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dc.contributor.authorBroekhoven-Fiene, H.
dc.contributor.authorMatthews, B.
dc.contributor.authorDuchêne, G.
dc.contributor.authorDi Francesco, J.
dc.contributor.authorScholz, A.
dc.contributor.authorChrysostomou, A.
dc.contributor.authorJayawardhana, R.
dc.date.accessioned2014-08-29T11:01:03Z
dc.date.available2014-08-29T11:01:03Z
dc.date.issued2014-07-10
dc.identifier.citationBroekhoven-Fiene , H , Matthews , B , Duchêne , G , Di Francesco , J , Scholz , A , Chrysostomou , A & Jayawardhana , R 2014 , ' The disk around the brown dwarf KPNO TAU 3 ' , Astrophysical Journal , vol. 789 , no. 2 , 155 . https://doi.org/10.1088/0004-637X/789/2/155en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 144252762
dc.identifier.otherPURE UUID: bb6ecf8b-9ea8-4535-966a-6634ef8d5368
dc.identifier.otherScopus: 84903317570
dc.identifier.otherBibCode: 2014ApJ...789..155B
dc.identifier.otherWOS: 000338674900064
dc.identifier.urihttps://hdl.handle.net/10023/5290
dc.descriptionH.B.F. and B.C.M. acknowledge a Discovery Grant from the Natural Science & Engineering Research Council (NSERC) of Canada.en
dc.description.abstractWe present submillimeter observations of the young brown dwarfs KPNO Tau 1, KPNO Tau 3, and KPNO Tau 6 at 450 μm and 850 μm taken with the Submillimetre Common-User Bolometer Array on the James Clerk Maxwell Telescope. KPNO Tau 3 and KPNO Tau 6 have been previously identified as Class II objects hosting accretion disks, whereas KPNO Tau 1 has been identified as a Class III object and shows no evidence of circumsubstellar material. Our 3σ detection of cold dust around KPNO Tau 3 implies a total disk mass of (4.0 ± 1.1) ×  10−4 M☉ (assuming a gas to dust ratio of 100:1). We place tight constraints on any disks around KPNO Tau 1 or KPNO Tau 6 of <2.1 × 10−4 M☉ and <2.7 × 10−4 M☉, respectively. Modeling the spectral energy distribution of KPNO Tau 3 and its disk suggests the disk properties (geometry, dust mass, and grain size distribution) are consistent with observations of other brown dwarf disks and low-mass T-Tauri stars. In particular, the disk-to-host mass ratio for KPNO Tau 3 is congruent with the scenario that at least some brown dwarfs form via the same mechanism as low-mass stars.
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectBrown dwarfsen
dc.subjectCircumstellar matteren
dc.subjectProtoplanetary disksen
dc.subjectStars: formationen
dc.subjectStars: individual (KPNO Tau 3)en
dc.subjectStars: low-massen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleThe disk around the brown dwarf KPNO TAU 3en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/789/2/155
dc.description.statusPeer revieweden


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