Akademik Veri Yönetim Sistemi
Astronomical Journal, cilt.171, sa.1, 2026 (SCI-Expanded, Scopus)
A method of obtaining bolometric corrections (BCV ) from observed high-resolution, high signal-to-noise spectra is described. The method is applied to the spectra of 128 stars collected from the literature with well-determined effective temperatures (Teff) with the Sλ(V) transparency profiles of Bessell and Landolt. The computed BCV values are found to be accurate within several millimagnitudes, and the effect of different Sλ (V) values is found to be no more than 0.015 mag. The measured visual-to-bolometric ratio (LV /L) from the sample spectra and classically determined BCV from bolometric (MBol) and visual (MV) absolute magnitudes helped us to determine the zero-point constant (C2) of the BCV scale. The determined C2 for each star for each Sλ(V) profile revealed C2 = 2.3653 ± 0.0067 mag if the Sλ(V) profile of Bessell is used and C2 = 2.3826 ± 0.0076 mag if the Sλ(V) profile of Landolt is used. Expanding CBol = 71.197425... mag and cBol = − 18.997351... mag announced by IAU2015GARB2, and using the definition of C2 = CBol–CV = cBol–cV, where capital C is the absolute magnitude and lowercase c is the apparent magnitude and subscripts indicate bolometric and visual, the zero-point constants—C V = 68.8321 ± 0.0067 mag and cV = −21.3627 ± 0.0067 mag, if LV and are in SI units—were determined corresponding to Sλ(V) of Bessell. The zero-point constants corresponding to Sλ(V) of Landolt are smaller, but the difference is not more than 0.02 mag. Typical and limiting accuracies for predicting a stellar luminosity from an apparent magnitude and a distance are analyzed.