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dc.contributor.authorChilcote, Jeffrey
dc.contributor.authorPueyo, Laurent
dc.contributor.authorDe Rosa, Robert J.
dc.contributor.authorVargas, Jeffrey
dc.contributor.authorMacintosh, Bruce
dc.contributor.authorBailey, Vanessa P.
dc.contributor.authorBarman, Travis S.
dc.contributor.authorBauman, Brian
dc.contributor.authorBruzzone, Sebastian
dc.contributor.authorBulger, Joanna
dc.contributor.authorBurrows, Adam
dc.contributor.authorCardwell, Andrew
dc.contributor.authorChen, Christine H.
dc.contributor.authorCotten, Tara
dc.contributor.authorDillon, Daren
dc.contributor.authorDoyon, Rene
dc.contributor.authorDraper, Zachary H.
dc.contributor.authorDuchêne, Gaspard
dc.contributor.authorDunn, Jennifer
dc.contributor.authorErikson, Darren
dc.contributor.authorFitzgerald, Michael P.
dc.contributor.authorFollette, Katherine B.
dc.contributor.authorGavel, Donald
dc.contributor.authorGoodsell, Stephen J.
dc.contributor.authorGraham, James R.
dc.contributor.authorGreenbaum, Alexandra Z.
dc.contributor.authorHartung, Markus
dc.contributor.authorHibon, Pascale
dc.contributor.authorHung, Li-Wei
dc.contributor.authorIngraham, Patrick
dc.contributor.authorKalas, Paul
dc.contributor.authorKonopacky, Quinn
dc.contributor.authorLarkin, James E.
dc.contributor.authorMaire, Jérôme
dc.contributor.authorMarchis, Franck
dc.contributor.authorMarley, Mark S.
dc.contributor.authorMarois, Christian
dc.contributor.authorMetchev, Stanimir A.
dc.contributor.authorMillar-Blanchaer, Maxwell A.
dc.contributor.authorMorzinski, Katie M.
dc.contributor.authorNielsen, Eric L.
dc.contributor.authorNorton, Andrew
dc.contributor.authorOppenheimer, Rebecca
dc.contributor.authorPalmer, David
dc.contributor.authorPatience, Jennifer
dc.contributor.authorPerrin, Marshall
dc.contributor.authorPoyneer, Lisa
dc.contributor.authorRajan, Abhijith
dc.contributor.authorRameau, Julien
dc.contributor.authorRantakyrö, Fredrik T.
dc.contributor.authorSadakuni, Naru
dc.contributor.authorSaddlemyer, Leslie
dc.contributor.authorSavransky, Dmitry
dc.contributor.authorSchneider, Adam C.
dc.contributor.authorSerio, Andrew
dc.contributor.authorSivaramakrishnan, Anand
dc.contributor.authorSong, Inseok
dc.contributor.authorSoummer, Remi
dc.contributor.authorThomas, Sandrine
dc.contributor.authorWallace, J. Kent
dc.contributor.authorWang, Jason J.
dc.contributor.authorWard-Duong, Kimberly
dc.contributor.authorWiktorowicz, Sloane
dc.contributor.authorWolff, Schuyler
dc.date.accessioned2017-06-02T00:26:56Z
dc.date.available2017-06-02T00:26:56Z
dc.date.issued2017-03-28
dc.identifier.citation1–2.4 μm Near-IR Spectrum of the Giant Planet β Pictoris b Obtained with the Gemini Planet Imager 2017, 153 (4):182 The Astronomical Journalen
dc.identifier.issn1538-3881
dc.identifier.doi10.3847/1538-3881/aa63e9
dc.identifier.urihttp://hdl.handle.net/10150/623806
dc.description.abstractUsing the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 mu m) spectrum of the planetary companion to the nearby, young star beta. Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9. +/- 0.2. M-Jup, an effective temperature of 1724. +/- 15 K, a radius of 1.46. +/- 0.01. R-Jup, and a surface gravity of log g = 4.18. 0.01 [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of log g = 3.5-4.0 [dex] depending upon the model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of beta Pic. b best matches a low surface gravity L2. +/- 1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677- 381210 and 2MASS J03552337 + 1133437.
dc.description.sponsorshipGemini Observatory; Dunlap Institute, University of Toronto; NSF Center for Adaptive Optics at UC Santa Cruz; NSF [AST-0909188, AST-1211562, AST-1405505]; NASA Origins [NNX11AD21G, NNX10AH31G, NNX14AC21G, NNX15AC89G]; NASA NExSS [NNX15AD95G]; University of California Office of the President [LFRP-118057]; Science and Technology Facilities Council [ST/H002707/1]; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; California Institute of Technology/Jet Propulsion Laboratory - NASA through Sagan Fellowship Program; NASA Exoplanets Research Program (XRP) [NNX16AD44G]; NASA through Hubble Fellowship - Space Telescope Science Institute [51378.01-A]; NASA [NAS5-26555]; NASAs Science Mission Directorateen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/1538-3881/153/i=4/a=182?key=crossref.d395686510ceddbbe285c40d7dfaddc3en
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectinstrumentation: adaptive opticsen
dc.subjectplanetary systemsen
dc.subjectstars: individual (beta Pictoris)en
dc.subjecttechniques:spectroscopicen
dc.title1–2.4 μm Near-IR Spectrum of the Giant Planet β Pictoris b Obtained with the Gemini Planet Imageren
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalThe Astronomical 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.dateFOA2018-09-11T19:45:50Z
html.description.abstractUsing the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 mu m) spectrum of the planetary companion to the nearby, young star beta. Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9. +/- 0.2. M-Jup, an effective temperature of 1724. +/- 15 K, a radius of 1.46. +/- 0.01. R-Jup, and a surface gravity of log g = 4.18. 0.01 [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of log g = 3.5-4.0 [dex] depending upon the model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of beta Pic. b best matches a low surface gravity L2. +/- 1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677- 381210 and 2MASS J03552337 + 1133437.


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