22000-3039 BUG 6 DENIS J220002.05-303832.9
Serendipitously discovered with SpeX near-IR imager/spectrograph.
Spectral types M9 + L0, masses 0.072-0.085 and 0.069-0.083 Msun. Bug2006b
22001+2909 BRT 60 The pair MLB 496 is identical Hei1980a
22002+0822 OSO 165 G018-012. Not a common proper motion pair, based on color Oso2004
22003-0724 LDS4935 NLTT 52648/52649 Chm2004
22007-5002 I 1450 Heintz (1984) value of omega was corrected from 313.5 to 133.5 Hei1984a
degrees by Ruymaekers & Nys (1985). Ruy1995
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 8.36 +/- 8.51, 1.75, and 1.05 Msun, respectively. Mlk2012
Gomez et al. (2016) derive dynamical parallax and component masses:
14.88 +/- 0.61 mas, 0.825 +/- 0.016 Msun, 0.778 +/- 0.015 Msun. Doc2016i
22008-2827 BU 276 eta PsA = 12 PsA. Bidelman calls A a spectroscopic binary, and says a
1972 plate shows a fairly strong H-alpha self-reversal.
22010+1626 BPM2418 [PM2000] 2554557 + [PM2000] 2554441. Gvr2010
22010+1116 BPM2419 [PM2000] 2554645 + [PM2000] 2554572. Gvr2010
22011+3915 A 1451 Usually too close for visual measures. Needs speckle.
AB,C: Possibly a 30" error in the declination of the secondary led to Sei1908
the erroneous 1894 Scheiner (1908) and WFC measures. WFC1998
22011+1307 HJ 289 20 Peg.
22013+4621 HJ 1714 B is BD+45@3762.
22015+0310 J 1726 BAL 2060.
22015-1537 HWE 59 The fainter star is apparently BD-16@5997.
22016+4921 ES 831 AD: Rectilinear solution by Hartkopf & Mason (2015). WSI2015
AE: Rectilinear solution by Hurowitz et al. (2014). USN2014b
22017-0925 JNN 135 The two components of the 2MASS J22014336-0925139 system that have
been resolved with AstraLux have very similar brightnesses and colors,
and it is therefore likely that they form a physical binary pair.
Common proper motion has not yet been demonstrated. Jnn2012
22017-1200 STF2851 Spectrum: G8/K0III/IV. B is BD-12@6153.
22018-0952 RST4095 Position angles discordant in 1950. 220@, 5 nights.
22019+5506 HJ 1718 AB: HJ 1719 = STI2607. Burnham's note for HJ 1719 quotes Herschel as Bu_1906
mentioning "a third star 12m from B, 4arcsec; also a fourth." Burnham
also says "The other stars referred to are 12.5m, 268.2deg:
15.9arcsec; and 12.0m, 145.4deg: 30.9arcsec." These appear to match
the BC, AC, and AE pairs in the HJ 1718 mutiple system. We therefore
conclude that HJ 1719AB and HJ 1718AB are the same pair.
22019+1407 BPM2420 [PM2000] 2555948 + [PM2000] 2555937. Gvr2010
22019+0446 STTA228 AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
22021+5800 TRN 34 14 Cep = LZ Cep.
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
The classification is from Conti & Alschuler (1971). Radial velocity Cti1971
and light curve solutions are given by Harries et al. (1998 MNRAS 295,
386). Msn1998a
22024-1658 S 802 29 Aqr. A is the Beta Lyrae-type system DX Aqr.
A orange, B white. The spectral type A2 given in the ADS must be the
companion's. B__1963a
22025-7719 SHY 786 BC: HIP 108799 + HIP 103587.
22027+1110 BPM2421 [PM2000] 2557008 + [PM2000] 2557200. Gvr2010
22028+1207 GIC 174 G018-017/G018-018.
NLTT 52768/52770 Chm2004
22029+4439 BU 694 A is variable, V1942 Cyg.
22029+1547 HDS3129 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.67 +/- 0.75, 2.80, and 1.25 Msun, respectively. Mlk2012
22029+1511 BPM2422 [PM2000] 2557327 + [PM2000] 2557452. Gvr2010
22031-7607 HJ 5306 A is a spectroscopic binary.
22032+5937 WNO 48 BC: Identified as WNO 18 in USN1976.
22032+0157 ARG 96 BAL 1594.
HJL 299. HJL1986
22032-0113 OSO 166 G027-008.
LDS4938 AB: NLTT 52787/52786 Chm2004
22033+5944 STI1083 Also known as SMA 160.
22033-4816 CPO 90 Aka SKF1179. Dam2015b
22034+3634 DAM 662 Identified by Damm as ALI 450, but apparently a different system. Dam2013
22034-5647 VLK 1 Ba,Bb: eps Ind. Cardoso et al. (2009) derive a system mass of
0.116 +/- 0.001 Msun = 121 +/- 1 Mjup for this pair of T dwarfs. Mcg2009
VLTI uniform disk diameter of A: 1.834 +/- 0.016 mas, LTI2009
VLTI limb-darkened disk diameter of A: 1.881 +/- 0.017 mas,
R = 0.732 +/- 0.006 \rsun, Teff = 4568 +/- 59 K,
M = 0.762 +/- 0.038 \msun.
Mass for Ba & Bb : 75.0 +/- 0.82 and 70.1 +/- 0.68 \mjup. Die2018
Teff for Ba & Bb : 1320 and 910 K.
The orbital parallax is 276.88 +/- 0.81 mas.
22035+4841 ES 530 Includes V394 Lac, a Beta Lyr type eclipsing binary, P = 1.65000d. Zas2012
22035+0340 JNN 293 Estimated age 1000-10000 Myr; masses 0.24 +/- 0.10 and 0.13 +/- 0.04
Msun; a ~6.8 au. Jnn2014
22036+1108 BPM2423 [PM2000] 2558304 + [PM2000] 2558485. Gvr2010
22037+0318 HJ 952 BAL 2062.
22038+6438 MCA 69 xi Cep = 17 Cep = Kurhah
Aa,Ab is an astrometric binary and SB2, with elements by Vickers & Scf1976
Combined solution by Farrington et al. (2014) yields masses 1.045 +/-
0.032 and 0.409 +/- 0.066 Msun, as well as an orbital parallax 38.11
+/- 2.82 mas. CIA2014a
STF2863 Scarfe (1976). The McAlister (1980) orbit is from speckle McA1980a
xi Cep interferometry, and in good agreement with the spectroscopic result.
Mt. Wilson spectrum of B F8s. Spectrum of A: A3m.
Pourbaix gives combined solution for this resolved SB2, yielding Pbx2000b
orbital parallaxes and component masses.
STF2863 AB: H 2 16. MEv2010
22039+5949 STT 461 15 Cep. STTA229.
EF: F is BD+59@2463.
E comp is V442 Cep, a Beta Lyr type eclipsing binary, P = 2.12919d. Zas2012
22039+2406 J 1246AB POU5624.
22039-2451 LDS6378 AC: 22039-2451 found to be same system as 22038-2450. LDS4939AB merged
with LDS6378AC, LDS4939AC changed to AD.
22041+7328 MLR 255 No significant movement since first resolution. Drd2009
22042+3804 FYM 296 Aka CVE 13.
22042+3507 SEI1554 A is the Mira-type variable RT Peg.
22043+1720 BPM2424 [PM2000] 2559313 + [PM2000] 2559495. Gvr2010
22044+2500 POU5629 LDS1488.
22045+2915 GRV 539 AC: Also known as GRV 538AB.
22045+1551 BU 696 AC and AE: Optical pairs, based on study of relative motion of the
components using the method of apparent motion parameters. Kiy2008
CE: The previous AD pair was determined to actually be CE by Arnold. Arn2008a
22046+3854 SEI1556 ALI 983.
22046+1122 OSO 167 G018-021. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
22048+3637 ALI 450 No star seen at AC catalog location of the purported secondary
- probably a plate flaw. Triple identified by Damm as matching ALI 450 Dam2013
moved to 22034+3634.
22049+2158 GAU 18 Measured for HJ 3089 which Gauchet could not find. Gau1926a
22050+1223 BPM2425 [PM2000] 2560281 + [PM2000] 2560265. Gvr2010
22050+1130 HJ 290 Erroneously merged with 22050+1128HJ 291. Corrected. Cur2018
22050+0838 OSO 168 G018-024. AB is not a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
LDS4942 See Allen et al. (2000) for information on metallicity, age, AlC2000
galactic orbital parameters, etc.
22051+6217 BU 697 19 Cep.
TRN 35 AD and AE: The image rotator was in an unknown state, so two possible
theta values are listed for the 2001.7367 observation - one for
zenith up and one for north up. Trn2008
22052+5502 STI2612 Primary appears to be typos or plate flaw in AC catalog.
22052+4403 HJ 1723 AB: Also known as LYS 19 and FAL 73.
22053-0125 STF2855 B is BD-02@5688.
22056+3620 TOB 224 Two 2010 measures of SEI1558 by Azcona et al. (2011) were actually of
this pair. SDA2011
22057+1223 HIP 109067 NLTT 52896. The 4.6 yr SB1 with estimated q > 0.23 and axis 53 mas is
below the NICI detection limit. This is a sub-dwarf with large PM,
below the main sequence. Tok2012a
22058+3618 SEI1558 Secondary not seen on Aladin; apparently either a typographical error
or a plate flaw in the AC Catalog.
22058+3059 ES 2361 SMA.
22058+0452 STF2856 BDS 11412 probably same star with error in position.
WHC 25.
22058-0019 BUP 232 alp Aqr = 34 Aqr = Sadalmelik
Mk III Limb-darkened diameter 3.20 +/- 0.05 mas. MkT2001
Mk III Limb-darkened diameter 3.237 +/- 0.057 mas. MkT2003
NPOI Limb-darkened diameter 3.08 +/- 0.03 mas, NOI1999
R = 77. +/- 15. \rsun.
NPOI Limb-darkened diameter 3.11 +/- 0.04 mas. NOI2001b
Common proper motion pair with 21316-0534 = bet Aqr. Skf2013
22059+4135 ES 1586 Aka DOO 90. Dam2016b
22059+3330 PLT 7 A is RZ Peg, B is RY Peg. Plt1934
22059-1155 WNO 57 GJ 4254 + LP 759-25. CPM pair. Mkr2008
22061+4159 A 407 An 11th magnitude star at 058@, 13".
22061+1623 BPM2426 [PM2000] 2561783 + [PM2000] 2561926. Gvr2010
22061-0521 TOK 373 SB with preliminary 13y period (CfA) and expected semi-major axis of
0".19 is tentatively resolved here for the first time at 0".07 and
dK=1.7. Strangely, it was not resolved previously be speckle or AO.
This is the young BY Dra variable NT Aqr and an X-ray source. Tok2013b
22064-2047 CLO 3 Assuming a parallactic distance of 26.67 +/- 2.63 pc (Costa et al. Jao2006
2006), Konopacky et al. (2010) derive system mass 0.16 +/- 0.05 Msun. Kon2010
Dupuy et al. (2009) also reprocessed the HST/WFPC2 data originally
published by Bouy et al. (2003), as well as the Gemini/Hokupa'a data Boy2003
originally published by Close et al. (2002). From their orbital Clo2002a
solution they derive a total system mass of 0.15 +0.05/-0.03 Msun.
Spectral types appear to be M8.0 +/- 0.5 for both components. Distance
is estimated at 26.7 +2.6/-2.1 pc. Dup2009b
22066+1416 HEI 293 TDT3346.
22067-4913 RSS 566 Also known as ENO 7.
22068+7058 HJ 3096 LDS1968.
22068+1444 BPM2427 [PM2000] 2562714 + [PM2000] 2562648. Gvr2010
22069+6405 WYL 1 Not found by Heintz at 22093+6401. This has been equated with TDT3347. Hei1987a
22069+4752 ES 2715 B is BD+47@3694.
22069+1807 BPM2429 [PM2000] 2562935 + [PM2000] 2563110. Gvr2010
22069+1313 BPM2428 [PM2000] 2562917 + [PM2000] 2562751. Gvr2010
22070+5930 OSO 169 G232-056. None is a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
22070+2521 STT 596 iot Peg = 24 Peg. The primary is a spectroscopic binary.
Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
PTI 1 SB2. Combined solution by Boden et al. (1999), including visibilities Bod1999a
from the Palomar Testbed Interferometer, plus spectroscopy. Authors
give two very similar solutions, made using two data sets. Values were
averaged in the orbit catalog.
See also discussion of iot Peg system by Morel et al. (2000). Mrl2000
Combined spectroscopic/astrometric solution, based on high-resolution
echelle spectra plus archival PTI visibility measurements.
Derived masses 1.33249 +/- 0.00086 and 0.83050 +/-0.00055 Msun,
distance 11.534 +/- 0.019 pc. Knc2010
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.27 +/- 4.55, 2.36, and 1.20 Msun, respectively. Mlk2012
22071-5908 HJ 5316 Spectrum: G8/K1V+F/G.
A=SB? No SB orbit. B at 3.3" is above MS, suspicious ptm in 2MASS. Tok2014d
22072+3555 SEI1559 ALI 223. GYL 94.
22075+3841 MLB 792 J 3158.
22075+2538 A 308 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.93 +/- 2.45, 3.66, and 2.09 Msun, respectively. Mlk2012
22077+0913 HJ 3090 J 1792. Not found by Heintz at IDS position. Hei1990b
22082+2921 ALP 27 2MASSW J2208136+292121
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in August 2002. AlP2007
22082+1645 BPM2430 [PM2000] 2564634 + [PM2000] 2564663. Gvr2010
22082-4658 RST5483 alp Gru = Alnair. Not seen by Holden on four nights 1963-1969.
Intensity Interferometer Limb-darkened diameter 1.02 +/- 0.07 mas. HBr1974
22083+4913 ES 685 Primary is V401 Lac, an Algol-type eclipsing binary, P = 1.95012d. Zas2012
22083+2409 HDS3145 Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.58 +/- 0.33, 2.86, and 1.00 Msun, respectively. Mlk2012
22086+5917 STF2872 A,BC: H 4 126. MEv2010
22088-2546 SEE 469 Previously known as HDS3147. Pair included in the BDS but Bu_1906
removed from the ADS and IDS. It matches the HDS observation A__1932a
quite well. IDS1963
22089+1539 BPM2431 [PM2000] 2565599 + [PM2000] 2565465. Gvr2010
22091-1831 BU 170 The wide pair in the field nf is HJ 3092. Bu_1906
22092+3310 BU 1511 pi 1 Peg = 27 Peg
22093+6401 FOX 44 Aka TDT3369.
22093+4451 HJ 1735 Primary is V402 Lac, an eccentric Algol-type eclipsing binary, period
3.78202d. B is BD+44@4060. Zas2011
22093+1142 OSO 170 G126-056. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
22093-0755 KUI 111 LDS4947. NLTT 53061/53062 Chm2004
22093-1859 HU 284 This is identical with HU, BDS 11518. Doo1915a
22094+1730 BPM2432 [PM2000] 2566327 + [PM2000] 2566245. Gvr2010
22095+0542 HWE 61 BDS 11521. BU 842.
22095-0733 GJ 9769 Combined solution, based on reduction of Hipparcos intermediate
astrometric data together with spectroscopic elements from Marcy CPS1999a
et al. (1999). HaI2001
22095-1827 HJ 3092 B is BD-19@6231, spectrum A8/F0V.
22100+1346 OL 222 OL 194.
22102+6811 MLB 370 MLR 104.
22102+0255 HJ 957 Aka BAL2063.
22103+0137 HJ 5526 BAL 1597.
22104+1925 BRT2527 J 2364. J__1962a
22104-0108 J 1727 BAL 628.
22104-5158 TOK 216 Possibly triple. The 1".4 companion found with NICI cannot explain the
RV variability and acceleration. Tok2012a
22105+1228 BPM2433 [PM2000] 2567677 + [PM2000] 2567773. Gvr2010
22106+7008 STF2883 HJL 301. HJL1986
H N 121. MEv2010
22107+3322 GYL 73 TOB 226. No sign of a 5.9" pair, although AC2000 shows coordinates
corresponding to this value. Apparently this is due to an error in the
catalog coordinate, as the true declination of the B component is ~15"
due north of the AC2000 coordinates for B.
22108+2151 J 2365 BRT 2528.
22109+5757 BU 436 Hough suspected a close companion, not confirmed.
22111+1624 BPM2434 [PM2000] 2568540 + [PM2000] 2568461. Gvr2010
22112+5049 HJ 1741 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
22115+5925 lam Cep Radial velocities are also discussed by Gies & Bolton (1986) and Gie1986
Underhill (1995 ApJS 100, 433). Msn1998a
22115+1806 CHR 119 Ross 270, G126-62.
OSO 171 G126-062. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
22115+1731 HD210647 Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Griffin (1984). Grf1984b
22115-0114 BAL 629 Also known as STF2871.
22116+2716 HO 289 CD of ADS should probably read BD.
22116+1803 OSO 172 G126-063. Neither is a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
22116-3428 CHR 230 Aa,Ab: This new component to the visual pair Bu 769 has moved through
more than 4 deg in about 10 months, implying a period of order 60 - 70
years. The wide pair has shown essentially no change since its Bu_1887
discovery by Burnham in 1879, on the other hand. Hrt1996b
22117+0612 OSO 173 G018-035. AC is not a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
22117-5850 HJ 5317 B is CPD-59@7774.
22118+5944 STF2880 STT 466.
H 1 49. MEv2010
22118+5650 GIC 176 The C component is G233-002.
22119+6342 STI1097 Appears to be identical with 22122+6344 BU 1512. measures merged.
Farman notes a 13th magnitude star in 355@. Frm1907
22120+3739 STF2876 Same as STF2864.
22121+1245 BPM2435 [PM2000] 2569827 + [PM2000] 2569969. Gvr2010
22122+5909 MLR 439 No significant movement since first resolution. Drd2009
22125+1749 BPMA255 [PM2000] 2570388 + [PM2000] 2570558. Gvr2010
22126+5253 ES 146 Identical with ROE 93. Heintz confirms the BD identity. Hei1983a
A measure 1902.89 is contained in a letter from Espin to Roe. The Es_1903
measure in BDS evidently belongs to another pair.
22129+7318 STF2893 Spectrum composite; K0II-III+A3V.
H 4 82. MEv2010
22129+4555 BUR 1 Measured by Burling (2005) on DSS plate and incorrectly identified as Bur2005
HJ 1723.
22130-4733 CPO 630 LDS 775.
22132+2148 HJ 958 HJL 302. HJL1986
22132-1111 BU 1215 EPIC 206135267. Primary is eclipsing binary, period 2.533d. SJR2016
22133+2352 HJ 1744 POU 5668.
22137+5636 SMA 162 Also known as STI2651.
22138+2445 POU5671 J 2705.
22138-0627 LDS4949 NLTT 53254/53255 Chm2004
22139+3943 MCA 70 A is a spectroscopic binary. Uncertain whether MCA pair is the same.
22139+1519 BPM2436 [PM2000] 2572221 + [PM2000] 2572211. Gvr2010
22143+1711 STF2877 AB: An optical pair. Measures of the BD WFC1998
pair from Urban et al., Burnham, Abetti, Bu_1913
Opik, and 2MASS were originally Abt1922
erroneously labelled as measures of the Opi1932
BC pair. TMA2003
22143-1109 BRT2792 J 3239.
22143-2104 H N 56 41 Aqr. Spectrum composite; K0III+F2V.
22144-0845 OSO 174 LHS 3780. Not a common proper motion pair, based on comparison with
POSS2 red plates. Oso2004
22146+1728 BPM2437 [PM2000] 2573096 + [PM2000] 2573005. Gvr2010
22147+1249 BPM2438 [PM2000] 2573244 + [PM2000] 2573421. Gvr2010
22150+5703 ENG 84 23 Cep = eps Cep. A is a Delta Scuti-type variable.
B is BD+56@2744.
AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
MWT 1 Aa,Ab: Candidate close companion to eps Cep is estimated to be of
spectral type K8-M2, mass ~0.5 Msun, radius ~0.7 Rsun, temperature 3
650K, age ~600 Myr. Distance from the primary >= 8.6au. Mwt2011
22151+3500 RAO 476 pa error = 348 deg. RAO2020b
22152-0535 A 2599 The close pair previously cataloged as MSN 1 was an error. This was
verified by the null detection of Hartkopf et al. and reinspection of Hrt2009
the original data. Msn1996b
22154+5104 ES 1113 Also known as WFC 239.
22155+3450 ES 214 Also known as J 3317.
22156+3811 ES 2530 Also known as ALI 700.
22156-4121 CHR 187 Abt & Biggs (1972) note variable RV. AbH1972
22157-1809 LDS4950 NLTT 53321/53320 Chm2004
22158+4354 POP 23 Erroneously listed as companions to 22156+4352COU1981 = BD+43 4164 Pal2005c
rather than +43 4165.
22159+5440 BU 377 AB: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AQ = BU 377Ab.
GIC 177 AT = G232-061/G232-062 = GJ 4268A+4269B.
BU 377 AC, AD: Rectilinear solutions by Friedman et al. (2011). USN2011a
22159+3125 BU 477 HJL 303. HJL1986
22161+3521 J 1211 Van Biesbroeck corrects the position by reference to BD+34@4642. VBs1954
22161-0705 HDS3158 Cvetkovic et al. (2014) derive spectral types G4 and K3, masses 1.07
and 0.79 Msun. Dynamical parallax is 17.56 +/- 0.44 mas. Cve2014
A 111.1d spectroscopic solution for the B component has been found Tok2018d
making this a triple system.
Synthetic Spectrum gives Bt mags of 12.19 & 14.02 for Ba,Bb and 11.12 Mda2019
and 12.67 for Vt. The solution for the three components A, Ba and Bb
Teff = 5836 +/- 80, 5115 +/- 80, and 4500 +/- 80, degrees Kelvin,
R = 1.09 +/- 0.039, 0.596 +/- 0.05, and 0.49 +/- 0.06, \rsun,
L = 1.24 +/- 0.10, 0.22 +/- 0.09, and 0.09 +/- 0.05, \lsun,
M = 1.05 +/- 0.16, 0.83 +/- 0.16, and 0.67 +/- 0.16, \msun.
22162+4229 COU1830 TDT3433.
22162+1145 BPM2439 [PM2000] 2575225 + [PM2000] 2575139. Gvr2010
22163+1736 BPM2440 [PM2000] 2575257 + [PM2000] 2575213. Gvr2010
22164+7321 LDS1975 NLTT 53440/53441.
22165+3708 SEI1561 ID uncertain - no sign of SEI pair, and ALADIN only indicates one
Astrographic Catalog star in vicinity of Scheiner's coordinates.
22166+0147 HJ 3102 BAL 1598.
22166-5543 SYO 2 LDS 781. B is CPD-56@9854.
22168+1746 BPM2441 [PM2000] 2575955 + [PM2000] 2575968. Gvr2010
22169+1258 HJ 293 Also known as STF2888.
22172+1725 BRT1358 J 3350. Nsn2016
22173-0042 STF2887 HJL 304. HJL1986
22173-0847 LDS 782 AB: NLTT 53397/53398 Chm2004
This system counts as single in our statistics, even though it appears
to be a triple system in reality. The reason for this is that the A
component was the AstraLux target, and the BC pair at ~7.8" is outside
of the completeness cut-off at 6". Since the BC pair is visible in the
AstraLux images, we can nonetheless analyze it astrometrically. This
pair was first reported by Beuzit et al. (2004) with rho = 0.978" and
theta = 305.8deg. There are no error bars quoted, but if we assume
that the quoted precision in decimal places corresponds to measurement
precision, and adopt errors of 5 mas and 0.5deg, which should be
conservative in that circumstance, we find that common proper motion
can be confirmed at a 76 sigma confidence level. Hence, physical
companionship can be confidently inferred, even if the errors should
be substantially larger than what we have assumed. Jnn2012
22174+1309 BPM2442 [PM2000] 2576735 + [PM2000] 2576704. Gvr2010
22174-0102 BAL 631 The secondary in the original measure appears to be either a
typographical error or a plate flaw.
22175+2335 GIC 179 G127-013/G127-014.
22175-2342 HJ 5324 LDS4954.
NLTT 53404/53403 Chm2004
WHC 27.
22180-6249 I 20 Ling (2004) derived an orbital parallax 0".00741 and a mass sum of Lin2004a
3.68 +/- 5.03 Msun.
22181+1126 BPM2443 [PM2000] 2577549 + [PM2000] 2577478. Gvr2010
22181-0014 CHR 107 This system, first announced by McAlister and recalled in a later McA1984b
McAlister paper after repeated attempts at confirmation, has been McA1993
restored. While perhaps still spurious, the subsequent confirmation or
suspected duplicity (by another technique) makes the discovery
measurement somewhat more probable.
22182+1414 BPM2444 [PM2000] 2577654 + [PM2000] 2577722. Gvr2010
22182-6300 LTT18565 Hipparcos astrometric solution assumes circular orbit (e = omega = 0). HIP1997d
22185+6313 STF2896 B is BD+62@2060.
22186+0827 OSO 175 G018-039. Not a common proper motion pair, based on color and
comparison with POSS2 red plates. Oso2004
22186-6014 alp Tuc Elements P, T, e in the astrometric solution of Alden (1939) were Ald1939a
taken from the spectroscopic orbit by Spencer Jones.
Hipparcos astrometric solution adopted some elements from the orbit of HIP1997d
Alden (1939). Ald1939a
22187-4954 I 303 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). USN2014b
22189+3746 STF2894 AB: HJL 305. HJL1986
AB: H 3 17. MEv2010
22191+5607 A 1461 One component is the Beta Lyrae-type system GP Cep.
22193+6319 WGT 4 Only quadrants were listed in the paper; position angles were
estimated from their figure.
Components D, E, F, and G are IR point-like sources near the massive
protostellar object S140 IRS1. Wgt2002a
BEI 2 A: SH 2-140 IRS 1. Includes monopolar nebula that extends towards the
SE at a PA ~150 +/- 15deg. Alv2004
22193+0800 J 179 OL 147.
22193-1047 STF2892 Probably a misprint in BDS Vol II: AD should read AB.
22195-6048 HJ 5323 B is CPD-61@6639.
Spectrum of system: K1/2III F2/3(IV).
22199+0526 OSO 176 G018-040. Not a common proper motion pair, based on astrometry and
color. Oso2004
22199-3642 HJ 5326 SWR 268. CPM pair Skf2004
22202-1307 EPI 17 EPIC 206061524. Planet Hunter Object of Interest (PHOI-5b), period
5.8797 +0.0018/-0.0015d. SJR2016
22204+4625 RAO 74 A is also a 765d spectroscopic binary. Tok2019b
22204+0520 CBL 540 Aka CRB 19.
22204-0847 LDS2941 LDS5248.
22205+0547 HJ 962 30 Peg.
22205-0041 SLP 1 Primary is the white dwarf PHL 5038; a model fit to its spectrum
yields Teff = 8000 +/- 100K and log g = 8.2 +/0 0.2, implying a mass
of 0.72 +/- 0.15 Msun and a distance of 64 +/- 10 pc. The B
component is likely a brown dwarf, spectral type L8-L9. SlP2009
22206+5349 BU 379 Bidelman classifies AB as composite gK+ early A.
22207+2457 STF2895 CD: Also known as POU5695.
22210+4632 HJ 1755 2 Lac. A is a spectroscopic binary.
22211+5428 ES 2718 B is BD+53@2854.
22211+3744 BRT2235 Aka ES 2531.
22211+3544 ES 2389 J 3318.
22213+5109 VBS 36 Van Biesbroeck called this HJ 1757, BDS 11679, but it looks like VBs1914
another pair.
22213+2820 HO 615 32 Peg.
22214+6828 OSO 177 G241-004. None is a common proper motion pair, based on comparison
with POSS2 red plates. Oso2004
22216+1207 BPM2445 [PM2000] 2581835 + [PM2000] 2581704. Gvr2010
22217-0123 HJ 3106 gam Aqr = 48 Aqr = Sadachbia. A is a spectroscopic binary.
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). USN2014b
22220-3431 SHY 805 AB: HIP 110419 + HIP 110433.
SHY 802 BC: HIP 110433 + HIP 109306.
22225+3021 HO 474 CD measure of Bu_1906 was erroneously also labelled as BD.
22226+1829 BPM2446 [PM2000] 2583171 + [PM2000] 2583192. Gvr2010
22226+0956 STTA231 B is BD+09@5031.
PU Peg, Beta Lyr (EB) type eclipsing binary, P = 0.862011 d. Zas2011
22227+2849 KU 64 CD: J 1796.
22227+1457 BPM2447 [PM2000] 2583245 + [PM2000] 2583248. Gvr2010
22227-4152 DON1030 Spectrum K1/2III/IV.
22227-4557 I 135 pi 1 Gru = 161 Gru. A is an irregular variable.
22229+1619 BB Peg Multiple system including contact binary. Pribulla & Rucinski (2006) Pbl2006
estimate the mass of the contact pair at 1.951 Msun and the minimum
mass of the wider component at 0.19 Msun.
22230+5533 BAR 58 D is the Mira-type variable SU Lac.
22231-4556 I 382 pi 2 Gru
22231-6509 HJ 5327 B is CPD-65@4028.
22233+3642 ES 2070 Aka J 3319. Dam2013
22234+3912 HJ 1759 ALI 987.
22234+3228 WOR 11 Also known as GJ 856, this is a well studied binary with several
astrometric data points over a long baseline. In Table 4, we present
the AstraLux data as well as one example data point from literature,
and otherwise refer to Seymour et al. (2002) for more information on USN2002
the astrometric data and a preliminary orbit fit. Lopez-Santiago et al
(2006 ApJ 643, 1160) classify the system as a member of subgroup B4,
with an estimated age of ~100 Myr. Jnn2012
22236+5431 ES 1021 STI2741.
22236+5214 CHR 108 bet Lac = 3 Lac
NPOI Limb-darkened diameter 1.92 +/- 0.02 mas, NOI1999
R = 10.7 +/- 0.3 \rsun.
NPOI Limb-darkened diameter 1.909 +/- 0.011 mas. NOI2001a
NPOI Limb-darkened diameter 1.957 +/- 0.037 mas, Sp = G8III, NOI2018
R = 10.96 +/- 0.23 \rsun, Teff = 4803 +/- 75 K, L = 57.7 +/- 3.0 \lsun,
M = 0.97 +/- 0.21 \msun, Age = 6.76 +/- 3.59 Gyr.
22236+4521 STF2902 AB: H N 64. MEv2010
22237+2051 STF2900 33 Peg.
STTA233. STFB 12.
AB: Additional notes may be found in Couteau (1955). Cou1955c
AC: Optical pair, based on study of relative motion of the components
using the method of apparent motion parameters. Kiy2008
AC: H 5 99. MEv2010
COU 139 CD: This may be the pair observed by Kuiper in 1934 and "suspected of Kui1961b
being a very close, equal pair of 0".1". Star was not retained in the
lists of Kuiper, nor in the IDS. Cou1967a
STF2900 AB: Rectilinear solution by Hartkopf & Mason (2013). Hrt2013b
22237-7248 HJ 5325 B is CPD-73@2252.
22240+0612 TOK 350 Triple system consisting of a close binary Aa,Ab with a separation of .
0".09 detected by Riddle et al. (2015) and a CPM companion with a RAO2015
separation of 171". The Aa,Ab system is unresolved in the Ks images, .
but elongated in the J images. We were unable to extract astrometry .
from the data. The separation has decreased since it was discovered .
in 2012; Tokovinin et al. (2014) resolved it with visible speckle Tok2014a
interferometry at the 4.1 m SOAR telescope on 2013.73 at 41 mas. Rbr2015d
22241-0450 BU 172 51 Aqr.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 5.81 +/- 1.40, 4.96, and 2.24 Msun, respectively. Mlk2012
1976.6164: This epoch was incorrectly given as 1976.6146 McA1982b
AB,C: H 5 95. MEv2010
22242+3831 BRT2236 ALI 988.
22243-0138 GIC 180 LDS5249. G027-026/G027-025.
NLTT 53754/53752 Chm2004
22246+1359 BPM2448 [PM2000] 2585544 + [PM2000] 2585676. Gvr2010
22246-4127 JC 19 B is CD-42@15902.
22246-7215 FIN 285 nu Ind. Measures uncertain, too close. Proper motion +1326 -690.
Needs speckle to elicit the nature of the motion.
22247-0159 ALP 28 2MASSW J2224438-015852
Physical companionship to this ultracool dwarf ruled out based on I-J
color, using I-band photometry taken at WIYN in August 2002. AlP2007
22248+2409 HJ 1763 52.5s p and 3' n of BD+23 4532. Doo1915a
22257+1641 BPM2449 [PM2000] 2586892 + [PM2000] 2586810. Gvr2010
22259-7501 DUN 238 AB + KO 5AC + TOK 434Ba,Bb: HIP 110712 and 110719 form the 20".6
pair DUN 238 AB. We observed both components. The A component has a
variable RV according to the GCS, but not confirmed by Jones et al.
(2002); it was unresolved. The newly found pair Ba,Bb has a period on CPS2002b
the order of 10yr. Considering the distant companion Cab2012
C found by Caballero (2012), the system contains at least 4 stars. Tok2015c