09001-1228 HU 225 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.38 +/- 1.07, 2.57, and 1.13 Msun, respectively. Mlk2012
WOR 36 A faint companion (mag. about 14, 5") found by Worley may be
physical.
09002+4258 LDS3840 NLTT 20703/20706 Chm2004
09003+0332 HJ 2479 The proper motion study was:
A component: mu(RA) = -0.006+-0.002 mu(DEC) = -0.005+-0.001,
B component: mu(RA) = 0.000+-0.006 mu(DEC) = -0.005+-0.001 FMR1999h
09004-0809 OL 171 Aka BRT2287. Dam2018n
09005+7526 HJ 1162 Also a spectroscopic binary with P = 1324d which cannot be the visual Grf2016a
pair.
09005+3225 HU 718 A premature orbit has been computed.
09005+0617 RAB 1 Rabe identifies this as BDS 4887? Looks like another pair. Rab1923
09006+4147 KUI 37 10 UMa. Hyad. Well observed RV variation in agreement with the visual
orbit. Spectral types and masses of components assigned by ten
Brummelaar et al., based on adaptive optics observations. TtB2000
Calculated mass sum is 2.44 +/- 0.12 Msun, consistent with spectral
types F5V. Mut2010b
AB: Additional notes may be found in Duruy (1941), Dur1941
Duruy (1942), and Dur1942b
Baize (1943). Baz1943a
AB: Martin et al. (1998) derive component masses 1.525 +/- 0.104 and
0.920 +/- 0.080 Msun. Mig1998
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.37 +/- 0.33, 2.39, and 2.14 Msun, respectively. Mlk2012
AB: A typographical error in the Muterspaugh et al. (2010) orbit has Mut2010b
been corrected; period is 7961.0d, not 7691.0d. Noticed by Rick Wasson
(2016, private comm.)
STT 566 AB,C: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
AB,C: Rectilinear solution by Hurowitz et al. (2014). USN2014a
09008+0516 OSV 2 Ross 686,7.
09012+0245 STF1302 AC: Rectilinear solution by Hurowitz et al. (2014). USN2014a
09013+1516 STF1300 NLTT 20763/20764 Chm2004
09013-3855 I 1513 CPD-38@2898.
09014+3215 STF1298 66 Cnc.
09015+3604 ALI 354 Bogus binary.
09018+2754 SHJ 101 67 Cnc. A is a spectroscopic binary. B is BD+28@1673.
H 6 41. MEv2010
09024-6547 WFC 78 SWR 62. CPM pair Skf2004
09024-6801 SWR 63 CPM pair Skf2004
09026-5956 HJ 4170 SWR 61.
09032+4232 LDS3848 SLW 323.
09032-1740 S 588 B is BD-17@2726.
09032-6221 HJ 4175 Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: Rectilinear solution by Hurowitz et al. (2014). USN2014a
09035+3750 MUG 1 Metchev & Hillenbrand say pair probably physical, based on proximity. Met2004b
Metchev & Hillenbrand (2009) estimate companion mass 0.49 Msun, Met2009
dK=2.10. Estimated V(B)=11.2, dV=4.0. Tok2014d
09036+4709 A 1585 kap UMa = 12 UMa = Alkaphrah.
Elongations and quadrant doubtful. B__1963b
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
1975.950: This observation was made under very poor conditions and
yielded a poor set of fringes. BLM1978
1981.350: This observation was incorrectly attributed to Fin 347 by Tok1982a
Tokovinin (1982a) (noted in Tokovinin 1982b) Tok1982b
Calculated mass sum is 6.30 +/- 0.98 Msun, not well-constrained. Mut2010b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 6.63 +/- 1.41, 9.53, and 2.19 Msun, respectively. Mlk2012
09036-2619 HJ 2482 SWR 60. CPM pair Skf2004
09037+4531 COU2686 Also known as HDS1312. While the HDS measure predates that of Couteau, Cou1994
the Couteau publication predates that of Hipparcos. HIP1997a
09040+1349 FAR 7 SKF 29. Primary is white dwarf WD 0901+140. Far2005b
09040+0259 GRV1017 SLW 327.
09040-3204 PRO 80 SWR 64.
09042+6446 LDS2301 LDS5201.
09042+0301 GRV 775 HJL 103. HJL1986
SHY 536. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
09045-5740 RST 375 Spectral type G2?
09048+3759 LDS3851 NLTT 20894/20892 Chm2004
09050+2250 HDS1318 A is SB2, P=893.5d. B not seen in 2MASS K,J-band images, likely bogus. Tok2014d
09050+1134 TOK 125 HIP 44579.
09050+1058 BPM 554 [PM2000] 925928 + [PM2000] 925978. Gvr2010
09053+3848 OSO 24 G115-049. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
09055+0020 RST5313 Appears to be 5' error in 1855 declination of BD coordinates.
Appears to be same as TDS6306; pairs merged.
09055-4919 JNN 65 This star has a probably brown dwarf companion, but since only one
epoch of data exists, this is still unconfirmed. Jnn2012
09056+5018 ES 2631 B is BD+50@1606.
09056-7433 SWR 66 CPM pair Skf2004
09057-0816 FAL 26 A = RX Hya, eclipsing binary of Algol-type, period 2.28165 days. Zas2015
09061+3537 WLY 4 The pair ALI 355 is bogus and was a measure of a plate flaw.
The WLY 4 pair was found while searching for the ALI pair.
09063-5904 LTT 3359 Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
09066+0249 STF1309 HJL 104. HJL1986
09067+2031 OSO 25 G009-047. Common proper motion pair Oso2004
09067-3334 EGN 10 Pair bound. B component colors consistent with it being an M1-M4 dwarf
with mass 0.30 +/- 0.01 Msun. Egn2007
09071+3037 AG 162 BDS 4940, H N 30 is the same star.
09074+2259 HO 644 AC: Physical pair according to Daley. Dal2006a
STF1311 AB: HJL 105. HJL1986
AB: H 3 92. MEv2010
09075-3445 HJ 4179 SWR 65. CPM pair Skf2004
09076+0004 TOK 126 HIP 44777. X-ray source 1RXS J090732.0+000352.
09077+1040 CHR 257 kap Cnc = 76 Cnc. Hipparcos suspected non-single.
09077-4438 I 492 A Beta Cephei-type variable.
09079-0708 TOK 64 Aa,Ab: Estimated masses 0.95 and 0.61 Msun; sep 29.3 au, period 130 y. Tok2010c
STF1316 HIP 44804. Close triple. Observed with NICI (Tokovinin et al. 2010). Tok2010c
BC: Rectilinear solution by Friedman et al. (2012). USN2012a
09080-2552 I 491 kap Pyx
09080-4326 SEE 109 lam Vel = Suhail. A is an irregular variable.
09080-5808 RST9001 Previously known as RST3624a.
09080-6402 HJ 4185 B is CPD-63@1097.
SWR 67. Probably dwarfs, not giants (as per Houk). CPM pair Skf2004
09081+4510 HJ 1164 Noted as not having been observed in a long time, but this is an error. WSI2008
That "105" note should have gone with 09147-0212BAL 517. Dam2011
09081-2204 HDO 121 Separation for 1870.18 >15" Win1882
09083+3641 BRT2220 ALI 591.
09083-3707 TOK 127 HIP 44851. NOMAD: PM(B)=(+102,+500) V=16.37 (??). B is physical,
despite crowded field with N*=98. PM(A)=(-59,-3). PMS star, X-ray
source RXS J090817.3-370649, variable CY Pyx. Tok2011a
09084+2732 STTA 97 B is BD+28@1698.
HJL 106. HJL1986
SHY 207. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
09085+2141 A 2134 Appears to be same pair as 09085+2142 TDS6348; systems merged.
09086-2550 RST2610 Possibly triple: the known companion RST 2610 at 1".7 with estimated
period 500 yr is unlikely to cause the RV variability and dmu. Tok2012a
AB: A is suspected SB, no orbit. Tok2014d
09086-3843 RST1416 CPD-38@3012.
09086-4841 LDS 251 B is CD-48@4456.
09087-0835 KUI 38 19 Hya. A is a spectroscopic binary.
09087-2159 RSS 191 CPD-21@4113
09088+2638 STT 567 AB: 75 Cnc. A is a spectroscopic binary. B is BD+27@1716.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
75 Cnc Combined spectroscopic/astrometric solution, based on high-resolution
echelle spectra plus archival PTI visibility measurements.
Derived masses 1.173 +/- 0.024 and 1.011 +/- 0.021 Msun,
distance 31.246 +/- 0.051 pc. Knc2010
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.13 +/- 4.27, 1.98, and 1.07 Msun, respectively. Mlk2012
09090+1728 ONL 1 OCC 238.
09091-1820 VIG 12 Optical/physical nature of the faint companion is undefined. Vig2012
09094+2203 WRH 16 xi Cnc = 77 Cnc. Uncertain binary, unresolved by speckle
interferometry. A long-period spectroscopic binary.
09095+3854 OSO 26 G116-009. Common proper motion pair Oso2004
09097-4207 CPO 40 LDS 253.
09098+1134 CHR 131 Suspected occultation binary.
09099-3022 H N 96 eps Pyx. A is a spectroscopic binary.
09103+2200 WRH 17 79 Cnc. Less than 0.1" 1954 (Finsen); not resolved by speckle despite Fin1954c
numerous attempts 1976-1983. Binary nature uncertain.
09104+6708 STF1306 sig 2 UMa = 13 UMa.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: H 3 54. MEv2010
09109+6331 H 5 73 H V 73. tau UMa = 14 UMa. A is metallic-line star and long-period SB.
A: Ren & Fu (2013) calculated an astrometric orbit, combining Ren2013
Hipparcos Intermediate Astrometric Data with spectroscopic elements by
Bretz (1961). Brz1961
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
09109-4519 HJ 4186 LDS 255.
09110+6331 tau UMa Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Bretz (1961). Brz1961
09110-1929 I 824 Spectrum: Fm delta Del.
09111+1757 BPM 555 [PM2000] 930950 + [PM2000] 930951. Gvr2010
09112+0128 GIC 83 G046-026/G046-027.
09115+2801 HJ 805 AB: HJL 107. HJL1986
09117-4653 SEE 110 Algol-type eclipsing binary, P = 2.61362 d. Zas2011
09118+1617 BPM 556 [PM2000] 931498 + [PM2000] 931492. Gvr2010
09119+1803 STT 568 AB: 80 Cnc.
BUP 124 BC: C is +18@2136.
09122-2555 JNN 150 2MASS J09121259-2555025 has the alternative identifier CD-25 6962B in
SIMBAD, implicitly implying companionship with the G2-type star
CD-25 6962 at 14" separation. However, given the apparently very
different proper motions of the components (e.g. Roser et al. 2010), XXX2010
we consider such a companionship questionable. Jnn2012
09123+1500 FIN 347 Aa,Ab: pi 1 Cnc = 81 Cnc.
1981.358: This observation was incorrectly attributed to ADS 7158 by Tok1982a
Tokovinin (1982a) (noted in Tokovinin 1982b) Tok1982b
1983.9371, 1983.9372: Interferometric observations indicate that Wor1983
Finsen's 1965 orbit (see Worley & Heintz, 1983) must be revised. Bnu1984
1990.9166: Residuals (4.0 deg in theta, 0".007 in rho) to the orbit of
Hartkopf (1989) are only fair, due to a combination of large zenith Hrt1989
distance and close angular separation at the time of this observation.
A combined astrometric/spectroscopic orbital solution is given by
Mason et al (1996). Msn1996a
Reversed Delta m and slightly larger parallax/smaller masses than in Msn1996a
the speckle-spectroscopic study by Mason et al.(1996).
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
Aa,Ab: Combined solution orbit. Mass_a = 0.983 +- 0.045 Msun,
Mass_b = 0.903 +- 0.049 Msun, orbital parallax = 48.78 +- 2.36 mas. Msn2012a
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.80 +/- 0.25, 1.86, and 0.91 Msun, respectively. Mlk2012
BUP 125 AB: Due to the high proper motion of the A component, a later
observation of this pair by Soulie was incorrectly entered as a new Sle1986a
component, SLE 478AD.
STT 569 AC: Optical pair, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
WIL 1 AE: CPM pair. Using data from 2MASS, Wilson et al. (2001) derive a Wil2001
spectral type of L8V and mass 40-74Mjup for the companion (called
Gl 337C in that paper). They also note that the C and D components for
the system appear to be background objects without CPM to the AB pair.
BUG 16 Ea,Eb: Burgasser et al (2005) resolved the E component (called Gl 337C
in the paper) into a 0.53" pair of near-equal magnitude. At a distance
to the system of 20.5 +/- 0.4pc, the close pair has a physical
separation of 10.9 +/- 0.6 au. Period of the pair is estimated at
140-180y. Primary is L8; secondary is possibly early- or mid-T dwarf. Bug2005
09124+2653 A 1977 1921-1922 elongation uncertain. Less than 0.1" in 1956.
09124-0707 GAA 7 KW Hya.
Ma,Mb = 1.975 +/- 0.028 , 1.487 +/- 0.013 \msun, GaA2019
orbital parallax = 11.462 +/- 0.074 mas.
09125+4912 MET 54 This cannot be the close 20.0-d spectroscopic binary. Grf2013f
09125-4337 FIN 317 Aa,Ab: FIN 317 is a close subsystem in the 2.9" AB pair HJ 4188. After
discovery of Aa,Ab in 1951 at 0.116", Finsen (1951) was unable to Fin1951b
resolve the star again on twelve occasions till 1968, except one other
tentative measure in 1962. Yet the object was resolved by speckle in Fin1964a
1989.94 at 0.144" and in 2006.18 at 0.123". Despite orbital period of
∼50 yr estimated from projected separation, the sub-system was not
detected in 3 runs at SOAR (2009-2012), while the wider pair AB was
measured. This may be yet another case of erratic measures and
non-resolutions. Possibly another "ghost" which isn't a real binary, Tok2012b
but not "X" coded yet.
09126+0915 HEI 483 This is apparently the same pair as HJ 121.
09128+6141 STF1315 B is BD+62@1055.
H N 79. MEv2010
09128-4329 HU 1456 Primary is GG Vel, Algol-type eclipsing binary, period 1.475216d. Zas2013
09128-6055 HDO 207 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 34.09 +/- 12.51, 5.38, 2.57 Msun, respectively. Mlk2012
09131+3633 ES 2106 BRT3251. Brt1951
09131-4128 CPO 41 LDS 258. A is CPD-40@3274, B is CPD-40@3273.
09133+0540 WFC 81 HJL 108. HJL1986
09136+4659 STF1318 A is SB2, P = 2536d. B is SB? Tok2014d
09138+4313 BAG 45 Primary is the rotationally variable star EI Lyn.
09139+0252 H 6 108 B is BD+03 2171.
09142-5021 HJ 4192 B is CD-49@4232.
09143+6125 16 UMa SB2. Combined orbit including RV data and Hipparcos Intermediate
Astrometric data. Semimajor axis derived from photocentric a0 plus
stellar evolutionary model. Derived properties for A and B:
M/Msun = 1.12 + 0.61, L/Lsun = 2.71 + 0.09, dm = 3.70 mag,
log age = 9.78. WaX2015b
Fekel et al. (2015) derive an astrometric orbit, with values of P, T,
e, and omega adopted from their spectroscopic solution. The secondary
is thought to be a mid- to late-K dwarf. Fek2015
09143-0817 BU 908 B is BD-07@2762.
09144+5241 STF1321 Proper motion of A = -2530,-563; PM of B = -2559,-656 (UCAC2).
B is BD+53@1321. A premature orbit has been computed. Both components
are suspected spectroscopic binaries (Abt & Levy 1973). AbH1973
AB: NLTT 21249/21251 Chm2004
CHARA Array Limb-darkened diameter of A,B: CIA2012f
R = 0.5773 +/- 0.0131, 0.5673 +/- 0.0137 \rsun,
L = 0.06974 +/- 0.00213, 0.06465 +/- 0.00194 \lsun,
Teff = 3907 +/- 35, 3867 +/- 37 K, M = 0.622, 0.600 \msun.
Epoch-2000 coordinates of C component 0914355+524209; current AC
separation ~2'.2 at 64deg. PM of D +035-003.
09144+0219 HJ 2489 the Hya = 22 Hya. A is a SB.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: H 5 54. MEv2010
B and C optical. No earlier measures of D. B__1963b
09149+0427 HEI 350 A long-period astrometric binary, now resolved.
09150+1253 HJ 2490 BDS 4982, HJ 2487 same star.
09151-0825 GCB 22 BRT 427. J 3248.
09152+2323 BUP 127 AB: A is exoplanet host. Tok2014d
STT 570 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
09152+1643 BPM 557 [PM2000] 934187 + [PM2000] 934230. Gvr2010
09156+0422 RED 17 2MASS J09153413+0422045. Confirmed as binary by Liu (private comm. to
Reid et al). Spectral types L7 and L7 Red2006b
09156-1036 MTG 2 LHS 6167. Estimated age 30-300 Myr; masses 0.15 +/- 0.04 and 0.09 +/-
0.03 Msun; a ~1.0 au. Jnn2014
Also known as G 161-7 or LHS6167.
Parallax = 134.9 +/- 12.1 mas. UR_2016
Parallax = 103.33 +/- 1.00 mas. JLB2017
09157-0114 STF1329 B is BD-00@2163.
09158-3725 SEE 111 A is a spectroscopic binary.
09161-4454 DON 329 Variable.
09163+2730 SLE 484 No sign of Soulie (1986) pair. Measured pair is obvious double; error
in Soulie (1986) coordinates? Sle1986a
09167+1955 LDS5162 LDS5202.
NLTT 21351/21352 Chm2004
09167-0621 KUI 40 23 Hya. A is a long-period spectroscopic binary.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Jones (1928). Jon1928c
09167-2448 JNN 67 We resolve this star into a close binary (as yet unconfirmed through
common proper motion). It was recently classified as a classical
Cepheid based on light curve analysis (Christiansen et al. 2008 MNRAS
385, 1749). We assume that this is a mis-classification, given that
the unresolved spectral type is M0.5V. Jnn2012
09167-5501 BRT3291 CD-54@2689.
09168-2157 I 493 Too close, position angle uncertain.
09169-0524 OSO 27 G161-009. Neither is a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
09171+0717 STTA 98 AB: Pair appears in an appendix list, not part of discoverer's regular
numbering sequence.
09172-2249 J 1543 CD-22@7068.
09173-6841 FIN 363 Speckle observations needed to refine relative orbit.
AB: Hipparcos parallax 30.64 +/- 0.70 mas. Dynamical parallax 27.2 mas,
masses 1.63 and 1.37 Msun. FIN 363 has an unusually short period of
only 3.44 yr. The Hipparcos photometry is doubtful because of close
0.1" separation. Tok2012b
AB: Martin et al. (1998) derive component masses 3.661 +/- 0.338 and
3.661 +/- 0.338 Msun. Mig1998
AB: Docobo & Andrade (2013) derive a dynamical parallax of 29.71 +/-
1.33 mas and component masses 1.43 +/- 0.25 and 1.06 +/- 0.20 Msun.
See paper for extensive notes on this system. Doc2013d
09175+7715 KUI 39 Proper motion of A -1059 -020.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 0.66 +/- 0.23, 1.17, and 0.65 Msun, respectively. Mlk2012
09176+3641 ES 1734 OL 109 is the same star, according to Barton.
09179+2834 STF3121 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.39 +/- 0.75, 1.57, and 0.85 Msun, respectively. Mlk2012
09179+1130 HJ 128 A is a spectroscopic binary.
09179-6948 RMK 10 Rectilinear solution by Letchford et al. (2018). Whi2018
09180-5453 JNN 69 2MASS J09180165-5452332 has a close (~0.49") companion to which it is
probably physically bound, although this still needs to be confirmed
through common proper motion. Jnn2012
09182-0036 HJ 126 STF1337. Pettit refers to his 1915 observation as of HJ 126, but Ptt1917
gives the cryptic note "Hard to identify with H star 1820. P.A. too
small, distance too great." It appears to be a measure of the HJ pair,
but typographically mangled. Earlier catalogued as PTT 25.
09184+3522 STF1333 Aka H 1 31. Bu_1906
Additional notes may be found in Fatou (1941). Fat1941
09184-2022 S 595 B is BD-19@2673.
09186+5231 HJ 2492 AB: B is the faint nebula NGC 2800.
09186+2134 ALP 15 2MASSW J0918382+213406
Physical companionship of C component to this ultracool dwarf ruled
out based on i-z and z-J colors, using photometry from SDSS. The B
component was not detected by SDSS; followup observations are needed
to determine its nature. AlP2007
09186+1953 SKF 31 FAR 55.
09188+3648 STF1334 38 Lyn. A is a spectroscopic binary.
CHR 173 Ba. Abt & Biggs (1972) note variable RV. AbH1972
STF1334 AB: H 1 9. MEv2010
09188+2647 LDS6226 NLTT 21428/21426 Chm2004
09188-2250 DON1080 J 1544. ARA1764.
09190+1742 83 Cnc Gontcharov & Kiyaeva (2002) photocentric (astrometric) orbit is based Gon2002a
on a combination of ground-based catalogs with Hipparcos.
09191-4128 CHR 239 Astrometric binary; dm 2.4 mag, period ~ 10y? Accelerated pm Tok2012b
Omega for Tokovinin et al. (2014) orbit flipped by 180deg, at request
of author. Tok2014a
09192+5824 LDS1226 NLTT 21416/21397 Chm2004
09193+5230 VBS 15 Identified as BDS 5000, HJ 2492 (Van Biesbroeck). May be another pair. VBs9999
09193+3831 GIC 84 G115-068/G115-069 = Melotte 25 EGG 33AB = GJ 1122AB.
09194-7739 KOH 83 Aa,Ab: Estimated masses 0.88 and 0.81 Msun; sep 6.8 au, period 14 y. Tok2010c
Orbital parallax 14.90 +/- 0.37 mas. Tok2020c
Mass of Aa, Ab = 1.12 +/- 0.04, 1.00 +/- 0.03 /msun.
HJ 4214 Physical B component is also binary with spectroscopic P ~ 0.556d.
HIP 45734. This is a PMS quadruple, both components are
slightly above the MS. Tok2011a
AB: B is X-ray source, SB2 (Desidera et al 2006 A&A 454,553) Tok2014d
09196-3513 SWR 70 Giants, not dwarfs Skf2004
09197+0444 LDS3876 SLW 348.
09198-1158 B 2529 26 Hya. 1936, 1938 position angles 139@-122@. Distance 3.0".
Invisible 1948 B__1951a
09200+0500 STF1343 HJL 109. HJL1986
09200+0103 J 2501 Radio galaxy UGC 4956. J__1962a
09202+3518 RED 11 2MASSW J0920122+351742
2000.107: HST WFPC2 observations by Reid et al. (2001). Paper includes Red2001
mass and age estimates, as well as discussion of L dwarf binary
frequency and semimajor axis distribution.
Assuming a spectrophotometric distance of 24.3 +/- 5.0 pc, Konopacky
et al. (2010) derive a system mass of 0.11 +/- 0.11 Msun. Kon2010
09203-0817 GCB 24 J 2898.
09205+0752 BRT2148 OL 172.
09205-0933 SHJ 105 27 Hya. A is a spectroscopic binary. Spectrum composite: G8III-IV+F5V.
AB: SHY 540. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
AB: H 6 85. MEv2010
Toyota et al. (2009) monitored the RV of the A component every 1-2
months between 2003 Mar - 2007 Nov, using a high-dispersion echelle
(precision ~10 m/s). The star exhibits a linear trend in RV, with a
slope -30 m/s/y. Toyota et al. assert that these variations are due to
an unseen companion. Assuming a circular orbit, period is estimated at
3400d; if the mass of A is 2.32 Msun, the minimum mass ~10 Mjup. Toy2009
09207+5116 ARN 71 AD: HJL1055. HJL1986
AD: SHY 208. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
09210+3811 STF1338 AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.01 +/- 0.61, 2.59, and 2.58 Msun, respectively. Mlk2012
09210+3643 STF1339 H 1 31. MEv2010
09210+3223 GIC 81 G047-035/G047-034. Typographical error led to this pair being
originally entered in the WDS as 08211+3226.
09210-0100 FOX 161 J 1546. Bal 859.
09211+4155 LDS3878 NLTT 21509/21510 Chm2004
09213+3426 STT 571 40 Lyn
STF1342 BC: H 4 55 = SHJ 369. MEv2010
09214+8123 STF1304 B is BD+81@288.
09214+0248 BAL2361 J 2497.
09215-4528 HJ 9003 Previously known as HJ 5452a.
09216-0243 FIL 21 BAL 202.
09218+4330 LAW 17 LSPM J0921+4330 = GJ 3554. Law et al (2008) derive a distance of Law2008
11.8 +5.6/-2.2 pc and a projected separation of 7.1 +3.7/-1.2 au.
Estimated spectral types are M4.5 and M4.5.
GJ 3554. Estimated age 300-1000 Myr; masses 0.30 +/- 0.06 and 0.21 +/-
0.04 Msun; a ~14.8 au. Jnn2014
09219+1156 BPM 558 [PM2000] 939493 + [PM2000] 939496. Gvr2010
09223-3209 RSS 199 Primary is 12.9d SB1, Period of AB pair ~4700y. Tok2006
09223-5428 SHY 541 AC: HIP 45952 + HIP 45937.
I 1107 AB: Rectilinear solution by Zirm (2013). Zir2013d
Despite the linear solution, proper motion and parallax favor a Grv2020a
physical connection. Long period and/or high eccentricity possible.
09223-5558 EVS 14 Primary is the Cepheid V Vel. Evs2016a
09226+6251 MLB 203 HJL 110. HJL1986
09228-0950 A 1342 A magnetic and variable star, KU Hya, , 3.41d, 0.05V, is in the system. Mlr1956a
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Combined analysis using speckle, radial velocity, various magnetic
field and polarization measurements. Wad2000
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 5.13 +/- 1.94, 4.25, and 2.00 Msun, respectively. Mlk2012
09233+0330 STF1347 HJL 111. HJL1986
09234-0503 GIC 85 G161-019/G161-020.
NLTT 21625/21628 Chm2004
09234-7753 HJ 4217 Agrees with Herschel's place but not his description. Daw1922
High proper motion of A accounts for the discrepancy.
The companion is clearly UCAC4 061-008434 and not UCAC2 497073 (UCAC4 Whi2013
061-008429) as suggested by SIMBAD.
09236-5454 HJ 4207 B is CPD-54@2239.
09243-1601 LDS6227 NLTT 21682/21683 Chm2004
09243-3926 FIN 348 Hipparcos detects a magnitude difference, which reverses the quadrant
of the prior measures, and indicates that nearly a revolution has been
completed.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 4.29 +/- 0.76, 5.18, and 1.66 Msun, respectively. Mlk2012
09247+2611 BU 105 kap Leo = 1 Leo
kap Leo. Engelmann speaks of a 10" star in the direction 65deg. There
is certainly no companion in this place, and no third star near in any
direction. Bu_1894
09249+5134 STT 200 A is a spectroscopic binary.
09251+2933 BU 1423 AC. Burnham's measure, X coded now, was actually a measure from NGC Dam2013
2893 to BD+30 1873.
09252+4606 HDS1353 Cvetkovic et al. (2016) estimate spectral types K4 and M1, masses 0.72
and 0.43 Msun. Dynamical parallax is 25.49 +/- 2.78 mas. Cve2016b
09252+1602 FAR 8 SKF 32. Primary is white dwarf WD 0922+162. Far2005b
09253-4816 HJ 4209 B is CD-47@4921.
09254+1137 BPM 559 [PM2000] 942111 + [PM2000] 942115. Gvr2010
09255+0009 LDS5703 LDS6228. LHS 2140.
09256+6329 JNN 275 G 235-25. Estimated age 1000-10000 Myr; masses 0.21 +/- 0.04 and 0.13
+/- 0.02 Msun; a ~2.4 au. Jnn2014
09256+5401 STF1346 AB: H 2 73. MEv2010
09257+4626 LDS3889 NLTT 21701/21699 Chm2004
09257+3837 ES 298 Four-component system. The question of whether the CDB system is a
hierarchical triple remains open. Kiy2012
09257-6958 HJ 4216 B is CPD-69@1061.
09260+2839 A 222 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.59 +/- 0.66, 2.49, and 1.10 Msun, respectively. Mlk2012
09260-1535 CLZ 15 GWP1172. Tob2012b
09261+5344 A 1343 Rectilinear solution by Rica & Zirm (2012). FMR2012i
09263+5847 BUG 9 SDSS J092615.38+584720.9
Estimated spectral types are T4: + T4:, effective temperatures ~1330
and ~1330 K. Masses are estimated at 0.029-0.073 and 0.029-0.073 Msun,
and the orbital period (assuming the semi-major axis = 1.26 * rho) is
~18yr. Bug2006a
09265+7826 STF1326 SHY 542. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
AB: CfA: A=SB? Tok2014d
09265-6618 RST 404 CD-65@769.
09266-3047 SWR 71 CPM pair Skf2004
09272-0913 A 1588 29 Hya.
09275+5338 LDS3893 SLW 356.
09275+3930 LEP 36 A is also a 8.5d spectroscopic binary. Tok2019b
09275+1054 J 388 STF1354.
09275-5806 CHR 240 Astrometric binary; dm 0.3 mag, period ~ 4y? Accelerated pm. Tok2012b
09276-0840 H 6 111 AB: H VI 111. alp Hya = 30 Hya = Alphard. B is BD-08@2681.
Mk III Limb-darkened diameter 9.727 +/- 0.097 mas. MkT2003
Primary unresolved in H alpha. Bla1977a
09276-3500 B 2215 Last position angle uncertain. Needs speckle.
Hipparcos astrometric solution assumed circular orbit (e = omega = 0) HIP1997d
Astrometric binary; dm 1.5 mag, period ~ 1.97y Tok2012b
09276-4311 SWR 73 A component is 0".6 CPM pair Skf2004
09278-0604 B 2530 There may have been a quadrant reversal about 1951. The 3-year
spectroscopic motion does not seem to relate to the visual pair.
Giant primary according to isochrone fit. Sod1999
Single line SB, P = 2.5 y, also a known visual binary. Primary is G2V,
so companion should likely be a cooler dwarf; this seems to be
confirmed from magnitude differences observed at 750, 550, and 450nm. Bag1984b
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses. Pbx2000b
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.06 +/- 0.31, 2.44, and 1.00 Msun, respectively. Mlk2012
09281+1150 BPM 560 [PM2000] 944081 + [PM2000] 944114. Gvr2010
09283-7815 HJ 4226 B is CPD-77@520.
09285+0903 STF1356 ome Leo = 2 Leo. Mlr1956a
Chevalier identified this star as ome Leo, but gave incorrect Che1911
coordinates, leading to its initial designation as 09283+0903 CHE 137. Hrt2012b
Giant primary according to isochrone fit.
1980.019: This observation of omega Leo by Weigelt (1983) was Wgt1983
incorrectly attributed to 09412+0954 = omi Leo in earlier editions
of both the interferometric catalog and the WDS. As a result, omi Leo
was incorrectly assigned the discoverer designation WGT 1.
H 1 26. MEv2010
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.67 +/- 0.24, 2.14, and 1.27 Msun, respectively. Mlk2012
09285+0811 H 4 47 H IV 47. 3 Leo.
09285-2426 B 181 Not seen 1959-1962. May exhibit rapid retrograde motion.
09286+1721 BPM 561 [PM2000] 944368 + [PM2000] 944357. Gvr2010
09287+7834 LDS1696 MLR 524.
09287+4536 S 598 41 Lyn = Intercrus. STTA 99. B is BD+46@1510.
09288-0722 GIC 87 G161-033/G161-034.
NLTT 21868/21870 Chm2004
09291-0246 HJ 1167 tau 1 Hya = 31 Hya. B is BD-02@2902.
HJL 112. HJL1986
H 6 71. MEv2010
GJ 348. A is an X-ray source; also SB1, P=2815d=7.685y (Halbwachs et HJL2012b
al. 2012) Tok2014d
09292+0024 BAL1151 J 3292.
09293-0409 GIC 88 G161-036/G161-037.
NLTT 21891/21892 Chm2004
09293-4432 DUN 77 B is CD-43@5332.
AB: SHY 210. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
EGN 11 Ba,Bb: Single epoch, but likely bound. If so, colors indicate Bb
component is M0-M3 dwarf with mass 0.43 +/- 0.01 Msun. Egn2007
DUN 77 sp, dDEC 24.65". Dun1829
09297+0433 HJ 137 Also known as STF1361.
09299-3629 HDS1364 AB + TOK 440BC: HIP 46572 is called a "high proper motion star" in
SIMBAD, although its PM and RV are actually quite moderate. The binary
AB has moved little in the 24 years since its resolution by Hipparcos.
We discover the subsystem BC with an estimated period of ~100yr. Tok2015c
09302+5339 TDS 538 Both A and B are eclipsing binaries. Lhr2015
09304-5822 RST 408 A is an irregular variable.
09305+3822 LDS3899 NLTT 21915/21914 Chm2004
09306+1036 STF1360 AB: HJL 113. HJL1986
09307+4502 FLA 1 Also known as ES 2632.
09307+3339 HJ 1166 7 LMi. STTA100 = H 5 69.
09307-2724 SWR 75 CPM pair Skf2004
09307-4028 COP 1 psi Vel. Identification of ascending node not quite certain.
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.70 +/- 0.50, 2.42, and 3.00 Msun, respectively. Mlk2012
09308-1623 LDS 272 GWP1189. Tob2012b
09308-3153 DUN 78 zet 1 Ant
09309+4441 STF1358 B is BD+45@1729.
09309+2658 LDS 909 AB: NLTT 21938/21941 Chm2004
09312+1407 BPMA 37 [PM2000] 946218 + [PM2000] 946038. Gvr2010
09313-1329 KUI 41 Ross 440. The primary is probably a flare star.
Pair often unresolved, so orbit probably eccentric with P<10y. Kui1943
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 0.74 +/- 0.21, 0.80, and 0.30 Msun, respectively. Mlk2012
09314-0012 BVD 77 GWP1190.
09315+6304 STF1351 23 Uma. The primary is a Delta Scuti-type variable.
AB: H 4 29. MEv2010
CHARA Array Limb-darkened diameter 1.133 +/- 0.009 mas, CIA2012e
R = 2.902 +/- 0.026 \rsun, L = 15.086 +/-0.330 \lsun,
Teff = 6693 +/- 45 K, M = 1.824 +/- 0.016 \msun,
Age = 1.4 +/- 0.1 Gyr.
09317+3830 AG 168 BD+39@2255a.
09320+0943 SHJ 107 6 Leo. STTA101 = H 5 26. A is spectroscopic binary. B is BD+10@2015.
09320-0111 CHR 174 tau 2 Hya = 32 Hya. A spectroscopic binary, now probably resolved.
Abt & Biggs (1972) note variable RV. AbH1972
09320-6720 RSS 12 This previously uncataloged double star was a Hipparcos double entry
system. The first measure is determined from the individual positions
listed by Rousseau et al. Rss1996
09321+3531 KU 97 AB: Same as KU 144.
09322-6247 FIN 140 A is a Mira-type variable, R Car.
09327+3458 ES 299 Erroneously identified as +35 2017. Dam2013
BC also known as POP 56.
09327+2659 LDS3903 NLTT 22012/22015 Chm2004
LAF 38 Heinze et al. (2010) determine the C component is a background object. Hze2010