Spectro-Thermometry Of M Dwarfs And Their Candidate Planets: Too Hot, Too Cool, Or Just Right?

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dc.contributor.utaustinauthorMann, Andrew W.en_US
dc.creatorMann, Andrew W.en_US
dc.creatorGaidos, Ericen_US
dc.creatorAnsdell, Meganen_US
dc.date.accessioned2016-04-28T19:31:33Z
dc.date.available2016-04-28T19:31:33Z
dc.date.issued2013-12en
dc.description.abstractWe use moderate-resolution spectra of nearby late K and M dwarf stars with parallaxes and interferometrically determined radii to refine their effective temperatures, luminosities, and metallicities. We use these revised values to calibrate spectroscopic techniques to infer the fundamental parameters of more distant late-type dwarf stars. We demonstrate that, after masking out poorly modeled regions, the newest version of the PHOENIX atmosphere models accurately reproduce temperatures derived bolometrically. We apply methods to late-type hosts of transiting planet candidates in the Kepler field, and calculate effective temperature, radius, mass, and luminosity with typical errors of 57 K, 7%, 11%, and 13%, respectively. We find systematic offsets between our values and those from previous analyses of the same stars, which we attribute to differences in atmospheric models utilized for each study. We investigate which of the planets in this sample are likely to orbit in the circumstellar habitable zone. We determine that four candidate planets (KOI 854.01, 1298.02, 1686.01, and 2992.01) are inside of or within 1 sigma of a conservative definition of the habitable zone, but that several planets identified by previous analyses are not (e.g., KOI 1422.02 and KOI 2626.01). Only one of the four habitable-zone planets is Earth sized, suggesting a downward revision in the occurrence of such planets around M dwarfs. These findings highlight the importance of measuring accurate stellar parameters when deriving parameters of their orbiting planets.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipNSF AST-0908419en_US
dc.description.sponsorshipNASA NNX10AI90G, NNX11AC33G, NAS5-26555en_US
dc.description.sponsorshipUniversity of Hawaii NNX-08AE38Aen_US
dc.description.sponsorshipNASA Science Mission directorateen_US
dc.description.sponsorshipNASA Office of Space Science NNX09AF08Gen_US
dc.identifierdoi:10.15781/T23B9V
dc.identifier.Filename2013_12_spectrothermometry.pdfen_US
dc.identifier.citationMann, Andrew W., Eric Gaidos, and Megan Ansdell. "Spectro-Thermometry of M dwarfs and their candidate planets: too hot, too cool, or just right?." The Astrophysical Journal, Vol. 779, No. 2 (Dec., 2013): 188.en_US
dc.identifier.doi10.1088/0004-637x/779/2/188en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34640
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.subjectastrobiologyen_US
dc.subjectplanetary systemsen_US
dc.subjectstars: fundamental parametersen_US
dc.subjectstars:en_US
dc.subjectlate-typeen_US
dc.subjectlow-mass starsen_US
dc.subjectintegral-field spectrographen_US
dc.subjectinfrared telescopeen_US
dc.subjectfacilityen_US
dc.subjectkepler target starsen_US
dc.subjectproper-motion starsen_US
dc.subjectdigital sky surveyen_US
dc.subjecthabitable zonesen_US
dc.subjectmodel atmospheresen_US
dc.subjectspectrophotometric standardsen_US
dc.subjectastrophysical parametersen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleSpectro-Thermometry Of M Dwarfs And Their Candidate Planets: Too Hot, Too Cool, Or Just Right?en_US
dc.typeArticleen_US

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