Table 1
Study sample sorted by HD number.
| 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 | 10 |
|---|---|---|---|---|---|---|---|---|---|
| ID | Name | SIMBAD | V | E(B − V) | AV | RV | Spectral type | Spectral type | Instrument |
| mag | mag | literature | this work | ||||||
| 1 | HD 023180 | * omi Per | 3.83 | 0.29 ± 0.03 | 0.91 ± 0.08 | 3.14 ± 0.31 | B1IV(F) | B1III | UVES (b) |
| 2 | HD 024263 | * 31 τ | 5.69 | 0.21 ± 0.06 | 0.72 ± 0.22 | 3.44 ± 0.65 | B5V(V) | B3.5V + binary | UVES (a) |
| ... | |||||||||
| 136 | HD 326364 | 9.60 | 0.62 ± 0.03 | 1.80 ± 0.08 | 2.91 ± 0.25 | B0IV(F) | B1IV + cloud | UVES (a) | |
Notes. Column (1) gives the identification number, Col. (2) the HD identifier, Col. (3) if different, the main name of the star as used in SIMBAD, Col. (4) the V magnitude, Col. (5) the reddening E(B − V), Col. (6) the visual extinction AV, Col. (7) the total-to-selective extinction RV, Col. (8) thespectral type from previous literature, Col. (9) the spectral type as derived in this work (see forthcoming paper), and Col. (10) the instrument used to obtain high-resolution spectroscopy. Columns 5–7 extracted from Gordon et al. (2009), Fitzpatrick & Massa (2007), with uncertainties revised as explained in the text. Spectral types as derived by (F) Fitzpatrick & Massa (2007), (G)Gordon et al. (2009), (H)Houk (1982), (HS) Houk & Swift (1999), and (V) Valencic et al. (2004). Spectroscopic data from: (a)this work; (b) Cox et al. (2017); (c) UVES programme ID 096.D-0008(A) (unpublished ESO archive); (d)UVES programme ID 099.C-0637(A) (unpublished ESO archive); (e) Bagnulo et al. (2013); (f)Sembach et al. (1993); (g)Welty & Crowther (2010); (h)Tolstoy et al. (2003); (i)Krełowski et al. (2010); (j)SAO 1.0 m; (k)SOPHIE archive; (l)ELODIE archive, (m)BOES (Kim et al. 2007). For the complete list, see Table A.1.
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