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    The Early Discovery of SN 2017ahn: Signatures of Persistent Interaction in a Fast-declining Type II Supernova

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    Author
    Tartaglia, L.
    Sand, D. J.
    Groh, J. H.
    Valenti, S. cc
    Wyatt, S. D.
    Bostroem, K. A.
    Brown, P. J.
    Yang, S.
    Burke, J.
    Chen, T.-W. cc
    Davis, S.
    Förster, F.
    Galbany, L.
    Haislip, J.
    Hiramatsu, D.
    Hosseinzadeh, G. cc
    Howell, D. A. cc
    Hsiao, E. Y.
    Jha, S. W. cc
    Kouprianov, V.
    Kuncarayakti, H.
    Lyman, J. D.
    McCully, C. cc
    Phillips, M. M.
    Rau, A. cc
    Reichart, D. E.
    Shahbandeh, M.
    Strader, J. cc
    Show allShow less
    Affiliation
    Steward Observatory, University of Arizona
    Issue Date
    2021-01-28
    
    Metadata
    Show full item record
    Publisher
    IOP Publishing Ltd
    Citation
    Tartaglia, L., Sand, D. J., Groh, J. H., Valenti, S., Wyatt, S. D., Bostroem, K. A., ... & Strader, J. (2021). The Early Discovery of SN 2017ahn: Signatures of Persistent Interaction in a Fast-declining Type II Supernova. The Astrophysical Journal, 907(1), 52.
    Journal
    Astrophysical Journal
    Rights
    © 2021. 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 high-cadence, comprehensive data on the nearby (D; 33 Mpc) Type II supernova (SN II) 2017ahn, discovered within about one day of the explosion, from the very early phases after explosion to the nebular phase. The observables of SN 2017ahn show a significant evolution over the;470 days of our follow-up campaign, first showing prominent, narrow Balmer lines and other high-ionization features purely in emission (i.e., flash spectroscopy features), which progressively fade and lead to a spectroscopic evolution similar to that of more canonical SNe II. Over the same period, the decline of the light curves in all bands is fast, resembling the photometric evolution of linearly declining H-rich core-collapse SNe. The modeling of the light curves and early flash spectra suggests that a complex circumstellar medium surrounds the progenitor star at the time of explosion, with a first dense shell produced during the very late stages of its evolution that is swept up by the rapidly expanding ejecta within the first ∼6 days of the SN evolution, while signatures of interaction are observed also at later phases. Hydrodynamical models support the scenario in which linearly declining SNe II are predicted to arise from massive yellow super- or hypergiants depleted of most of their hydrogen layers. © 2021. The American Astronomical Society. All rights reserved.
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/abca8a
    Version
    Final published version
    Sponsors
    NSF
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/abca8a
    Scopus Count
    Collections
    UA Faculty Publications

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