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dc.contributor.authorKonopacky, Quinn
dc.contributor.authorRameau, Julien
dc.contributor.authorDuchêne, Gaspard
dc.contributor.authorFilippazzo, Joseph C.
dc.contributor.authorGodfrey, Paige A. Giorla
dc.contributor.authorMarois, Christian
dc.contributor.authorNielsen, Eric L.
dc.contributor.authorPueyo, Laurent
dc.contributor.authorRafikov, Roman R.
dc.contributor.authorRice, Emily L.
dc.contributor.authorWang, Jason J.
dc.contributor.authorAmmons, S. Mark
dc.contributor.authorBailey, Vanessa P.
dc.contributor.authorBarman, Travis S.
dc.contributor.authorBulger, Joanna
dc.contributor.authorBruzzone, Sebastian
dc.contributor.authorChilcote, Jeffrey K.
dc.contributor.authorCotten, Tara
dc.contributor.authorDawson, Rebekah I.
dc.contributor.authorDe Rosa, Robert J.
dc.contributor.authorDoyon, René
dc.contributor.authorEsposito, Thomas M.
dc.contributor.authorFitzgerald, Michael P.
dc.contributor.authorFollette, Katherine B.
dc.contributor.authorGoodsell, Stephen J.
dc.contributor.authorGraham, James R.
dc.contributor.authorGreenbaum, Alexandra Z.
dc.contributor.authorHibon, Pascale
dc.contributor.authorHung, Li-Wei
dc.contributor.authorIngraham, Patrick
dc.contributor.authorKalas, Paul
dc.contributor.authorLafrenière, David
dc.contributor.authorLarkin, James E.
dc.contributor.authorMacintosh, Bruce A.
dc.contributor.authorMaire, Jérôme
dc.contributor.authorMarchis, Franck
dc.contributor.authorMarley, Mark S.
dc.contributor.authorMatthews, Brenda C.
dc.contributor.authorMetchev, Stanimir A.
dc.contributor.authorMillar-Blanchaer, Maxwell A.
dc.contributor.authorOppenheimer, Rebecca
dc.contributor.authorPalmer, David W.
dc.contributor.authorPatience, Jenny
dc.contributor.authorPerrin, Marshall
dc.contributor.authorPoyneer, Lisa A.
dc.contributor.authorRajan, Abhijith
dc.contributor.authorRantakyrö, Fredrik T.
dc.contributor.authorSavransky, Dmitry
dc.contributor.authorSchneider, Adam C.
dc.contributor.authorSivaramakrishnan, Anand
dc.contributor.authorSong, Inseok
dc.contributor.authorSoummer, Remi
dc.contributor.authorThomas, Sandrine
dc.contributor.authorWallace, J. Kent
dc.contributor.authorWard-Duong, Kimberly
dc.contributor.authorWiktorowicz, Sloane J.
dc.contributor.authorWolff, Schuyler
dc.date.accessioned2017-01-13T23:22:24Z
dc.date.available2017-01-13T23:22:24Z
dc.date.issued2016-09-14
dc.identifier.citationDISCOVERY OF A SUBSTELLAR COMPANION TO THE NEARBY DEBRIS DISK HOST HR 2562 2016, 829 (1):L4 The Astrophysical Journalen
dc.identifier.issn2041-8213
dc.identifier.doi10.3847/2041-8205/829/1/L4
dc.identifier.urihttp://hdl.handle.net/10150/621980
dc.description.abstractWe present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3 +/- 0.3 au (0".618 +/- 0".004) from the star. With the high astrometric precision afforded by GPI, we have confirmed, to more than 5 sigma, the common proper motion of HR 2562B with the star, with only a month-long time baseline between observations. Spectral data in the J-, H-, and K-bands show a morphological similarity to L/T transition objects. We assign a spectral type of L7 +/- 3 to HR 2562B. and derive a luminosity of log(L-bol/L-circle dot) = -4.62 +/- 0.12, corresponding to a mass of 30 +/- 15 M-Jup from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle that is consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown-dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk.
dc.description.sponsorshipFonds de Recherche du Quebec; NSF [AST-1518332, AST-1411868, AST-141378, AST-1211568, DGE-1232825, AST-1313132]; NASA [NNX15AD95G/NEXSS, NNX15AC89G, NNX14AJ80G]; U.S. Department of Energy [DE-AC52-07NA27344]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/2041-8205/829/i=1/a=L4?key=crossref.33d2aedc82fd4c31e50ea2590b78f63een
dc.rights© 2016. The American Astronomical Society. All rights reserved.en
dc.subjectbrown dwarfsen
dc.subjectinstrumentation: adaptive opticsen
dc.subjectplanet-disk interactionsen
dc.subjectstars: individual (HR 2562)en
dc.titleDISCOVERY OF A SUBSTELLAR COMPANION TO THE NEARBY DEBRIS DISK HOST HR 2562en
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalThe Astrophysical Journal Lettersen
dc.description.noteNo embargo.en
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.dateFOA2018-04-26T01:10:30Z
html.description.abstractWe present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3 +/- 0.3 au (0".618 +/- 0".004) from the star. With the high astrometric precision afforded by GPI, we have confirmed, to more than 5 sigma, the common proper motion of HR 2562B with the star, with only a month-long time baseline between observations. Spectral data in the J-, H-, and K-bands show a morphological similarity to L/T transition objects. We assign a spectral type of L7 +/- 3 to HR 2562B. and derive a luminosity of log(L-bol/L-circle dot) = -4.62 +/- 0.12, corresponding to a mass of 30 +/- 15 M-Jup from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle that is consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown-dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk.


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