How to Constrain Your M Dwarf. II. the Mass-Luminosity-Metallicity Relation from 0.075 to 0.70 Solar Masses

dc.contributor.authorMann, Andrew W.
dc.contributor.authorDupuy, Trent
dc.contributor.authorKraus, A L
dc.contributor.authorGaidos, Eric
dc.contributor.authorAnsdell, Megan
dc.contributor.authorIreland, Michael
dc.contributor.authorRizzuto, Aaron C.
dc.contributor.authorHung, Chao-Ling
dc.contributor.authorDittmann, Jason
dc.contributor.authorFactor, Samuel
dc.contributor.authorFeiden, Gregory
dc.contributor.authorRuiz-Rodriguez, Dary
dc.date.accessioned2022-05-02T00:39:38Z
dc.date.available2022-05-02T00:39:38Z
dc.date.issued2019
dc.date.updated2020-12-27T07:22:31Z
dc.description.abstractThe 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 Me < M* < 0.70 Me. 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).en_AU
dc.description.sponsorshipA.W.M. was supported through Hubble Fellowship grant 51364 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. T.J.D. acknowledges research support from Gemini Observatory. This work was supported by a NASA Keck PI Data Award (award nos. 1554237, 1544189, 1535910, and 1521162), administered by the NASA Exoplanet Science Instituteen_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0004-637Xen_AU
dc.identifier.urihttp://hdl.handle.net/1885/264197
dc.language.isoen_AUen_AU
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/6401..."Published version can be archived in any website" from SHERPA/RoMEO site (as at 2/05/2022).en_AU
dc.publisherIOP Publishingen_AU
dc.rights© 2019. The American Astronomical Society.en_AU
dc.sourceThe Astrophysical Journalen_AU
dc.subjectbinaries: visualen_AU
dc.subjectstars: late-typeen_AU
dc.subjectstars: low-massen_AU
dc.subjectstars: luminosity functionen_AU
dc.subjectmass function Supporting material: machine-readable tablesen_AU
dc.titleHow to Constrain Your M Dwarf. II. the Mass-Luminosity-Metallicity Relation from 0.075 to 0.70 Solar Massesen_AU
dc.typeJournal articleen_AU
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue63en_AU
local.bibliographicCitation.lastpage41en_AU
local.bibliographicCitation.startpage1en_AU
local.contributor.affiliationMann, Andrew W., University of North Carolina at Chapel Hillen_AU
local.contributor.affiliationDupuy, Trent, Gemini Observatoryen_AU
local.contributor.affiliationKraus, A L, The University of Texasen_AU
local.contributor.affiliationGaidos, Eric, University of Hawaii at Manoaen_AU
local.contributor.affiliationAnsdell, Megan, University of California at Berkeleyen_AU
local.contributor.affiliationIreland, Michael, College of Science, ANUen_AU
local.contributor.affiliationRizzuto, Aaron C., University of Texas at Austinen_AU
local.contributor.affiliationHung, Chao-Ling, Manhattan Collegeen_AU
local.contributor.affiliationDittmann, Jason, Massachusetts Institute of Technologyen_AU
local.contributor.affiliationFactor, Samuel, The University of Texas at Austinen_AU
local.contributor.affiliationFeiden, Gregory, University of North Georgiaen_AU
local.contributor.affiliationRuiz Rodriguez, Dary, College of Science, ANUen_AU
local.contributor.authoremailu5544212@anu.edu.auen_AU
local.contributor.authoruidIreland, Michael, u5544212en_AU
local.contributor.authoruidRuiz Rodriguez, Dary, u5455528en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systemsen_AU
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciencesen_AU
local.identifier.ariespublicationu3102795xPUB1027en_AU
local.identifier.citationvolume871en_AU
local.identifier.doi10.3847/1538-4357/aaf3bcen_AU
local.identifier.scopusID2-s2.0-85062009961
local.identifier.uidSubmittedByu3102795en_AU
local.publisher.urlhttp://iopscience.iop.org/0004-637Xen_AU
local.type.statusPublished Versionen_AU

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