2012A&A...541A..96R


Query : 2012A&A...541A..96R

2012A&A...541A..96R - Astronomy and Astrophysics, volume 541A, 96-96 (2012/5-1)

An investigation of binary stars in the Pleiades with high contrast and spatial resolution.

RICHICHI A., CHEN W.P., CUSANO F., FORS O., MOERCHEN M. and KOMONJINDA S.

Abstract (from CDS):

It is widely recognized that binarity is a very common feature during star formation; however, different regions and clusters display significantly different binary fractions. This appears to be related to the initial density of the star forming region. The Pleiades cluster has been shown to have a binary fraction similar to that of field stars in the solar neighborhood. We have taken advantage of a passage of the Moon over the Pleiades cluster, to investigate at high angular resolution two small but similar and consistent samples of cluster members and field stars. We have employed the technique of lunar occultations (LO). Although LO in the Pleiades have been reported several times in the past, we have for the first time employed the superior performance of the VLT, achieving about 1 milliarcsecond (mas) resolution and detecting sources as faint as K≃12mag. We have recorded 17 LO light curves of stars recognized as cluster members, and 17 of field stars. The average magnitude was K≃8.5mag and the average limiting resolution ≃0.002", for both samples. We detect 5 binaries among the cluster members, and 2 among the sample of field stars. Three systems are new detections, while two were previously only suspected to be binaries. The projected separations are in the range 0.017" to 0.642" and the brightness ratios in the range 1 to 90. One more star is suspected to have a companion. Although the fraction of binary detections appears higher among the members than among the non-members, the two samples are too small to draw firm conclusions. Our observations show that, in spite of extensive investigations carried out previously in the Pleiades cluster, the binarity census is not yet complete. We have detected significant orbital motion in four binary systems, which stand up as candidates for dynamical mass estimations.

Abstract Copyright:

Journal keyword(s): techniques: high angular resolution - occultations - binaries: general - stars: fundamental parameters

Simbad objects: 39

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Number of rows : 39
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 23157 ** 03 43 41.5325750160 +23 38 56.977320660   8.25 7.95     A5V 80 0
2 HD 23158 SB* 03 43 42.8773509420 +23 35 41.208537362   10.04 9.58     F5V 68 0
3 Cl Melotte 22 332 * 03 44 20.4716519688 +23 31 04.015988868     12.74     ~ 5 0
4 2MASS J03442602+2336480 * 03 44 26.0301142488 +23 36 48.076146828     13.20     ~ 2 0
5 HD 23289 * 03 44 51.2354703456 +23 16 08.116761576   9.33 9.01   8.37 F3V 100 0
6 HD 23326 PM* 03 45 05.2834818672 +23 42 09.619748244 9.632 9.34 8.99   8.49 F3V 96 0
7 2MASS J03452219+2328182 Y*O 03 45 22.1866155551 +23 28 18.151660642 14.494 13.54 12.48   11.28 ~ 54 0
8 UCAC4 567-007996 * 03 45 27.4068516456 +23 15 25.931229660   13.940 12.800 12.460   ~ 2 0
9 V* V1041 Tau Y*O 03 45 39.4002482170 +23 45 15.469362585 14.355 13.52 12.41 11.99 10.83 G9V 58 0
10 Cl Melotte 22 803 * 03 45 50.6988708336 +23 37 15.259655100   13.39 11.97     K0IV 9 0
11 Cl Melotte 22 815 * 03 45 51.6173942136 +23 25 54.384846816   12.89 12.06 11.81   ~ 6 0
12 Cl Melotte 22 1021 * 03 46 24.1485971208 +23 19 24.285317952   11.6 10.4     F7V 11 0
13 Cl Melotte 22 OpC 03 46 24 +24 06.8           ~ 3260 0
14 V* V641 Tau Y*O 03 46 27.7743108351 +23 35 33.771415161 15.602 14.28 13.05   11.52 K0V 82 0
15 HD 23512 PM* 03 46 34.1921924832 +23 37 26.494987584 8.72 8.44 8.09 7.79 7.49 A2V 140 0
16 HD 282975 Y*O 03 46 37.6798897555 +23 47 15.790663787 11.533 10.8 10.0   9.43 G6V 73 0
17 V* FL Tau Er* 03 47 08.5260384216 +23 42 38.740347036   14.73 13.44 13.04   K5V: 55 0
18 HD 23609 * 03 47 17.1423427464 +23 43 36.294494628   7.487 6.97     F5 52 0
19 HD 23632 * 03 47 20.9688302904 +23 48 12.036277512   7.04 7.02   7.01 A1V 113 0
20 * eta Tau Be* 03 47 29.0765529 +24 06 18.488347 2.44 2.78 2.87 2.84 2.88 B7III 524 1
21 HD 23654 PM* 03 47 36.9621558960 +23 36 32.817351240   9.016 7.78     K0 29 0
22 BD+22 559 * 03 47 54.9697439184 +23 26 13.912812348   11.1 10.0     G8 9 0
23 Cl Melotte 22 1660 * 03 47 57.3204707736 +23 35 15.426131028   14.25 12.84     M: 7 0
24 HD 23753 PM* 03 48 20.8167826752 +23 25 16.495877028 5.06 5.38 5.45 5.42 5.48 B8V 168 0
25 Cl Melotte 22 1901 * 03 48 31.3855985904 +23 37 01.817813712     12.57     ~ 5 0
26 2MASS J03483451+2326053 Y*O 03 48 34.5103551864 +23 26 05.248800743   11.2 10.7   9.66 G0V 63 0
27 * 26 Tau PM* 03 48 56.9419001352 +23 51 25.674800292   6.84 6.464     F0 56 0
28 V* V1282 Tau RS* 03 49 06.1083396732 +23 46 52.469922436   11.63 10.803 9.8 9.831 G7IV 83 0
29 HD 23863 * 03 49 12.1871337168 +23 53 12.438137328   8.36 8.15   7.88 A7Vn 95 0
30 Cl Melotte 22 2294 V* 03 49 25.1343660048 +23 47 42.093976704   14.04 12.32 11.82   M: 13 0
31 BD+23 566 * 03 49 53.2755311976 +23 31 50.344472208   11.19 9.95     K2 8 0
32 HD 23964A SB* 03 49 58.0556899152 +23 50 55.288075236   6.82 6.81 6.3 6.74 B9.5VspSiSrCr 137 0
33 Cl Melotte 22 2698 * 03 50 26.4411522096 +23 34 20.820327780   11.94 11.37     ~ 5 0
34 TYC 1800-462-1 * 03 50 36.1211432616 +23 29 35.644443684   13.52 11.44     ~ 3 0
35 V* V1176 Tau Er* 03 50 54.3588780269 +23 50 05.237700840   12.43 11.48 10.99 10.47 K2 64 0
36 BD+23 572 * 03 51 15.3216819240 +23 37 18.409630188   10.96 10.46     F0 6 0
37 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1311 0
38 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4049 0
39 NAME Sco-Oph Region reg 16 30.0 -21 00           ~ 72 0

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2022.11.28-11:53:56

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