberg et al. (2013): D at 64" is CPM, WD(DA9.9) Hbg2013
04022+2808 STF 481 AD: Declination difference 11.18".
AD: Component D is 04039+2808VBS 9.
04024-2832 DAW 79 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.29 +/- 0.72, 2.25, and 1.07 Msun, respectively. Mlk2012
04025+0638 HDS 510 Cvetkovic et al. (2016) estimate spectral types K2 and K3, masses 0.81
and 0.79 Msun. Dynamical parallax is 13.24 +/- 0.28 mas. Cve2016b
04025-6121 LDS 109 Jenkins et al. (2010 A&A 515, 17): RV(A) var with P>6.5yr, M2min=66 CPS2002b
Mjup. However, Jones et al. (2002) do not detect RV variation. Tok2014d
04027+3210 HJ 670 SEI 34. Nsn2017a
04029+1228 BPM 88 [PM2000] 152895 + [PM2000] 152883. Gvr2010
04030-3322 BRT1587 A likely plate flaw. Grv2021b
04031-1149 GAL 362 Object #113a in Gallo's original list. Gal1912b
04032+2553 DCH 45 HBC 356/357 = V1067 Tau.
Member of Taurus-Auriga molecular cloud. Dae2015
04033+3516 OSO 16 Not a common proper motion pair, based on comparison with POSS2 red
plates. PM of A = +1732 -1356. Oso2004
04033+1820 BPM 89 [PM2000] 153212 + [PM2000] 153228. Gvr2010
04036-3611 WHI 5 Listed as possibly resolved by White et al. (1991). Whi1991
04037-1545 A 2913 1989.9413: This system closed steadily from its discovery at 0".45 in
1915 to 0".22 in 1959; this is the first observation in 30 years so it
is unknown whether the pair has passed through periastron. Hrt1993
04038+3758 ES 2085 A is V380 Per.
04038-4429 LCL 120 AB: B is CD-44@1388.
AB: Additional notes may be found in Herschel (1847). HJ_1847a
SHY 458 AC: HIP 18958 + HIP 18888.
04039+2808 VBS 9 An Algol-type binary, RW Tau.
This is the D component of 04022+2808.
04040+3932 L 51 Not found in Heintz at IDS position. Hei1987a
04042+2324 OSO 17 Not a common proper motion pair, based on comparison with POSS2 red
plates Oso2004
Suspected non-single. Hor2002b
04043-1231 GAL 363 Object #116 in Gallo's original list. Gal1912b
04044+2406 MCA 13 36 Tau. A is an occultation binary, first detected by Dunham et al. Dnh1973
Now resolved by speckle interferometry.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 16.02 +/- 8.21, 11.83, 2.92 Msun, respectively. Mlk2012
04044+2025 RED 1 1996.0656: RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al. (1981) Luy1981
Candidate Hyades member; Reid considers definite binary. Red1997
04045+1512 BPM 90 [PM2000] 154069 + [PM2000] 154068. Gvr2010
04046+5504 HO 221 Both A and B are above the MS. AC: reflex PM(A), likely optical. Tok2014d
04047+2205 STT 558 AB: 37 Tau.
04047-0303 LDS3555 NLTT 12486/12488 Chm2004
04049-3527 CHR 224 AC. Surprisingly, no record of this wide companion to the 0".8 pair
I 152 is listed in the WDS, despite 17 observations spanning 90+ years
since Innes' discovery in 1896. Misidentification appears ruled out, I__1897b
since both the Innes pair and the new component are seen on two
separate occasions. Hrt1996b
04050+3705 KU 83 AB: HJL 55. HJL1986
04050-0600 BFR 4 BD-06 813 + 2MASS J04050209-0600409. Baron et al. (2015) estimate
spectral types K0 and M6.5 +/- 1, distances 68 +/-10 and 86 +2/-37 pc,
masses 0.925-1.014 and 0.096-0.114 Msun. BFr2015
04053+2201 CHR 158 Aa,Ab: 39 Tau. Variable?
Aa,Ab: Observed 7 times 1985-1998, then resolved at 0.22" in 1988 McA1993
(note: "uncertain"), unresolved in 2002 (3.6m AO), and finally Rbr2005
resolved at 0".41 in late 2003 Hrt2009
04056+1255 BPM 91 [PM2000] 154891 + [PM2000] 154924. Gvr2010
04057+2248 COU 151 Metchev & Hillenbrand say the AB pair is probably physical, based on
proximity. Met2004b
04058+7117 LDS1589 NLTT 12426/12424 Chm2004
04059+3438 ES 238 A measure in 1946 gives distance as 7.2".
04063+3548 BRT3241 ALI 57.
04063+1952 BAG 4 A preliminary circular orbit is determined Bag2001
04064+4325 A 1710 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.72 +/- 0.73, 2.49, and 0.95 Msun, respectively. Mlk2012
04065+1422 S 443 B is BD+13@643.
04066+2018 BNV 2 V1300 Tau. DAE 17. Member of Taurus-Auriga molecular cloud. Dae2015
Primary is F8-G1, mass = 1.14 +/- 0.05 Msun, age = 25 +25/-10 Myr,
Teff = 5970-6100K. Secondary is M8-L1, mass = 32 +18/-14 Mjup,
Teff = 2537 +95/-182K. Bnv2014
04066-6019 R 40 B is CPD-60@292. Spectral type of B may be G8.
04067+1309 BPM 92 [PM2000] 155660 + [PM2000] 155680. Gvr2010
04067+0324 HJ 2221 A component: V = 11.8; B-V = +0.9; Spectral type: K-M.
B component: V = 13.5; B-V = +0.8; Spectral type: M FMR2000a
04068+5035 HU 547 Variable of unknown type.
04069+3327 STT 71 A is an Algol-type eclipsing binary, AG Per, P = 2.03d.
04070-1000 SHY 165 AB: HIP 19206 + HIP 21489.
HDS 521 Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.68 +/- 0.48, 2.13, and 1.96 Msun, respectively. Mlk2012
04070-2200 HU 1363 1994.8069: Quadrant determined by speckle imaging analysis. Hor1996
04072+2731 TOK 241 Makarov & Kaplan (2005) note as astrometric companion to A, but there Mkr2005
is RV data for A to support this astrometric sub-system. Tok2014d
04073-2429 BEU 5 Rectilinear solution by Miles & Mason (2016) and Msn2016b
Mason et al. (2018). Despite linear solution, based on proper motion Msn2018a
and parallax appears to be physical.
04075-5234 TOK 15 Astrometric binary in Hipparcos catalog. Estimated period of visual
pair 6y. Primary is 2.5d SB1. G-solution in HIPPARCOS. Tok2006
Triple system, consisting of 2.5d SB and 0".1 tertiary companion
discovered by Tokovinin (2006) and previously revealed by Hipparcos Tok2006
acceleration and RV trend. It is not resolved here; apparently it
closed in. Tok2013b
04076+3804 STT 531 A: V491 Per. CPM with BD+37@882 (50 Per), 12' distant. Cou1955c
Premature orbits have been calculated. Motion retrograde.
G039-001. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
ALC 1 AE: Also known as BU 545CA.
AE: SHY 19. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
E: 50 Per = V582 Per.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
04077+1510 STF 495 A is a Delta Scuti-type variable. A = Hyades vB 11, B = Hyades vB 12.
AB pair, with rho = 3".8 is outside our detection window. Msn1993a
04077+1413 LDS5187 old LDS6164.
04078+6220 ES 2603 SZ Cam
STF 485 The classification is from Chocol (1980 Bull. Astron. Inst. Czech. 31,
CHR 209 321). The discovery of speckle companion CHR 209 Ea,Eb with a period
WSI 20 of some 60 y confirms the third body model advocated by Mayer et al.
HZG 2 (1994 A&A 288, L13) based on the appearance of the spectrum and
HLM 3 variations in the time of light curve minimum (they suggest a third
body period of 50.7 y). Another light curve solution is given by
Harries et al. (1998 MNRAS 295, 386). The B component was also
observed and appeared to be single. Classification of the B component
is from the WDS. Msn1998a
This complex multiple system has had numerous identification errors
due to various difficulties. The diagram of Lewis in his catalog of L__1906b
the Struve pairs, which seemed a good first step, was hampered by the
quadrant error of the pair he designated Ca. This quadrant error was
repeated in the ADS, IDS, and in earlier editions of the WDS. In the
ADS (where this pair is listed as #2984, but note that #2989 is part
of this system, too) the errors multiplied. The pair Holmes AF (WDS
designation HLM 3AF) is apparently the same as STF 485Ac. Inspection
of scanned images of this region of the sky have allowed the
Hertzsprung pairs (HZG 2) whose components are given within
quotation marks in the ADS to be identified. Of the HZG pairs, the
"CD" pairing is the same as STF 484AC and the "CE" pairing is the
same as STF 484AB. The ADS note to the "AJ" pairing of HZG 2 is a
typographical error. The correct position angle is 77 degrees, which
corresponds to the AD (now AO) pair. Below outlines the changes from
the WDS 2001.0 to the current version.
ES 2603Aa ---> ES 2603AB
STF 485Ab ---> STF 485AC
STF 485Ac ---> STF 485AD
STF 485AB ---> STF 485AE
STF 485BE ---> STF 485EF
STF 485 ---> STF 485EG (formerly STF 485B to STF 484A)
STF 484AB ---> STF 484GH
STF 484AC ---> STF 484GI
STF 485Bb ---> STF 485EC
HLM 3AF ---> STF 485AD
STF 485AD ---> STF 485AO
STF 485 ---> STF 485AL (formerly STF 485A to HLM 3A)
HLM 3AB ---> HLM 3LM
HZG 2AC ---> STF 484AI
HZG 2AD ---> STF 484AG
HZG 2AE ---> STF 484AH
HZG 2AG ---> HZG 2AN
HZG 2BC ---> STF 484EI
HZG 2BE ---> STF 484EH
HZG 2CD ---> STF 484GI
HZG 2CE ---> STF 484HI
HZG 2JK ---> HZG 2OP
HZG 2 ---> HZG 2JK
SLV 3 ---> STF 485AF
CHR 209Ba ---> CHR 209Ea,Eb
CHR 209 Ea,Eb: The primary of this pair is the Beta Lyrae-type O9/B0 eclipsing
system SZ Cam, with a period of 2.698d. The Gorda et al. (2007) orbit Grd2007a
is based on changes in the period of SZ Cam to determine P, omega, e, Grd2007b
and T, and speckle measures to derive i, Omega, and a. They derive a
distance of 1125 +/- 135 pc, which exceeds by 30% the 800pc distance
to the open cluster NGC 1502; they conclude that SZ Cam is not a
member of the cluster. The mass of the eclipsing pair (Ea) is 28.5
+/- 0.5 Msun, that of the third body (Eb) 23.4 +/- 2.4 Msun.
Eb is also a close binary.
STF 484 GH: STI 492.
04079+1750 DAE 18 V1302 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04080+4311 AG 308 B is BD+42@897.
04080+0119 HJ 2223 BAL 1262.
04082+1957 DAE 19 V1196 Tau. Dae2015
04083+1327 BPM 93 [PM2000] 156773 + [PM2000] 156823. Gvr2010
04087+2553 OCC 777 Griffin (2013) notes that the magnitude and parallax of this pair
suggest a star of luminosity class III, rather than the published
spectral type of G8II. He derived a spectroscopic orbit of P=2224.4
+/- 2.3 days, e=0.477 +/- 0.009. Grf2013g
04088+1126 LDS5188 LDS5508.
04089+2911 BU 1232 Only elements P, T, and a in the Starikova (1980) orbit have been Sta1980b
amended from the orbit of Muller (1978). Mlr1978a
Griffin et al. (1988) find this to be a SB but doubt its Grf1988
membership in the Hyades in spite of its inclusion by Sym1965
Wayman et al. (1965). Msn1993a
Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
However, this is a Hyades non-member Grf1988
Grf2013c
04089+2306 STF 494 H N 17. MEv2010
04090-5153 HJ 3625 B is CPD-52@499.
04091+2901 KOH 3 Young member of Taurus-Auriga molecular cloud. Dae2015
04091+2839 HO 326 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 9.61 +/- 4.45, 2.43, and 1.10 Msun, respectively. Mlk2012
04091-1624 SKF 950 GWP 556. Tob2012b
04092+2105 ALP 11 2MASSI J0409095+210439
Physical companionship of B component to this ultracool dwarf ruled
out based on I-J color, using I-band photometry taken at WIYN in
August 2002. C component seen as elongated; its physical companionship
also ruled out. AlP2007
04093+1835 LDS1154 NLTT 12637/12636 Chm2004
04093-0756 A 469 Only elements P and T in the Starikova (1984) orbit have been amended Sta1984
from the orbit of Baize (1981). Baz1981b
Typographical error in semimajor axis for Brendley & Mason (2007) USN2007b
orbit corrected from 2".435 to 0".2986.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 8.49 +/- 6.33, 3.80, and 2.09 Msun, respectively. Mlk2012
04094+2328 POU 412 LDS5509.
04094+0546 LAW 12 LSPM J0409+0546 = NLTT 12648. Law et al (2008) derive a distance of Law2008
19.9 +9.1/-3.8 pc and a projected separation of 4.9 +2.7/-0.7 au.
Estimated spectral types are M4.5 and secondary later than M6.
04094-0125 BAL 290 J 3334. Nsn2016
04095-0742 BRT 533 Not found by Heintz at IDS position. Hei1990b
04095-1729 ENG 17 B is BD-17@806.
04096+3139 HO 327 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
SEI 36. Nsn2017a
AB: Rectilinear solution by Hurowitz et al. (2013). USN2013a
04096-6023 R 41 B is CPD-60@297.
04096-8151 RST2345 A semi-regular variable, U Men. Hipparcos suspected non-single.
04097+1154 BPM 94 [PM2000] 157774 + [PM2000] 157781. Gvr2010
04097+0006 GRV 207 HJL 56. HJL1986
04099+2446 ITO 16 V1306 Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04100+8042 STF 460 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 7.24 +/- 2.42, 5.27, and 4.54 Msun, respectively. Mlk2012
04100+0944 LDS1155 LIT 10.
04102-0217 FIL 10 BAL 27.
04105+5751 HDS 529 Pair originally X coded due to lack of resolution, however, elsewhere Msn1999b
it is noted as a "very close double" so uncertain. Ambiguity from old MCK1956
reference recently found. Dam2015a
04107+3808 WNT 2 IRAS 04073+3800 = Parsamian 13. Weintraub (1992) suggests that both Wnt1992
the northern and southern components are double, with separations of
about 5" and 8", respectively.
04107-0452 A 2801 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.83 +/- 0.33, 2.34, and 1.05 Msun, respectively. Mlk2012
Docobo et al. (2017) derive an orbital parallax of 16.18 +/- 0.23 mas
and component masses 1.203 +/- 0.059 and 1.114 +/- 0.054 Msun. Age of
of the system is estimated at 5 Gyr. Doc2017d
04108-1252 PHB 1 LP 714-37
Phan-Bao et al. (2005) derive distance 18.1 +/- 2.2 pc, spectral types PhB2005
M5.5 and M7.5, masses 0.11 +/- 0.01 and 0.09 +/- 0.005 Msun.
Phan-Bao et al. (2006) derive spectral types, absolute K-band mags, PhB2006
masses of components as follows:
A M5.5 +/- 0.5 9.11 +/- 0.25 0.11 +/- 0.01 Msun
B M8.0 +/- 0.5 10.05 +/- 0.30 0.09 +/- 0.01 Msun
C M8.5 +/- 0.5 10.35 +/- 0.30 0.08 +/- 0.01 Msun
04111-1826 UPT 1 No change in angle; distance decreased 2" in 70 years. B__1951a
04112+2630 STF 502 LDS5514 (both AB and BC).
04112+1538 CHR 202 First detected as an occultation binary by Radick & Lien. Rad1982a
04113+0531 ENG 18 45 Tau. Hyades vB 14. CPM companion with rho = 124".1 is outside
detection window. An additional component was noted as spectroscopic Grf1988
by Griffin et al. (1988). Msn1993a
04119+2338 CHR 14 Observed under poor seeing conditions. Griffin & Gunn (1981) found a Grf1981d
2.4-day SB. Msn1993a
04120-0916 A 471 Motion increasing, but only three measures since 1933.
04123+6908 HJ 1141 A 13.3 magnitude star is 20" preceding.
04125+3538 HJ 341 ALI 59. BU gives 1880 position +35 25.
04125-3609 HJ 3628 B is CD-36@1632.
04128+1937 KOH 4 V1307 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04130+5237 PRV 1 GJ 164. Discovered by Palomar 5m/STEPS astrometry and confirmed
using HST/NICMOS, the combined solution by Pravdo et al. (2004)
yielded an absolute parallax of 0".0820 +/- 0".008, spectral types of
M4.5V and M6-8V and masses 0.170 +/- 0.015 and 0.095 +/- 0.015 Msun.
Inclination = 57 +13/-17, omega = 133 +45/-20 deg. Prv2004
Combined AO+STEPS analysis of this M dwarf binary yields a total mass
0.343 +/- 0.026 Msun, individual masses 0.257 +/- 0.020 and 0.086 +/-
0.007 Msun. Metallicity is at least solar. Mtc2009
Inclination = 57 +13/-17, omega = 133 +45/-20 deg.
GJ 164 = LHS 1642. A known close binary system with a well-determined
orbit (Pravdo et al. 2004; Martinache et al. 2009). Its separation is Prv2004
smaller than 100 mas at all times, and it therefore remains unresolved Mtc2009
by AstraLux. We do detect one other point source in the field of view,
but it is a suspected background contaminant based on its blue color,
with dz'= 5.8 +/- 0.1 mag and di' = 5.3 +/- 0.1 mag. Jnn2014
04130-2832 HWE 10 Rectilinear solution by Hartkopf et al. (2012). Hrt2012a
04132+5032 CHR 15 Ross 29. Van Maanen (1941) suspected this star to be a binary, but Maa1941
these are the first measurements of a companion. McA1987b
04132+2258 HU 302 A premature orbit has been computed.
04135+2816 KSA 102 Primary is variable star V1096 Tau.
04135+1813 BPM 95 [PM2000] 160209 + [PM2000] 160214. Gvr2010
04135-2554 LDS3564 NLTT 12805/12807 Chm2004
04136+0743 A 1938 46 Tau. Hipparcos astrometric solution adopted some elements from the HIP1997d
orbit of Heintz. Hei1984b
Combined spectroscopic/astrometric solution of SB1. Calculated masses
1.38 +/- 0.26 and 0.82 +/- 0.21 Msun. Mut2010b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.17 +/- 0.14, 2.77, and 2.55 Msun, respectively. Mlk2012
04139+0916 BU 547 47 Tau.
Spectral types of primary and secondary assigned by ten Brummelaar et
al., based on adaptive optics observations. TtB2000
04140+8216 LUH 7 LHS 1643 + WISE J041328.73+821854.7. Companion is likely not physical,
based on proper motion. Luh2012b
04140-1222 GAL 364 Object #120 in Gallo's original list. Gal1914
04141-3155 TS 1 The triply eclipsing TESS multiple TIC 168789840. Pair A has a period TS_2021
of 1.570d and masses of 1.25 +/- 0.05 and 0.56 +/- 0.04 \msun. Pair B
has a period of 1.306d and masses of 1.30 +/- 0.08 and 0.66 +/- 0.03
\msun. Pair C has a period of 8.217d and masses of 1.23 +/- 0.10 and
0.59 +/- 0.07 \msun. The estimated period of AC is 3.7y and AC,B of 2
kyr.
04142+5149 HU 212AC Also known as SCA 183. Sca2018b
04142+2813 GHE 1 Aa,Ab: V773 Tau. Orbital elements and dynamical mass determinations
were published by Tamazian et al. (2002). Tam2002
Aa,Ab: The combined solution by Boden et al. (2012) yields a mass and Bod2012
luminosity for the Ab component of 2.35 +/- 0.67 Msun and 2.6 +/- 0.6
Lsun. This mass is higher than expected, and suggests the Aa,Ab pair
may instead be a multiple system.
Young member of Taurus-Auriga molecular cloud. Dae2015
04142-4608 RST2338 Half-period solution equally good, but gives large mass-sum.
More speckle obs needed (the only existing one erroneous?).
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.72 +/- 0.26, 2.26, and 1.07 Msun, respectively. Mlk2012
Gomez et al. (2016) derive dynamical parallax and component masses:
20.75 +/- 0.42 mas, 1.245 +/- 0.012 Msun, 0.954 +/- 0.009 Msun. Doc2016i
04143-2742 SWR 7 CPM pair Skf2004
04144+1523 BPM 96 [PM2000] 160726 + [PM2000] 160650. Gvr2010
04144-1015 STF 516 39 Eri.
AB: H N 24. MEv2010
04144-6228 HJ 3638 alp Ret. Possible spectroscopic binary.
04145+2851 GRV 208 2MASS J04143060+2851298 and J04143109+2851518, both from the Riaz et
al (2006) sample, are separated by only 23" and although the estimated Ria2006
spectroscopic distances of 55 and 72 pc are not fully equal, they are
consistent to within the 37% error. In addition, they have very
similar proper motions (e.g. Roser et al. 2010) and thus probably form XXX2010
a physical pair. Jnn2012
04148+2813 GHE 2 FO Tau. Orbital elements and dynamical mass determinations were
published by Tamazian et al. (2002). Tam2002
M_Aa = 0.35 +0.06-0.05 \msun, M_Ab = 0.34 +/- 0.05 \msun. Tof2024
04148+2753 GHE 3 HBC 368 = V1098 Tau = LkCa 3. Torres et al. (2013) find that both
components of this 0".5 pre-MS pair are spectroscopic binaries, with
periods for Aa,Ab and Ba,Bb of 12.942 and 4.068d, respectively. Trr2013
04148+2648 DAE 21 CX Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04148+2646 DAE 20 FP Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04148-6212 HJ 3641 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
04149+5824 LDS9165 Old LDS6165.
04149+4825 STT 73 mu Per = 51 Per. A is a Beta Lyrae-type system.
The elements P, T, and e of Alden (1925) were adopted from the Ald1925
spectroscopic orbit of Cannon (Pub. DAO Ottawa 2, 365, 1915).
H 6 20 H VI 20. SHJ 364.
04152+5052 AG 309 B is BD+50@944.
04153+2044 KOH 6 Metchev & Hillenbrand say the pair is probably physical, based on
proximity. Met2004b
V1199 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04153-0739 STF 518 A: omi 2 Eri = 40 Eri = Keid
LDS 114 = STFB 1. Proper motion of A -2224 -3423.
C is a flare star, DY Eri, and a strong X-ray source.
AE: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
BC: NLTT 12868/12869 Chm2004
BC at 83" is physical, and is a Delta Scuti star showing coronal X-ray
emission.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
HIP 19849. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
BC: Additional notes may be found in Worley (1956). Wor1956b
B: M = 0.575 +/- 0.018 \msun, C: M = 0.2041 +/- 0.0064. Msn2017d
P = 230.09 +/- 0.68 y.
VLTI uniform disk diameter of A: 1.405 +/- 0.038 mas, LTI2009
VLTI limb-darkened disk diameter of A: 1.437 +/- 0.039 mas,
R = 0.770 +/- 0.021 \rsun, Teff = 5269 +/- 35 K,
M = 0.877 +/- 0.044 \msun.
CHARA Array Limb-darkened diameter of A : CIA2012f
R = 0.8061 +/- 0.0036 \rsun, L = 0.40782 +/-0.00319 \lsun,
Teff = 5143 +/- 14 K, M = 0.816 \msun.
B: Teff = 17,200 +/- 110 K, log g = 7.957 +/- 0.020, R = 0.01308 +/- BdH2017b
0.00020 \rsun, M = 0.565 +/- 0.031 \msun, l = 0.01349 +/- 0.00054
\lsun. Inferred cooling age 122 Myr. Assuming a pre-WD progenitor of
1.8 \msun with a lifetime of 1.7 Gyr gives a total system age of ~1.8
Gyr. It has a thin outer hydrogen layer.
AD, AE: Rectilinear solutions by Friedman et al. (2011). USN2011a
BD, BE: Rectilinear solutions by Mason & Hartkopf (2016). Msn2016a
04155+0611 STTA 45 AB: H VI 98. A is V774 Tau. B is BD+05@613, and a suspected variable.
AB: SHY 21. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
AB: H 6 98. MEv2010
Toyota et al. (2009) monitored the RV of both the A and B components
every 1-2 months between 2003 Mar - 2007 Nov, using a high-dispersion
echelle (precision ~10 m/s). Standard deviations of the RVs of both
components are <40 m/s and velocities show no periodic variation.
These results rejects the association of a planet of mass > 1.8 Mjup
with either star. Toy2009
04157+2049 CIA 62 Aa,Ab : M_Aa = 1.0714+/- 0.0038\msun, M_Ab = 0.9682 +/- 0.0031 \msun,
pi_orb = 20.411 +/- 0.026 mas, A_dia = 0.186 mas, B_dia = 0.163 mas. CIA2024d
TOK 659 Hyades, vB162. primary is SB2, P=55.130d Tok2014d
The 55.1-day SB of Griffin & Gunn (1981) is outside our detection Grf1981d
window. Msn1993a
RED 2 1996.1230: RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al. (1981). Luy1981
Candidate Hyades member; Reid considers definite binary. Red1997
04158+4524 STF 512 HJL 58. HJL1986
04158+3100 KOH 7 V952 Per. Member of Taurus-Auriga molecular cloud. Dae2015
04158+1524 BUP 51 A: 48 Tau = V1099 Tau
04159+3142 STT 77 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 4.90 +/- 3.64, 2.97, and 1.10 Msun, respectively. Mlk2012
STTA 43 AB,C: HJL 59. HJL1986
04162+1648 RED 3 1995.8821: RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al. (1981). Luy1981
Candidate Hyades member; Reid considers possible binary. Red1997
04163+3644 YSC 128 Also a 7.3d spectroscopic binary. Tok2019b
04163+0710 WSI 97 This is a single-lined nearby binary. Using the radial velocities
measured by D. Latham (2012, private communication), we computed a
combined orbit (the previous visual orbit reported by Riddle et al. RAO2015
(2015) had a wrong period). The inclination is close to 180deg and had
to be fixed in order to match the RV amplitude. Tok2015c
04163-6057 GLE 1 Variable: TT Ret. A premature orbit has been computed.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
04164+0710 WSI 97 Provisionally designated WSI9102. Tok2010
04165+0041 J 1458 BAL 971.
04165-5918 JSP 56 eps Ret
The companion is a possible white dwarf. Cvn2006
Companion confirmed as DA white dwarf. Cvn2007
Optical spectroscopy suggests the companion is a mid- to late-B
(B3-B9) dwarf. Mug2007b
04166+2447 LDS1158 NLTT 12896/12897 Chm2004
04170+1941 HO 328 Only elements P and T in the Starikova (1980) orbit were amended from Sta1980b
the orbit of Heintz (1978). Hei1978a
Additional notes may be found in Van Biesbroeck (1954) and VBs1954
Couteau (1963). Cou1963a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 6.92 +/- 2.37, 2.74, and 1.20 Msun, respectively. Mlk2012
04171+6408 STF 503 BD is +63 489a.
04171+0409 BAL2119 J 1814.
04173+4613 STTA 44 B is BD+45@904.
04173+2035 LDS5535 HJL1032. HJL1986
04176+2833 SAR 2 HBC 371 = LkCa 5.
04176+1658 LDS3568 This cannot be the close 3079-d or 5.609-d spectroscopic binaries of Grf2012b
Griffin. The 3079-d pair has an estimated separation of 0.06", but
delta-mag may be considerable.
04176+1657 HD 27130 Hyades vB 22. The 5.6-day SB of Griffin et al. (1985) is outside our Grf1985b
detection window. Msn1993a
04177-6315 RMK 3 the Ret
Rectilinear solution by Letchford et al. (2018). LRR2018a
04179+5847 STF 511 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.60 +/- 1.54, 3.37, and 2.09 Msun, respectively. Mlk2012
04179-3348 I 270 ups 4 Eri = 41 Eri. Duplicity of AB doubtful.
A is a spectroscopic binary, and possible variable.
HMM 2 Aa1,Aa2: close SB resolved by VLTI. A combined spectroscopic/
interferometric orbit by Hummel et al. (2017) yields component masses
3.17 +/- 0.07 and 3.07 +/- 0.07 Msun, luminosities 100.6 +/- 4.3 and
87.4 +/- 3.3 Lsun, and an orbital parallax of 18.05 +/- 0.17 mas. Hmm2017
04180+1815 CIA 63 V1232 Tau.
M_A = 1.1028 +/- 0.0011 \msun, M_B = 1.01736 +/- 0.00091 \msun,
pi_orb = 21.4783 +/- 0.0078 mas, A_dia = 0.199 mas, B_dia = 0.179 mas. CIA2024d
Hyades vB 23. The 75.6-day SB of Batten & Wallerstein (1973) is Bte1973
outside our detection window. Msn1993a
04180-0031 SKF 848 Pair originally published as BVD 45, but with incorrect sign given to Bvd2010b
declination. Pair later "rediscovered" and published with correct
declination; this latter discoverer designation has been maintained.
04181+0446 TOB9003 Measured as BAZ 3 = STF1063 but with an error of -3h in RA! Tob2012c
04181-1448 LDS9166 Old LDS6166.
NLTT 12975/12973 Chm2004
04182+5018 b Per Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Hill et al. (1976). HlG1976
04182+2248 STF 520 Measured separation too large, estimated at probably 0.30". Cou1955c
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 14.33 +/- 9.16, 3.42, and 1.20 Msun, respectively. Mlk2012
04183-3000 LDS3571 NLTT 12992/12990 Chm2004
04184+2135 MCA 14 51 Tau. Hyad (vB 24). B is BD+21@619. A is a long-period spectroscopic
binary, resolved by speckle interferometry. Analysis of the
spectroscopic/interferometric orbit is given by McAlister (1977). McA1977
1978.1490: Theta was incorrectly given as 325.5 degrees McA1980b
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
A new orbit with a period of 11.3 years was determined by Dombrowski Dmb1991
(1991). Msn1993a
Torres et al. (1997) derive a combined spectroscopic/astrometric Trr1997a
solution, yielding an orbital parallax 0.01792 /- 0.00058 and masses
1.80 +/= 0.13 and 1.46 +/- 0.18 Msun.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Deutsch & Lowen (1971). Deu1971
Aa,Ab: Martin et al. (1998) derive component masses 1.756 +/- 0.343
and 0.953 +/- 0.247 Msun. Mig1998
Pourbaix (2000) gives a combined solution for this resolved SB2, Pbx2000b
yielding orbital parallaxes and component masses.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.96 +/- 0.47, 2.99, and 1.45 Msun, respectively. Mlk2012
04184-2347 RST2344 BRT2832. Brt1947
04185+2828 GHE 4 Aka V410 Tau.
04185+2817 HAT 4 AB: Additional notes may be found in Herbig (1962). Her1962
04186+1606 BPM 97 [PM2000] 163490 + [PM2000] 163456. Gvr2010
04187+2819 SKW 2 V892 Tau.
Circumbinary disk approximately five times larger than the binary
separation. Mnr2008
Total mass estimated to be 6.0 +/- 0.2 \msun. Orbit is nearly coplanar
with circumbinary disk. Mild inner and outer disk misalignment may be
due to interaction with the eccentric binary. Lon2021
04187+2819 SKN 1 Measure of 1990.725 made by the VLA at radio wavelengths. Skn1993
04187-5252 SHY 462 AB: HIP 20109 + HIP 20074.
04188+2820 KSA 104 Primary is variable star V1023 Tau.
04189+0146 STTA 49 B is BD+01@734.
04190-0725 STF 527 H 2 80. MEv2010
04192+6135 STF 513 Same as STF 507.
04192+1100 BPM 98 [PM2000] 163846 + [PM2000] 163809. Gvr2010
04193-4416 HJ 3643 B is CD-44@1505.
04195+3800 HDS 552 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.74 +/- 0.86, 2.77, and 1.45 Msun, respectively. Mlk2012
04195+2808 DAE 23 Member of Taurus-Auriga molecular cloud. Dae2015
04196+3355 HJ 674 The discovery observation of 220 deg may be in error. The AC2000
catalog include one measurement for 1924.381: 22.3 deg and 16.1".
Proper motion of B is mu(AR) = +0.004+-0.007, mu(DEC) = -0.022+-0.002 FMR2000b
04196-2847 SHY 463 HIP 20184 + HIP 19926.
04197+1416 GIC 45 G008-027/G008-026 = Melotte 25 VA 174 + 170.
04198+1538 BLM 1 gam Tau = 54 Tau = Prima Hyadum. SB resolved by speckle interferometry.
This object was misidentified as HR 1349 by McAlister (1978). McA1978c
Observed under rather poor seeing conditions. Morgan et al. (1982) BLM1982
also report a large magnitude difference. Msn1993a
04199+3145 J 934 Jonckheere gives the 1950 position: 04 17.0 +31 43. J__1958
Couteau corrects the position. Cou1953a
04199+1631 STT 79 Hyad (vB 29). SB according to Griffin et al. (1988). Grf1988
1978.6183: The date of this observation was given incorrectly as
1977.6183 by McAlister & Fekel (1980). McA1980b
Observed under poor seeing conditions. Msn1993a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.57 +/- 1.41, 2.25, and 1.07 Msun, respectively. Mlk2012
04200+1402 BUP 53 57 Tau. A is a Delta Scuti-type variable, V483 Tau.
04201+1953 LDS1164 LDS9167 (old LDS6167). NLTT 13024 = LP 414-169 Chm2004
NLTT 13024/13026 Chm2004
04202+3336 FAR 4 Primary is white dwarf WD 0416+334 = GD 60. Aka SKF 316. Far2005b
04203+3150 HJ 5460 SEI 40. Nsn2017a
04203+1833 LDS5540 Companion at 264" agrees with Luyten's astrometry, but star at 307" is Luy1984
in much better magnitude and proper motion agreement. This pair added
as AC pair, until proper identification can be determined.
04204+3434 BU 1382 54 Per.
04204+2721 SHJ 40 phi Tau = 52 Tau. STTA 48 = H 5 13. B is BD+26@712.
04205-0119 RST4769 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.54 +/- 0.98, 3.17, and 2.00 Msun, respectively. Mlk2012
04206+2429 COU 704 Probably the A component of POU 442.
04207+1514 JNN 261 LP 475-7. Estimated age 1000-10000 Myr; masses 0.45 +/- 0.04 and 0.21
+/- 0.03 Msun; a ~7.4 au. Jnn2014
04208+3009 KOH 8 Member of Taurus-Auriga molecular cloud. Dae2015
04209+1352 CIA 60 Hyad - Melotte 25 VA 201 = vB 34.
Aa,Ab : M_Aa = 1.363 +/- 0.010 \msun, M_Ab = 1.3323 +/- 0.0099 \msun,
pi_orb = 21.174 +/- 0.073 mas, A_dia = 0.265 mas, B_dia = 0.257 mas. CIA2024d
The combined spectroscopic/interferometric solution by Konacki et al. Knc2004
(2004) uses data from the Palomar Testbed Interferometer and assumes
the eccentricity = 0.0 and the K-band brightness ratio = 1.0. Results
include P = 3.0591080 +/- 0.000011 d, T = 44497.185696 +/- 0.0026 MJD,
derived masses 1.38 +/- 0.13 and 1.39 +/- 0.13 Msun, spectral types
F6V, and diameters 0.25 mas.
Aa,Ab is resolved with PTI, orbit (Konacki & Lane 2004). The B Knc2004
component is a white dwarf (Barstow et al. 2001), DA3.1; mass 0.98 Bas2001
Msun. Shaya & Olling (2011): co-moving HIP 1996 at 0.75pc, prob. Shy2011
0.96: another Hyades star? Tok2014d
HD 27483 Mel 25 VA 201: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.04 +/- 6.10, 2.70, and 3.17 Msun, respectively. Mlk2012
04209-1156 GAL 365 Object #125 in Gallo's original list. Gal1914
04210+5015 S 445 STTA 47. B is BD+49@1161.
04211+5532 STTA 46 B is BD+55@869.
04215+1704 BPM 99 [PM2000] 165579 + [PM2000] 165489. Gvr2010
04215-2055 LDS9168 Old LDS6168.
AC: NLTT 13102/13095 Chm2004
AC: SHY 167. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
04215-2544 BU 744 Star A is SB1, P = 4.0 d, tho this may be spurious, Wor1983
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.42 +/- 1.00, 2.96, and 1.35 Msun, respectively. Mlk2012
04216-1559 LDS9169 Old LDS6169.
NLTT 13109/13110 Chm2004
04217+1046 TOK 84 HIP 20366. Small PM(A)=(-31,-12). NOMAD: PM(B)=(+39,-63), V=13.95. Tok2011a
04218+1949 KNT 2 LDS2228. The variable U Tau.
04218+1929 SIG 1 LP 415-20 = Bryja 262. Spectral types M7.0, M9.5. Probable Hyades
member. Estimated orbital period 23 +7/-6 yrs. Sig2003
Konopacky et al. (2010) derive a distance of 21. +/- 5. pc and a
system mass of 0.09 +/- 0.06 Msun. Kon2010
04219+5749 BRG 34 XO-3. Bergfors et al. (2013) estimate spectral types F5V and G0-M2.5V. Brg2013
04219+1530 CHX 1 IRAM 04191+1522. Primary is a Class 0 protostar, resolved into 7.8"
pair in 1.3mm continuum observations at Submillimeter Array (SMA). ChX2012
Chen et al. quote position angle as "SE/NW"; followup check on Aladin
by cataloguer suggests angle approximately 290deg.
04220+2826 ISM 1 RY Tau, a T-Tauri star.
04220+2818 ITO 21 V987 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04220+2658 SMN 9 FS Tau.
Measure of 1989.5 made by triangulation of multiple measures and was
in a red filter.
Tamazian et al. (2002) solution includes a mass determination based on Tam2002
an estimated distance.
AB: Additional notes may be found in Simon et al. (1992). Smn1992
04220+1932 GHE 6 Components A, Ba, and Bb of this system are also commonly designated
as N, Sa, and Sb, respectively, due to the north-south orientation of
the wider pair.
AB: Measure of 1982.5 made by the VLA at radio wavelengths. Scw1984
Measure of 1983.75 made by the VLA at radio wavelengths. Scw1986
Measures of Johnston et al. and Loinard et al. made by the VLA at Jnt2003
radio wavelengths. Loi2003
AB: Rho and theta errors for Ghez et al. (1995), Furlan et al. (2003), Ghe1995
and Roddier et al. (2000) measures have been added/updated as noted by Fun2003
Koehler et al. (2008). Koehler et al. derive a preliminary orbit for Rod2000
the AB pair, yielding a system mass of 5.57 +0.11/-0.29 Msun. Koh2008b
A,Ba: The 2000.886 Duchene et al. (2002) theta value was corrected by Dch2002
Duchene et al (2006). Also, the Duchene et al. (2006) theta value for Dch2006
2005.801 was changed by 90deg to correct for the orientation of the
camera (Schaefer, priv. comm. cited by Koehler et al. 2008) Koh2008b
KRS 2 Ba,Bb: Tamazian derives a total system mass of 2.82 +/- 0.74 Msun, Tam2005
consistent with the IRC model of Koresko et al. (1997). Krs1997
T Tau Sa-Sb orbit gives range 1991-2001 for T, 0.09-0.87 for e,
11-60 for i. Values for P and a are lower limits. Sfr2006
Duchene et al. (2006) derive masses for the Ba and Bb components of Dch2006
2.73 +/- 0.31 and 0.61 +/- 0.17 Msun, respectively.
Ba,Bb: The 2000.886 Duchene et al. (2002) theta value was corrected by Dch2002
Duchene et al (2006) Dch2006
The 2002.829 Schaefer et al. (2006) measure is a reanalysis of data Sfr2006
from Beck et al. (2004). Bck2004
Koehler et al. (2008) derive a system mass of 2.96 +0.15/-0.24 Msun Koh2008b
and individual masses of 2.13 +0.14/-0.20 and 0.83 +0.10/-0.11 Msun
for the Ba and Bb components, respectively.
Ba,Bb: The Schaefer et al. (2014) orbit, combined with a VLBA parallax
of 6.90 +/- 0.09 mas (147.6 +/- 0.6pc; Loinard et al. 2007, ApJ 671,
546) yields a total mass for Ba+Bb of 2.70 +/- 0.22 Msun. Sfr2014
Ba,Bb: Csepany et al. (2015) generated new orbital parameters for T
Tau N-S (KRS 2Ba,Bb), but their grid search yields a wide range of
possible solutions (P 475-27000y, a 0.57-16.8", etc.) Cse2015b
Based on the new orbit and the Gaia parallax the masses of Ba(Bb) is Sfr2020
is 2.049(0.430) +/- 0.137(0.055) \msun. Using the slightly grater
distance from the VLBA parallax the result is 2.268(0.476) +/-
0.147(0.060) \msun. The brightnesa of Ba and Bb are both variable.
04220+1405 HD 27628 Hyades vB 38 = V775 Tau. The 2.14-day SB of Abt (1961) is outside our AbH1961
detection window. Msn1993a
BUP 54 60 Tau. A is a specroscopic binary and variable, V775 Tau.
04221+2826 KSA 105 V1071 Tau = LkCa 21. Young member of Taurus-Auriga molecular cloud. Dae2015
04221-2849 BWL 15 Pair is a 0".7 equal-flux K7V2 binary. Torres et al. (2006 A&A 460,
695) found strong Halpha emission and lithium absorption. Age is
consistent with that of the Pleiades, so an age range of 50-200 Myr
is adopted for this system. Bwl2015
04221+1934 KOH 9 Young member of Taurus-Auriga molecular cloud. Dae2015
04224+1118 PAT 5 The 3-year SB of Griffin et al. (1988) is outside our detection Grf1988
window. Msn1993a
The double-lined spectroscopic solution of this 1043.5-d pair Grf2012b
determined by Griffin.
04226+2538 STF 528 chi Tau = 59 Tau
H 4 10. MEv2010
The secondary is SB2 (F8+G6), with period 17.6 days for Ba,Bb; RV
residuals indicate the presence of a more distant Bc companion. Based
on spectroscopic observations obtained at CfA 1988-2004, Torres (2006)
derived an orbit for Bab,Bc with period 9.447 +/- 0.017 yr. Mass for
the A component is determined to be 2.60 +/- 0.5 Msun. Inclination
angle for the Ba,Bb orbit is 53.5 +/- 0.5deg, yielding masses 1.19 and
1.02 Msun for Ba and Bb. Bc appears to be over-massive; based on
infrared excess this could be well explained as an equal-mass binary
composed of late-type stars of masses ~0.70 Msun (spectral type ~K4).
Total mass of B is 3.6 Msun. Torres estimates the Bab,Bc semi-major
axis at about 83.6 mas and the magnitude difference dV~3.3mag
(dK~1.5mag), making the pair potentially resolvable by speckle
interferometry. Trr2006b
04227+1503 STT 82 Hyades vB 40A. The primary is SB1, P = 4.00 d (Sanford 1921). San1921
Primary is SB2, P=4.0002d (Griffin 2012) Grf2012b
Also a wider companion (LDS 1166 AC, rho = 62", M = 17.8).
The 255.5-year binary, ADS 3169 = STT 82 AB is outside our detection
window, although part of a peak is seen at the edge of the window at
the expected position angle, according to the orbit in the Worley &
Heintz (1983) orbit catalog. A wider companion (LDS 1166AC, rho = 62", Wor1983
M = 17.8) and the 4d SB are also outside our detection window. Msn1993a
A component of pair determined to be a 4.0-d spectroscopic binary. Grf2012b
04228+1647 HD 27685 Hyades vB 39. Spectroscopic binary with P > 7 yr, according to Griffin Grf1988
et al. (1988). Msn1993a
04230+1732 CHR 262 del 1 Tau = 61 Tau = Secunda Hyadum. The primary is a long-period
BUP 55 spectroscopic and occultation binary.
Mk III Limb-darkened diameter 2.338 +/- 0.033 mas. MkT2003
CHARA Array Limb-darkened diameter 2.408 +/- 0.038 mas. CIA2009a
R = 12.3 +/- 0.4 \rsun, Teff = 4826 +/- 51 K.
This system, first announced in Mason et al. but considered of Msn1993a
uncertain veracity, has been included. While its status is not
definitive, subsequent confirmation or suspected duplicity (by another
technique) makes the discovery measurement somewhat more probable.
1991.8995: This is a particularly unexpected result, given the four
previous epochs at which our observations have shown no indications of
duplicity. All four of the earlier observations were reanalyzed using
the same procedures employed here, but no additional supporting
evidence of duplicity was found. If this additional component is
confirmed, vB 41 will be the second K0 giant binary that has been
resolved in the Hyades (HR 1411 being the other). The common proper
motion companion at a separation of 195".5 is far outside our window
of observation, and the 530-day spectroscopic component of Griffin &
Gunn (1977) would have an angular separation below the diffraction Grf1977d
limit of the KPNO 4-m telescope. Msn1993a
Aa,Ab : If real, this pair could be the 530.1-d spectroscopic binary Grf2012b
of Griffin.
04231-0117 BU 402 Aka OL 201.
04232+7510 MLR 459 Also known as TDS 138.
04232-1135 GAL 366 Object #127 in Gallo's original list. Gal1914
04233+1123 STF 535 A premature orbit has been computed.
Ruymaekers & Nys (1995) noted discrepancies in the orbit of Popovic Ruy1995
(1982), and calculated elements from their Thiele-Innes elements. Pop1982a
04233-0500 HJ 342 Same as STF 539 and H IV 117.
AB: H 4 117. MEv2010
04233-2138 B 2571 CPD-21@545.
04234+1940 V988 Tau Hyades vB 43. Hipparcos astrometric solution adopted some elements HIP1997d
from the orbit of Griffin et al. (1985). Grf1985b
The 1.6-year SB of Griffin et al. is outside our detection window. Msn1993a
04234+1647 HD 27749 Hyades vB 45. The 8.418-day SB of Abt & Levy (1985) is outside our AbH1985
detection window. Msn1993a
04234+1546 TOK 876 V989 Tau.
04235+2059 CHR 16 An occultation binary, now resolved.
04236+4226 STT 80 1977.7420: The date of this observation was given incorrectly as
1978.7420 by McAlister & Fekel (1980). McA1980b
04236+2503 MTZ 2 FU Tau
04237+1538 MET 3 Metchev & Hillenbrand say the pair is probably optical, based on
proximity. Met2004b
04238-0414 BUG 7 SDSS J042348.57-041403.5
Estimated spectral types are L6.5 + T2, effective temperatures 1490
+/- 100 and 1250 +/- 80 K. Masses are estimated at 0.039-0.062 and
0.029-0.051 Msun, and the orbital period (assuming the semi-major axis
= 1.26 * rho) is ~19yr. Bug2006a
04239+0928 HU 304 66 Tau.
Spectral types and masses of components assigned by ten Brummelaar et
al., based on adaptive optics observations. TtB2000
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 4.81 +/- 1.40, 6.11, and 4.43 Msun, respectively. Mlk2012
04239-1102 GAL 367 Object #128 in Gallo's original list. Gal1914
04240+2418 STF 534 62 Tau.
AB: H 4 109. MEv2010
04241+1727 BUP 56 del 2 Tau = 64 Tau. Hyades vB 47. A is spectroscopic binary.
04242+1445 HDS 564 1991.8992: Noted as a possible spectroscopic binary by Griffin et al. Grf1988
(1988), it is uncertain whether the system we detect here is also
producing the radial velocity variation. Msn1993a
Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
The spectroscopic solution of this ~42000-d pair determined by Griffin, Grf2012b
its gamma velocity "removing any remaining doubt about the systems Grf2013c
credentials as a Hyades member."
04242-5704 RMK 4 Rectilinear solution by Letchford et al. (2018), however, common
parallax and proper motion argues for their orbital solution. LRR2018a
04244+3419 STF 533 AB: H 4 72. MEv2010
Primary is V590 Per, a Beta Lyr type eclipsing binary, P = 5.6866d. Zas2012
04245+5051 TOK 245 AC: The physical nature of C is not certain: CPM, but the PM is small. Tok2014d
COU2459 AB: Rectilinear solution by Hartkopf & Mason (2013). Hrt2013b
04245+2244 BU 1235 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.22 +/- 2.00, 2.88, and 1.35 Msun, respectively. Mlk2012
04245+1653 PAT 6 Noted as a possible spectroscopic binary by Griffin et al. Grf1988
(1988). Msn1993a
Hyades vB 52. Mass of B 0.49 Msun (Metchev & Hillenbrand 2009). Met2009
04246+3358 STT 81 AB: 56 Per.
04247+0442 HJL1115 Hyades vB 140. The 156.4-day SB of Griffin et al. (1985) is outside Grf1985b
our detection window. Msn1993a
A combined interferometric/spectroscopic solution by Halbwachs et al.
(2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun. HJL2016
Mass = 0.9798 +/- 0.0019, 0.72697 +/- 0.00094 \msun for A and B. HJL2020
orbital parallax = 16.703 +/- 0.034 mas.
04247-0845 STF 544 Primary is SB1, P=1248d = 3.41y. RV(B)=var? Tok2014d
04247+0442 HJL1115 A combined interferometric/spectroscopic solution by Halbwachs et al.
(2016) yields masses 0.9808 +/- 0.0040 and 0.7269 +/- 0.0019 Msun. HJL2016
04248+1552 PAT 7 SB with P > 7 yr according to Grf1988
Griffin et al. (1988). Msn1993a
The spectroscopic solution of this 5688-d pair determined by Griffin. Grf2012b
04248-5037 RST1273 HIP 20606. Both components A,B are above the MS, young? B is too red in
the (Kabs,V-K) CMD, infrared companion? Planetary companion to A = HD
28254 is detected with RV. No relevant references in SIMBAD. Tok2011a
A is exoplanet host, P=1116d. Roell et al. (2012 A&A 542, A92) list B
as physical, confirmed by Naef et al. (2010 A&A 532, A15). Tok2014d
04249-3445 I 59 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
04251+8603 WFC 23 HJL 57. HJL1986
04252+2545 TOK 247 Not Hyades member: different PM and RV. (Griffin 2013). Grf2013c
04252+1716 AST 4 V805 Tau.
The visual A consists of an M3.5V main sequence star (A) and an
unresolved WD (D) with a period of 20.82d. B consists of a pair of
unresolved M dwarfs with an orbital period of 0.75d. V band fits of the
masses of A, B and C are 0.46, 0.40 and 0.38 \msun, respectively. K
band fits of the masses of A, B, C and D are 0.60, 0.46, 0.44 and 0.53,
respectively. AST2021
04252-6415 HJ 3656 B is CPD-64@333.
04253-0932 GAL 368 Object #129 in Gallo's original list. Gal1914
04254+2218 STF 541 A: kap 1 Tau = 65 Tau = K Tau
A,CD: H 6 8. MEv2010
AB: HJL1034. HJL1986
STF 541 04253+2215STF 541CD and 04254+2218STFA 9AB were found to
STFA 9 be the same wide pair, so designations for these two
multiple systems were combined, as follows:
04253+2215STF 541AB --> 04254+2218STF 541CD
04253+2215STF 541AB,C --> 04254+2218STF 541A,CD
04253+2215STF 541AB,D --> 04254+2218STF 541B,CD
04254+2218STFA 9AB --> 04254+2218STF 541AB
04254+2218STFA 9Aa --> 04254+2218STF 541AE
04254+2218STFA 9Bb --> 04254+2218STF 541BF
A : kap 1 Tau = 65 Tau = K Tau. Occult. binary, Hyades member (vB 54)
B : kap 2 Tau = 67 Tau. Delta Scuti variable, Hyades cluster member.
CD : J 2722. This faint pair is between kap 1 and kap 2 Tau.
Pairs STFA 9AB (rho = 339"), STFA 9Aa (rho = 141") and STFA 9Bb
(rho = 107") are all far outside our detection window. Msn1993a
04255+1756 KUI 17 del 3 Tau = 68 Tau. A is spectroscopic binary and variable, V776 Tau.
H 6 101 H VI 101. There is a wide faint pair noticed by John Herschel, 320@
Class VI. H__1867
The B, C, D, and E components all fall outside our detection window. Msn1993a
04256+1556 FIN 342 Aa,Ab: Hyad (vB 57). HR 1391 = 70 Tau.
Combined spectroscopic/astrometric solution. Orbital parallax 0.02144 Trr1997b
+/- 0.00067, masses 1.363 +/= 0.073 and 1.253 +/- 0.075 Msun.
Quadrant determinations made at several epochs by McAlister et al. McA1988
(1988) have shown that this system is best represented by an eccentric
orbit of period 6.3 years, rather than a circular 13-year orbit.
1977.7421 Theta was incorrectly given as 6.0 degrees by McAlister &
Fekel 1980). McA1980b
This resolved spectroscopic binary (with P = 6.28 yr) is discussed by McA1988
McAlister et al. (1988) and by Dombrowski (1991). Dmb1991
The published measure for 1988.6582 (McAlister et al. 1990) is McA1990
is spurious. The data leading to this measure are actually the same as
those for HR 1331 (= McA 14) for the same epoch. These two stars were
observed in immediate sequence but with different microscope
objectives, and the final reductions calculated two results from the
same data set, but with different scale factors; the HR 1331 measure
for 1988.6582 is the correct one. Reanalysis of the correct data for
FIN 342 gives the 25 mas result shown here. Peterson (1992, private
communication) pointed out the inconsistency of our originally
published measure with respect to our previous orbital analysis of
this Hyades binary (McAlister et al. 1988). Hrt1992b
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
Aa,Ab : New spectroscopic solution determined by Griffin. Grf2012b
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.50 +/- 0.47, 2.48, and 1.13 Msun, respectively. Mlk2012
04257+6340 HJL1033 SHY 464. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
04257-0214 BU 403 Linear elements fit nicely at present, but this is a physical pair and
an orbit can be computed at some future date.
Rectilinear solution by Hartkopf et al. (2012). Hrt2012a
04258+1800 COU2682 Spectroscopic binary with P > 15 yr, according to Griffin et al. Grf1988
(1988). Msn1993a
The spectroscopic solution of this 15650-d pair determined by Griffin. Grf2012b
04258+1733 RED 4 1996.1449: RHy ID and coordinates from Reid (1992). Red1992
Candidate Hyades member; Reid considers definite binary. Red1997
04259+1852 BU 1185 Hyad (vB 58).
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
1982.7579: This autocorrelogram was remeasured; the new results are McA1987b
listed here.
The 27.67-year binary (see Dombrowski 1991) ADS 3210 was observed at Dmb1991
a time when atmospheric seeing was rated as poor. Also noted as a SB Grf1988
in Griffin et al. (1988). Msn1993a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.01 +/- 0.36, 2.00, and 0.98 Msun, respectively. Mlk2012
04260+4515 ES 567 B is BD+44@946.
Measures attributed to BC are all AC. Component designation changed.
04261-1059 GAL 369 Object #130 in Gallo's original list. Gal1914
04262+3313 HJ 676 AC: SEI 44. Nsn2017a
04263+3443 HU 609 Only elements P and T have been amended from the orbit of Sta1978c
Heintz (1967). Hei1967d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 12.01 +/- 10.65, 3.16, and 1.20 Msun, respectively. Mlk2012
A is also a 141d spectroscopic binary. B is a possible Tok2019b
spectroscopic binary (~1600d), too.
04263+2249 BUP 58 ups Tau = 69 Tau. A is an occultation binary.
04263+2128 TOK 16 Hyades vB 62. Primary is 8.55d SB1 (Griffin & Gunn 1978); estimated Grf1978b
period of visual pair 9300y. Unresolved by Patience et al. Tok2006
The SB is outside our detection window. Msn1993a
04263+1538 HD 28052 Hyades vB 141. A CPM companion with rho = 134".4 is outside our Msn1993a
detection window. Also, noted as a 14.24-year SB by Abt (1965). AbH1965
04263+1537 BUP 59 71 Tau. A is a long-period spectroscopic binary,
P = 5200d, and occultation pair. V777 Tau.
Peirce noted a close companion to A component (1868.13, 70deg) which
he said was "much closer than 80 Tau". His 1868.13 separation
measure for 80 Tau (= 04301+1538 STF 554) was 0".75. Pei1882
04263+1400 HJ 3256 LDS5558.
04264+2249 HD 28024 Hyades vB 60. A CPM companion with rho = 110".2 is outside our
detection window. Msn1993a
04264+1651 HD 28068 Hyades vB 63. A spectroscopic binary B with P ~ 7 yr, according to Grf1985b
Griffin et al. (1985). Msn1993a
04268+1525 LDS2236 LDS5559.
04268+1052 PAT 8 1991.8990: This K dwarf is noted as a binary with a period in excess
of 16 years in Griffin et al. (1988), and it is likely that we have Grf1988
detected the spectroscopic companion. Msn1993a
The spectroscopic solution of this 6950-d pair determined by Griffin. Grf2012b
04268+0843 HJ 678 This is not BD+08 690, according to Heintz. Hei1992a
AB: Rectilinear solution by Friedman et al. (2012). USN2012a
04268-0143 UC 1168 Candidate on Tokovinin list, now reconfirmed as CPM. Tok2013c
AB is CPM according to Hartkopf et al. (2013). A is on Keck RV UC_2013b
program, RV trend. Tok2014d
04269+2607 LEI 2 Measure of 1987.8 made by triangulation of multiple measures and was
in a red filter.
SMN 10 Ca,Cb: Called FV Tau-c by Simon, therefore given component designation
of Ca,Cb. Relationship to LEI 02 uncertain. Smn1992
Measure of 1987.8 made by triangulation of multiple measures and was
in a red filter.
aka COR 3Ca,Cb
FV Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04270+1907 STF 546 HJL 60. HJL1986
H 2 54. MEv2010
04270-7238 B 2091 Composite spectrum: G8III+(A/F).
04271+2542 THB 1 Preliminary orbital elements give total mass 2.8 +/- 1.5 Msun. Thb1995b
Tamazian et al. (2002) solution includes mass determination based on Tam2002
estimated distance.
DF Tau orbit by Schaefer et al. (2006) gives range 1974-2022 for T, Sfr2006
0.05-0.76 for e. Values for P and a are lower limits.
Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total
mass 1.17 +/- 0.13 Msun. The orbital period of 43.7y closely matches
the 44yr timescale of photometric variations; this is consistent with
a suggestion by Lamzin et al. (2001 A&A 372, 922) that the variability
is caused by the circumstellar accretion rate onto the primary being
modulated by the orbital motion of the companion. Sfr2014
04271+1812 STF 545 AB: H 4 74. MEv2010
04275+1113 BU 1186 A is variable.
04275-1707 HU 440 Primary is HH Eri, eclipsing binary (Algol-type), P=8.5d. Tok2014d
04275-2427 I 413 Baize (1993) value of omega incorrectly listed as 96.0, same as Omega. Baz1993b
04276+1927 RED 5 1995.6986: RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al.(1981). Luy1981
Candidate Hyades member; Reid considers definite binary. Red1997
04277+2631 GIC 47 LDS1171. G008-035/G039-014.
NLTT 13302/13303 Chm2004
04278+1001 STF 549 AB: H 4 75. MEv2010
04280+2137 BUP 60 A is a spectroscopic and occultation binary.
04281-1033 GAL 370 Object #131 in Gallo's original list. Gal1914
04282+5303 RUC 3 AO Cam. Spectral type of resolved companion later than M5V. Ruc2007
04282+0600 LDS9170 Old LDS6170.
04283-1400 GAL 371 Object #132 in Gallo's original list. Gal1914
04284+1622 RCH 2 Measure of 1998.921 made by triangulation of multiple measures. Rch2002
04284+1444 CIA 25 76 Tau.
04284-0736 GRV1248 Both A and B have approximately the same radial velocity. Grv2019b
04284-6543 HJ 3662 B is CPD-65@@345.
04285+1742 GUE 5 The spectroscopic solution of this 7022-d pair determined by Griffin. Grf2012b
04285+1458 BPM 100 [PM2000] 170962 + [PM2000] 171001. Gvr2010
04285+0505 HJ 2233 BAL 2614.
04286+1944 HD 28291 Hyades vB 69. The 41.66-day SB of Griffin et al. (1985) is outside Grf1985b
our detection window. Msn1993a
04286+1911 BUP 61 eps Tau = 74 Tau = Ain
Mk III Limb-darkened diameter 2.67 +/- 0.04 mas. MkT2001
Mk III Limb-darkened diameter 2.671 +/- 0.032 mas. MkT2003
NPOI Limd-darkened diameter 2.41 +/- 0.11 mas. NOI2001b
CHARA Array Limb-darkened diameter 2.734 +/- 0.031 mas. CIA2009a
R = 13.4 +/- 0.2 \rsun, Teff = 4827 +/- 44 K.
NPOI Limb-darkened diameter 2.592 +/- 0.050 mas, Sp = G8III, NOI2018
R =12.53 +/- 0.28 \rsun, Teff = 4880 +/- 77 K, L = 80.3 +/- 4.4 \lsun,
M = 2.69 +/- 0.11 \msun, Age = 0.55 +/- 0.10 Gyr.
04287+2714 KON 2 Estimated masses 0.15 and 0.06 Msun. Primary spectral type M5.25 Kon2007b
04287+2613 HDS 576 Cvetkovic et al. (2014) derive spectral types M0 and M0, masses 0.46
and 0.46 Msun. Dynamical parallax is 25.86 +/- 0.27 mas. Cve2014
04287+1552 STFA 10 AB: the 2 Tau = 78 Tau = Chamukuy. Hyades vB 72 = HR 1412.
Pair appears in an appendix list, not part of discoverer's regular
numbering sequence. B is BD+15@631.
Also variable, probably of Delta Scuti type.
The 140.7-day SB of Ebbighausen (1959 Pub. DAO, 11, 235) is outside
our detection window. Msn1993a
UBAD 2.1 relative astrometry measures computed. Table 1 mean positions USN2022
for 2017.0 and Table 2 mean dates computed as well when appropriate.
MKT 13 Aa,Ab: Data from lunar occultation, spectroscopy, and Mark III
astrometry are combined by Torres et al. to generate orbital elements. Trr1997c
Distance and component masses and absolute magnitudes are derived from
these elements.
Period is fixed for the Armstrong et al. (2006) orbit. The resulting MkT2006
component masses are 2.15 +/- 0.12 Msun and 1.87 +/- 0.11 Msun.
Aa,Ab: Orbit determined by fitting revised Hipparcos intermediate
astrometric data. Derived component masses are 2.03 +/- 0.87 and
1.78 +/- 0.76 Msun. Ren2010
Aa,Ab: Combined spectroscopic/astrometric solution, using data from
Mark III interferometer plus high-resolution spectroscopy from ELODIE,
HERMES, and CfA. Torres et al. (2011) determine an orbital parallax of Lmp2011
20.90 +/- 0.14 mas and component masses 2.86 +/- 0.06 and 2.16 +/-
0.02 Msun. Effective temperatures for both components are 7800 +/-
170K, absolute magnitues are 0.33 +/- 0.03 and 1.44 +/- 0.03 mag.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 4.46 +/- 0.29, 3.81, and 2.00 Msun, respectively. Mlk2012
MCA 15 Ba,Bb:The primary of 04286+1558 was found to be the B component of
physical pair 04287+1552; systems were merged.
the 1 Tau = 77 Tau. Hyad (vB 71). Physical companion to the 2 Tau.
A spectroscopic, occultation, and interferometric binary.
First detected as an occultation binary by White. Wit1979
1979.698, 1979.857: possible third component Heg1983
This is a long period interferometric companion in addition to the
spectroscopic component suggested by Griffin & Gunn (1977) to have a Grf1977d
period of about 16 years. An estimate of Delta m = 0.76 was made by Dmb1991
Dombrowski (1991). Msn1993a
Masses and distance of the 2 Tau are derived from spectroscopic
elements, adopting astrometric elements from Pan et al. (1992) MkT1992e
Combined spectroscopic/astrometric solution by Torres et al. (1997). Trr1997c
Distance (from relative proper motions and orbital parallax of the 2
Tau) 47.6 +/- 1.9 pc, masses 2.91 +/= 0.88 and 1.31 +/- 0.14 Msun.
CHARA Array Limb-darkened diameter of B 2.305 +/- 0.043 mas. CIA2009a
R = 11.7 +/- 0.2 \rsun, Teff = 4811 +/- 50 K.
Ba,Bb : New spectroscopic solution determined by Griffin. Grf2012b
Ba,Bb: Malkov et al. (2012) derive dynamical and spectroscopic masses
4.14 +/- 0.35 and 2.88 Msun, respectively. Mlk2012
BPMA 7 BC: [PM2000] 171052 + [PM2000] 171309. Gvr2010
04288+1617 BPMA 8 [PM2000] 171281 + [PM2000] 171421. Gvr2010
04289+3022 STF 548 AB: B=HIP 20907 is bluer than A, below the MS. A is 1.7mag above. But
they are physical: CPM, parallax, same RV! Primary is SB1, P=460.7d. Tok2001
A,B have same RV (Tokovinin & Gornya 2001), both rotate fast Tok2014d
04289-0236 BRT 366 A likely plate flaw. Grv2021b
04290+1610 HU 1080 Hyad (VB 75); RV possibly variable, as noted by Wilson (1948). WOC1948
The spectroscopic solution of this 14697-d pair determined by Griffin. Grf2012b
B is also a close 21.3-d pair.
M_A = 1.341 +/- 0.025 \msun, M_Ba = 1.210 +/- 0.021 \msun, M_Bb = Trr2019b
0.781 +/- 0.014 \msun. Orbital parallax = 21.75 +/- 0.11 mas.
04290+1338 SIG 2 LP 475-855. Spectral types M7.5, M9.5. Probable Hyades member.
Estimated orbital period 86 +20/-19 yrs. Sig2003
04292-1206 LDS3591 NLTT 13376/13372 Chm2004
04293+1733 HD 28394 Hyades vB 77. The 238.9-day SB of Griffin et al. (1985) lies outside Grf1985b
our detection window. Msn1993a
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin et al. (1985). Grf1985b
04293-3124 SIG 4 Aka 2MASS 0429-3123AB. Significant H\alpha emission. Appears to be JLB2017
young, but not a member of any known moving group or association.
Parallax = 58.71 +/- 1.25 mas.
04294+2701 KON 3 Estimated masses 0.1 and 0.06 Msun. Primary spectral type M6.0 Kon2007b
04294-3335 HJ 3652 Primary is CT Eri, a Beta Lyr type eclipsing binary, P = 0.63420d. Zas2012
04295+2617 SMN 11 Measure of 1990.25 made by triangulation of multiple measures and was
in a red filter.
AB: Additional notes may be found in Simon et al. (1992). Smn1992
WHT 2 AC: Primary is the Orion-type variable FW Tau. Multi-epoch astrometry
by Kraus et al. (2014) confirm the AC pair is co-moving, and estimate
mass of the companion at 10 +/- 4 Mjup for a system age of 1-5 Myr. KsA2014
HER 8 AD: Additional notes may be found in Herbig (1962). Her1962
04295+1752 BGH 2 LDS 2244. Variable, V921 Tau. B is +17@ 734.
HJL1035. HJL1986
04295+0025 BAL 972 RST 5206.
04296+0350 BAL2121 J 2725.
04297+2633 HAT 6 AB: Additional notes may be found in Herbig (1962). Her1962
DI Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
ITO 13 BC: B component is the Orion-type variable DH Tau = HBC 38. Colors of
both B and C are consistent with T Tauri stars. The B component has a
lower effective temperature than A (2700-2800K, vs 3580K), and is
redder. The stars are probably early and late M stars; mass of the
companion is estimated at 30-50 Mjup. Ito2005
Kraus et al. (2014) estimate mass of the companion at 18 +/- 4 Mjup. KsA2014
04298-0949 LDS3592 NLTT 13393/13392 Chm2004
04299+2607 HER 9 Aka IQ Tau. Additional notes may be found in Herbig (1962). Her1962
04300+8320 HR 1304 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Prieur et al. (2006). Pru2006
04300-6955 OGL 193 LMC157.7.150 + LMC157.7.333 Pli2012
04301+1814 JOY 2 A RW Aur-type variable, UX Tau. Her1962
04301+1538 STF 554 80 Tau. Hyad. Star A is SB1, P = 30.5d Hei1981e
Spectral types and masses of components assigned by ten Brummelaar et
al., based on adaptive optics observations. TtB2000
04301+1538 STF 554 The 1897 measure by Burnham was "... made under not the best Bu_1900
conditions ..." and "... is difficult to reconcile ...". Aitken did
not include it in the ADS. It was, then, not in the IDS list of A__1932a
measures transferred to Washington in 1964, so this measure was lost IDS1963A
for many years and recently found by G. Torres, and the observation Trr2019
of this high eccentricity binary was made shortly after periastron
passage, which resulted in the unexpected result.
Ma = 1.63 (+0.30 or -0.13) \msun, Mb = 1.11 (+0.21 or -0.14) \msun,
orbital parallax = 20.984+/-0.060 mas.
04302+3516 TTH 1 HBC 40 = LkHA 101. Herbig Ae/Be star imaged at multiple wavelengths
shows evidence of a companion at ~180 mas to the East-Northeast of the
primary. Derived physical parameters for A and B for three possible
distances are:
160pc: L/Lsun = 1300 and 340 R/Rsun = 1.9 and 1.0
340pc: L/Lsun = 5900 and 1500 R/Rsun = 4.1 and 2.1
800pc: L/Lsun = 30000 and 8500 R/Rsun = 9.7 and 5.0 Tth2002
04302-0303 PRB 2 Primary is WD 0427-03 = NLTT 13402, secondary is LP 655-33. Possible
CPM pair, according to Probst (1983). Prb1983
04302-6753 TOK 85 HIP 20998. Not observed, but J-K=2.92 for B in the 2MASS PSC, hence
optical. Tok2011a
04303+1950 PAT 10 Noted as a probable SB in Grf1988
Griffin et al. (1988). Msn1993a
Member of the Hyades (vB 81) and "probable SB" according to Griffin et Grf1988
al. (1988). This WDS pair PAT 10 was resolved by speckle. Tok2012a
The spectroscopic solution of this 4023-d pair determined by Griffin. Grf2012b
04306+1612 LDS2246 Hyades vB 82. A is possibly variable. B is BD+15@640.
The primary was noted as a possible occultation binary by Peterson Pts1981a
et al. (1981). Msn1993a
HJL1036. HJL1986
04306+1545 HD 28545 Hyades vB 182. The 358.4-day SB of Griffin & Gunn (1981) is outside Grf1981d
our detection window. Msn1993a
04306+1542 BUP 62 81 Tau = LDS2247. Hyades vB 83. B is BD+15@638.
AB: HJL1037. HJL1986
ARN 36 The CPM B companion with rho = 161".8 is outside our detection window,
as are C and D. Msn1993a
CIA 65 Ca,Cb : M_Ca = 0.9717+/- 0.0056\msun, M_Cb = 0.6859 +/- 0.0028 \msun,
pi_orb = 20.318 +/- 0.042 mas, A_dia = 0.159 mas, B_dia = 0.118 mas. CIA2024d
D component is primary of 04309+1547 TDS2876. Pair does not appear to .
be physical, so systems not merged.
04306+1344 HD 28556 Hyades vB 84. A CPM companion with rho = 111".9 lies far outside our
detection window with a large Delta m of 5.8. Msn1993a
04306+1343 BUP 63 83 Tau.
04307+2601 SMN 12 Measure of 1990.77 made by triangulation of multiple measures and was
in a red filter. Smn1992
04307-1627 HJ 3653 B is BD-16@879.
04308+1609 PAT 11 Hyades. The 0".3 binary PAT 11 was not resolved by speckle. The GCS did
not detect RV variability despite large scatter of 4.8 km s-1 in their
three measures. Tok2012a
04309+2442 SMN 13 ZZ Tau. Sfr2003 astrometry for 1995.081 and 1996.124 was based on
interpolation of one-dimensional data by Simon. Smn1996a
The first ZZ Tau orbit by Schaefer et al. (2006) gives range 1994-1999 Sfr2006
for T, 0.35-0.88 for e, 115-134 for i, 111-129 for Omega, 268-336 for
omega. Values of P and a are lower limits. The second orbital
solution includes a lunar occultation measure by Simon et al. (1995). Smn1995
Assuming a distance of 140 pc, Schaefer et al. (2014) derive a total
mass of 0.83 +/- 0.16 Msun. Sfr2014
04309+1547 TDS2876 D component of 04306+1542. ARN 36AD does not appear to be physical,
so systems not merged.
04309-0849 KO 2 CPM pair; A = LP 655-23 (spec early M), B = 2MASS J0430516-084901
(M8.0V). Mean separation (1953-2000) 0.328 +/- 0.004 arcmin. Data
sources: Palomar Sky Survey red (1953.2), UK Schmidt blue (1982.8), UK
Schmidt red (1985.9), 2MASS (1998.7), DENIS I (1998.9), UK Schmidt
near-IR (2000.0). Masses of components estimated at 0.26 +/- 0.04 and
0.086 +/- 0.004 Msun. Cab2007b
A known component of the wide binary Konigstuhl 2AB with a separation
of 20" (Caballero 2007), 2MASS J04305203-0849193 is single closer in, Cab2007b
in the AstraLux images. Jnn2012
04310+7724 MLR 461 Also known as TDS 142.
04310-6911 OGL 194 LMC156.6.7 + LMC156.6.6 Pli2012
04311+0647 STT 84 HJL 61. HJL1986
04311-4522 TOK 208 Possibly triple. The new companion at 1".6 should not produce RV
variability by 3.8 km s-1. Tok2012a
04312+5858 STI2051 A is an astrometric binary. B (mag. 12.44, 8", DC) is a white dwarf,
in slow retrograde motion about the mass-center. A very large proper
proper motion brought this pair close to a 13th magnitude star which
was measured as the C component by Pauwels & Lampens. Pws1993
Also known as HDS 584.
B: Teff = 7122 +/- 122 K, R = 0.0114 +/- 0.0004 \rsun, M = 0.675 +/- BdH2017b
0.051 \msun.
AB: Rectilinear solutions by Cvetkovic (2015) Cve2015b
and Cvetkovic et al. (2016). Cve2016
Despite the linear solution, based on proper motion and parallax
is physical.
04312+0621 LDS9171 Old LDS6171.
04313-6959 OGL 195 LMC157.7.2247 + LMC157.7.2249 Pli2012
04314+4001 STF 552 H N 44. MEv2010
04314-0934 GAL 372 Object #136 in Gallo's original list. Gal1914
04314-1339 STF 560 B is BD-13@905.
04315+1706 SAR 3 HBC 392 = V1074 Tau. SB2. Sar1998
Member of Taurus-Auriga molecular cloud. Dae2015
04316+1743 HD 28634 This is a 2.31-year spectroscopic binary, according to Griffin et al. Grf1985b
(1985). Msn1993a
vA 627 VVO 394. Hipparcos astrometric solution adopted some elements from the HIP1997d
orbit of Griffin et al. (1985). Hyad. Grf1985b
Perturbation orbit by McArthur et al. (2011) is based on HST FGS AST2011
astrometry, plus radial velocities from Griffin et al. (1985). Derived Grf1985b
masses are 0.83 +/- 0.05 and 0.42 +/- 0.05 Msun.
04316-7037 OGL 196 LMC158.1.29 + LMC158.1.122 Pli2012
04317+2330 POU 458 LDS 886 = LDS1173.
04317+1814 HER 10 AB: Additional notes may be found in Herbig (1962). Her1962
XZ Tau.
GHE 9 Aa,Ab: Dodin et al. (2016) generated the following preliminary orbital
elements: P = 155-256y, a = 27.2-37.2au, i <47deg, e = 0.29-0.64. Dod2016
Carrasco-Gonzalez et al. (2009) found a close companion to the Aa CGo2009
component at 7mm wavelength (~6deg, 0.09", dm 0.4 +/- 0.3 mag).
However, subsequent observations by Forgan et al. (2014) and the ALMA Fgn2014
Partnership (2015) found no evidence of this additional component and ALM2015
concluded it was a false detection.
04317+1538 WOR 16 The A component is a known Hyad.
LDS1174 The C component may or may not be a physical companion, possibly
sharing CPM only as a member of the cluster.
04318+2424 CHN 3 Formerly known as LEI 15.
04319-0851 HJ 2234 B is BD-09@917.
04320+5355 STF 550 1 Cam. A spectroscopic binary.
AB: H N 67. MEv2010
04320+1822 CHN 4 Formerly known as LEI 16.
AB: Additional notes may be found in Herbig (1962). Her1962
HER 11 AD: Additional notes may be found in Herbig (1962). Her1962
04320-6939 OGL 197 LMC157.5.2454 + LMC157.5.2477 Pli2012
04322+3630 AG 80 ALI 293.
04322+1820 KSA 107 Primary is variable star V827 Tau.
04322+1757 MSR 1 HBC 397 = V1075 Tau. Msr2005
04323+2423 GHE 10 Aka V928 Tau.
04323+2422 KON 4 Estimated masses 0.07 and 0.06 Msun. Primary spectral type M6.5 Kon2007b
04323-6918 OGL 198 LMC156.7.3411 + LMC156.7.3620 Pli2012
04324+0128 HDO 307 Aka BAL 1273. Hei1983a
04325+2420 HAT 7 A and B are FY Tau and FZ Tau.
Additional notes may be found in Herbig (1962). Her1962
04325+2044 RED 6 1996.0902 RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al. (1981). Luy1981
Candidate Hyades member; Reid considers possible binary. Red1997
04325+1732 LEI 3 Aa,Ab: GG Tau.
Tamazian (2002) solution includes mass determination based on an Tam2002
estimated distance.
Aa,Ab: Kohler (2011) derives orbits both coplanar and not coplanar
with the disk; only his "most plausible" orbit is tabulated in the
orbit catalog. Elements are as follows: P = 403 +67/-32 y, a = 0".429,
i = 132.5 +1.0/-2.5 deg, Omega = 131 +13/-8 deg, e = 0.44 +0.02/-0.03,
T = 2463400 +1470/-5420, omega = 19 +9/-10. Koh2011
CHN 5 AB: formerly known as LEI 3.
DIF 1 Ab1,Ab2: Di Folco et al. estimate spectral types for Ab1 and Ab2 of M2V
and M3.5V, respectively. Assuming the close pair is coplanar with the
outer diskof the system, the stars were separated by 5.1au in Dec 2012. DiF2014
04326+2628 GIC 48 LDS1176 = G008-040/G039-021.
NLTT 13455/13456 Chm2004
HD 283702. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
04326-0313 H 6 64 H VI 64. Probably a variable of Delta Scuti type,
DZ Eri. B is BD-03@810.
04327+2553 GHE 11 Aa,Ab: Measure of 1990.77 made by triangulation of multiple measures
and was in a red filter. Smn1992
JOY 3 AB: A RW Aur-type variable, UZ Tau.
Measure of 1990.77 made by triangulation of multiple measures and was
in a red filter. Smn1992
AB: Additional notes may be found in Herbig (1962). Her1962
04327+1855 DAE 26 V1203 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04327+1803 SAR 4 HBC 403 = V1076 Tau.
04328+1600 CHR 152 This is probably the spectroscopic system found by Griffin et al. Grf1988
(1988) to have a period in excess of 15 years. Msn1993a
The spectroscopic solution of this 9377-d pair determined by Griffin. Grf2012b
04329+0007 LDS 121 BC: NLTT 13492/13491 = LSPM J0432+0006. Law et al (2008) derive a Law2008
distance of 16.5 +8.2/-2.7 pc and a projected separation of
76.2 +38.7/-11.8 au. Estimated spectral types are M4.5 and M5.5.
04330-3817 BU 747 RZ Cae, Algol-type eclipsing binary, P = 2.486955 d. Zas2011
04331+2410 GHE 13 Ab1,Ab2: Second and third Schaefer et al. (2006) orbits for Elias 12 Sfr2006
Na-Nb include a lunar occultation measure by Simon et al. (1995) Smn1995
Schaefer et al. (2012) derive spectral types, Teff, luminosities, and
masses for the Aa, Ab1, and Ab2 components (assuming a distance of
140pc for M and L) as follows:
Aa: K7 4060K 1.05 +/-0.20 Lsun 1.040+/-0.016 Msun (Mtotal)
Ab1: M2 3560 0.447+/-0.058 0.564+/-0.018
Ab2: M2-M2.5 3560 0.356+/-0.038 0.476+/-0.017 Sfr2012
Aa,Ab: V807 Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
HAT 9 AB: Additional notes may be found in Herbig (1962). Her1962
GHE 12 Ba,Bb: GH Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04331-1208 STF 564 The pair GAL 145 is identical Hei1983a
04331-4646 SKF1205 The pair also show matching radial velocities, but primary is a SB1. TrC2006
04332+2434 SAR 5 HBC 405 = V830 Tau.
04332-6829 OGL 199 LMC155.5.3403 + LMC155.6.576 Pli2012
04333+6847 LDS9172 Old LDS6172.
04333+5921 TOR 7 Formerly known as PAN 4.
04333+5248 MLR 695 Aa,Ab: Also known as HDS 591.
ES 2607 B is BD+52@844.
04333+2505 LDS5190 old LDS6173.
04334+4304 SHJ 44 57 Per. STTA 50 = H 6 99.
04335+7232 HJ 2228 AB: A is a spectroscopic binary.
Also an unresolved 4.194d spectroscopic binary. Mug2017b
LDS1595 AC: Initially merged with AB under mistaken belief was same pair.
04335+1801 STF 559 H N 132. MEv2010
04336+2610 GHE 14 Aa,Ab: IS Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04336+2421 POU 460 AB: Haro 6-22. Both components variable (A: 13.9-15.5, B: 14.1-16.1)
according to Wenzel (1957 Nach. astr. Zentralst. 11,28) Her1962
A is GK Tau. B is GI Tau.
04336-6249 HJ 3670 B is CPD-63@343.
04337+1824 DAE 27 V1323 Tau. Dae2015
04337+1752 CHN 7 Formerly known as LEI 17.
HN Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04338+1451 CIA 51 rho Tau = 86 Tau.
Hipparcos astrometric solution assumes circular orbit (e = omega = 0); HIP1997d
Hyades VA 725 = vB 95. 1.337-year SB according to Abt (1965). AbH1965
04339-0644 BU 881 46 Eri. A is variable EH Eri, P = 3.8d, small amplitude.
04340+1510 CHR 17 This rapidly moving system within the wide binary ADS 3317 is probably Grf1988
the spectroscopic system with P ~13 yr found by Griffin et al. (1988). Msn1993a
New spectroscopic solution determined by Griffin. Grf2012b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.27 +/- 0.34, 1.66, and 0.95 Msun, respectively. Mlk2012
04340-5503 B 2092 alp Dor. Hyad (vB 96).
High mass-sum, illustrative solution only, speckle/spectroscopic orbit
needed, cf. Griffin et al. (1988). Grf1988
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 5.51 +/- 1.51, 4.25, and 2.69 Msun, respectively. Mlk2012
HJ 3668 AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
04342+2612 SMN 14 Measure of 1990.77 made by triangulation of multiple measures and is
in a red filter. Smn1992
04343+1830 SAR 6 HBC 407 = V1077 Tau.
04344+6928 HJ 1145 Aka TDS2898. Skf2016a
04344+1630 OL 107 The ES pair formerly listed at 04350+1631 (= ADS 3313)
is identical to this pair. Hei1980a
04345-6859 OGL 200 LMC156.4.9 + LMC156.4.130 + LMC155.1.775 Pli2012
04345-6958 OGL 201 LMC157.2.3089 + LMC157.2.3113 Pli2012
04346-6948 OGL 202 LMC157.3.2891 + LMC157.3.2890 Pli2012
04346-7015 OGL 203 LMC151.5.4 + LMC151.5.38 + LMC151.6.4891 Pli2012
04348+3206 SEI 49 Neither component seen on POSS plate; may be flaws on AC Potsdam plate
04349-7651 HJ 3691 B is CPD-77@176.
04350-1246 GAL 373 Object #143 in Gallo's original list. Gal1914
04352+1822 SAR 7 TAP 51 = V1078 Tau.
04352-0944 STF 570 B is BD-10@958.
H 3 100. MEv2010
04353+2254 KSA 108 Primary is variable star FF Tau.
04353+2232 HER 23 HAT 11.
04354+1045 RED 7 Identification with GCS2 uncertain.
1996.8130 RHy ID and coordinates from Reid (1992). Red1992
LP ID from Luyten et al. (1981). Luy1981
Candidate Hyades member; Reid considers definite binary. Red1997
04356+2408 HRM 1 AB = DCH 56. IRAS 04325+2402.
04356+1206 TOK 17 Hyades vA 771.
Primary is 1.9d SB2. Estimated period of visual pair 400y. Tok2006
04357+2411 CHN 8 Formerly known as LEI 19.
04357+1953 L 4 First resolved by Lewis in 1902, this system was unconfirmed for GrO1932A
several decades despite numerous attempts, notably those of Aitken
with the 36inch between 1910 and 1922. In the ADS, Aitken concluded A__1932b
"It is very doubtful whether the star is double". The system was
subsequently removed from the WDS, until its resolution by Prieur et
al. over 90 years after its discovery. Pru2002b
04357+1010 CHR 18 Aa,Ab: 88 Tau. A is an Alpha CVn-type variable, and spectroscopic
binary, now resolved by speckle interferometry.
B is BD+09@606.
1997.071: Absolute quadrant determined by triple-correlation
techniques Pru2002b
88 Tau Lane et al. (2007) combine PHASES astrometry with speckle and radial Lne2007
velocity data to derive an orbit for the Aa,Ab components of the
nearby sextuple 88 Tau, as well as the Aa1,Aa2 and Ab1,Ab2 subsystems.
The parallax of the system is determined at 0".01973 +/- 0".00034,
with semimajor axes for Aa,Ab; Aa1,Aa2; and Ab1,Ab2 of 12.17 +/- 0.17,
0.0689 +/- 0.0012, and 0.0997 +/- 0.0021 au, respectively. Other
derived quantities for the four components are as follows:
Star Mass (Msun) M_K (mag) Spec Type
Aa1 2.06 +/- 0.11 0.69 +/- 0.26 A6m
Aa2 1.361 +/- 0.073 2.20 +/- 0.28 F5V
Ab1 1.069 +/- 0.069 2.31 +/- 0.27 G2-3:V
Ab2 1.057 +/- 0.068 2.00 +/- 0.27 G2-3:V
SHJ 45 STTA 52.
AB: H 6 31. MEv2010
04358-6655 OGL 204 LMC152.7.209 + LMC152.7.891 Pli2012
04359+2352 KOH 15 V1324 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04359+2254 LEI 21 Primary is V1025 Tau.
HAT 12 C component is HP Tau.
04359+1631 BU 550 alp Tau = 87 Tau = Aldebaran. A is an unclassified variable.
Mk III Limb-darkened diameter 21.21 mas. MkT1991
Mk III Limb-darkened diameter 21.099 +/- 0.211 mas. MkT2003
STFB 2 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
Incorrectly listed as STFA 2.
STFA 2 AC: H 6 66. MEv2010
STFB 2 AC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
04359-0332 LDS9174 Old LDS6174.
04360-0337 STF 571 AB: H 3 95. MEv2010
04361+5525 HIP 21433 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos
Intermediate Astrometric Data with spectroscopic elements by
Tokovinin et al. (1994). They derived component masses 0.88 and 0.24 Tok1994c
Msun and an estimated semimajor axis of 28.68 mas. Ren2013
04362+0814 A 1840 Observations suggest eccentricity >0.80 and period 150-200y. Mlr1956a
Star C (mag. 9, 6") is probably physical.
04363+5502 RAO 35 Triple, consisting of a 2.6 day spectroscopic binary (Gorynya &
Tokovinin 2014 MNRAS 441, 2316) and the Robo-AO and 2MASS companion at
5".7. The field is crowded and PM(A) is small. Our photometry places B
slightly above the MS. The star is young and active according to
Guillout et al (2009 A&A 504, 829) and we retain B as likely physical. Rbr2015d
04363+4722 S 451 STTA 51. B is BD+47@1012.
04363-0321 BUP 64 nu Eri = 48 Eri. A is a Beta CMa-type variable.
04363-6655 OGL 205 LMC152.7.23 + LMC152.7.88 Pli2012
04364+3413 HU 610 Only elements P, T, and a have been amended by Starikova (1978) from Sta1978c
the orbit of Baize (1961). Baz1961b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.70 +/- 1.07, 2.11, and 0.95 Msun, respectively. Mlk2012
04365-0559 LDS9175 Old LDS6175.
04365-0611 LDS 843 Aka LDS9175.
04366+1930 LDS3597 The primary is a BY Draconis-type variable.
04366+1845 RUC 4 RZ Tau. Spectral type of resolved companion M3-5V or possibly later. Ruc2007
04367+4116 58 Per Wyller orbit rejected from Fourth Orbit Catalog Wye1957
("not confirmed by subsequent observations") Wor1983
04367+4105 STF 563 H 3 65. MEv2010
04367+1155 LDS1181 Hyades vB 210.
NLTT 13608/13606 Chm2004
04367-6733 OGL 206 LMC153.7.3072 + LMC153.7.3092 Pli2012
04368+2708 GIC 49 LDS1180 = G008-044/G039-027 = GJ 171.2AB. A component is the variable
V833 Tau = Melotte 25 301.
NLTT 13601/13599 Chm2004
Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
04368-6205 HJ 3679 A is a long-period variable, R Dor.
04372+3108 KOH 16 V961 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04372+1108 GIC 50 LDS1182 = G083-024/G083-023.
04372-6658 OGL 207 LMC152.7.3126 + LMC152.7.3127 Pli2012
04373+1748 BPM 101 [PM2000] 178584 + [PM2000] 178531. Gvr2010
04373-6853 OGL 208 LMC155.1.4867 + LMC155.1.5999 Pli2012
04373-6905 OGL 209 LMC149.7.8 + LMC149.7.35 + LMC149.5.668 Pli2012
04374+0034 STTA 53 B is BD+00@801.
Pair appears in an appendix list, not part of the discoverer's
regular numbering sequence.
SHY 465. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
04375+1509 CHR 153 1991.9021: Reprocessing of archival speckle data have confirmed this
already strong detection and have shown a change in theta of 15 deg in
2.7 yr. CHR 153 cannot be the 734.2-d spectroscopic system of Griffin Grf2012b
et al. (1988). In the Hyades. Msn1993a
The preliminary orbital solution is clearly in error as the visual Ole2003b
companion was better fit by linear motion and it previously appeared in Hrt2012a
the linear catalog. However, with more observations an orbit solution
was possible. Tok2021b
04376-0228 WAL 32 After analysis of proper motions, radial velocities, etc. conclude
that A (= 51 Eri) and C (= GJ 330) comprise a wide physical binary and
are members of the young bet Pic moving group. Distance is ~30pc and
estimated orbital period is ~60,000y; pair form a very fragile system. Fgl2006
C component is GJ 3305; A and C are members of bet Pic moving group. Zuc2001b
BU 88 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
KAS 1 Ca,Cb: Better known as GJ 3305, this binary is part of the beta Pic
moving group (Zuckerman et al. 2001), and is also bound to 51 Eri in a Zuc2001b
wide orbit (Feigelson et al. 2006) with a projected separation of 66". Fgl2006
The binarity of GJ 3305 was first reported by Kasper et al. (2007), Kas2007b
and has been observed with AstraLux on several occasions. Jnn2012
Ca,Cb: Montet et al (2015) derive a combined spectroscopic/astrometric
orbital solution, yielding masses 0.67 +/- 0.05 and 0.44 +/- 0.05
Msun, luminosities 0.112 +/- 0.007 and 0.043 +/- 0.005 Lsun, and an
age of 37 +/- 9 Gyr. Mtt2015
04379-6701 OGL 210 LMC152.2.1 + LMC152.2.31 Pli2012
04379-6915 OGL 211 LMC149.7.39 + LMC149.7.80 Pli2012
04380-1302 STF 576 B is BD-13@938.
04381+1457 LDS5582 LDS6138.
04382+2813 BEU 6 GJ 3304 = G039-029. Daemgen et al. (2007) derive a distance of 14.5 Dae2007
+/- 3.8 pc, a separation of 11.4 +/- 3.4 au, and a predicted orbital
period of 76 +36/-35 yr. Spectral types are M4.0 +/- 0.5 and M4.5 +/-
0.5; masses are 0.23 +0.10/-0.07 and 0.20 +0.07/-0.05 Msun.
Estimated age 60-300 Myr; masses 0.28 +/- 0.06 and 0.19 +/- 0.05 Msun;
a ~13.4 au. Jnn2014
04382+1603 PAT 12 Aa,An. CPM companion (rho = 140".5) is outside our detection window. Msn1993a
04382+1602 BUP 65 89 Tau.
04382+1231 BUP 66 Hyades vB 104. 90 Tau. A is a spectroscopic binary.
Two CPM companions (rho = 44" and 120") fall outside detection window. Msn1993a
MRN 2 Aa,Ab: Marion et al. (2014) estimate the companion to this Hyades
member as K4V. Assuming a face-on, circular orbit with a semi-major
axis of 11.1 mas (0.52 au), the minimum period would be ~84d. Mrn2014
04382-1315 TOK 660 Resolved using ANDICAM2. PM(A) is small, B is considered physical from
photometry and low crowding Tok2014d
04382-1418 KUI 18 53 Eri = Sceptrum.
04384+2611 ITO 6 AC: Itoh et al. (2008) estimate that if the AC pair is physical, the
H-band magnitude of C suggests a mass of order 1 Mjup. Followup
astrometry and spectroscopy is needed to confirm its companionship. Ito2008b
04385+2656 STF 572 AB: One component is a spectroscopic binary.
Has an orbital solution and while proper motion is close, parallax Izm2019
indicates it is non-physical.
04385+2611 SMN 15 Aka HV Tau.
04385+2611 Measure of 1990.77 made by triangulation of multiple measures
and is in a red filter. Smn1992
04385+1752 BPM 102 [PM2000] 179567 + [PM2000] 179474. Gvr2010
04386-0921 TOK 387 HIP 21265 is an X-ray source and an SB2 according to GCS (only one
observation). It is resolved here at 56mas, which corresponds to a
period of ~5yr. Tok2015c
04387-6822 OGL 212 LMC148.5.112 + LMC148.5.706 Pli2012
04388+2147 JNN 262 G 8-48. Estimated age 300-1000 Myr; masses 0.12 +/- 0.04 and 0.10 +/-
0.03 Msun; a ~21.9 au. Jnn2014
04388-2702 TOK 661 CA: Resolved using ANDICAM2. Tuc-Hor moving group. PM(C) is small,
physical from ptm only. Tok2014d
04388-7015 OGL 213 LMC151.4.44 + LMC151.4.45 Pli2012
04389+1406 HD 29461 Hyades vB 106. This is SB with P ~ 10 yr according to Griffin et al. Grf1988
(1988). Msn1993a
04389+1406 MET 41 This optical companion cannot be 3760d spectroscopic binary of Griffin Grf2012b
04389-1207 HDS 599 Cvetkovic et al. (2014) derive spectral types A1 and F2, masses 2.28
and 1.56 Msun. Dynamical parallax is 15.50 +/- 0.75 mas. Cve2014
04390+2149 LDS1183 NLTT 13673/13674 Chm2004
04391+0752 BUP 67 B is BD+07@680.
04392+2553 TER 1 IRAS 04361+2547.
04393+3331 JNN 263 Estimated age 1000-10000 Myr; masses 0.32 +/- 0.16 and 0.20 +/- 0.10
Msun; a ~2.6 au. Jnn2014
04393+2545 SMN 16 GN Tau.
04393+2221 LKCA 15 Sallum et al. (2015) resolve three planetary companions to LkCa 15.
Companion b has a best-fit orbital semi-major axis 14.7 +/- 2.1 au,
that of companion c is 18.6 +2.5/-2.7 au. Companion d is only seen in
the L' band, so less information can be gleaned. Sll2015b
04393+1555 STFA 11 A: sig 2 Tau = 92 Tau. A is a spectroscopic binary.
B: sig 1 Tau = 91 Tau. B is BD+15@665, SB and occultation binary.
04394-6938 OGL 214 LMC150.4.33 + LMC150.4.139 Pli2012
04395-1141 GAL 374 Object #147 in Gallo's original list. Gal1914
04395-4507 I 1489 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.49 +/- 0.82, 1.60, and 0.79 Msun, respectively. Mlk2012
04396-2115 BU 1236 AC: SHY 467. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
04397+0952 HDS 601 Also a 610d spectroscopic binary. Tok2019b
GIC 51 LDS1184. AB = G083-028/G083-029 = GJ 9162AB.
04397-6722 OGL 215 LMC153.3.3746 + LMC153.3.4025 Pli2012
04399+5305 BU 1043 3 Cam. A is an eclipsing binary of the W UMa-type.
04399+1940 RED 8 1996.0929 RHy ID and coordinates from Reid (1992). Candidate Hyades Red1992
member; Reid considers possible binary. Red1997
04399+1631 BU 1044 Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 of
04404+1631 = CHR 154 were actually of this pair. Those measures have
been included here.
04400+5328 BU 1295 2 Cam.
The high-eccentricity solution for AB by Valbousquet (1980) is Val1980b
questioned by Heintz (1962) on grounds of a mass discrepancy. Hei1962
The equinox-1900 position was incorrectly given as 04320+5310 in
McAlister & Hendry (1982). McA1982d
Argument of periastron flipped for Tok2021b orbit since WDS refers to
fainter star as primary.
STF 566 A is the D component of 04404+5328.
04400+3534 HJ 681 ALI 64.
04400+2556 KON 5 Estimated masses 0.1 and 0.06 Msun. Primary spectral type M5.75 Kon2007b
04403-6924 OGL 216 LMC149.2.6 + LMC149.2.26 Pli2012
04404+5328 D 4 AD: D component is primary of 04400+5328BU 1295AB. AD not physical, so
systems not merged.
04404+1631 CHR 154 Measures made by CHARA/USNO in 1991, 1993, 1995, 1996 and 1998 were
actually of 04399+1631 = BU 1044. Measures X coded here but retained
to maintain original catalog pedigree.
04404-1940 STN 9 54 Eri. A semiregular variable, DM Eri. No very positive observations
as a visual double. Needs speckle.
04404-2935 DAW 81 BC: Rectilinear solution by Hurowitz et al. (2013). USN2013a
04406-4152 HDO 190 AB: alp Cae. A is a Delta Scuti-type variable.
AB: Physical/optical nature undefined. Ehr2010
04407+2519 KON 6 Estimated masses 0.15 and 0.08 Msun. Primary spectral type M5.5 Kon2007b
04407-2812 TOK 209 Resolved with NICI, uncertain measure. Not resolved with speckle. Tok2012a
Direct motion by 16deg since first resolution at Gemini on 2011.80;
estimated period is 15 yr. Tok2013b
04408-3951 RSS 5 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. Rss1996
04408-6741 OGL 217 LMC146.8.31 + LMC146.8.30 Pli2012
04409+0058 STF 583 AB: H 2 81. MEv2010
04410-6935 OGL 218 LMC150.4.7439 + LMC150.4.8170 Pli2012
04413+3242 JNN 264 Estimated age 300-1000 Myr; masses 0.54 +/- 0.04 and 0.40 +/- 0.06
Msun; a ~58.9 au. Jnn2014
04414+2715 KOH 20 V1328 Tau. Dae2015
04413+2054 LWR 5 V834 Tau
04415-4328 Anon EQ 0439-4333. ID as EQ 0439-4333 is uncertain, as it was based on a
Simbad search using epoch-1950 coordinates 043955-433318 from White et Whi1991
al. (1991).
04416-4302 WHI 6 Possibly resolved. Whi1991
04417+2302 KSA 29 Primary is of spectral type M8.5 and shows evidence of a circumstellar
disk and active accretion. The Ab companion is estimated as type
M9.5-L0, mass 5-10 Mjup. Todorov et al. (2010) also resolved the B
component into a 0.23" pair. Tod2010
04418+2658 KOH 21 Member of Taurus-Auriga molecular cloud. Dae2015
04419-6714 OGL 219 LMC146.5.3639 + LMC146.5.3827 Pli2012
04421+2523 LEI 24 V955 Tau.
GHE 15 The measures and component designations of the Ba and Ca pair were
assigned incorrectly and were correctly re-assigned 5/22/02. The
designations LEI 24Ba <---> GHE 15Ca were flipped and the
designation LEI 25Aa became LEI 24Aa.
04422+3731 STF 577 CfA: SB? Not clear if it is A or B. Tok2014d
04422+2257 MCA 16 Aa,Ab: tau Tau = 94 Tau. Occultation binary and short-period SB.
Hough suspected duplicity due to a slow occultation. Finally resolved
by McAlister in 1980. McA1983
1983.9337, 1983.9391: Interferometric observations are incompatible Jef1963
with the large delta m reported by Jeffers et al. (1963). Bnu1984
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 12.44 +/- 4.14, 7.48, and 6.92 Msun, respectively. Mlk2012
Uniform disk diameter 0.220 +/- 0.016 mas,
Limb darkened diameter 0.226 +/- 0.016 mas,
Teff = 18500 +/- 800 K based on LDD.
Radius is 2.27 +/- 0.20 \rsun. CIA2019a
S 455 STTA 54 = H 6 7.
04422+0259 A 2424 Position angles uncertain.
04423+8103 LDS1596 NLTT 13589/13587 Chm2004
04423+0932 TOB 369 Aka GWP 610.
04423-2943 LDS 126 NLTT 13802/13804 Chm2004
04423-6657 OGL 220 LMC145.7.3953 + LMC145.7.4003 Pli2012
04426+2516 KSA 111 Primary is variable star DP Tau.
04427-2147 LDS3608 NLTT 13805/13809 Chm2004
04428-7030 OGL 221 LMC144.7.6 + LMC144.7.441 Pli2012
04429+1843 LDS2266 BC: HJL1038. HJL1986
RV(A)=+14.5, not Hyades member! On Lick RV program. B is SB2, HJL2012b
P=56.445d (Halbwachs et al. 2012) Tok2014d
04430+5712 A 1014 Only elements P, T, and a have been amended by Starikova (1978) from Sta1978c
the orbit of Baize (1958). Baz1958
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.27 +/- 0.48, 2.37, and 1.10 Msun, respectively. Mlk2012
04431+3356 HJ 348 Also known as STF 580.
04431-0725 A 476 KP Eri, Algol-type eclipsing binary, P = 7.447126 d. Zas2011
04431-6844 OGL 222 LMC148.2.7773 + LMC148.2.7774 + LMC148.2.7791 Pli2012
04432-5436 TOK 87 HIP 21960.
04432-6723 OGL 223 LMC146.3.22 + LMC146.3.117 Pli2012
04433+5931 A 1013 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 5.20 +/- 2.40, 3.42, and 1.82 Msun, respectively. Mlk2012
04434+1558 BPM 103 [PM2000] 183754 + [PM2000] 183745. Gvr2010
04436-0848 STF 590 55 Eri. B is a Delta Scuti-type variable, DW Eri., BD-09@969. Spectral
type F4IIIpSr. Both components are spectroscopic binaries.
H 3 99. MEv2010
04441+1739 LDS2268 NLTT 13828/13829.
04441+0205 HL 1 This is a measure of HL 04441+0204 and A 3006 04440+0204
04442-6959 OGL 224 LMC143.8.7618 + LMC143.8.8368 Pli2012
04443+2017 KOH 22 V1205 Tau. Dae2015
04444+1952 KOH 23 V1333 Tau. Dae2015
04444+1109 BUP 68 Hyades vB 111. A may be variable. Two CPM companions with rho = 74".7
and rho = 10".0, both outside our detection window. Msn1993a
04445+3953 COU1524 Primary is eclipsing binary V592 Per (period 0.71572 day). Zas2010
04448-6946 OGL 225 LMC143.6.9637 + LMC143.6.10050 Pli2012
04449+2717 KOH 24 Member of Taurus-Auriga molecular cloud. Dae2015
04449+1757 LDS2271 LDS5590.
04450+1605 BPM 104 [PM2000] 185037 + [PM2000] 185149. Gvr2010
04453-6943 OGL 226 LMC143.6.9561 + LMC143.6.9815 Pli2012
04454+2955 NI 12 BVD 47.
04454+2421 POU 477 Also known as GRV 215.
04454-5949 FIN 89 A is the Mira-type variable, T Dor.
04454-7006 OGL 227 LMC143.8.7703 + LMC143.8.7822 Pli2012
04455-0512 HJ 27 B is BD-05@1021.
04455-2226 DON 77 CD-22@1801.
04455-7018 OGL 228 LMC144.3.38 + LMC144.3.177 Pli2012
04458+3515 ES 2410 ALI 65.
04459+1911 AG 311 B is BD+18@714.
04460+1616 BPM 105 [PM2000] 185978 + [PM2000] 185928. Gvr2010
04460+1142 BUP 69 A is possibly a spectroscopic binary.
04464+4221 COU2031 1985.740: The separation of this partially resolved pair was
calculated under the assumption of zero or otherwise known magnitude
difference. Tok1985
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.53 +/- 0.35, 2.85, and 1.05 Msun, respectively. Mlk2012
Combined spectroscopic/interferometric orbit. Resulting masses are
1.75 +/- 0.08 and 1.32 +/- 0.08 Msun. Spectral types are estimated as
G3IV and F6V. Doc2014i
04465+1528 HD 30246 Hyades vB 142. Grf1988
Noted as a SB in Griffin et al. (1988). Msn1993a
04465+1528 MET 42 This optical companion cannot be 989.8-d SB of Griffin. Grf2012b
04466+4002 BRT2206 ALI 1040.
04468+1745 PAT 15 This pair is noted as a slow spectroscopic binary in Griffin et al. Grf1988
(1988). Msn1993a
04468+1744 LDS1187 LDS5601.
04468+0901 PAT 16 This pair is a spectroscopic binary with P ~ 7 yr according to Griffin Grf1988
et al. (1988). Msn1993a
Hyades. The 0".1 pair PAT 16 was not resolved with speckle; its
estimated period is 7 yr. Tok2012a
The spectroscopic solution of this 2446-d pair determined by Griffin. Grf2012b
04468-2618 VIG 6 The B component appears to be a faint background star. Vig2012
04469+1700 DAE 35 DQ Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04469-1117 JNN 28 2MASS J04465175-1116476 has a companion that has not yet been tested
for common proper motion. Since the brightness and color match
expectations, the system counts as an unconfirmed binary. Jnn2012
04469-4630 LDS9177 Old LDS6177.
04469-6036 GAL 6 AL Dor.
Ma,Mb = 1.1029 +/- 0.0004, 1.1018 +/- 0.0005 \msun, GaA2019
orbital parallax = 15.200 +/- 0.056 mas.
TOK 388 First resolution of HIP 22229 at 0".043, dI=1.2. The measure is
uncertain, but the elongation is confirmed with 2-ms exposure and is
not seen in other observed stars, so it is not caused by vibration.
This is a triple system containing an eclipsing binary AL Dor
(Algol-type) with an eccentric orbit (Bulut & Demirkan, 2007 MNRAS,
378, 179). The separation implies an orbital period of the outer
system ~5yr Tok2015c
04470-6954 OGL 229 LMC143.2.264 + LMC143.2.1526 Pli2012
04472+2027 KU 85 Also known as STF 593.
04472+1332 LDS1188 LDS5603.
04472-1715 ARG 11 B is BD-17@951, spectrum G2/3V.
04476+1816 PAT 17 This pair is a spectroscopic binary with P >5 yr according to Griffin Grf1988
et al. (1988). Msn1993a
The spectroscopic solution of this 4822-d pair determined by Griffin. Grf2012b
04476-0534 GRE 1 IRAS 04451-0539 = PDS 11. Gre1992
04477+4014 A 1545 Primary is V593 Per, a Beta Lyr type eclipsing binary, P = 3.2437d. Zas2012
04477-6945 OGL 230 LMC143.3.10488 + LMC143.3.11560 Pli2012
04478+3643 GAA 2 AW Per. This Cepheid is an SB with an orbital period of ~40 yr. First
discovered by Miller & Preston (1964 PASP 76, 47), it took several
years to derive the first orbit from radial velocity data (Evans 1989
AJ 97, 1737). It is likely that this companion is itself a binary, as
argued by Evans and by Evans et al. (2000 AJ 120, 407), because the
magnitude difference between the Cepheid and its companion is not
consistent with equal masses and predictions from evolutionary tracks.
Unfortunately, Gallenne et al. (2015) note they did not have enough
angular resolution and sensitivity to detect this third companion. The
properties of the brightest companion were studied based on IUE
spectra by Evans (1994 ApJ 436, 273; 1995 ApJ 445, 393), who found its
spectral type to be B8.3V. This is in agreement with their detection
with a flux ratio f = 1.22 +/- 0.30%, i.e., a spectral type in the
range B6-B9V (using d = 853 pc from a P-L relation and K = 4.63 mag .
for the Cepheid). They estimate the companion mH = 9.6 +/- 0.3 mag .
(using for the Cepheid at theirgiven phase mH = 4.84 +/- 0.01 mag from .
Monson & Pierce (2011 ApJS 193, 12). Massa & Evans (2008 MNRAS 383,
139) also determined the angular separation of the component for
another epoch, which will allow an estimate all the orbital elements,
(see also Gallenne et al. 2013 EAS Pub. Ser. 64, 197). Gallenne et al.
(2015) derived a maximum sensitivity limit at 3sigma of 0.62%, i.e.,
dmH> 5.5 mag, so can therefore exclude any additional components with .
a spectral type earlier than B9V. GaA2015
Spectroscopic binary orbit with P = 13954d determined. Grf2016c
04478+3643 M_Aa = 6.79 +/- 0.85 \msun, M_Ab = 8.79 +/- 0.50 \msun, Uniform
disk diameter = 0.559 +/- 0.051 mas in H Band. Based on Gaia DR3
parallax = 58.9 +/- 5.6 \rsun. CIA2024e
04478+2925 CHN 10 Additional notes may be found in Herbig (1962). Her1962
DS Tau. Young member of Taurus-Auriga molecular cloud. Dae2015
04478-3043 LDS3620 NLTT 13968/13970 Chm2004
04479+2755 KOH 26 V1337 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04479+1902 LDS3619 LDS5604.
04480+5645 BU 1387 4 Cam.
04480+5307 STF 587 H 4 73. MEv2010
04480-4154 TOK 490 AD: D component is the primary of 04490-4128 RST1285.
04481+7810 MLR 464 Also known as TDS 148.
04483-7036 OGL 231 LMC137.8.142 + LMC137.8.140 Pli2012
04485+1056 HJ 684 CD: Also known as STF 601.
04486+1748 STF 598 HJL 62. HJL1986
04486-6648 OGL 232 LMC138.6.5554 + LMC138.6.5870 Pli2012
04487+2106 HD 284787 Hyades vB 115. This pair is a spectroscopic binary SB with P ~ 4 yr Grf1988
according to Griffin et al. (1988). Msn1993a
04487-6830 OGL 233 LMC141.4.9 + LMC141.4.22 Pli2012
04488+5308 STF 586 Same position, and in field of, STF 587.
04488-6124 JSP 60 AC, 180deg, 8" 14th mag noted. Hln1966
04488-6902 OGL 234 LMC142.4.13828 + LMC142.4.14777 Pli2012
04489-6951 OGL 235 LMC136.7.1220 + LMC136.7.2869 Pli2012
04491+1408 BPM 106 [PM2000] 189268 + [PM2000] 189301. Gvr2010
04491+0513 STTA 55 B is BD+04@755.
04492+2448 HD 283882 Hyades vB 117. The 11.93-day SB of Griffin & Gunn (1978) is outside Grf1978b
our detection window. Msn1993a
CIA 61 Aa,Ab : M_Aa = 0.8252+/- 0.0029\msun, M_Ab = 0.7816 +/- 0.0025 \msun,
pi_orb = 20.174 +/- 0.072 mas, A_dia = 0.134 mas, B_dia = 0.127 mas. CIA2024d
04492-3505 TOK 210 The companion is close to the detection limit, but it is considered to
be real. The measurement is uncertain. Tok2012a
Retrograde motion by 5deg since resolution on 2011.78; period is about
20y. Measurements are uncertain because of large dm. The "blue" color
of the companion is caused by measurement error. Tok2013b
04492-6736 OGL 236 LMC139.2.2 + LMC139.2.1 Pli2012
04492-6901 OGL 237 LMC142.4.13837 + LMC142.4.14005 Pli2012
04493+3235 CHR 19 A spectroscopic binary with P = 7.05d.
Fekel et al. (2013) derive a new spectrosopic orbit with P=7.051d and
e (adopted) = 0.0. Estimated masses are 1.95 and 1.2 Msun. Differences
between early DAO and more recent data suggest the possibility of a
3rd component in the system. It in uncertain whether this corresponds
to the never-confirmed speckle companion, however. Fek2013a
04493+2934 RAS 18 Magnetic star; primary is A0 silicon star. Companions A8-F0. Ras2014
LSC 31. V473 Tau.
04494+4828 JNN 265 G 81-34. Estimated age 30-300 Myr; masses 0.27 +/- 0.14 and 0.18 +/-
0.09 Msun; a ~13.5 au. Jnn2014
04497+1554 HJ 3261 96 Tau. BU 551A,BC.
04498+0658 STT 560 pi 3 Ori = 1 Ori = Tabit. Obviously an optical pair. A spectroscopic
binary and possibly a variable of Delta Scuti type.
CHARA Array Limb-darkened diameter 1.526 +/- 0.004 mas, CIA2012e
R = 1.323 +/- 0.004 \rsun, L = 2.822 +/-0.030 \lsun,
Teff = 6516 +/- 19 K, M = 1.283 +/- 0.006 \msun,
Age = 1.3 +/- 0.2 Gyr.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
04499+2230 LDS9178 Old LDS6178. G085-017. See Allen et al. (2000) for information on AlC2000
metallicity, age, galactic orbital parameters, etc.
NLTT 14005/13996 Chm2004
04500+2230 KOH 27 V1341 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04501+6632 STF 584 May be H 2 92. Bu_1906
04501-6635 OGL 238 LMC138.4.30 + LMC138.4.63 Pli2012
04502-0413 SLW 172 GWP 619. Tob2012b
04502-3113 B 1474 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.59 +/- 1.09, 1.93, and 0.91 Msun, respectively. Mlk2012
04503+0657 H 6 83 H VI 83.
04503-4119 HJ 3697 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
04503-6649 OGL 239 LMC138.3.160 + LMC138.3.161 + LMC138.3.468 Pli2012
04504+1712 HD 30676 Hyades vB 119 Grf1988
This pair is noted as a SB in Griffin et al. (1988). Msn1993a
04504+1712 CIA 64 M_A = 1.262 +/- 0.042 \msun, M_B = 0.822 +/- 0.016 \msun,
pi_orb = 23.16 +/- 0.22 mas, A_dia = 0.156 mas, B_dia = 0.126 mas. CIA2024d
04505+0103 A 2622 A premature orbit has been computed.
04505-3834 GC 5916 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
04506+1505 CHR 20 Hyad (vB 120). Preliminary circular orbit, speckle/spectroscopic
orbit needed, cf. Griffin et al. (1988). Grf1988
1991.9023: This may be the spectroscopic system found by Griffin et
al., but more observations are needed to determine the orbital motion. Msn1993a
New spectroscopic solution determined by Griffin. Grf2012b
This is a Hyades binary for which Griffin (2012) published an SB2 Grf2012b
orbit. We combined his RVs with the speckle data, resulting in a very
accurate period. The combined orbit corresponds to a mass sum of 2.1
Msun and an orbital parallax of 22mas, in good agreement with the HIP2
parallax of 23.69 +/- 0.87mas. Tok2015c
Orbital parallax is 21.30 +/- 0.75 mas. Mass of the primary is
1.129 +/- 0.169 \msun. Mass of the secondary is 1.090 +/- 0.160 \msun. Doc2018h
M1 = 1.065 +/- 0.018 \msun, M2 = 1.008 +/- 0.016 \msun,
R1 = 0.968 +/- 0.012 \rsun, R2 = 0.878 +/- 0.013 \rsun,
Teff1 = 5656 +/- 56 K, Teff2 = 5489 +/- 60 K,
orbital parallax = 21.86 +/- 0.15 mas. Trr2024
04506-6711 OGL 240 LMC139.4.89 + LMC139.4.1334 Pli2012
04507-4540 HJ 3699 old LDS6179.
04508+1613 HD 30738 Hyades vB 121
The 5.751-day SB of Griffin & Gunn (1978) is outside our detection Grf1978b
window. Msn1993a
04508-4013 I 1492 Variable, Y Cae.
04509+3746 TOK 249 Cmp? Crowded field (N*=81), small PM, hence B can be optical. Tok2014d
04509-5328 DUN 18 iot Pic
SHY 172 AC: HIP 22531 + HIP 22562.
SHY 173 BC: HIP 22534 + HIP 22562.
In addition to the three visual components, which are physical, the A Tok2020h
component has two spectroscopic components with periods of 1.6d and
1003d. The B component also has a spectroscopic component with a period
of 208d making this a physical sextuple. The AB visual pair has an
estimated period of 6k yr and the wide AB,C pair has an estimated
period of 600k years.
04511-2731 TOK 88 HIP 22538. The original Hipparcos gives parallax 13.9 mas. A is X-ray
source 1RXS J045103.5-273115. Tok2011a
04512+1104 BU 883 Hyad (vB 122).
Mass-sum calls for sp subsystem, but RV-ampl <1km/s according to
Griffin et al. (1988). Grf1988
AO photometric analysis by ten Brummelaar et al. (2000) includes mass
determination. TtB2000
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.58 +/- 0.49, 2.36, and 2.24 Msun, respectively. Mlk2012
Argument of periastron flipped for Sod1999 orbit since WDS refers to
fainter star as primary.
AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
AB,C: Rectilinear solution by Hurowitz et al. (2013). USN2013a
04512-2213 BRT1378 CD-22@1851.
04512-6843 OGL 241 LMC134.7.16981 + LMC134.7.17012 Pli2012
04513-3040 BRT2856 A likely plate flaw. Grv2021b
04513-6804 FIN 362 Only one observation, with many negative results. Duplicity
questionable. Needs speckle.
04514+1850 BUP 70 97 Tau = LDS1190. A is a Delta Scuti-type variable, V480 Tau.
B is BD+18@742.
04515+5550 LDS5615 relative motion of AB is 0.1"/yr, too fast. optical? Tok2014d
04515-3454 FIN 320 Appears to have completed a revolution if the quadrants are correct.
Period about 40y.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 4.50 +/- 1.29, 3.59, and 2.19 Msun, respectively. Mlk2012
Docobo & Andrade (2013) derive a dynamical parallax of 13.78 +/- 0.41
mas and component masses 1.85 +/- 0.21 and 1.58 +/- 0.18 Msun. See
paper for extensive notes on this system. Doc2013d
04515-6653 OGL 242 LMC138.3.7274 + LMC138.3.7555 Pli2012
04515-6933 OGL 243 LMC136.5.13108 + LMC136.5.13830 Pli2012
04516-6841 OGL 244 LMC134.7.20843 + LMC134.7.21738 Pli2012
04518+3047 JOY 4 A is the RW Aur-type variable, UY Aur. Her1962
Hioki et al. (2007) calculate a period of 1640 +/- 90 yr and a total Hio2007
mass of 1.73 +/- 0.29 Msun.
04518+1339 BU 552 Hyad (vB 124). Wor1963a
The primary is 143d SB (Griffin et al. 1985). Grf1985b
The spectroscopic system of Griffin et al. would be too close for us
to resolve by speckle interferometry. Msn1993a
A: Ren & Fu (2013) calculated an astrometric orbit, combining
Hipparcos Intermediate Astrometric Data with spectroscopic elements by
Turner et al. (1986). They derived component masses 1.42 and 0.55 Msun TrD1986
and an estimated semimajor axis of 15.67 mas. Ren2013
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.67 +/- 1.47, 2.30, and 1.00 Msun, respectively. Mlk2012
A faint component (about mag. 13, 45") is unobserved since 1906; its
physical nature is unknown.
04519-3414 BVD 48 AC: SHY 470. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
04519-6058 JSP 62 CD-61@974.
04519-6635 OGL 245 LMC138.4.6967 + LMC138.4.6968 Pli2012
04521-6706 OGL 246 LMC138.1.8041 + LMC138.1.8261 Pli2012
04525-3631 LDS9180 Old LDS6180.
04526+4302 ES 1526 BC: BRT 111
04526-2646 LDS3625 NLTT 14126/14125 Chm2004
04527-2546 TOK 662 With plx(A), B is on the MS, likely physical. Tok2014d
04527-6936 OGL 247 LMC136.4.307 + LMC136.4.140 Pli2012
04527-7043 OGL 248 LMC137.1.262 + LMC137.1.650 Pli2012
04531-0117 S 457 B is BD-01@743.
04531-0853 BRT 369 A likely plate flaw. Grv2021b
04533+1401 BPM 107 [PM2000] 194282 + [PM2000] 194455. Gvr2010
04534-0925 RST4256 BRT 2834.
04535-5551 LDS 131 See note to 05287-6527 SHY 27AD.
04537-4539 GRV1249 Both A and B have approximately the same radial velocity. Grv2019b
04538-6831 OGL 249 LMC134.3.20577 + LMC134.3.20575 Pli2012
04540-6943 OGL 250 LMC136.3.223 + LMC136.3.524 Pli2012
04540-7022 OGL 251 LMC137.3.14145 + LMC137.3.18362 Pli2012
04541+8125 MLR 490 Also known as TDS 152.
04541+6621 alp Cam Fullerton (1990) presents high quality profiles that indicate the Ful1990
presence of line profile variations; his associated radial velocity
measurements do not confirm any of the periods suggested by Zeinalov &
Musaev (1986 SvAL 12, 125) and Musaev & Snezhko (1988 SvAL 14, 68). Msn1998a
04542+4935 STF 603 AB: H N 77. MEv2010
04543+0722 STF 612 HD 31208. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
AB: HJL 64. HJL1986
04544-6720 OGL 252 LMC132.6.11391 + LMC132.6.12002 Pli2012
04545-0314 RST5501 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.79 +/- 1.45, 3.77, and 1.20 Msun, respectively. Mlk2012
04547+1221 TOK 251 A is exoplanet host, P=466d. RV(A)=+12.1, not Hyades Tok2014d
04547-0257 J 1348 GCB 7. BRT 370.
04548+1126 MCA 17 6 Ori.
04549+1009 ENG 19 7 Ori = pi 1 Ori. B is BD+09@682.
04549+0836 STT 90 V1834 Ori, Algol-type eclipsing binary, P = 1.51058 d. Zas2011
04549-6934 OGL 253 LMC136.4.18656 + LMC136.4.18660 Pli2012
04550+3411 HJ 351 AB: Rectilinear solution by Friedman et al. (2011). USN2011a
04551+5516 BU 1187 5 Cam.
04551+3535 MLB 923 Not found by Heintz at IDS position. Hei1985a
04551-6718 OGL 254 LMC132.4.88 + LMC132.4.1271 Pli2012
04552+1827 DAE 39 V1349 Tau. Dae2015
04552-6656 OGL 255 LMC131.7.14509 + LMC131.7.14673 Pli2012
04552-6908 OGL 256 LMC135.3.30074 + LMC135.3.30071 Pli2012
04552-7923 HJ 3733 B is CPD-79@163.
04554-7109 OGL 257 LMC130.7.31 + LMC130.7.349 + LMC130.7.1118 Pli2012
04555+1711 BPM 108 [PM2000] 197155 + [PM2000] 197180. Gvr2010
04556+3018 MSR 3 HBC 426 = V396 Aur. Msr2005
04556+1653 HJ 3263 Rectilinear solutions by Cvetkovic (2015) Cve2015b
and Cvetkovic et al. (2016). Cve2016
04557+1742 DAE 40 V1350 Tau. Member of Taurus-Auriga molecular cloud. Dae2015
04557-6637 OGL 258 LMC131.4.8 + LMC131.4.7 Pli2012
04558+3033 BNS 1 HBC 78 = MWC 93 = AB Aur
04558-3100 LDS3628 NLTT 14212/14213 Chm2004
04558-6741 OGL 259 LMC132.1.137 + LMC132.1.297 Pli2012
04558-7056 OGL 260 LMC130.6.29 + LMC130.6.186 Pli2012
04559+0440 LDS9181 Old LDS6181.
EGN 4 Aa,Ab pair bound. Ab component is likely an early M dwarf with mass
0.43 +/- 0.02 Msun Egn2007
Aa,Ab: A is on Keck program, RV var. Tok2014d
04560+3021 SFN 1 Aa,Ab: Steffen (2000, 2001) combined solutions each yield values for Sfn2000
the masses, as well as an orbital parallax. Sfn2001
Simon et al. (2013) derive masses 0.86 +/- 0.11 and 0.55 +/- 0.05 Msun
and distance 187.7 +/- 3.9 pc for this pre-MS binary. Smn2013
KSA 31 HBC 427 = V397 Aur. Msr2005
04560-6938 OGL 261 LMC128.5.315 + LMC128.5.772 Pli2012
04560-7040 OGL 262 LMC129.8.308 + LMC129.8.309 Pli2012
04561-7116 OGL 263 LMC130.8.10926 + LMC130.8.11364 Pli2012
04562+2554 GIC 52 G039-042/G039-041.
NLTT 14180/14179 Chm2004
04563+5206 STF 608 AB,C: HJL 65. HJL1986
04563+2415 LDS6148 Also known as GRV 220.
04564+1331 BU 553 omi 2 Ori = 9 Ori
04564-0510 SHJ 48 62 Eri. B is BD-05@1093.
AB: H 6 106. MEv2010
04566+0422 TOB9004 Measured as BAL2622 but actually an anonymous pair added here. Tob2012c
04566-6629 DON 89 Variable.
04566-7027 OGL 264 LMC129.7.22 + LMC129.7.188 Pli2012
04567+3917 HU 1091 V560 Aur, Algol-type eclipsing binary, P = 1.528311 d. Zas2011
04567-7106 OGL 265 LMC130.7.12419 + LMC130.7.12474 Pli2012
04568+1825 BPM 109 [PM2000] 199012 + [PM2000] 199066. Gvr2010
04569-6721 OGL 266 LMC132.3.14233 + LMC132.3.14300 Pli2012
04570+1716 BPMA 9 [PM2000] 199271 + [PM2000] 199591. Gvr2010
04570+1517 MET 4 Metchev & Hillenbrand say the C component is probably optical, based
on proximity. Met2004b
04572+3838 ES 2338 ALI 780.
04573+5345 D 5 7 Cam. A premature orbit has been computed for AB. The primary is SB1,
P = 3.884 d (Lucy & Sweeney). Lcy1971
Drummond linear elements have been modified. Dru2014
STF 610 AB,C: Star C (mag. about 11.3, 26") may be physical.
D 5 AB: Rectilinear solution by Drummond (2014). Dru2014
04573+1524 HEI 38 KOH 36.
Young member of Taurus-Auriga molecular cloud. Dae2015
04573-7055 OGL 267 LMC130.6.14234 + LMC130.6.16118 Pli2012
04574+0100 A 2624 Aa,Ab : Hipparcos identified the pair as a candidate for Hyades HIP1998
membership. However, it is not. Grf1988
Grf2013c
04574+0100 SHY 471 AB: HIP 23044 + HIP 23266. B component = A component of 05003+0100.
04575-2358 LDS3630 NLTT 14263/14262 Chm2004
04576+1356 BPM 110 [PM2000] 200066 + [PM2000] 200068. Gvr2010
04576+0344 BAL2132 A likely plate flaw. Grv2021b
04576-0545 STF 624 B is BD-05@1103.
04576-6950 OGL 268 LMC128.6.11701 + LMC128.6.11986 Pli2012
04578+2357 BU 1045 99 Tau.
04580-2248 I 473 CD-22@1917.
04580-6735 OGL 269 LMC124.7.79 + LMC132.2.17928 Pli2012
04581+0141 STF 622 A,BC: H 1 68. MEv2010
04582+8015 OSO 18 GD 288. Not a common proper motion pair, based on comparison with
POSS2 red plates Oso2004
04582+2503 BU 1390 98 Tau. A is a spectroscopic binary.
04582+1423 BPM 111 [PM2000] 201029 + [PM2000] 201109. Gvr2010
04583+0027 FR 11 V1198 Ori.
04584-6739 OGL 270 LMC124.8.20199 + LMC124.8.20752 Pli2012
04585-2749 RST 117 CPD-28@715.
04585-6834 OGL 271 LMC126.6.46772 + LMC126.6.46857 Pli2012
04587-7053 OGL 272 LMC130.3.25 + LMC130.3.4226 Pli2012
04588-7027 OGL 273 LMC129.2.10 + LMC129.7.17168 Pli2012
04589+6435 GNO 1 Distance is estimated at about 10.5 +/- 1.4 pc, giving a projected
component separation of ~5 au. Estimated orbital period ~70 yr, for an
assumed age of 1 Gyr. Spectral types are estimates at T8.5 and T9;
total system mass ~25 Mjup. Gno2011
04590+1433 SHJ 49 STTA 58 = H 5 113. B is BD+14@795. Probably same as BDS 2461, H V 57.
AB: H 5 57. MEv2010
04590-1623 BU 314 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.87 +/- 0.28, 2.66, and 2.36 Msun, respectively. Mlk2012
AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
AB,C: Rectilinear solution by Hurowitz et al. (2013). USN2013a
04591+6322 HU 1090 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 12.31 +/- 4.18, 2.27, and 1.10 Msun, respectively. Mlk2012
04591+1123 BPM 112 [PM2000] 202364 + [PM2000] 202525. Gvr2010
04593+3753 STF 616 ome Aur = 4 Aur
AB: H 2 14. MEv2010
04595-4927 HJ 3715 Primary is VW Pic, a W UMa type eclipsing binary, P = 0.42576d. Zas2012
04595-6802 OGL 274 LMC125.6.10758 + LMC125.6.10639 Pli2012
04595-6958 OGL 275 LMC128.2.17 + LMC128.2.402 Pli2012
04596+3135 HO 222 Hipparcos identified the pair as a candidate for Hyades membership. HIP1998
However, radial velocity classifies this as not a Hyades member. Grf2013c
The colors from Tycho photometry are also not consistent with a Fab2000a
physical pair.
04597+1555 BUP 73 Hyades vB 128
A CPM companion with rho = 106".4 is outside our detection window. Msn1993a
04597-6940 OGL 276 LMC128.4.12 + LMC128.4.92 Pli2012
04598-1016 63 Eri Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Vennes et al. (1998). Ven1998
04599+5327 A 1303 A premature orbit has been computed.
T corrected from 200.74 to 2000.74 by Ruymaekers & Nys (1995) Ruy1995
04599+0031 J 47 Despite having an orbit, an optical pair based on parallax and proper Mlk2022
motion. Izm2019
05001-6217 B 1942 Composite spectrum: G5/8III + F/G.
05001-6953 OGL 277 LMC128.2.32346 + LMC128.2.32381 Pli2012
05002+1811 GIC 53 LDS1198. G083-047/G083-048.
05003+3924 CHR 159 5 Aur.
05004+6925 STF 606 B is BD+69@289.
05005+0506 STT 93 Hyperbolic orbit by Janova (1966). Jnv1966
sigma = areal constant in the true orbit = 0.00576 arcsec^2/yr
q = periastron distance in the true orbit = 0".366
05006+0337 STF 627 B is BD+03@736.
05007-0204 VIG 7 Optical/physical nature of the six faint companions (B-G) is undefined. Vig2012
05007-6856 SKF1044 OGL 278. LMC126.1.9 + LMC126.1.100 Pli2012
05008+3913 STF 621 Same as AG 83.
05008+3811 SEI 52 Secondary not seen on POSS plate; may be either variable star or flaw
on AC Potsdam plate.
05009-7052 OGL 279 LMC130.4.19979 + LMC130.4.21083 Pli2012
05010-0818 BRT 372 A likely plate flaw. Grv2021b
05010-6948 OGL 280 LMC128.3.14335 + LMC128.3.14552 Pli2012
05012+3430 COU1229 Primary is V410 Aur, a W UMa type eclipsing binary, P = 0.36636d. Zas2012
05013+5015 STF 619 Rectilinear solution by Scardia et al. (2017). Sca2017c
Very different proper motion. Despite having an orbit, Kis2009
an optical pair based on parallax. Mlk2022
05015+3733 BRT2207 ALI 523.
05015-7107 OGL 281 LMC122.7.267 + LMC122.7.1784 Pli2012
05016+6105 HU 1093 Primary is possible astrometric pair? Tok2014d
05016-7056 OGL 282 LMC122.6.146 + LMC122.6.918 Pli2012
05017+2640 A 1844 Masses and bolometric magnitudes are derived for the two components Msn1999a
of this system by Maosn et al. (1999), based on assumed spectral types
and available parallaxes.
Visual separations systematically too small.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.83 +/- 0.31, 2.12, and 1.00 Msun, respectively. Mlk2012
S 461 STTA 59 = STFA 12.
BAG 21 Ca,Cb: SB2, P=186.28d Tok2014d
05017+2050 HU 445 Quadrant uncertain, Delta m at least 0.3. B__1963b
Only elements P and T have been amended by Starikova (1977) from the Sta1977a
orbit of Baize (1957). Baz1957a
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 0.15 +/- 0.04, 1.78, and 1.05 Msun, respectively. Mlk2012
05019-7638 RST2368 Rectilinear solution by Hartkopf et al. (2012). Hrt2012a
05020+4349 BU 554 AB: eps Aur = 7 Aur = Almaaz. Strand orbit rejected from Fourth Orbit Str1959
Catalog ("amplitude below noise level") Wor1983
Mk III Limb-darkened diameter 2.17 +/- 0.03 mas. MkT2001
Mk III Limb-darkened diameter 2.096 +/- 0.086 mas. MkT2003
NPOI Limb-darkened diameter 2.28 +/- 0.09 mas. NOI2001b
NPOI Limb-darkened diameter 2.210 +/- 0.012 mas, Sp = A2I, NOI2018
Teff = 7977 +/-292 K, M = 2.16 +/- 0.39 \msun, Age = 0.62 +/- 0.22 Gyr.
eps Aur A is a enigmatic supergiant eclipsing system. Also a spectroscopic and
eclipsing binary Fin1970b
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Heintz & Cantor (1994). Hei1994b
05020+0137 STF 630 A,BC: H 3 52. MEv2010
05021+6910 BU 313 The AB component, BU 313 AB, originally in the BDS and IDS, was
removed by Worley following multiple unresolved observations. The new
Hipparcos binary (AB), is almost certainly not the Burnham AB star,
which was seen at 10", 250 deg, and had a Delta-M of 5.0.
AC: Burnham (BDS) notes 1874 observation made with 6-in telescope but
says no 10" companion was found during subsequent searches with either
the 36-inch or 40-inch. Bu_1906
05022+3116 RUC 5 V402 Aur. Spectral type of resolved companion later than M5V. Ruc2007
05023-1932 LPM 201 NLTT 14407/14408 Chm2004
05023-5605 LDS 135 B is CPD-56@767.
Primary is SB1; Jenkins et al. (2010 A&A 515, 17) estimate P(Aa,Ab)
~6.5y, M2min=55 Mjup. Tok2014d
05023-6821 OGL 283 LMC125.1.12039 + LMC125.1.12040 Pli2012
05024+1628 BPM 113 [PM2000] 207217 + [PM2000] 207230. Gvr2010
05024-6454 GLI 32 B is CPD-65@416.
05025+4105 MKT 6 zet Aur = Saclateni. The first of the zeta Aurigae-type binaries (K4IB
+ B5V). This object was misidentified as rho Aur by McAlister (1978). McA1978c
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Wright (1970). Wri1970
Bennett et al. (1996) orbit is combined solution, using astrometry MkT1996
from the Mark III interferometer, spectroscopy from HST Goddard High
Resolution Spectrograph, and published photometry to determine masses,
radii, etc. Positions of component stars on theoretical H-R diagram
are compared to current evolutionary models.
Errors to individual measures are given as "error ellipses"; these
values are tabulated below, together with filters used. The columns
include date (BY), major and minor axes of the ellipse (in mas),
ellipse orientation (deg), and filter effective wavelengths (nm):
1989.7857 1.63 0.31 98.1 800,550,450
1989.7994 0.56 0.14 86.9 800,550,450
1989.8213 0.58 0.12 84.5 800,550,450
1989.8240 0.73 0.15 78.6 800,550,450
1989.8350 0.50 0.12 85.3 800,550,450
1989.9281 0.48 0.17 96.1 800,550,450
1989.9363 1.24 0.27 86.1 800,550,450
1990.7029 1.14 0.16 104.0 800,550,500
1990.8124 0.56 0.17 97.5 800,550,500
1990.8179 0.69 0.14 91.7 800,550,500
1991.7488 2.00 0.20 111.9 800,550,500
1991.7871 0.65 0.12 92.4 800,550,500
1991.8364 0.32 0.09 94.1 800,550,500
1991.9048 0.21 0.07 86.4 800,550,500
1992.0855 1.31 0.15 90.4 800,550,500
1992.0965 1.50 0.25 73.5 800,550,500
1992.7700 0.63 0.14 99.5 800,550,500
1992.7946 0.65 0.11 98.5 800,550,500
1992.7974 0.44 0.08 104.2 800,550,500
1992.8932 1.82 0.24 111.3 800,550,500
1992.9206 1.39 0.27 99.0 800,550,500
1992.9452 1.23 0.23 101.9 800,550,500
Malkov et al. (2012) derive dynamical and spectroscopic masses
8.40 +/- 3.79 and 10.96 Msun, respectively. Mlk2012
05025-2115 DON 91 Good period, indeterminate a/e/i, more obs needed! Hei1978c
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
05027-3309 HJ 3718 B is CD-33@2076.
05028-4909 RST 120 AB: Physical/optical nature undefined. Primary is eta 1 Pic. Ehr2010
EHR 6 AC: Physical/optical nature undefined. Ehr2010
05028-7020 OGL 284 LMC121.6.34935 + LMC121.6.34941 Pli2012
05029+1433 BPM 114 [PM2000] 208075 + [PM2000] 208110. Gvr2010
05031+4933 BU 315 ID uncertain. Listed as BD+49 1288 in ADS, but no obvious 10" pair at A__1932a
those coordinates. X-coded measures of a 45" pair refer to a wide
companion to BD+49 1288.
05031+2523 MSR 5 HBC 429 = V836 Tau. Msr2005
Young member of Taurus-Auriga molecular cloud. Dae2015
05031+2135 OCC 230 iot Tau.
05031-6944 OGL 285 LMC120.6.45262 + LMC120.6.45347 Pli2012
05033+2125 LAW 13 Ba,Bb: LSPM J0503+2122 = NLTT 14406. Law et al (2008) derive a Law2008
distance of 13.7 +6.5/-2.5 pc and a projected separation of
4.4 +2.3/-0.7 au. Estimated spectral types are M4.5 and M5.5.
Ba,Bb: LP 359-186. Estimated age 1000-10000 Myr; masses 0.38 +/- 0.03
and 0.16 +/- 0.01 Msun; a ~8.3 au. Jnn2014
05033-1722 B 2583 LPM 202. L 736-49.
05034+6027 S 459 bet Cam = 10 Cam. STTA 57 = H 6 36.
05034-7104 OGL 286 LMC122.7.14740 + LMC122.7.14741 Pli2012
05035+1449 BPM 115 [PM2000] 209034 + [PM2000] 208947. Gvr2010
05036+6305 STF 618 LDS 889. STTA 56. D is BD+62@721.
AB: HJL 66. HJL1986
05037-0232 J 307 Reality of BC is in doubt.
05037-6834 OGL 287 LMC118.6.42400 + LMC118.6.42472 Pli2012
05038+1457 BPM 116 [PM2000] 209491 + [PM2000] 209477. Gvr2010
05039-6738 OGL 288 LMC124.1.32825 + LMC124.1.32850 Pli2012
05042-6956 OGL 289 LMC120.7.16863 + LMC120.7.18028 Pli2012
05043+4013 ES 1718 Espin incorrectly identified this pair as BD+40 1144 in 1919, but Es_1919
corrected this to +40 1158 in 1925. Error in transcribing to catalog; Es_1925a
WDS designation originally 05041+4023 = VIG 7, corrected when
matched with 05043+4013TDS3056.
05043+2319 J 1816 POU 523.
05043-6946 OGL 290 LMC120.6.17556 + LMC120.6.17583 Pli2012
05044+6237 HU 1094 Stein measure 1901.3, 289@, 4.2", 9.5-9.9. For this position A__1932a
Hussey finds no such pair. Hu_1905b
05044-3529 JC 9 gam 1 Cae. The secondary is variable (IBVS 2736, 1985).
05044-6706 OGL 291 LMC115.8.111 + LMC115.8.177 Pli2012
05045+1622 BPM 117 [PM2000] 210663 + [PM2000] 210510. Gvr2010
05045-2402 LDS3638 NLTT 14472/14466 Chm2004
05046+5852 STF 625 A,BC: H 2 53. MEv2010
05047+7404 STT 89 Judged single by Hussey, Burnham, and Aitken, and not inserted in ADS.
Rediscovered by Kuiper in 1935 (PASP 47, 230). Obvious in 1938. Baz1942b
05047-0925 GAL 375 Object #161 in Gallo's original list. Gal1914
05047-2017 WHC 2 CPD-20@742.
05049+1520 BPMA 10 [PM2000] 211239 + [PM2000] 211233. Gvr2010
05050-6740 OG