SHOTGLAS II. BHB stars in omega Cen and NGC 6752

We use dedicated model atmospheres and synthetic spectra grids computed using a hybrid LTE/NLTE modeling approach to fit the MUSE spectra of HB stars hotter than 8000K in both clusters. The spectral fits provide estimates of the effective temperature (Teff), surface gravity (logg), and helium abundance of the stars.

The model grids are further used to fit the HST magnitudes, meaning the spectral energy distributions (SED), of the stars. From the SED fits, we derive the average reddening, radius, luminosity, and mass of the stars in our sample. The atmospheric and stellar properties that we derive for the stars in our sample are in good agreement with the theoretical expectations.