Theoretical Mass-Luminosity Relations in Gaia G-Band

TL;DR

This paper derives theoretical mass-luminosity relations in Gaia G-band for main-sequence and subgiant stars, enabling stellar mass estimation from Gaia photometry within 1-10 solar masses, validated by limited observational data.

Contribution

It provides new analytical relations for mass and luminosity in Gaia G-band for specific stellar classes based on theoretical models.

Findings

Relations are accurate for 1-10 solar mass stars.

Validation with observational data supports their practical use.

Relations for other luminosity classes are less informative.

Abstract

We have analyzed the retrieval of the relation between mass and absolute Gaia G magnitude as obtained from theoretical models by \cite{2012MNRAS.427..127B} for the stars of different luminosity classes. For subgiant and main-sequence stars, we provide approximate analytical direct and inverse relations based on the most probable value of G magnitude in the course of evolution within the given stage. A comparison with (albeit few) observational data confirms that our results can be used for the estimation of the stellar mass from Gaia photometry in the range of 1 to 10 solar mass. We argue that similar relations for other luminosity classes are not informative.