SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

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  • Jennifer E. Andrews, University of Arizona
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  • D. J. Sand, Steward Observatory, University of Arizona, Tucson, University of Arizona
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  • S. Valenti, University of California at Davis
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  • Nathan Smith, Steward Observatory, University of Arizona, Tucson, University of Arizona
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  • Raya Dastidar, Aryabhatta Research Institute of Observational Sciences, University of Delhi
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  • D. K. Sahu, Indian Institute of Astrophysics
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  • Kuntal Misra, University of California at Davis, Aryabhatta Research Institute of Observational Sciences
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  • Avinash Singh, Indian Institute of Astrophysics, Indian Institute of Science
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  • D. Hiramatsu, University of California at Santa Barbara, Las Cumbres Observatory Global Telescope Network, Inc
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  • P. J. Brown, Texas A and M University
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  • G. Hosseinzadeh, Harvard-Smithsonian Center for Astrophysics
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  • S. Wyatt, University of Arizona
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  • J. Vinko, Hungarian Academy of Sciences, University of Texas at Austin
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  • G. C. Anupama, Indian Institute of Astrophysics
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  • I. Arcavi, Tel Aviv University
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  • Chris Ashall, Florida State University
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  • S. Benetti, INAF - Osservatorio Astronomico di Padova
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  • Marco Berton, University of Turku, Aalto University
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  • K. A. Bostroem, University of California at Davis
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  • M. Bulla, Stockholm University
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  • J. Burke, University of California at Santa Barbara, Las Cumbres Observatory Global Telescope Network, Inc
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  • S. Chen, INAF - Osservatorio Astronomico di Padova, Center for Astrophysics, Guangzhou University
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  • L. Chomiuk, Michigan State University
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  • A. Cikota, Lawrence Berkeley National Laboratory
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  • E. Congiu, Carnegie Institution of Washington, Osservatorio Astronomico di Brera
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  • B. Cseh, Hungarian Academy of Sciences
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  • Scott Davis, Florida State University
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  • N. Elias-Rosa, CSIC, Institute of Space Studies of Catalonia
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  • T. Faran, The Hebrew University
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  • Morgan Fraser, University College Dublin, Dublin
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  • L. Galbany, University of Pittsburgh
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  • C. Gall
  • A. Gal-Yam, Department of Chemical Physics, Weizmann Institute of Science, Rehovot, Israel.
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  • Anjasha Gangopadhyay, Aryabhatta Research Institute of Observational Sciences, Pt. Ravishankar Shukla University
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  • M. Gromadzki, University of Warsaw
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  • J. Haislip, The University of North Carolina at Chapel Hill, Department of Genetics, Chapel Hill, United States
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  • D. A. Howell, University of California at Santa Barbara, Las Cumbres Observatory Global Telescope Network, Inc
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  • E. Y. Hsiao, Florida State University
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  • C. Inserra, Cardiff University
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  • E. Kankare, University of Turku
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  • H. Kuncarayakti, University of Turku, University of Turku
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  • V. Kouprianov, The University of North Carolina at Chapel Hill, Department of Genetics, Chapel Hill, United States, Central Astronomical Observatory at Pulkovo of Russian Academy of Sciences
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  • Brajesh Kumar, Indian Institute of Astrophysics
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  • Xue Li, Tsinghua University
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  • Han Lin, Tsinghua University
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  • K. Maguire, Trinity College Dublin
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  • P. Mazzali, Liverpool John Moores University, Max-Planck-Institut für Astrophysik
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  • C. McCully, University of California at Santa Barbara, Las Cumbres Observatory Global Telescope Network, Inc
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  • P. Milne, University of Arizona
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  • Jun Mo, Tsinghua University
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  • N. Morrell, Carnegie Institution of Washington
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  • M. Nicholl, University of Edinburgh, Institute for Astronomy
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  • P. Ochner, INAF - Osservatorio Astronomico di Padova
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  • F. Olivares, Universidad de Atacama, Millennium Institute of Astrophysics
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  • A. Pastorello, INAF - Osservatorio Astronomico di Padova
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  • F. Patat, European Southern Observatory
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  • M. Phillips, Carnegie Institution of Washington
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  • G. Pignata, Millennium Institute of Astrophysics, Universidad Andres Bello
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  • S. Prentice, Trinity College Dublin
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  • A. Reguitti, Millennium Institute of Astrophysics, Universidad Andres Bello
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  • D. E. Reichart, The University of North Carolina at Chapel Hill, Department of Genetics, Chapel Hill, United States
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  • Rodríguez, Millennium Institute of Astrophysics, Universidad Andres Bello
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  • Liming Rui, Tsinghua University
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  • Pankaj Sanwal, Aryabhatta Research Institute of Observational Sciences, Pt. Ravishankar Shukla University
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  • K. Sárneczky, Hungarian Academy of Sciences
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  • M. Shahbandeh, Florida State University
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  • Mridweeka Singh, Aryabhatta Research Institute of Observational Sciences, Pt. Ravishankar Shukla University
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  • S. Smartt, Queen's University, Belfast
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  • J. Strader, Michigan State University
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  • M. D. Stritzinger
  • R. Szakáts, Hungarian Academy of Sciences
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  • L. Tartaglia, Department, Stockholm University, AlbaNova University Center, SE-106 91 Stockholm
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  • Huijuan Wang, CAS - National Astronomical Observatories
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  • Lingzhi Wang, CAS - National Astronomical Observatories, Chinese Academy of Sciences South America Center for Astronomy
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  • Xiaofeng Wang, Tsinghua University
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  • J. C. Wheeler, University of Texas at Austin
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  • Danfeng Xiang, Tsinghua University
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  • O. Yaron, Department of Chemical Physics, Weizmann Institute of Science, Rehovot, Israel.
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  • D. R. Young, Queen's University, Belfast
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  • Junbo Zhang, CAS - National Astronomical Observatories

We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M o of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

Original languageEnglish
Article number43
JournalAstrophysical Journal
Volume885
Number of pages23
ISSN0004-637X
DOIs
Publication statusPublished - 1 Nov 2019

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