Dynamical masses of M-dwarf binaries in young moving groups: II - Toward empirical mass-luminosity isochrones

TL;DR

This study measures the dynamical masses and luminosities of M-dwarf binaries in young moving groups to develop empirical mass-luminosity relations, aiding in more accurate stellar age determinations and calibration of theoretical models.

Contribution

It provides new dynamical mass and luminosity measurements for M-dwarf binaries, contributing to the creation of empirical isochrones in mass-luminosity space.

Findings

Young M-dwarfs are consistent with models, older ones are underluminous.

Dynamical masses improve the calibration of stellar evolution models.

Empirical isochrones help assess stellar ages independently of models.

Abstract

Low-mass stars exhibit substantial pre-main sequence evolution during the first ~100 Myrs of their lives. Thus, young M-type stars are prime targets for isochronal dating, especially in young moving groups (YMGs), which contain large amounts of stars in this mass and age range. If the mass and luminosity of a star can both be directly determined, this allows for a particularly robust isochronal analysis. This motivates in-depth studies of low-mass binaries with spatially resolvable orbits, where dynamical masses can be derived. Here we present the results of an observing campaign dedicated to orbital monitoring of AB Dor Ba/Bb, which is a close M-dwarf pair within the quadruple AB Dor system. We have acquired eight astrometric epochs with the SPHERE/ZIMPOL and NACO instruments, which we combine with literature data to improve the robustness and precision for the orbital characterization of the pair. We find a system mass 0.66+/-0.12 Msun and bolometric luminosities in log(L/Lsun) of -2.02+/-0.02 and -2.11 +/- 0.02 for AB Dor Ba and Bb, respectively. These measurements are combined with other YMG pairs in the literature to start building a framework of empirical isochrones in mass-luminosity space. This can be used to calibrate theoretical isochrones and to provide a model-free basis for assessing relative stellar ages. We note a tentative emerging trend where the youngest moving group members are largely consistent with theoretical expectations, while stars in older associations such as the AB Dor moving group appear to be systematically underluminous relative to isochronal expectations.