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Table 3

Stellar parameters.

No. Star Cluster Binary log ga T eff b υsini Ref. υ eq Ref. Massc
[km s-1] [km s-1] [M⊙]
1 BD +56°576 χ Per Eclipse 3.40 22 500 17 1 ... 13.5
2 HD 886 ... ... 3.75 22 500 10 ± 1 2 ... 10.7
3 HD 3360 CasTau OB1 ... 3.70 22 000 19 ± 1 3 55 ± 28 7 10.6
4 HD 16582 CasTau OB1 ... 3.80 23 000 14 ± 1 2 14/28 8 10.7
5 HD 22951 Per OB Visual 4.40 27 900 23 4 ... 11
6 HD 29248 Ori OB1 ... 3.75 23 500 36 ± 3 2 6 9 11.5
7 HD 30836 Ori OB1 Spect. 3.35 21 500 43 ± 3 5 ... 13.0
8 HD 34816 Ori runaway ... 4.20 28 900 35 4 ... 13.5
9 HD 35039 Ori OB1a Spect. 3.74 20 600 4 6 ... 9.0
10 HD 35299 Ori OB1a ... 4.25 24 000 8 6 ... 9.1
11 HD 35337 Ori OB1c ... 4.20 23 600 15 4 ... 9.0
12 HD 35468 Ori OB1 ... 3.50 22 000 51 ± 4 5 ... 11.8
13 HD 36285 Ori OB1c ... 4.40 21 900 10 4 ...  <9
14 HD 36351 Ori OB1a Visual 4.16 22 000 42 6 ...  <9
15 HD 36430 Ori OB1c ... 4.36 19 600 26 6 ...  <9
16 HD 36591 Ori OB1b Visual 4.00 27 000 16 ± 2 5 ... 12.8
17 HD 36629 Ori OB1c ... 4.35 22 300 4 6 ...  <9
18 HD 36959 Ori OB1c ... 4.41 24 900 11 6 ... 9
19 HD 36960 Ori OB1c Visual 4.33 28 900 33 4 ... 12
20 HD 37209 Ori OB1c ... 4.13 24 000 50 6 ... 9.7
21 HD 37356 Ori OB1c ... 4.13 22 400 23 6 ...  <9
22 HD 37481 Ori OB1c ... 4.17 23 300 67 6 ...  <9
23 HD 37744 Ori OB1b ... 4.40 24 500 39 6 ... 9
24 HD 44743 ... ... 3.50 24 000 23 ± 2 2 31 ± 5 10 14.5
25 HD 46328 Coll. 121 ... 3.75 27 500 10 ± 2 2 ... 15.5
26 HD 50707 Coll. 121 ... 3.60 26 000 45 ± 3 5 ... 15.6
27 HD 52089 ... ... 3.30 23 000 28 ± 2 5 ... 15.3
28 HD 111123 Sco Cen ... 3.65 27 500 48 ± 3 5 ... 16.6
29 HD 205021 Cep OB1 Spect. 3.70 26 000 29 ± 2 2 ... 14.5
30 HD 214993 Lac OB1 ... 3.65 24 500 42 ± 4 2 45 11 13.5
31 HD 216916 Lac OB1 Eclipse 3.90 23 200 13 1 ... 9.7

Notes.

(a)

The typical 1-σ error for log g is between 0.15 and 0.2 (see e.g. Morel et al. 2008).

(b)

The typical 1-σ error for Teff is about 1000 K (see e.g Morel et al. 2008).

(c)

The masses of the stars are only rough estimates from the comparison of the models and the stellar positions in the log g − log Teff diagram under the assumption of slow rotation.

References. [1] Venn et al. (2002); [2] Morel et al. (2006); [3] Briquet & Morel (2007); [4] Mendel et al. (2006); [5] Morel et al. (2008); [6] Proffitt & Quigley (2001); [7] Neiner et al. (2003); [8] Aerts et al. (2006); [9] Pamyatnykh et al. (2004); [10] Mazumdar et al. (2006); [11] Aerts (1996).

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