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    Characterizing 51 Eri b from 1 to 5 mu m: A Partly Cloudy Exoplanet

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    Rajan_2017_AJ_154_10.pdf
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    Description:
    FInal Published Version
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    Author
    Rajan, Abhijith cc
    Rameau, Julien cc
    De Rosa, Robert J. cc
    Marley, Mark S. cc
    Graham, James R.
    Macintosh, Bruce cc
    Marois, Christian cc
    Morley, Caroline V. cc
    Patience, Jenny cc
    Pueyo, Laurent
    Saumon, Didier cc
    Ward-Duong, Kimberly cc
    Ammons, S. Mark cc
    Arriaga, Pauline cc
    Bailey, Vanessa P.
    Barman, Travis S. cc
    Bulger, Joanna cc
    Burrows, Adam cc
    Chilcote, Jeffrey cc
    Cotten, Tara cc
    Czekala, I. cc
    Doyon, Rene
    Duchêne, Gaspard cc
    Esposito, Thomas M. cc
    Fitzgerald, Michael P. cc
    Follette, Katherine B. cc
    Fortney, Jonathan J. cc
    Goodsell, Stephen J. cc
    Greenbaum, Alexandra Z. cc
    Hibon, Pascale cc
    Hung, Li-Wei cc
    Ingraham, Patrick cc
    Johnson-Groh, Mara cc
    Kalas, Paul
    Konopacky, Quinn cc
    Lafrenière, David cc
    Larkin, James E. cc
    Maire, Jérôme
    Marchis, Franck cc
    Metchev, Stanimir A. cc
    Millar-Blanchaer, Maxwell A. cc
    Morzinski, Katie M. cc
    Nielsen, Eric L. cc
    Oppenheimer, Rebecca cc
    Palmer, David cc
    Patel, Rahul I. cc
    Perrin, Marshall cc
    Poyneer, Lisa
    Rantakyrö, Fredrik T. cc
    Ruffio, Jean-Baptiste cc
    Savransky, Dmitry cc
    Schneider, Adam C. cc
    Sivaramakrishnan, Anand cc
    Song, Inseok cc
    Soummer, Remi cc
    Thomas, Sandrine cc
    Vasisht, Gautam
    Wallace, J. Kent cc
    Wang, Jason J. cc
    Wiktorowicz, Sloane cc
    Wolff, Schuyler cc
    Show allShow less
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2017-06-16
    Keywords
    instrumentation: adaptive optics
    planets and satellites: atmospheres
    planets and satellites: composition
    planets and satellites: gaseous planets
    stars: individual (51 Eridani)
    
    Metadata
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    Publisher
    IOP PUBLISHING LTD
    Citation
    Characterizing 51 Eri b from 1 to 5 mu m: A Partly Cloudy Exoplanet 2017, 154 (1):10 The Astronomical Journal
    Journal
    The Astronomical Journal
    Rights
    © 2017. The American Astronomical Society. All rights reserved.
    Collection Information
    This 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.
    Abstract
    We present spectrophotometry spanning 1-5 mu m of 51 Eridani b, a 2-10 M-Jup planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90-2.19 mu m) and K2 (2.10-2.40 mu m) spectra taken with the Gemini Planet Imager as well as an updated L-P (3.76 mu m) and new M-S (4.67 mu m) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13-1.35 mu m) and H (1.50-1.80 mu m) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri. b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 (logL/L circle dot),leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M-circle plus.
    ISSN
    1538-3881
    DOI
    10.3847/1538-3881/aa74db
    Version
    Final published version
    Sponsors
    NSF [AST1411868, AST-1518332, DGE-1311230]; NASA [NNX14AJ80G]; Fonds de Recherche du Quebec; NASA Exoplanets Research Program (XRP) [NNX16AD44G]; JPL's ESI program for GPIrelated; NASA's Science Mission Directorate; NExSS [NNX15AD95G]; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
    Additional Links
    http://stacks.iop.org/1538-3881/154/i=1/a=10?key=crossref.1003c48a2a47e76fe3105f3696486f43
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-3881/aa74db
    Scopus Count
    Collections
    UA Faculty Publications

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