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dc.contributor.authorSheehan, Patrick D.
dc.contributor.authorWu, Ya-Lin
dc.contributor.authorEisner, Josh A.
dc.contributor.authorTobin, John J.
dc.date.accessioned2019-07-18T23:41:35Z
dc.date.available2019-07-18T23:41:35Z
dc.date.issued2019-04-01
dc.identifier.citationPatrick D. Sheehan et al 2019 ApJ 874 136en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/ab09f9
dc.identifier.urihttp://hdl.handle.net/10150/633400
dc.description.abstractThe Keplerian rotation in protoplanetary disks can be used to robustly measure stellar masses at very high precision if the source distance is known. We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of spatially and spectrally resolved (CO)-C-12 (2-1) emission toward the disks around 2MASS J16262774-2527247 (the tertiary companion to ROXs 12 at 5100 au), CT Cha, and DH Tau. We employ detailed modeling of the Keplerian rotation profile, coupled with accurate distances from Gaia, to directly measure the stellar masses with similar to 2% precision. We also compare these direct mass measurements with the masses inferred from evolutionary models, determined in a statistically rigorous way. We find that 2MASS J16262774-2527247 has a mass of 0.535(-)(0.007)(+0.006) M-circle dot and CT Cha has a mass of 0.796(-0.014)(+0.015) M-circle dot, broadly consistent with evolutionary models, although potentially significant differences remain. DH Tau has a mass of 0.101(-0.003)(+0.004) M-circle dot, but it suffers from strong foreground absorption that may affect our mass estimate. The combination of ALMA, Gaia, and codes like pdspy, presented here, can be used to infer the dynamical masses for large samples of young stars and substellar objects, and place constraints on evolutionary models.en_US
dc.description.sponsorshipHeising-Simons Foundation; Homer L. Dodge Endowed Chair; National Science Foundation Graduate Research Fellowship [2012115762]; NSF AAG grant [1311910]; NASA's Science Mission Directorateen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttps://iopscience.iop.org/article/10.3847/1538-4357/ab09f9/metaen_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectparallaxesen_US
dc.subjectprotoplanetary disksen_US
dc.subjectradio lines: starsen_US
dc.subjectstars: fundamental parametersen_US
dc.subjectstars: pre-main sequenceen_US
dc.titleHigh-precision Dynamical Masses of Pre-main-sequence Stars with ALMA and Gaiaen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume874
dc.source.issue2
dc.source.beginpage136
refterms.dateFOA2019-07-18T23:41:35Z


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