Predicted masses of Galactic Cepheids in the Gaia Data Release 2
Marcella Marconi, Giulia De Somma, Vincenzo Ripepi, Roberto Molinaro,, Ilaria Musella, Silvio Leccia, Maria Ida Moretti

TL;DR
This study uses theoretical pulsation models and Gaia DR2 data to estimate the masses of Galactic Cepheids, providing insights into their mass distribution and Gaia parallax offsets.
Contribution
It introduces new mass-dependent Period-Wesenheit relations in Gaia bands and validates them against Gaia data and binary Cepheids, improving distance and mass estimates.
Findings
Mass distribution peaks around 5.6 M_sun for F pulsators.
Applying Gaia parallax offset shifts mass estimates lower.
Results support the predictive capability of theoretical models.
Abstract
On the basis of recently computed nonlinear convective pulsation models of Galactic Cepheids, spanning wide ranges of input stellar parameters, we derive theoretical mass-dependent Period-Wesenheit relations in the Gaia bands, namely , and , that are found to be almost independent of the assumed efficiency of super-adiabatic convection. The application to a selected sub-sample of Gaia Data Release 2 Galactic Cepheids database allows us to derive mass-dependent estimates of their individual distances. By imposing their match with the astrometric values inferred from Gaia, we are able to evaluate the individual mass of each pulsator. The inferred mass distribution is peaked around 5.6 and 5.4 for the F and FO pulsators, respectively. If the estimated Gaia parallax offset =0.046 mas is applied to Gaia parallaxes before imposing…
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