Table 1
Stellar parameters of the observed sources.
| Star name | Alt. name | RA (2000.0) | Dec | Region | d | Sp.T. | Teff | A v | log(L∗) | v rad | Incl. | |
| [pc] | [K] | [mag] | [km s-1] | |||||||||
|
|
||||||||||||
| HD 163296 | MWC 275 | 17 56 21.29 | –21 57 21.8 | Sco OB2-1 | 119 HIP | A3Ve G98 | 8720 | 0.1 | 1.4 | –4.0 B00 | 46°I07 | |
| HD 250550 | MWC 789 | 06 01 59.99 | +16 30 56.7 | L1586 | 280 K98 | B8–A0IVe G98 | 10750 | 0.4 | 1.3 | +16 F84 | 10°F11 | |
| Hen 2-80 | PK 299-00.1 | 12 22 23.18 | -63 17 16.8 | >750 B15 | B6Ve C10 | 14000 | 4.2 | >2.7 | –22 C10 | |||
| MWC 137 | V1308 Ori | 06 18 45.50 | +15 16 52.4 | >1000 B15 | B0ep S81 | 30000 | 4.0 | >4.1 | +43 Z03 | |||
| T Ori | MWC 763 | 05 35 50.44 | –05 28 34.9 | Orion OB1c | 510 D99 | A3IVe M01 | 8660 | 1.2 | 1.79 | +52 T09 | ||
| Hen 3-1227 | PK 338+01.1 | 16 38 28.62 | –45 23 41.5 | >400 B15 | Be P03 | 20000 | 4.0 | >2.0 | ||||
Notes. The effective temperatures, Teff, were derived based on the spectral type and the calibrations by Schmidt-Kaler (1982). The Av and the luminosity were derived using the distances and the SEDs shown in Fig. 1. For sources where no distance is known, the spectral type was used to infer a stellar luminosity using the Schmidt-Kaler (1982) calibrations, and a minimum distance was then computed.
Reference. B15 = This paper (minimum distance based on luminosity), C10 = Carmona et al. (2010), D99 = de Zeeuw & Norris (1999), F84 = Finkenzeller & Jankovics (1984), F11 = Fedele et al. (2011), G98 = Gray & Corbally (1998), HIP = Hipparcos distance, K98 = Kawamura et al. (1998), M01 = Mora et al. (2001), P03 = Pereira et al. (2003), S81 = Sabbadin & Hamzaoglu (1981), I07 = Isella et al. (2007), Z03 = Zickgraf (2003), T09 = Tobin et al. (2009), B00 = Barbier-Brossat & Figon (2000).
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