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    L-BAND SPECTROSCOPY WITH MAGELLAN-AO/Clio2: FIRST RESULTS ON YOUNG LOW-MASS COMPANIONS

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    Stone_2016_ApJ_829_39.pdf
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    Description:
    FInal Published Version
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    Author
    Stone, Jordan M. cc
    Eisner, Josh A. cc
    Skemer, Andrew J. cc
    Morzinski, Katie M. cc
    Close, Laird M. cc
    Males, Jared R. cc
    Rodigas, Timothy J. cc
    Hinz, Phil
    Puglisi, Alfio
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2016-09-21
    Keywords
    binaries: close
    stars: atmospheres
    stars: low-mass
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    L-BAND SPECTROSCOPY WITH MAGELLAN-AO/Clio2: FIRST RESULTS ON YOUNG LOW-MASS COMPANIONS 2016, 829 (1):39 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2016. 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
    L-band spectroscopy is a powerful probe of cool low-gravity atmospheres: the P, Q, and R branch fundamental transitions of methane near 3.3 mu m provide a sensitive probe of carbon chemistry; cloud thickness modifies the spectral slope across the band; and H-3(+) opacity can be used to detect aurorae. Many directly imaged gas-giant companions to nearby young stars exhibit L-band fluxes distinct from the field population of brown dwarfs at the same effective temperature. Here we describe commissioning the L-band spectroscopic mode of Clio2, the 1-5 mu m instrument behind the Magellan adaptive-optics system. We use this system to measure L-band spectra of directly imaged companions. Our spectra are generally consistent with the parameters derived from previous near-infrared spectra for these late M to early L type objects. Therefore, deviations from the field sequence are constrained to occur below 1500 K. This range includes the L-T transition for field objects and suggests that observed discrepancies are due to differences in cloud structure and CO/CH4 chemistry.
    Note
    No embargo.
    ISSN
    1538-4357
    DOI
    10.3847/0004-637X/829/1/39
    Version
    Final published version
    Sponsors
    NASA [NNX11AK57G, NAS 5-26555]; NSF AAG grant [121329]; state of Arizona Technology Research Initiative Fund Imaging Fellowship; National Aeronautics and Space Administration through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51349, HST-HF2-51366.001-A]; California Institute of Technology - NASA through the Sagan Fellowship
    Additional Links
    http://stacks.iop.org/0004-637X/829/i=1/a=39?key=crossref.366e033367b4bd2b3ca8fe05a5fcc9d3
    ae974a485f413a2113503eed53cd6c53
    10.3847/0004-637X/829/1/39
    Scopus Count
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    UA Faculty Publications

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