AcknowledgementWe have used Python/Astropy, Python/extinction, Python/SpectRes, HDF5 for Python, Topcat, GNU-Parallel, CFITSIO. We thank the the authors of spectral libraries or softwares: Phoenix, ATLAS9, PoWR, MARCS, COMARCS, WMbasic, Koester WD library.
Q1. There is already CMD website using YBC, why a separate YBC web site? A: The CMD website and the Trilegal code can be seem as a test case of using the YBC, but YBC can be used beyond this. For example, you can use it in your simulation, based on isochrones. Or if you wanna compare different isochrones from different research groups, but wish to distinguish from the differentce resulted by using different bolometric corrections.
Q2. What are the values for Solar Mbol and Luminosity? A: We adopt the IAU 2015 resolution with Mbol_Sun=4.74 and L_Sun=3.828E33 erg/s. Be careful that CMD is using Mbol_Sun=4.77 and L_Sun=3.846E33 erg/s, which can produce~0.025 mag difference compared to YBC.
Q3. Are the appended columns absolute magnitudes? A: Yes, they are.
Q4. How is the ISM extinction treated? A: You are talking about the ISM extinction other than the cirsumstellar dust. Every spectrum used has been convlved with the extinction curve (Cardelli et al. (1989) + O'Donnell (1994) with RV=3.1.), therefore the spectral variation effect hass been considered. The non-lineararity as a function of Av amount has been also taken into account by computing grids with Av=[0., 0.5, 1., 2., 5., 10., 20] and interpolating among them.
Q5. How is the PoWR library being used? A: Usually logg and logTeff are used for the interpolation. For WR stars, the transformed radius logRt is the more influential quantity other than logg. The tranformed radius is defined as: