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dc.contributor.authorShan, Yutong
dc.contributor.authorYee, Jennifer C.
dc.contributor.authorBowler, Brendan P.
dc.contributor.authorCieza, Lucas A.
dc.contributor.authorMontet, Benjamin T.
dc.contributor.authorCánovas, Héctor
dc.contributor.authorLiu, Michael C.
dc.contributor.authorClose, Laird M.
dc.contributor.authorHinz, Phil M.
dc.contributor.authorMales, Jared R.
dc.contributor.authorMorzinski, Katie M.
dc.contributor.authorVaz, Amali
dc.contributor.authorBailey, Vanessa P.
dc.contributor.authorFollette, Katherine B.
dc.date.accessioned2018-03-23T17:22:47Z
dc.date.available2018-03-23T17:22:47Z
dc.date.issued2017-09-05
dc.identifier.citationThe Multiplicity of M Dwarfs in Young Moving Groups 2017, 846 (2):93 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa859d
dc.identifier.urihttp://hdl.handle.net/10150/627110
dc.description.abstractWe image 104 newly identified low-mass (mostly M-dwarf) pre-main sequence (PMS) members of nearby young moving groups (YMGs) with Magellan Adaptive Optics (MagAO) and identify 27 stellar binaries with instantaneous projected separation as small as 40 mas. Fifteen were previously unknown. The total number of multiple systems in this sample including spectroscopic and visual binaries from the literature is 36, giving a raw stellar multiplicity rate of at least 35(-4)(+5)% for this population. In the separation range of roughly 1-300 au in which infrared AO imaging is most sensitive, the raw multiplicity rate is at least 24(-4)(+5)% for binaries resolved by the MagAO infrared camera (Clio). The M-star subsample of 87 stars yields a raw multiplicity of at least 30(-4)(+5)% over all separations, 21(-4)(+5)% for secondary companions resolved by Clio from 1 to 300 au (23(-4)(+5)% for all known binaries in this separation range). A combined analysis with binaries discovered by the Search for Associations Containing Young stars shows that stellar multiplicity fraction as a function of mass over the range of 0.2 to 1.2M(circle dot) appears to be linearly flat, in contrast to the field, where multiplicity increases with mass. After bias corrections are applied, the multiplicity of low-mass YMG members (0.2-0.6M(circle dot)) is in excess of the field. The overall multiplicity fraction is also consistent with being constant in age and across YMGs, which suggests that multiplicity rates for this mass range are largely set by 10 Myr without appreciable evolution thereafter.
dc.description.sponsorshipNatural Science and Engineering Research Council (NSERC) of Canada; NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51369.001-A]; NASA [NAS5-26555]; NASA through the Sagan Fellowship Program; CONICYT-FONDECYT [1171246]; Millennium Science Initiative (Chilean Ministry of Economy) [RC130007]; Spanish Ministerio de Economia y Competitividad [AYA 2014-55840-P]; NASA Exoplanets Research Program (XRP) [NNX16AD44G]; National Aeronautics and Space Administration; National Science Foundation; Space Telescope Science Institute under U.S. Government [NAG W-2166]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/846/i=2/a=93?key=crossref.ed8d39466d83a2e263d6540c7396d1a8en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectbinaries: visualen
dc.subjectmethods: observationalen
dc.subjectmethods: statisticalen
dc.subjectstars: low-massen
dc.subjectstars: pre-main sequenceen
dc.subjecttechniques: photometricen
dc.titleThe Multiplicity of M Dwarfs in Young Moving Groupsen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
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
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-29T05:37:26Z
html.description.abstractWe image 104 newly identified low-mass (mostly M-dwarf) pre-main sequence (PMS) members of nearby young moving groups (YMGs) with Magellan Adaptive Optics (MagAO) and identify 27 stellar binaries with instantaneous projected separation as small as 40 mas. Fifteen were previously unknown. The total number of multiple systems in this sample including spectroscopic and visual binaries from the literature is 36, giving a raw stellar multiplicity rate of at least 35(-4)(+5)% for this population. In the separation range of roughly 1-300 au in which infrared AO imaging is most sensitive, the raw multiplicity rate is at least 24(-4)(+5)% for binaries resolved by the MagAO infrared camera (Clio). The M-star subsample of 87 stars yields a raw multiplicity of at least 30(-4)(+5)% over all separations, 21(-4)(+5)% for secondary companions resolved by Clio from 1 to 300 au (23(-4)(+5)% for all known binaries in this separation range). A combined analysis with binaries discovered by the Search for Associations Containing Young stars shows that stellar multiplicity fraction as a function of mass over the range of 0.2 to 1.2M(circle dot) appears to be linearly flat, in contrast to the field, where multiplicity increases with mass. After bias corrections are applied, the multiplicity of low-mass YMG members (0.2-0.6M(circle dot)) is in excess of the field. The overall multiplicity fraction is also consistent with being constant in age and across YMGs, which suggests that multiplicity rates for this mass range are largely set by 10 Myr without appreciable evolution thereafter.


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