An Empirical Calibration To Estimate Cool Dwarf Fundamental Parameters From H-Band Spectra

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dc.contributor.utaustinauthorMann, Andrew W.en_US
dc.creatorNewton, Elisabeth R.en_US
dc.creatorCharbonneau, Daviden_US
dc.creatorIrwin, Jonathanen_US
dc.creatorMann, Andrew W.en_US
dc.date.accessioned2016-04-28T19:39:38Z
dc.date.available2016-04-28T19:39:38Z
dc.date.issued2015-02en
dc.description.abstractInterferometric radius measurements provide a direct probe of the fundamental parameters of M dwarfs. However, interferometry is within reach for only a limited sample of nearby, bright stars. We use interferometrically measured radii, bolometric luminosities, and effective temperatures to develop new empirical calibrations based on low-resolution, near-infrared spectra. We find that H-band Mg and Al spectral features are good tracers of stellar properties, and derive functions that relate effective temperature, radius, and log luminosity to these features. The standard deviations in the residuals of our best fits are, respectively, 73 K, 0.027R(circle dot), and 0.049 dex (an 11% error on luminosity). Our calibrations are valid from mid K to midMdwarf stars, roughly corresponding to temperatures between 3100 and 4800 K. We apply our H-band relationships to M dwarfs targeted by the MEarth transiting planet survey and to the cool Kepler Objects of Interest (KOIs). We present spectral measurements and estimated stellar parameters for these stars. Parallaxes are also available for many of the MEarth targets, allowing us to independently validate our calibrations by demonstrating a clear relationship between our inferred parameters and the stars' absolute K magnitudes. We identify objects with magnitudes that are too bright for their inferred luminosities as candidate multiple systems. We also use our estimated luminosities to address the applicability of near-infrared metallicity calibrations to mid and late M dwarfs. The temperatures we infer for the KOIs agree remarkably well with those from the literature; however, our stellar radii are systematically larger than those presented in previous works that derive radii from model isochrones. This results in a mean planet radius that is 15% larger than one would infer using the stellar properties from recent catalogs. Our results confirm the derived parameters from previous in-depth studies of KOIs 961 (Kepler-42), 254 (Kepler-45), and 571 (Kepler-186), the latter of which hosts a rocky planet orbiting in its star's habitable zone.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipNational Science Foundation Graduate Research Fellowshipen_US
dc.description.sponsorshipUniversity of Texas at Austinen_US
dc.description.sponsorshipDavid and Lucille Packard Fellowship for Science and Engineeringen_US
dc.description.sponsorshipNational Science Foundation AST-0807690, AST-1109468, AST-1004488en_US
dc.description.sponsorshipJohn Templeton Foundationen_US
dc.description.sponsorshipNASAen_US
dc.description.sponsorshipNSF, NASAs Astrophysics Data System (ADS)en_US
dc.description.sponsorshipSIMBAD database, operated at CDS, Strasbourg, Franceen_US
dc.identifierdoi:10.15781/T2VR72
dc.identifier.Filename2015_02_empiricalcalibration.pdfen_US
dc.identifier.citationNewton, Elisabeth R., David Charbonneau, Jonathan Irwin, and Andrew W. Mann. "An empirical calibration to estimate cool dwarf fundamental parameters from H-band spectra." arXiv preprint arXiv:1412.2758 (Feb., 2014)en_US
dc.identifier.doi10.1088/0004-637x/800/2/85en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35052
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjectstars: atmospheresen_US
dc.subjectbinaries: generalen_US
dc.subjectstars: fundamental parametersen_US
dc.subjectstars: low-mass supporting material: machine-readable tablesen_US
dc.subjectlow-mass starsen_US
dc.subjectstellar effective temperaturesen_US
dc.subjectinfrared flux methoden_US
dc.subjectnearby m dwarfsen_US
dc.subjectangular diametersen_US
dc.subjectmain-sequenceen_US
dc.subjectsolar neighborhooden_US
dc.subjecteclipsing binariesen_US
dc.subjectcandidate planetsen_US
dc.subjecttransit detectionen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleAn Empirical Calibration To Estimate Cool Dwarf Fundamental Parameters From H-Band Spectraen_US
dc.typeArticleen_US

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