12001+7039 STT 242 C is BD+71@595 according to ADS, but A and C may be reversed.
12001+4107 LDS5212 LDS6257.
12001-7812 FGL 2 DX Cha. Hen 3-741. Noted as possible binary (separation > 0".040) by
Baines et al. (2006) Bns2006
B, C, D, and E components were resolved by Feigelson et al. (2003) Fgl2003
using Chandra ACIS-I (Advanced CCD Imaging Spectrometer Imager).
Additional wide components G, H, I, J, and K, as well as closer F
companion were resolved by Grady et al (2004) using data from HST/STIS Gry2004
and VLT/NACO. Their theta values for AD and AE appear to be in error;
correct values are perhaps 180-71=109deg and 180-74=106deg?
Grady et al. provided no relative astrometry for the H, I, J, and K
companions. Coarse values were extracted by the cataloguer using
Aladin, based on their Figure 4.
12002+8700 STF1583 STT 238. B is BD+87@100.
12002+3644 STTA114 B is BD+37@2239.
12003-3552 SWR 123 CPM pair Skf2004
12005-0433 EGN 13 Pair bound. B component is likely an M2.5-M4.5 dwarf with mass 0.23
+/- 0.01 Msun. Egn2007
12006+6911 A 1088 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 21.73 +/- 14.44, 4.11, and 1.35 Msun, respectively. Mlk2012
12007+2051 BDK 5 G 121-42 + 2MASS J12003292+2048513. Distance 30 +14/-7 pc for primary,
26 +/- 3 pc for secondary. Estimated age of system 4-5 Gyr. Mass of
secondary estimated at 0.085-0.103 Msun. Fah2010
12007-1027 SCP 1 Schnupp et al. (2010) determine spectral types G8-K0IV and M4V, masses
1.01 and 0.21 +0.03/-0.02 Msun for the two components. Scp2010
12009+0637 pi Vir Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Abt (1965). AbH1965
12015-0023 STF1591 STTA115. B is BD+00@2877.
12016+4731 KZA 24 30' error in WDS designation
12016-6000 WFC 121 JAW 30.
12018-3439 I 215 A premature orbit has been computed. The motion is nearly rectilinear,
but the sizable proper motion proves the physical nature.
The position given by Bespalov is that of HLD 114. Bsp1961
The primary is a double-lined SB, now SB3. Tokovinin et al. (2014)
derived a solution (P=148.14d, e=0.430) and estimated the angular
separation at 13 mas, meaning it should be resolvable by speckle on an
8m telescope. They also revised the orbit of the AB pair. Estimated
masses for Aa, Ab, and B are all similar: 1.15, 1.16, and 1.12 Msun. Tok2015a
12019+0006 STTA116 B is BD+00@2881.
12019-4617 TDS8181 KZ Cen.
12021+4303 FOR 1 67 UMa. A is a Delta Scuti-type variable, DP UMa.
Position of B (+43@2182): 12 02.5 +43 05.
12023-8538 HJ 4490 B is CPD-84@372.
12025+2145 HO 535 Despite the linear solution, proper motion and parallax favor a Grv2020a
physical connection. Long period and/or high eccentricity possible.
12025+1646 OSO 44 LHS2500. Not a common proper motion pair, based on astrometry and
color. Oso2004
12027-1043 SHY 588 AC: HIP 58722 + HIP 58751.
12028+4205 BFR 7 NLTT 29392 + 2MASS J12025009+4204531. Baron et al. (2015) estimate
spectral types M6.0 +/- 0.5 and L0.0 +/- 0.5, distances 33 +2/-16 and
38 +2/-11 pc, masses 0.102-0.133 and 0.074-0.081 Msun. BFr2015
12029+0004 GRV1068 Aka GWP1737.
12029-1908 B 2536 J 1602.
12030-6319 CPO 55 the 1 Cru. A is a spectroscopic binary.
12031+4719 OSO 45 G122-069. Not a common proper motion pair, based on astrometry and
color. Oso2004
12033+2902 LDS1275 AB: NLTT 29413/29414 Chm2004
12036+7932 LDS1746 CBL 553. The pair was long lost, due to a 1deg error in the published
declination, until its rediscovery by Caballero (2012). Cbl2012b
12036-3901 SEE 143 89 Cen.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.31 +/- 1.26, 2.46, and 1.13 Msun, respectively. Mlk2012
12038-4407 HJ 4491 LDS 380. B is CD-43@7447.
SHY 589. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
12039+4257 LDS4174 NLTT 29456/29454 Chm2004
12040+0321 ENG 46 B is BD+04@2568.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
12042+2407 A 682 A close approach took place from about 1960-1975.
12043+2128 STF1596 2 Com. A spectroscopic binary.
H 2 47. MEv2010
12047-0546 RST4492 A is the semiregular variable RX Vir.
12048-4003 RST1641 CPD-39@5381.
12048-6200 DUN 117 B is CPD-61@2935.
12048-6704 DON1095 CD-66@1160.
12049+1729 LEP 49 NI 29.
12049+0910 STF1597 B is BD+09@2580.
12051+1933 GIC 103 LDS5748. G121-052/G121-053.
NLTT 29534/29540 Chm2004
12051-6111 FIN 421 The composite spectrum is unlikely to refer to B.
12054-2636 RST2777 Motion direct, companion optical.
HIP 58962. See Allen et al. (2000) for information on metallicity, AlC2000
LDS 383 age, galactic orbital parameters, etc.
AC: NLTT 29556/29553 Chm2004
12056+6848 STF1599 Djurkovic measured component Ee: 70@, 0.2", 8-8,
but van den Bos found this round in 1958.
12056+5659 A 1358 Aka HDS1700.
12058+5355 CBL 52 Also known as DAL 43.
12058-1853 WNO 54 GJ 9387 + NLTT 29580. CPM pair. Mkr2008
A spectroscopic binary of indeterminate period. Tok2019b
12058-6934 GS Mus Harmanec (1987 Bull. Astron. Inst. Czech. 38, 283) gives a preliminary
orbit with P = 1.74 d and K = 12.4 km/sec. The same period and its
double also appear in photometry (van Genderen et al. 1989 A&A 213,
161), so the radial velocity variations may be related to pulsation
instead of orbital motion. The radial velocity variations are also
discussed by Walborn et al. (1980 PASP 92, 284) and Levato et al. Lev1988
(1988). Msn1998a
12059-4951 HJ 4494 CPD-49@4827.
AB = SWR 124. CPM pair.
Third component 24" N, CPD-49 4827, is not CPM Skf2004
12060+6842 STF3123 AB: Additional notes may be found in Fu et al. (1997). McA1997
Star C (mag. 15, 3") is probably physical.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.51 +/- 0.88, 3.36, and 1.17 Msun, respectively. Mlk2012
12060+2312 WSI 103 MS Com.
12061+7022 A 76 LDS1748. B is BD+71@603.
AB: HJL 163. HJL1986
12061-3258 HJ 4495 HIP 59021. Both components A,B are above the MS by 1.5 mag. Wrong Tok2011a
parallax? The photometric parallax would be ~40 mas. See Holmberg et Nrd2009
al. (2009) for improved distance. Planet host? Nid2002
AB: B is SB2, P=148.26d. A is SB and possible astrometric binary, Tok2010c
although not resolved with NICI (Tokovinin et al. 2010) Tok2014d
12062-2002 B 1714 A rapid binary, angles and period uncertain.
12063+5243 SKF2827 Superposed on west side of galaxy NGC 4102. Pair first noticed by Skf2017f
Steve Gottlieb.
12064-1315 JNN 77 Due to the small separation (~0.42") of the companion detected in the
AstraLux images, it is likely a physical companion, although common
proper motion has not yet been tested. Jnn2012
Bowler et al. (2015) confirm the physical nature and detect orbital
motion. Riaz et al. (2006 AJ 132, 866) identify the pair as
chromospherically active. Bwl2015
12064-4858 BRT 805 CPD-48@4508.
12064-6543 FIN 367 Composite spectrum; G8-K0III+A3.
Aa,Ab: Docobo & Andrade (2013) derive a dynamical parallax of 8.11 +/-
0.42 mas and component masses 2.0 +/- 0.5 and 2.0 +/- 0.1 Msun. See
paper for extensive notes on this system. Doc2013d
12066-3752 HJ 4500 B is CD-37@7665.
12067-6114 JAW 32 Also known as R 187.
12068+4450 FAR 13 BC: Primary is white dwarf WD 1204+450. Far2005b
12069+7008 SKF 237 Aside from the spatially resolved companion, the primary in the 2MASS
J1206557+700749 system is a known spectroscopic binary with a
semi-major axis less than 0.03 au. This is well consistent with our
AstraLux data, where the primary is significantly brighter than the
secondary, despite having about equal spectral type. Hence, the system
is a triple in reality. Jnn2012
12069-6437 HJ 4501 eta Cru. A is a spectroscopic binary.
12071+6905 STF1602 The A component is a spectroscopic triple, P = 3.87d and 6.5y.
12073+4306 HJ 2596 Burnham measured a separation of 224.8" at approximately the same Bu_1913
position angle (239.3) on 1911.22 to NGC 4111 with the 40".
12073-7338 NZO 27 Not found by Heintz at IDS position. Hei1990b
12075+1302 LDS4179 HIP 59126. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 29665/29661 Chm2004
12076-3933 CVN 12 Relative astrometry from Chauvin et al. (2004) was slightly modified Cvn2004
by Chauvin et al. (2005). Cvn2005b
SON 1 AC: C component is a field star. Son2006
12081+5528 STF1603 LDS1278. B is BD+56@1569.
HJL 164. HJL1986
H 4 108. MEv2010
12082+3227 HJ 844 SEI 528. Nsn2017b
12084-5043 JC 2 A: del Cen. Both A and B are Be stars.
B: CD-49 6813. B is the variable V863 Cen.
MLD 1 Aa,Ab: A component was resolved in K-band using the A0-K0-G1 and Mld2008
E0-G0-H0 baselines with VLTI/AMBER. The magnitude difference in K was
2.89 +/- 0.16 mag.
12088-4023 Anon EQ 1206-4006
ID as EQ 1206-4006 uncertain; based on Simbad search using epoch-1950
coordinates 120613-400627 from White et al. (1991). Whi1991
12089+2147 LDS 930 G059-001. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
12091-7847 SHY 592 HIP 59243 + HIP 58490.
12092+1450 TOK 148 HIP 59250.
12093-8459 R 188 Also appears to be R 182.
12094-3409 RST2782 Spectrum: G5/6III/IV.
12094-5127 I 1218 AC = SWR 126. CPM pair Skf2004
12094-6349 HRG 74 Pretty pair. Three distant companions. I__1917a
12095+3838 MET 8 Metchev & Hillenbrand say the pair is probably optical, based on
proximity. Met2004b
12095-1151 STF1604 AB: Mt. Wilson spectral types are G2 and K8. A is a spectroscopic
binary, and slightly variable. Large relative proper motion, coupled
with the fact that the C component is brighter than B, has led to some
confusion in identification of components.
AB: NLTT 29769/29772 Chm2004
HIP 59272. Tok2011a
BC: Rectilinear solution by Friedman et al. (2012). USN2012a
12099-1004 LIM 2 2MASS J12095613-1004008. T dwarf, spectral types estimated by Liu et LiM2010
el. (2010) at T2.0 +/- 0.5 and T7.5 +/- 0.5. Photometric distance 21
+/- 4 pc. Possible masses and effective temperatures are determined
for a range of age estimates.
12101+0526 TOK 282 AC: 12100+0527 TOK 282 and 12101+0526 WOR 22 found to share same
primary; systems merged.
12101-4334 CPO 56 B is CD-42@7455.
12102+1438 BPM 586 [PM2000] 1025354 + [PM2000] 1025384. Gvr2010
12103-0627 HJ 1213 LDS 387.
12105+1649 CHR 135 3 Com.
12108+3953 STF1606 A: Preliminary orbit by van der Wiele (1974) calculated to fit vdW1974
perturbations seen to long-period orbit.
12110+8143 SHJ 136 BDS 6074, STTA117 = STTA118. B is BD+82@357.
12110+1704 BPM 587 [PM2000] 1025639 + [PM2000] 1025679. Gvr2010
12113+3316 HJ 2600 LDS 932.
12113-1958 LDS 390 NLTT 29876/29879 Chm2004
12114+4334 LDS4186 B is BD+44@2169.
A, B, and C are NLTT 29895, 29881, and 29896. B and C are below MS in
(K,V-K) and to the left in (J,J-K). Sub-dwarfs? Tok2014d
12114-1647 S 634 A 211.6d spectroscopic solution for the A component has been found Tok2019g
making this a triple system.
12114-6057 RST4493 Spectral type B5?
12115+5325 STF1608 AB: LDS1284. Mt. Wilson spectral types are K2 and G9.
HJL 165. HJL1986
SHY 233 AC: HIP 59432 + HIP 60121.
12118+2400 LDS6258 AB: SAND 26.
LDS5749 AC: Assignment of LDS6258 and 5749 as AB and AC pairs is uncertain.
12118+2319 GC 16657 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin (1985). Cluster Melotte 111 #AV442. Grf1985a
12119+2552 4 Com Hipparcos astrometric solution adopts some elements from the orbits of HIP1997d
Harper (1930) and Harper (1930). Hrp1930a
Cluster Melotte 111 #AV448. Hrp1930b
Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Harper (1930). Hrp1930a
12120+3850 LDS4188 SLW 693.
12121+2459 LAS 4 Lasgoity (2014) determines that the two components of the pair in the
region of the Coma Berenice star cluster share common proper motion.
He derives spectral types of M3.5V for both components, and estimates
distance, mass, and radius for both stars. Las2014a
12123+5429 VYS 5 LDS5213.
NLTT 29950/29949 Chm2004
12123-0621 LDS4189 NLTT 29948/29967 Chm2004
12125+2509 LAS 5 Lasgoity (2014) determines that the two components of the pair in the
region of the Coma Berenice star cluster share common proper motion.
He derives spectral types of K0V and K3V for the two components, and
estimates distance, mass, and radius for both stars. Las2014a
12125-0305 LPM 416 HIP 59532. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
No companions detected with NACO (Eggenberger et al. 2007). Egn2007
12127+1631 BPM 588 [PM2000] 1026292 + [PM2000] 1026283. Gvr2010
12128-7009 EVS 17 Primary is the Cepheid S Mus. Evs2016a
GAA 13 Aa,Ab : Cepheid with a period of 9.66d. Distance = 858 +/- 17 pc. GaA2019b
M_Aa, M_Ab = 4.44 +/- 0.91, 3.98 +/- 0.21 /msun.
12129-4454 HJ 4507 B is CD-44@7860.
12130+2146 JNN 277 Estimated age 1000-10000 Myr; masses 0.24 +/- 0.08 and 0.12 +/- 0.03
Msun; a ~4.7 au. Jnn2014
12135-4847 CBL 142 AC: Secondary of 12135-4848 CBL 142 found to be primary of 12135-4847
TDS8273; systems merged, with quadrant of CBL 142 flipped 180deg.
12137-1123 JNN 78 LP 734-84.
A companion to 2MASS J12134173-1122405 is detected in the AstraLux
images which has not yet been tested for common proper motion, but the
color and brightness is consistent with the expectation for a
physically bound companion. Jnn2012
12138+4643 A 1849 Rectilinear solution by Rica & Zirm (2012). FMR2012i
12140-4543 RMK 14 A is a spectroscopic binary.
12141+3247 STF1615 B is a spectroscopic binary.
AB: HJL 166. HJL1986
12143+1149 HU 1137 A is a W UMa-type system, AH Vir.
Pribulla & Rucinski (2006) estimate the mass of the contact pair at Pbl2006
1.900 Msun and the minimum mass of the wider component at 0.65 Msun.
12143-0543 HJ 203 A is the Delta Scuti-type variable FG Vir.
12145+0847 STF1616 The declination differences between A and BD+09@2600 have been
measured. See ADS. A__1932a
AC: HJL 167. HJL1986
AB: H 4 114. MEv2010
12148-5547 HJ 4508 B is CPD-55@4937.
SHY 597 AC: HIP 59716 + HIP 59960.
SHY 582 AD: HIP 59716 + HIP 57950.
12151-0715 STF1619 AB: NLTT 30106/30107 Chm2004
C is BD-06@3533.
A rectilinear solution to AB gives a poor fit, due to slight apparent
curvature suggesting very long-period orbital motion.
AB: The AB pair is comprised of a K0V and a K1V star, at a distance of
35.19 +/- 0.74pc. The C component is not a physical companion. Rica et
al. (2017) derive a combined spectroscopic/astrometric orbit of AB,
finding a period of 4800 years and a separation of 345au. The orbit is
perturbed by a circumprimary planet of mass 9.6 Mjup, previously
discovered through radial velocity variations (Mayor et al., 2011 A&A
submitted, arXiv:1109.2497M) FMR2017
12152-1019 BUP 139 Proper motion of A +036 -1016.
A: Hipparcos astrometric solution assumed circular orbit (e = omega HIP1997d
= 0). Spectroscopic solution to this astrometric pair given by Griffin Grf2013a
(2013). Periods match "tolerably well," other common elements less so.
A: Ren & Fu (2013) calculated an astrometric orbit, combining
Hipparcos Intermediate Astrometric Data with spectroscopic elements by
Carney et al. (2001). They derived component masses 1.09 and 0.48 Msun Crn2001
and an estimated semimajor axis of 91.99 mas. Ren2013
12154+5702 BLL 29 69 UMa = del UMa = Megrez. Smyth's quoted separation is difference in Smy1844
RA only.
12158-1733 RBR 5 = gam Crv = Gienah
Found to be a common proper motion companion. Jnn2011b
Intensity Interferometer Limb-darkened diameter 0.75 +/- 0.06 mas. HBr1974
12158-2321 BU 920 Bespalov orbit rejected from Fourth Orbit Catalog Bsp1961
("orbit completely faulty and irreparable") Wor1983
Rica (2012) derived a dynamical parallax of 15.6 mas (compared with FMR2012g
14.37 +/- 0.71 mas from Hipparcos) and a mass sum (using the Hipparcos
parallax) of 3.60 +/- 0.93 Msun.
12159-4417 SWR 128 CPM pair Skf2004
12160+4807 HU 736 Value of Omega inadvertently copied as omega as well by Baize (1993). Baz1993b
12160+0538 STF1621 Additional notes may be found in Baize (1948) and Baz1948b
Couteau (1955). Cou1955a
One component probably has variable RV (Wilson 1967, AJ, 72, 905).
Indeterminate (long) period, useable a^3/P^2. Poor Hipparcos parallax. Sod1999
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
12161+4040 STF1622 2 CVn. A is a spectroscopic binary.
H 3 85. MEv2010
12162+8008 STF1625 B is BD+80@380.
12162+0443 STF1623 HJL 168. HJL1986
12163+4057 FMR 103 BC: Primary of 12166+4058 FMR 103 found to be secondary of LDS4198;
systems merged.
12165+3304 CHR 37 A Delta Scuti-type variable and long-period (1300d) SB.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin (1984). Grf1984a
A spectroscopic orbit with a period of 1300 days was determined by
Christie (1936 ApJ, 83, 433). The many negative results listed here
may be due to a large or variable magnitude difference.
12166+1200 BPM 589 [PM2000] 1027880 + [PM2000] 1027935. Gvr2010
12166-6312 SHY 595 HIP 59865 + HIP 59913.
12169+0258 LDS 935 LDS6259.
12169-2228 LDS 399 NLTT 30204/30203 Chm2004
12171-6542 SHY 596 HIP 59898 + HIP 60183.
12176+3205 LDS1288 Also known as LDS6260.
NLTT 30242/30241 Chm2004
12176+1427 DEA 48 AB + TOK 399Aa,Ab: HIP 59933 has a variable RV according to GCS. The
32mas separation corresponds to an orbital period of ~2yr. However,
the separations in the y and I filters are somewhat discordant;
further confirmation is needed. Tok2015c
12177-6410 JNN 79 The two targets 2MASS J12173945-6409418 and J12174012-6409389 are
physically bound, as shown by common proper motion analysis. However,
this means that one of the targets likely has an error in the Riaz et
al. (2006) spectral type determination, since J12174012-6409389 is Ria2006
classified as M2 but is fainter than J12174012-6409389, which is
classified as M3.5. The fact that J12174012-6409389 is fainter holds
true both in 2MASS and in the AstraLux images. Both components are
resolved as close binaries with AstraLux, so we consider it a strong
candidate for a quadruple system, with J12173945-6409418A as the
primary. Concerning which spectral type determination is incorrect, we
consider that it is more likely that J12174012-6409389 is mis-
classified, as the flux ratio to the close companion is closer to
unity than in the J12174012-6409389 case. We thus set the spectral
type of J12174012-6409389A to M3+/-1, and determine the other spectral
types on the basis of flux ratios. Component Bb is not visible in the
i' data, but becomes visible in z' thanks to the higher Strehl ratio
and intrinsic brightness of the component. A fifth object is visible
in the field, but its color reveals it to be a likely background star. Jnn2012
12179+1627 LIM 4 Liu et al. (2012) derive near-IR spectral types of T9 +/- 0.5 and
Y0 +/- 0.5. At a derived photometric distance of 10.5 +/- 1.7 pc, the
two stars are separated by 8.0 +/- 1.3 au. Various evolutionary models
yield masses of 11.5-14.4 Mjup for the primary, 5.5-8.3 Mjup for the
secondary. LiM2012
Based on resolved IR spectroscopy (0.9-2.5micron), Leggett et al.
(2014) derive spectral types T8.5 and Y0-Y0.5 for this brown dwarf
pair. Assuming an age range 4-8Gyr, they also estimate:
Teff = 550-600 and 450K,
mass = 30+/-5 and 22+/-2 Mjup,
radius = 0.091 +/- 0.004 and 0.096 +/- 0.003 Rsun,
log g = 5.0 +/- 0.1 and 4.8 +/- 0.1 Leg2014
12179-5559 BYV 1 Bailey et al. (2014) derive spectral types F5V and L2.5, and estimate
masses (1.5 +/- 0.10 Msun, 11 +/- 2 Mjup) and luminosities (log L/Lsun
= 0.75 +/- 0.06 and -3.64 +/- 0.08). Distance to the system is 92 +/-
6 pc, age is 13 +/- 2 Myr. ByV2014
12180-1456 RST3783 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
Additional notes may be found in van den Bos (1963). B__1963b
Rectilinear solution by Hurowitz et al. (2014). USN2014a
12182+0515 HJ 2609 C is a nebula, HJ 1178.
12182-0357 STF1627 B is BD-03@3262.
H N 22. MEv2010
12183-6317 HDS1734 SU Cru.
12184-6400 HJ 4512 zet Cru
12187+1148 STF1628 BDS 6116, HJ 1216 same star.
12189-2130 LDS 403 NLTT 30297/30298 Chm2004
12190+0555 GIC 105 G012-032/G012-031.
NLTT 30312/30313 Chm2004
12190+0005 GRV1075 SLW 709.
12190-3318 HJ 4513 B is CD-32@8628.
12191+1036 BPM 590 [PM2000] 1028960 + [PM2000] 1028910. Gvr2010
12192-0319 TOK 283 Secondary appears to be a WD, mass estimated at 0.6 Msun. Mug2014
A is exoplanet host, P=48.05d. Tok2014d
12194+1744 A 2059 Rectilinear solution by Rica & Zirm (2012). FMR2012i
12195+2809 LEP 53 HJL1068. HJL1986
B is SB1, RV=+17.97. RV(A)=-9.80. Tok2014d
12196-4642 SWR 130 CPM pair Skf2004
12199-0040 MCA 37 eta Vir = 15 Vir = Zaniah. A spectroscopic and occultation binary now
resolved by speckle interferometry.
Observed parallax corroborates closely the orbital value given by
Hartkopf et al. (1992). Primary is 72d SB2 (#718 in Batten et al., Hrt1992a
1989). This is not the SB2 because the observed angular separations Bte1989
are much larger than the 12 mas maximum predicted by Halbwachs (1981) HJL1981
from the spectroscopic elements. See discussion in Balega et al. Bag1984b
(1984), who give preliminary orbital elements based entirely on
speckle observations.
1985.2053, 1985.2491: These measures agree well with the preliminary
orbit of Balega et al. (1984), who adopted a period of 13 years. The
orbit proposed by Tokovinin (1984) with P = 9.8 years fails to fit the Tok1984
speckle observations. Bnu1986
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
A new speckle/spectroscopic orbit of the early A type triple system
eta Vir has been determined by Hartkopf et al. (1992). Hrt1992a
Martin et al. (1998) derive component masses 6.009 +/- 2.164 and
0.673 +/- 0.800 Msun. Mig1998
12201+1351 BU 27 A is variable.
12201-6132 TOB 148 Also known as JAW 34.
12202+3754 STF1632 A is a spectroscopic binary.
HJL 169. HJL1986
H N 52. MEv2010
12203+2637 PIN 6 Primary is Melotte 111 AV 1113, a variable star.
12203+0319 BUP 141 16 Vir.
12206-2213 BU 1245 zet Crv. HDO 132. A is a spectroscopic binary.
BU 605 CD: Rectilinear solution by Rica & Zirm (2012). FMR2012i
12207+2703 STF1633 LDS1294.
H N 31. MEv2010
12207+1748 HO 52 11 Com.
CHARA Array Limb-darkened diameter 1.651 +/- 0.016 mas, CIA2014b
R = 15.781 +/- 0.3444 \rsun, T = 4705 +/- 24 K,
L = 109.51 +/- 4.3256 \lsun.
12208+2546 HJ 517 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
12211+4927 FAR 36 Primary is white dwarf WD 1218+497. Far2006
12213-6217 EVS 18 Primary is the Cepheid T Cru. Evs2016a
12214+1223 LDS1295 BC: LDS6261. Erroneously listed as AC pair.
12215+3038 GIC 106 LDS1296. G148-047/G148-048.
NLTT 30450/30451 Chm2004
12215-2413 HWE 26 HDO 133
12216-2716 B 227 Motion direct.
12219+2833 LDS1300 LDS5214.
12221-6731 HDO 215 zet 2 Mus
12222+7315 TOK 26 Visual pair has estimated period 6800y. Tok2006
A is SB2, P=5.415d. AB not confirmed by RoboAO, but B is seen on J and
K frames, seems to be real. Tok2014d
12222+5805 WNC 4 Aka Messier 40. Definitively non-physical. Nug2002
12222-3453 SWR 132 CPM pair Skf2004
12223+3644 DEA 78 NLTT 30510 + 2MASS J12221837+3643485. Baron et al. (2015) estimate
spectral types M3 +/- 1 and L0, distances 45 +47/-23 and 70 +/-10 pc,
masses 0.377-0.431 and 0.074-0.081 Msun. BFr2015
12225+2551 SHJ 143 12 Com. A is a spectroscopic binary. Spectrum composite: G0III-IV+A3V
AC: H 5 121. MEv2010
SMR 57 Aka LAS 6. Lasgoity (2014) determines that the two components of the
pair in the region of the Coma Berenice star cluster share common
proper motion. He derives spectral types of F5V and K5V for the two
components, and estimates distance, mass, and radius for both stars.
The primary is the D component of 12225+2551ARN 6AD. These stars show
very different proper motions than any of the components of 12225+2551,
however, suggesting that ARN 6AD just an optical double linking the
two systems. Las2014a
12225+0518 STF1636 17 Vir. B may be variable.
H 4 50. MEv2010
12226-4920 SEE 153 Aka FAL 38.
12228-0405 BWL 29 AC: 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 13-33. Bwl2015
12229+1725 GIC 107 LDS1301. G059-015AB.
12236-6138 EVS 19 Primary is the Cepheid R Cru. Evs2016a
12240-6206 COO 137 Spectrum A0/2+K1/2III
12241+3827 KZA 30 RA cos(DEC) was in error by 1 arcmin in Kazeza measures. KZA1984
12242+6655 LDS2641 SLW 716.
12242+0558 STT 248 FK Vir
12244-5250 HJ 4520 B is CPD-52@5564.
12247+0225 AG 177 AB: HJL 170. HJL1986
12248-2827 BRT2993 CPD-27@4502.
12249-5807 BSO 8 Spectrum F8/G2IV/V+A.
12250-0414 TOK 400 HIP 60574 is a spectroscopic triple with periods 14d and 22yr (Latham
2012, private communication), also an acceleration binary. We resolved
the outer pair at 0".22 separation, matching the spectroscopic period.
The lines of the visual secondary Ab could potentially be detected in
the spectrum by cross-correlation, leading eventually to a full 3-D
orbit. Tok2015c
12251+6025 GIC 108 LDS1306. G197-057/G197-058.
NLTT 30676/30680 Chm2004
12265+3858 LDS4208 NLTT 30746/30750 Chm2004
12266-6306 DUN 252 alp 1 Cru = Acrux. According to R.G. Aitken, this was discovered by A__1935f
the Jesuit missionary, Father Fontenay, at the Cape of Good Hope, in Fon1733
1685, although the triple was first measured by Dunlop and called Dun1829
DUN 123AB and DUN 122AC. Spectroscopic binary. CPM with HR 4729 and
HR 4731, so there are at least five components in the system.
Hyperbolic orbit by Hopmann (1960). Hop1960b
q = periastron distance in the true orbit = 0".916
Both A and B appear to be spectroscopic binaries with undetermined Bte1967
periods (see Batten 1967). Fin1970b
12268-0536 A 78 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.95 +/- 0.56, 2.88, and 1.25 Msun, respectively. Mlk2012
12269+2816 SMR 58 gam Com.
NPOI Limb-darkened diameter 2.179 +/- 0.057 mas, Sp = K1III, NOI2018
R =12.01 +/- 0.34 \rsun, Teff = 4660 +/- 84 K, L = 61.4 +/- 3.3 \lsun,
M = 1.78 +/- 0.25 \msun, Age = 1.69 +/- 0.56 Gyr.
12269-3728 HJ 4510 B is CD-36@7850. BC: C is CPD-36@5498.
12270-0332 HJ 210 LDS2880.
12272+2701 STF1643 A premature orbit has been computed. Omega and omega in Hopmann (1964) Hop1964b
have been flipped in the orbit catalog to better match observations.
Data appear equally well fit by rectilinear solution - see catalog.
12272-1958 S 637 B is BD-19@3492.
12273-2026 I 513 PTT 23.
12274+0723 STF1644 Optical pair with large relative motion, noted by Muller in his list
of neglected pairs. Cou1953d
12274-2843 B 228 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.91 +/- 3.62, 2.73, and 1.51 Msun, respectively. Mlk2012
12275-7705 RST1668 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.26 +/- 0.25, 1.14, and 1.05 Msun, respectively. Mlk2012
12276+7525 LDS1751 NLTT 30801/30819 Chm2004
12278-1010 HDS1754 Primary is KP Vir, an Algol-type eclipsing binary, P = 2.27720d. Zas2012
12279+3110 LDS1310 LDS5215.
12280-5014 RIZ 3 sig Cen.
12281+4448 STF1645 Alternative spectra F5+K. (Mt. Wilson F8+G0). Statistically the same
parallax within the errors would indicate the components are physical.
12281-6002 HJ 4524 B is CPD-59@4236.
12283-6146 CPO 12 A,BC: A is SB, no orbit. AD can be physical. Moved by 1"in 40y (WDS),
while the PM implied 6" motion. Tok2014d
12284+1223 LDS1311 LIT 23. NLTT 30838/30837. Chm2004
12286+0433 TMA 1 Incorrectly identified as J 1022. Pairs are close, and have similar
position angles (mod 180deg). However, the Jonckheere pair is closer,
and all published measures indicated a small magnitude difference.
This pair has been resolved by 2MASS, so added under that designation.
12286+0431 J 1022 See note to TMA 1.
12287-7129 LDS 410 Proper motion -419 +1091.
12288-1040 RST3792 LDS4217. NLTT 30870 = Ross 948 = GJ 3727. Chm2004
12289+2555 STFA 21 AB: A is an Alpha CVn-type variable, AI Com.
B is a spectroscopic binary.
BU 1080 BC: Faint companion was suspected sf on both nights. B__1963b
12290+4144 BWL 31 AC: 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 3729. Bwl2015
12290+0826 WSI 113 GJ 469. Initally added to WDS as 12297-0320AST 4 with GJ 469.1.
12297-0320 TOK 27 GJ 469.1. Visual pair has estimated period 3400y. Tok2006
A is SB1, P=25.939d Tok2014d
12298-0527 B 2737 LDS5216.
Also known as LHS2567/8. Parallax = 47.68 +/- 1.29 mas. Rdl2010
12299-1631 SHJ 145 7 Crv = del Crv = Algorab. B is BD-15@3481.
NLTT 30918/30916 Chm2004
A may be variable.
AB: H 4 105. MEv2010
12300+5132 BUP 143 7 CVn = del CVn. C is BD+52@1630.
12301-1324 BU 28 Wilson & Seabroke note seeing a distant (290".8) companion in 1874.26 WS_1877
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.80 +/- 0.97, 1.81, and 1.07 Msun, respectively. Mlk2012
12302-5336 RSS 16 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
12303+2157 HJL1069 Spectral type of comoving secondary estimated F6-G4, mass 1.02 Msun. Mug2014
12306+0943 STF1647 Hopmann (1964) orbit rejected from Fourth Orbit Catalog Hop1964b
("period over 4000 years") Wor1983
12307+5352 ES 726 AB: Also known as STI2284.
AB: Rectilinear solution by Hurowitz et al. (2014). USN2014a
12309+2555 LAS 7 Lasgoity (2014) determines that the two components of the pair in the
region of the Coma Berenice star cluster share common proper motion.
He derives spectral types of M3V for both components, and estimates
distance, mass, and radius for both stars. Las2014a
12310-5312 HJ 4526 B is CPD-52@5648.
B 2738 CD: Additional notes may be found in van den Bos (1930). B__1930b
12311+6116 LDS1314 NLTT 30989/30986 Chm2004
12312+0120 SHJ 146 STTA119. B is BD+02@2551.
12312-5707 DUN 124 gam Cru = Gacrux. A variable? B is CPD-56@5274, spectrum A3V.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
12313+5507 BAG 50 GJ 1160. Primary is the variable NO UMa. Bag2013
Arenou (2000) gives combined solution of astrometric orbits and DSBs. Are2000
Paper includes masses and distances.
Schlieder et al. (2016) derive the following properties for A and B:
spectral types K2V +/- 0.5 K6.5V +/- 0.5
masses (Msun) 0.83 +/- 0.03 0.65 +/- 0.02
Teff (K) 5020 +/- 50 4150 +/- 30
log (L/Lsun) -0.48 +/- 0.03 -0.96 +/- 0.03. SJE2016
Improved resolved SB2 orbit for this pair. Kie2018
A: Teff = 5105 +/- 21 K, M = 0.834 +/- 0.017 \msun.
B: Teff = 4175 +/- 35 K, M = 0.640 +/- 0.011 \msun.
Orbital parallax = 38.82 +/- 0.23 mas.
Age = 0.4 Gyr.
12316+1631 BPM 591 [PM2000] 1034110 + [PM2000] 1034136. Gvr2010
12316-1104 STF1649 B is BD-10@3486. Mt. Wilson spectral types A3, F2.
12317+1208 SHY 607 HIP 61135 + HIP 61416.
12317-5925 GAA 12 Classical Cepheid BG Cru = 35 Cru.
12321+7449 STF1654 H N 118. MEv2010
12323+2000 HU 571 Possible quadrant reversal about 1920-1930.
12323+1335 LDS1317 AC: NLTT 31039/31038 Chm2004
12324+1717 BPM 592 [PM2000] 1034422 + [PM2000] 1034445. Gvr2010
12324+1211 LDS 937 LDS1316.
NLTT 31034/31037 Chm2004
12325+2106 STF1652 Primary is KK Com, a Beta Lyr type eclipsing binary, P = 1.06788d. Zas2012
12328+4828 LDS4227 NLTT 31062/31063 Chm2004
12329+5448 A 1600 Primary is II UMa, a W UMa type eclipsing binary, P = 0.82522d. Zas2012
12333-2410 ARA2180 May be HJ 4527 = BDS 6203 with a quadrant flip. Dam2015
12334+3202 STF1653 STF1655.
SEI 532. Nsn2017b