VizieR Online Data Catalog: Teff and Fbol from Infrared Flux Method (Casagrande+, 2010)

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_⊙=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. BC_V=mBol-V0, where BC_V 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).