Physics
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35129054c&link_type=abstract
VizieR On-line Data Catalog: J/A+A/512/A54. Originally published in: 2010A&A...512A..54C
Physics
Stars: Dwarfs, Stars: Giant, Effective Temperatures, Photometry: Infrared, Models: Atmosphere
Scientific paper
Sample stars used and fundamental physical parameters (Teff, Fbol, diam) derived via IRFM. The apparent bolometric magnitudes (mBol) have been computed according to Casagrande et al. (2006MNRAS.373...13C), where the absolute bolometric magnitude of the Sun MBol&sun;=4.74. For each star mBol is obtained using its bolometric flux (Fbol) and effective temperature (Teff) and therefore it is already corrected for reddening, if present. Notice however that the observed magnitudes given here are not: before computing bolometric corrections, the observed magnitudes should be dereddened using the E(B-V) given here. The correction into dereddened magnitudes as been done iteratively, as described in Section 2.1 of the paper. However, average relations between E(B-V) and various photometric bands can be found in literature e.g. McCall (2004AJ....128.2144M). Bolometric corrections in each band can be readily obtained using the dereddened magnitudes. E.g. BCV=mBol-V0, where BCV is the bolometric correction in V band, mBol is thw apparent bolometric magnitude, V0 is the dereddened apparent V magnitude (=Vmag if E(B-V)=0). Errors have been computed as described in the paper, without accounting for the uncertainty in E(B-V): changing it by +/-0.01 would affect Teff by approximately +/-50K.
(1 data file).
Asplund Martin
Bessell Michael
Casagrande Luca
Melendez Jorge
Ramirez Ignacio
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