Astrophys. J., 871, 63-63 (2019/January-3)
How to constrain your M dwarf. II. The Mass-Luminosity-Metallicity relation from 0.075 to 0.70 solar masses.
MANN A.W., DUPUY T., KRAUS A.L., GAIDOS E., ANSDELL M., IRELAND M., RIZZUTO A.C., HUNG C.-L., DITTMANN J., FACTOR S., FEIDEN G., MARTINEZ R.A., RUIZ-RODRIGUEZ D. and THAO P.C.
Abstract (from CDS):
The mass-luminosity relation for late-type stars has long been a critical tool for estimating stellar masses. However, there is growing need for both a higher-precision relation and a better understanding of systematic effects (e.g., metallicity). Here we present an empirical relationship between MKS_ and M* spanning 0.075 M☉ < M* < 0.70 M☉. The relation is derived from 62 nearby binaries, whose orbits we determine using a combination of Keck/NIRC2 imaging, archival adaptive optics data, and literature astrometry. From their orbital parameters, we determine the total mass of each system, with a precision better than 1% in the best cases. We use these total masses, in combination with resolved KS magnitudes and system parallaxes, to calibrate the MKS–M*_ relation. The resulting posteriors can be used to determine masses of single stars with a precision of 2%-3%, which we confirm by testing the relation on stars with individual dynamical masses from the literature. The precision is limited by scatter around the best-fit relation beyond measured M* uncertainties, perhaps driven by intrinsic variation in the MKS–M*_ relation or underestimated uncertainties in the input parallaxes. We find that the effect of [Fe/H] on the MKS–M*_ relation is likely negligible for metallicities in the solar neighborhood (0.0% ± 2.2% change in mass per dex change in [Fe/H]). This weak effect is consistent with predictions from the Dartmouth Stellar Evolution Database, but inconsistent with those from MESA Isochrones and Stellar Tracks (at 5σ). A sample of binaries with a wider range of abundances will be required to discern the importance of metallicity in extreme populations (e.g., in the Galactic halo or thick disk).
© 2019. The American Astronomical Society. All rights reserved.
binaries: visual - stars: late-type - stars: low-mass - stars: luminosity function, mass function
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<Available at CDS (J/ApJ/871/63): table1.dat table2.dat table5.dat>
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