Fourth Catalog of Interferometric Measurements of Binary Stars: Notes
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
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 Che191
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. Shy2001
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 +2860 +390. Proper motion of B +2884 +410.
Premature orbits have been calculated. RV of star A possibly variable.
B component is the BY Dra-type variable CQ And and a SB.
AB: NLTT 919/923 Chm2004
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
PTI Limb-darkened diameter = 1.014 +/- 0.05 mas, PTI2001
R = 0.389 +/- 0.021 \rsun.
VLTI Limb-darkened diameter 1.000 +/- 0.05 mas, LTI2003a
M = 0.414 +/- 0.021 \msun, R = 0.383 +/- 0.02 \rsun,
T = 3698 +/- 95 K.
CHARA Array Limb-darkened diameter of A : 0.988 +/- 0.016 mas CIA2006
R = 0.379 +/- 0.006 \rsun, Teff = 3730 +/- 49 K.
CHARA Array Limb-darkened diameter of A : CIA2012f
R = 0.3874 +/- 0.0023 \rsun, L = 0.02173 +/-0.00021 \lsun,
Teff = 3563 +/- 11 K, M = 0.423 \msun.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. 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. Hrt201
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
00210-7429 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