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    The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction

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    Author
    Bhirombhakdi, Kornpob
    Chornock, Ryan
    Miller, Adam A
    Filippenko, Alexei V
    Cenko, S Bradley
    Smith, Nathan
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2019-07-25
    Keywords
    circumstellar matter
    supernovae: individual (SN 2008es)
    
    Metadata
    Show full item record
    Publisher
    OXFORD UNIV PRESS
    Citation
    Kornpob Bhirombhakdi, Ryan Chornock, Adam A Miller, Alexei V Filippenko, S Bradley Cenko, Nathan Smith, The Type II superluminous SN 2008es at late times: near-infrared excess and circumstellar interaction, Monthly Notices of the Royal Astronomical Society, Volume 488, Issue 3, September 2019, Pages 3783–3793, https://doi.org/10.1093/mnras/stz1928
    Journal
    MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
    Rights
    Copyright © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
    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
    SN 2008es is one of the rare cases of a Type II superluminous supernova (SLSN), showing no narrow features in its early-time spectra, and therefore, its powering mechanism is under debate between circumstellar interaction (CSI) and magnetar spin-down. Late-time data are required for better constraints. We present optical and near-infrared (NIR) photometry obtained from Gemini, Keck, and Palomar Observatories from 192 to 554 d after explosion. Only broad H α emission is detected in a Gemini spectrum at 288 d. The line profile exhibits red-wing attenuation relative to the early-time spectrum. In addition to the cooling SN photosphere, an NIR excess with blackbody temperature ∼1500 K and radius ∼1016 cm is observed. This evidence supports dust condensation in the cool dense shell being responsible for the spectral evolution and NIR excess. We favour CSI, with ∼2–3 M⊙ of circumstellar material (CSM) and ∼10–20 M⊙ of ejecta, as the powering mechanism, which still dominates at our late-time epochs. Both models of uniform density and steady wind fit the data equally well, with an effective CSM radius ∼1015 cm, supporting the efficient conversion of shock energy to radiation by CSI. A low amount (≲0.4 M⊙) of 56Ni is possible but cannot be verified yet, since the light curve is dominated by CSI. The magnetar spin-down powering mechanism cannot be ruled out, but is less favoured because it overpredicts the late-time fluxes and may be inconsistent with the presence of dust.
    ISSN
    0035-8711
    DOI
    10.1093/mnras/stz1928
    Version
    Final published version
    Sponsors
    National Aeronautics and Space Administration (NASA)National Aeronautics & Space Administration (NASA) [80NSSC18K0665]; NSFNational Science Foundation (NSF) [PHY-1607611]; TABASGO Foundation; Christopher R. Redlich Fund; Miller Institute for Basic Research in Science (U.C. Berkeley); NSF (United States)National Science Foundation (NSF) [GN-2009A-Q-48]; National Research Council (Canada) [GN-2009A-Q-48]; CONICYT (Chile)Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) [GN-2009A-Q-48]; Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) [GN-2009A-Q-48]; Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) [GN-2009A-Q-48]; W. M. Keck FoundationW.M. Keck Foundation; NASANational Aeronautics & Space Administration (NASA)
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stz1928
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