08001-0937 J 2862 RST 3562.
08003+1138 HJ 74 aka ROE 32. Friedrich Damm commented on the declination sign being
wrong for the HJ pair. The 1825 coordinates, precessed to 2000
match this pair, as does the second measure by John Herschel.
08005+2900 OSO 20 G090-036. Common proper motion pair Oso2004
08005+0955 A 2954 Magnitude underestimated by Aitken; should be ~0.7 mag. Baz1951a
08007+1635 BPM 431 [PM2000] 843821 + [PM2000] 843697. Gvr2010
08008+1719 OCC9068 3 Cnc.
08009+4452 ES 1325 aka 08017+4451TDS5455.
08009-0405 LDS6211 NLTT 18799/18798 Chm2004
08014-5431 DUN 60 One component is variable and a spectroscopic binary.
dRA = 1.83s. Dun1829
08016-3430 JSP 216 CPD-34@1901.
08017+6019 MCA 33 53 Cam. A variable of the Alpha CVn type, AX Cam, and a spectroscopic
binary now resolved by interferometry.
Value of omega in Baize (1993) orbit incorrectly listed as 113.0, same Baz1993b
as Omega (erratum noted in Inf. Circ. 121, 1994). Baz1993d
Combined spectroscopic/interferometric orbit by Balega et al. (2004), Bag2004b
yielding mass sum 3.61 +/- 0.38 Msun. Spectral types are estimated as
A2V and F0V.
Combined spectroscopic/interferometric orbit by Carrier et al. (2002), CrF2002
yielding a = 275.1 x 10^6 km, parallax 10.2 +/- 1.0 mas and mass sum
1.49 +/- 0.66 Msun. Authors note that Scholz & Lehmann (1988) Slz1988
attempted to scale their spectroscopic solution using then-available
speckle data, deriving masses for the components of 2.5 and 1.6 Msun,
considerably larger than found here.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.62 +/- 3.60, 3.94, and 2.09 Msun, respectively. Mlk2012
08017+2505 H 6 75 ome 2 Cnc = 4 Cnc. H VI 75.
08017+1521 BPM 432 [PM2000] 845760 + [PM2000] 845621. Gvr2010
08017-0836 A 1580 A is the Algol-type system V635 Mon.
08018-3429 I 187 CD-34 4230, mag 11.7, is 46.5" S and a 13.0 is 20" preceding. Daw1927a
08021+5437 STF1165 Same as STF1166.
08021-0049 BAL 845 J 3285.
08021-1710 HDS1140 AB + TOK 394AC: This is the high-PM M-dwarf LP 784-12 (HIP 39293) at
30pc. A new distant component C was found at 1".8 in addition to the
known pair HDS 1140 which closed from 0".4 in 1991.25 to 0".33 now. It
is confirmed as physical by its fixed position during one year, the
quadrant of the triple was determined in run 5. Tok2015c
08024+0409 STF1175 A premature orbit has been computed. Data appear equally well fit by
rectilinear solution - see linear elements catalog.
08024+0320 LDS5160 LDS5196.
08025+6305 SHJ 86 STTA 90. B is BD+63@750.
08025-4440 I 8 QQ Pup.
08025-5502 HJ 4044 B is CPD-54@1480.
08026+2028 DOO 47 Doolittle identifies this as BDS 4392, HJ 437 but it seems to be a Doo1915b
different pair.
08026+1309 SLE 320 CD: SLE 456.
08027-2632 LDS 200 NLTT 18855/18856 Chm2004
08027-4119 HJ 4038 A component variable? B is CD-40@3775.
08029+0419 BRT2140 BAL 2801.
08030-5720 SWR 38 CD-56@ 2090.
08031+1637 BPM 433 [PM2000] 848557 + [PM2000] 848413. Gvr2010
08031-0625 A 1581 A premature orbit has been computed.
08031-3228 HJ 4035 B is CD-32@4768.
08032-3812 HJ 4039 V626 Pup, EA per 1.425902 d. Zas2011
08033+5251 HDS1149 An additional component at a distance of 40 mas from the secondary is
suspected in the system. The magnitude difference is between 1.5 and
2 mag. Bag2004
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.42 +/- 0.46, 1.07, and 1.00 Msun, respectively. Mlk2012
08035+2748 ES 2628 chi Gem. See Espin. Es_1908a
08035+1211 HO 350 A=SB? AB is seen in the 2MASS J,K-band images, but A seems saturated. Tok2014d
08036-4000 zet Pup = Naos. The distance estimate is from Reid & Howarth (1996 A&A 311,
616). Van Rensbergen et al. (1996 A&A 305, 825) discuss the star's
trajectory and possible runaway status. Msn1998a
08037-4634 HJ 4043 B is CD-46@3727.
08038-1055 J 2492 J 2863.
08039-3133 LDS 201 AB: B is CD-31@5466.
AB: SHY 520. Bayesian analysis by Shaya & Olling (2011) indicates very Shy2011
high (near 100%) probability pair is physical.
AC: C is CPD-31@2104.
B 2164 CD: TDS5491.
08040-5822 BRT3117 TDS5496.
08041+3302 STT 187 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.79 +/- 1.42, 4.53, and 2.14 Msun, respectively. Mlk2012
08044+1217 BU 581 See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 1.96 +/- 0.38, 1.75, and 0.85 Msun, respectively. Mlk2012
Star C (mag. 10.5, 5") is in slow direct motion about AB.
AB,C: Additional notes may be found in Burnham (1894). Bu_1894
08047+2831 MLB 565 Faint pair, 32s p, 3' n of ADS 6557. Baz1951a
08047-6250 DUN 62 A is the variable V375 Car.
B is CPD-62@952.
08049-0223 GWP 968 ABL 181. Tob2012b
08050-3419 B 1579 Despite the linear solution, proper motion and parallax favor a Grv2020a
physical connection. Long period and/or high eccentricity possible.
08052-4525 JC 12 B is CD-45@3742.
08053-4626 CPO 192 TDS5515.
08055-6952 HJ 4055 SWR 39. CPM pair Skf2004
08056+2830 MLB 566 The Barton pair formerly at 08049 is identical Hei1985a
08056+2732 STF1177 17 Cnc
08056-6617 GLI 81 B is CPD-65@867.
08057+6823 STF1164 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. (2014). USN2014a
08059-2014 ALD 84 CPD-19@3088.
08061-0047 A 1971 A premature orbit has been computed. Cou1953d
08062+0201 J 420 Appears to be in rapid retrograde motion.
08063-4021 RSS 9 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
08068+3303 AG 147 SEI 487. Nsn2017b
08068-0900 GWP 972 ABL 182. Tob2012b
08069-1320 GWP 973 ABL 183. Tob2012b
08069-2707 DUN 61 B is CD-26@5531.
08069-6618 LUH 5 Primary is the DQ white dwarf WD 0806-661 = GJ 3483, mass 0.62 +/-
0.03 Msun. Mass of companion estimated at ~7 Mjup, Teff ~300K. Luh2011
Companion Teff 300-345K, mass 6-9 Mjup, distance 19.2 +/- 0.6 pc. Luh2012
08071-2138 B 2168 CPD-21@3163.
08072+1615 BPM 434 [PM2000] 856195 + [PM2000] 856322. Gvr2010
08072+0723 AG 149 HJL 86. HJL1986
08075+1318 BPM 435 [PM2000] 856648 + [PM2000] 856681. Gvr2010
08075-2418 RST5284 rho Pup = 15 Pup = Tureis. A is a Delta Scuti-type variable.
08076-0814 GWP 976 ABL 184. Tob2012b
08079-0215 GWP 977 ABL 185. Tob2012b
08079-6837 RMK 7 eps Vol. A is a spectroscopic binary.
08081+4916 HJ 2428 Rectilinear solution by Cvetkovic et al. (2018). Cve2018
08081-2415 BRT1448 Aka ARA2099.
08082+7155 LDS1667 NLTT 18921/18913 Chm2004
08082+2106 COU 91 LDS 902.
NLTT 18979/18980 Chm2004
08082-2208 BU 334 Despite the linear solution, proper motion and parallax favor a Grv2020a
physical connection. Long period and/or high eccentricity possible.
08084-0005 GWP 979 ABL 186. Tob2012b
08085+5130 ES 70 27 Lyn.
08086-0259 STF1190 zet Mon = 29 Mon. C is BD-02@2449.
AB: H 4 97. MEv2010
08087+5750 A 1075 Also known as HDS1161. These two pairs were recognized to be the same
by Brian Skiff. Skf2004
08089+2437 NLTT 18995 Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos
Intermediate Astrometric Data with spectroscopic elements by
Latham et al. (2002). They derived component masses 0.92 and 0.62 Msun Lat2002
and an estimated semimajor axis of 25.73 mas. Ren2013
08089+1213 J 375 AB: Rectilinear solution by Cvetkovic et al. (2018). Cve2018
08090+3249 BDT 2 Aa,Ab : Combined solution yield Ma = 0.72 +/- 0.04 \msun, Miz2018
Mb = 0.30 +/- 0.03, distance of 24.83 +/- 0.22 pc, Age = 42 +/- 6/5
Myr, and Teff = 4100 +/- 200/400.
DYR 1 AB: VYS 250. A is a flare star, and B is a double-lined spectroscopic
binary, P = 6.21d.
08090-6118 EHR 11 Companion appears to be a background star. Ehr2010
08091-3719 BRT1615 CPD-36@1978.
08091-3931 GLI 80 B is CD-39@4038.
08092+1836 SLE 466 BC: Hipparcos suspected non-single.
08094+3752 STF1184 B is BD+38@1869.
08095+3213 STF1187 Hopmann orbit rejected from Fourth Orbit Catalog Hop1971
("period over 4000 years") Wor1983
CHR 190 Aa,Ab: Four observations 1991-1996, with separation decreasing from
0.15" to 0.06"; next observed in 2004 at 0.16". Two possible orbits
are suggested: a short-period (11.3y) solution predicts a separation
of 0.074", while a long-period (28.8y) solution predicts 0.143". Hrt2009
08095-4720 DUN 65 A: gam 2 Vel. Spectrum WC8+O7.5e, probably the nearest Wolf Rayet.
B: gam 1 Vel. CD-46@3846. Variable, spectrum B1IV.
AB: Both components are spectroscopic binaries.
The AB pair was formerly known as DUN 64.
I 1175 DE: DE is I 1175 (= RST 4878) at 08 09.5 -47 25.
The Hipparcos distance suggests a position in front of the Vel OB2
association (van der Hucht et al. 1997 NewA 2, 245; Schaerer et al.
1997 ApJ 484, L153) at a distance of 258 +41/-31 pc; however, the
Hipparcos distances for the B stars in Vel OB2 (Brandt et al. 1971 ApJ
1623, L99) yield a comparable distance of 317 +/- 42 pc. This is also
consistent with the distance from the resolution of the binary by
Hanbury Brown et al. (1970) of 350 +/- 50 pc. Thus, we have chosen to HBr1970
keep gam 2 Vel as a member of Vel OB2. Classification is from van der
Hucht et al. (1997). The B component was also observed and appeared
to be single. Classifications of the B, C, and D components are from Msn1998a
Hoffleit & Warren (1991). Hof1991
TOK 2 Aa: The primary is a close WR+O binary. Although the pair is
unresolved, VLTI/AMBER observations on 2004.984 over baselines of
46-85m and wavelength range 1950-2170 nm are fit by a binary model
giving a separation of 3.65 +/- 0.06 mas, position angle 72.7 +/- 8.7
deg, flux ratio 0.62 +/- 0.04 (dm 0.52 +/- 0.07 mag. MiF2007
Intensity Interferometer Limb-darkened diameter 0.44 +/- 0.05 mas. HBr1974
08098-1658 A 3101 Spectrum: A3/5II/III.
08099-4911 SYO 3 Aka R 81.
08100-4241 CPO 195 CPD-42@2143.
08102+5548 SHY 524 AC: HIP 40006 + HIP 40536.
08102+3527 WSI 100 Provisionally designated WSI9105. Hrt2008
HJ 3308 AB: Rectilinear solution by Friedman et al. (2012). USN2012a
08102+3347 ANR 1 MLB 1049.
08102+2551 BUP 111 B is BD+26@1729.
08103-0607 GWP 984 ABL 187. Tob2012b
08104+0020 BAL1133 HJL 87. HJL1986
08105+2530 BUP 112 psi Cnc = 14 Cnc.
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
08106-1842 GWP 987 ABL 188. Tob2012b
08106-2024 ARA1030 Aka BRT1454. Dam2016b
08107-1348 LDS 204 18 Pup. NLTT 19073/19072 Chm2004
AB: Both A and B possible SBs? Tok2014d
08107-1751 GWP 989 ABL 189. Tob2012b
08110+7955 LDS1668 AB: NLTT 18931/18924 Chm2004
OSO 21 G251-054. AD is not a proper motion companion Oso2004
08113+0117 STF1198 B is BD+01@2018.
08113-1256 BU 1064 19 Pup. Not seen in 1936, 1939 B__1951a
08114-4259 HJ 4057 B is CD-42@3976.
08116+3227 CRJ 2 Aa,Ab: Primary is GJ 9256. Crepp et al. (2012) derive spectral types
G4V and M5, masses 0.85 +0.04/-0.03 and 0.16 +/- 0.02 Msun. CrJ2012
STT 564 AB and AC: Optical pairs, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
08116-0014 GWP 993 ABL 190. Tob2012b
08116-3722 JSP 236 CPD-37@1984.
08117-0636 J 2054 LAC.
08117-3209 B 2170 According to Brian Skiff, while the WDS has the correct position, this
is not CD-31 5661 (a B giant), but instead is CPD-31 2177 an F/G pair.
Appears to be an IDS error. Skf2003
08118-0717 GWP 994 ABL 191. Tob2012b
08118-3521 J 2301 Nova Puppis = PK 252-00.1 = CP Pup. J__1962a
08121-1540 HJ 4050 B is BD-15@2309, spectrum A9/F0V.
08122+1739 STF1196 zet Cnc = Tegmine. Reductions of measures in position angle
untrustworthy because of confusion among the eithr position angles of
minimum visibility. Distance too great for interferometer measures. WRH1941a
AB: H 1 24. MEv2010
AB: Additional notes may be found in Burnham (1894), Bu_1894
Simonov (1937), and Smw1937
Muller (1955). Mlr1955c
AB,C: H 3 19. MEv2010
AB,C: 2-orbit AB,Cc quadruple solution (AB,C in HIP). Sod1999
AC: Additional notes may be found in Vyssotsky (1936), Vys1936
Simonov (1937), and Smw1937
Simonov (1951). Smw1951
AB,D: D is BD+18@1870.
The system Cc has been resolved by infrared speckle interferometry. Mcy1983
Typographical error in the Mason et al. (2006) published elements: WSI2006b
omega = 330.2 +/- 6.7, not 6.7 +/- 1.2.
zet 1 Cnc B This object was misidentified as HR 3210 by McAlister (1978). McA1978c
08122-0150 J 421 The note in ADS says that the 1906 measures by Morgan, attributed to A__1932a
HJ 778, may belong to this pair. Mrg1907
08124-0059 GWP 995 ABL 192. Tob2012b
08125-1502 GWP 996 ABL 193. Tob2012b
08125-4616 CHR 143 Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 27.06 +/- 23.28, 9.94, 4.79 Msun, respectively. Mlk2012
08129+1044 BPM 436 [PM2000] 865688 + [PM2000] 865603. Gvr2010
08129-0733 LDS5175 LDS6213.
08130+5026 GRV1004 SLW 226.
08130-5402 HJ 4065 B is CPD-53@1569.
08131-3435 EVS 13 Primary is the Cepheid RS Pup. Evs2016a
08132-1227 J 1510 BRT 2703.
08132-1354 HU 115 Present parallax value adopted instead of poor HIP-value. Sod1999
See Baize & Petit (1989) catalog of doubles with variable component. Baz1989d
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.46 +/- 0.62, 1.20, and 0.55 Msun, respectively. Mlk2012
08136+1527 CLZ 43 Aka FMR 204.
08136-0545 HJ 2435 AB: HDO 117
AB: H 2 87. MEv2010
08136-3144 HDO 201 B is below MS, not CPM (NOMAD, WDS). C is below MS, optical. Tok2014d
08136-4700 GLI 87 A is variable. B is CD-46@3928.
08137+0407 ARG 68 A is +04 1934b while B is +04 1934a.
08138-2206 LDS 207 CPD-21@3323.
NLTT 19163/19166 Chm2004
08138-3444 I 193 For the 1997.1201 measure a smaller annulus was used in the power
spectrum fit due to the faintness of the source. As a consequence, the
separation and position angle uncertainties may be larger than other
measures. Hor1997
08140-3619 DUN 67 Variable, OS Pup. B is CD-35@4360.
320 Arg. dRA 1.2s, dDEC 1' 12.3". Four stars forming a parallelogram
(with DUN 68, dRA 3.3s, dDEC 1' 41.0", mags 7,7). Dun1829
08140-4021 HJ 4062 The primary is a long-period spectroscopic binary.
h 2 Pup Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Christie (1936). Crs1936
08142+1741 H 6 78 AC: H VI 78.
SKF1627 DE: Primary of 08140+1744 found to be D component of 08142+1741.
08142-3208 HJ 4059 A is a spectroscopic binary.
08143-3129 B 1592 Spectrum: A1/2III/IV.
08147-6616 HJ 4075 SWR 41. CPM pair Skf2004
08149-0001 J 72 J 1511. J__1962a
08149+1058 BPM 437 [PM2000] 868831 + [PM2000] 868623. Gvr2010
08149-0120 J 2055 +1s, +1.5' from BD-00 1945. Companion variable. J__1955
08153-1126 J 2875 BRT 2704.
08153-6255 RMK 8 Rectilinear solution by Letchford et al. (2018). Whi2018
08155+0202 DOB 9 BAL 1840.
08155-3722 HJ 4063 B is CD-36@4387.
08156+1126 LEP 30 NI 18.
08157+0738 STF1209 B is BD+08@2015.
08158+0550 ADM 3 WSP 51. HTP 30. HAT-P-30. Primary is exoplanet host star. Adm2013
08159+5047 STF1199 Opik reverses quadrant.
08159-3056 BU 454 Spectrum composite; G5-8III+G:.
08159-6252 HJ 4077 B is CPD-62@987.
08161+5706 ENG 34 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
GIC 79 AD: LDS2568. AD = G194-017/G194-018.
ENG 34 AB: Rectilinear solution by Hurowitz et al. (2014). USN2014a
08161+1942 LDS3781 G040-014. See Allen et al. (2000) for information on metallicity, AlC2000
age, galactic orbital parameters, etc.
NLTT 19210/19207 Chm2004
08161-2847 HLD 95 Spectrum: A2/3III/IV.
08164-0314 HWE 21 A 29d spectroscopic solution for the A component has been found making Tok2019g
this a triple system.
08165+7930 STF1169 HJL 88. HJL1986
AB: A is SB1, P=4.884d Tok2014d
08165+0911 BU 1065 bet Cnc = 17 Cnc. Burnham measured BD+09@1922 and BD+09@1926 with A__1932a
respect to A. A may be variable.
Mk III Limb-darkened diameter 5.20 +/- 0.07 mas MkT2001
Mk III Limb-darkened diameter 5.238 +/- 0.069 mas. MkT2003
NPOI Limb-darkened diameter 5.03 +/- 0.04 mas, NOI1999
R = 48. +/- 4. \rsun.
NPOI Limb-darkened diameter 5.13 +/- 0.06 mas. NOI2001b
NPOI Limb-darkened diameter 5.167 +/- 0.035 mas, Sp = K4III, NOI2018
R = 51.66 +/- 0.98 \rsun, Teff = 4094 +/- 53 K,
L = 676.7 +/-41.4 \lsun, M = 1.75 +/- 0.11 \msun,
Age = 1.49 +/- 0.22 Gyr.
08167+3216 ES 293 SEI 489. Nsn2017b
08167+0113 OL 179 Aka HEI 344.
08166-7914 HJ 4105 SWR 42.
08169+5503 LDS3780 BC: SLW 231.
08169+3331 SEI 490 None of the components seen on POSS plate; may be flaws on AC Potsdam
plate.
SEI 491 AC. See note to SEI 490.
08170+5911 STT 565 B is BD+59@1153.
08170+0001 CHM 5 NLTT 19241 + 19240.
08172+3515 BRT3250 ALI 120.
08173-0522 A 337 Only elements P and T have been amended from the orbit of Sta1977a
Baize (1959). Baz1959
08174-1125 BRT2708 J 1513.
08175+3623 GRV 756 HJL 89. HJL1986
08178+3738 BRT2219 ALI 587. Heintz describes this as identical to PTT 20. Hei1985a
08178-1927 LDS 211 = GWP1002 = ABL 194. Tob2012b
08178-6128 HRG 14 Aka HDS1179.
08179+0628 STF1213 BDS 4546, HJ 87 probably same star.
08179-5910 HJ 4084 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AB: Rectilinear solution by Hurowitz et al. (2014). USN2014a
08180-0022 GAU 11 BAL 850.
08182-3722 HJ 4073 A is a spectroscopic binary.
08183+3859 STF1211 AD: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
08184-0803 GWP1003 AB: ABL 195AB. Tob2012b
GWP1004 AC: ABL 195AC. Tob2012b
08184-2017 HJ 2441 A component is close double of spectral types A5III+G0III,
C component is also a close double of types A0-2III+K0III AbH2000
08185-0616 GWP1006 ABL 196. Tob2012b
08186-0554 GIC 71 G113-026/G113-027. LDS6214. A 1-hour error in transcribing coordinates
led to an incorrect WDS designation for this system of 07185-0550.
It is assumed that Giclas' original value for theta (28deg) was due to
a math error, so it was corrected to 180-28=152deg.
NLTT 19298/19299 Chm2004
08186-4254 CPO 198 CPD-42@2341.
08187-2033 RSS 154 CPD-20@3578
08187-3407 RST2547 CPD-33@2077.
08188+6806 LDS2571 NLTT 19229/19230 Chm2004
08189-3142 PRO 51 Aka TDS5709.
08190+4927 HU 1124 AB: Rectilinear solution by Hurowitz et al. (2014). USN2014a
08190-7330 HJ 4095 AC = SWR 44. Brightest two stars in a 1' group. Skf2004
08191+1607 BPM 438 [PM2000] 875251 + [PM2000] 875178. Gvr2010
08193+6230 OS UMa Ren & Fu (2013) calculated an astrometric orbit, combining Hipparcos Ren2013
Intermediate Astrometric Data with spectroscopic elements by
Carquillat et al. (1983). Crq1983
08193-0537 TOK 121 HIP 40765. Small PM(A)=(-1,+42). NOMAD: PM(B)=(+66,-16), V(B)=12.83.
B can be optical (crowded field, N*=42). Tok2011a
08194-3807 JSP 260 CPD-37@2202.
08195+3503 STTA 91 B is BD+35@1801.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
08198-7131 BSO 17 A: kap 1 Vol. A is a spectroscopic binary.
B: kap 2 Vol
08199-2418 B 152 HDO 114.
08200-5740 CPO 200 B is CPD-57@1483.
08201+3834 GIC 80 G111-072/G111-071.
NLTT 19314/19311 Chm2004
08202-5642 SWR 43 CPM pair Skf2004
08206-7729 I 799 the Cha
08207-0001 SLW 241 ABL 197. GWP1007. Tob2012b
08211+6527 SHY 199 HIP 40918 + HIP 40882.
AB: A is SB1, P=17.6y; suspected non-single star in Hipparcos Tok2014d
08211+4725 STT 190 A,Ca: AB,Ca may be a quadruple system, as the proper motions are in
fair agreement..
AB (mag. 8.6-12.0, 4") is HU 224, 39" distant.
AD: D is BD+47@1565.
STT 190 AC: HJL 90. HJL1986
08211+1552 BPM 439 [PM2000] 878193 + [PM2000] 878305. Gvr2010
08213+3419 LEP 31 NI 19.
BVD 161 AD: X-ray aRX J0821.3+3418 and 2MASS at 5" from A, is it D? Tok2014d
08213-0136 STF1216 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 8.24 +/- 5.59, 4.58, and 2.09 Msun, respectively. Mlk2012
08214-3545 BRT1623 CPD-35@2261.
08214-3629 HJ 4085 A is a spectroscopic binary.
08217+1717 PAR 1 A is the Mira-type variable V Cnc.
08217+1048 BPM 440 [PM2000] 879031 + [PM2000] 878978. Gvr2010
08217-5841 LDS 216 LDS5695.
08221-7324 HJ 4103 eta Vol
08223+1558 BPM 441 [PM2000] 879905 + [PM2000] 879851. Gvr2010
08223-3458 BRT1625 CPD-34@2328.
08225+2638 BUP9115 See note to 08231+2648 BUP 115.
08225-2942 B 1600 Spectrum: Fm Delta Del.
08225-4829 I 67 B Vel
08225-5931 HDS1190 = eps Car = Avior
08228-2621 B 767 Many negative or uncertain observations.
08228-5727 BRG 27 Aa,Ab: As noted in Bergfors et al (2010), this is a triple system with Brg2010
component B outside of 6". Hence, we do not include component B in
Table 4, but we note that at 8.429+/-0.001" separation in 2008.88 and
8.374+/-0.003" in 2010.09, there is statistically significant orbital
motion also for this component. Jnn2012
08228-7626 HJ 4109 B is CPD-76@515.
08229-5207 SHY 525 HIP 41081 + HIP 40916.
08231+2648 BUP 115 The IDS incorrectly associated this pair with BD+28 1598, rather than
+27 1602. As a result, it was initially assumed to be a member of a
quadruple system with two other pairs in the IDS. Eventually all were
assigned the discoverer designation BUP 115 and component designations
AB, AC, and CD. However, the two A components differ in precise
position by some 12.8 arcminutes. They were later assigned different
WDS designations but discoverer and component designations were not
corrected. The AC and CD pairs have now been assigned the designation
BUP9115, with component designations AB and BC.
08231-4912 DENIS-P... DENIS-P J082303.1-491201 is an L1.5 dwarf at 20.77 +/- 0.08 pc.
Observations with FORS2 on the VLT reveal an astrometric companion in
an eccentric orbit with period 246.4 +/- 1.4 days. Masses of the
primary and secondary are estimated at 78.4 +/- 7.8 and 28.5 +/- 1.9
Mjup for an age of 1 Gyr, or 70.2-82.8 and 26.7-29.4 Mjup for ages
0.6-3 Gyr. SaJ2013
Sahlmann et al. (2015) refine the orbit of this juvenile binary brown
dwarf, deriving spectral types L1.5 +/- 0.6 and L5.5 +/- 1.1, Teff =
2150 +/- 100 and 1670 +/ 140K, log (Lbol/Lsun) = -3.73 +/- 0.08 and
-4.25 +/- 0.20, masses 0.028-0.063 and 0.018-0.045 Msun (mass ratio
0.64-0.74), delta I = 2.3 +/- 1.2 mag. The distance is 20.7pc, the age
estimated to be in the range 80-500 Myr. SaJ2015b
08234-1016 GWP1010 ABL 198. Tob2012b
08234-1115 J 2878 BRT 2709.
08234-2207 BRT1457 CPD-21@3515.
08234-2310 BRT1458 CD-22@6089.
08234-4248 HJ 4090 B is CD-42@4188.
08235+1434 LDS1210 NLTT 19425/19426 Chm2004
08236-1920 GWP1011 ABL 199. Tob2012b
08237-1150 GWP1012 ABL 200. Tob2012b
08237-2137 B 2654 J 1517. Nsn2016
08237-5519 SHY 526 HIP 41147 + HIP 41579.
08238+5725 STTA 92 B is BD+57@1136.
AB: HJL 91. HJL1986
08239+1038 A 2961 21 Cnc.
08240-1548 RST4396 A 25d spectroscopic solution for the A component has been found Tok2019g
making this a triple system.
08242-0150 GWP1014 ABL 201. Tob2012b
08243+4457 STF1217 LDS 904. B is BD+45@1575.
NLTT 19431/19428 Chm2004
HJL 92. HJL1986
08243-0424 GWP1015 ABL 202. Tob2012b
08244-0432 GWP1016 AC: ABL 203. Tob2012b
08243-0432 and 08244-0431 found to share primary. Systems merged.
08244-4601 CPO 204 CPD-45@2479.
08245-3039 HJ 2446 B is CD-30@6203.
08246-0109 B 2527 FIN measures 1951-1959 distance less than 0.1".
AB pair bound; change in separation and angle consistent with orbital
motion. B component likely M2-M5 dwarf with mass 0.24 +/- 0.01 Msun.
C and D components likely unrelated. Egn2007
AB: Likely a spurious pair. Last measured 1961 and unresolved by SOAR
on 3 occasions 2010–2013. Tok201
AB: Tentative resolution by Finsen, 1 speckle measure at 0.040" in
2001.08, unresolved by Hipparcos, 3 non-resolutions by SOAR 2010-2013.
AB can be "ghost". Tok2014d
EGN 27 AE: E companion was not detected by RoboAO in 2013.05, below limit. Tok2014d
08246-0345 CHR 172 Aa,Ab. Abt & Biggs (1972) note variable RV. AbH1972
Aa,Ab: Likely a spurious pair. Last measured 1988 and unresolved by
SOAR on 3 occasions 2011–2013. Tok201
TOK 20 AB: GJ 306. AB has estimated period 23,000y; Close triple? Tok2006
AB: A is SB, P=1.563d. Tok2014d
08247+4200 S 565 STTA 93. B is BD+42@1860.
08247-2849 RST1393 A is an Algol-type system, AW Pup.
08248+2009 STT 191 B is BD+20@2078.
08249+1214 BPM 442 [PM2000] 883581 + [PM2000] 883518. Gvr2010
08249-4418 DAW 194 Turner (1979 A&A 76, 350) includes this star in the Vel OB1 group at a
distance of 1.8 kpc. Photometric spectral classifications of the B and
C components are from Lindroos (1985), who also finds a Lnd1985
distance of 2.7 kpc. Msn1998a