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dc.contributor.authorMacGregor, Meredith A.
dc.contributor.authorWilner, D.
dc.contributor.authorCzekala, I.
dc.contributor.authorAndrews, S. M.
dc.contributor.authorDai, Y. Sophia
dc.contributor.authorHerczeg, Gregory J.
dc.contributor.authorKratter, Kaitlin M.
dc.contributor.authorKraus, Adam L.
dc.contributor.authorRicci, Luca
dc.contributor.authorTesti, L.
dc.date.accessioned2017-03-27T21:42:38Z
dc.date.available2017-03-27T21:42:38Z
dc.date.issued2017-01-16
dc.identifier.citationALMA MEASUREMENTS OF CIRCUMSTELLAR MATERIAL IN THE GQ LUP SYSTEM 2017, 835 (1):17 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/835/1/17
dc.identifier.urihttp://hdl.handle.net/10150/622871
dc.description.abstractWe present Atacama Large Millimeter/submillimeter Array observations of the GQ Lup system, a young Sun-like star with a substellar-mass companion in a wide-separation orbit. These observations of 870 mu m continuum and CO J = 3-2 line emission with beam size similar to 0."3 (similar to 45 au) resolve the disk of dust and gas surrounding the primary star, GQ Lup A, and provide deep limits on any circumplanetary disk surrounding the companion, GQ Lup b. The circumprimary dust disk is compact with an FWHM of 59 +/- 12 au, while the gas has a larger extent with a characteristic radius of 46.5 +/- 1.8 au. By forward-modeling the velocity field of the circumprimary disk based on the CO emission, we constrain the mass of GQ Lup. A to be M-* = (1.03 +/- 0.05) * (d/156 pc) M-circle dot, where d is a known distance, and determine that we view the disk at an inclination angle of 60 degrees 5 +/- 0 degrees 5 and a position angle of 346 degrees +/- 1 degrees. The 3s upper limit on the 870 mu m flux density of any circumplanetary disk associated with GQ Lup b of <0.15 mJy implies an upper limit on the dust disk mass of <0.04M(circle dot) for standard assumptions about optically thin emission. We discuss proposed mechanisms for the formation of wide-separation substellar companions given the non-detection of circumplanetary disks around GQ Lup b and other similar systems.
dc.description.sponsorshipNational Science Foundation Graduate Research Fellowship [DGE1144152]; NRAO Student Observing Supporten
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/835/i=1/a=17?key=crossref.01ef6673c14afa27fd9da2d99156af18en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectcircumstellar matteren
dc.subjectstars: individual (GQ Lup)en
dc.subjectsubmillimeter: planetary systemsen
dc.titleALMA MEASUREMENTS OF CIRCUMSTELLAR MATERIAL IN THE GQ LUP SYSTEMen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Astronen
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.dateFOA2018-06-16T11:19:06Z
html.description.abstractWe present Atacama Large Millimeter/submillimeter Array observations of the GQ Lup system, a young Sun-like star with a substellar-mass companion in a wide-separation orbit. These observations of 870 mu m continuum and CO J = 3-2 line emission with beam size similar to 0."3 (similar to 45 au) resolve the disk of dust and gas surrounding the primary star, GQ Lup A, and provide deep limits on any circumplanetary disk surrounding the companion, GQ Lup b. The circumprimary dust disk is compact with an FWHM of 59 +/- 12 au, while the gas has a larger extent with a characteristic radius of 46.5 +/- 1.8 au. By forward-modeling the velocity field of the circumprimary disk based on the CO emission, we constrain the mass of GQ Lup. A to be M-* = (1.03 +/- 0.05) * (d/156 pc) M-circle dot, where d is a known distance, and determine that we view the disk at an inclination angle of 60 degrees 5 +/- 0 degrees 5 and a position angle of 346 degrees +/- 1 degrees. The 3s upper limit on the 870 mu m flux density of any circumplanetary disk associated with GQ Lup b of <0.15 mJy implies an upper limit on the dust disk mass of <0.04M(circle dot) for standard assumptions about optically thin emission. We discuss proposed mechanisms for the formation of wide-separation substellar companions given the non-detection of circumplanetary disks around GQ Lup b and other similar systems.


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