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

Andrews, Jennifer E. and Sand, D. J. and Valenti, S. and Smith, Nathan and Dastidar, Raya and Vinkó, József and Cseh, Borbála and Sárneczky, Krisztián and Szakáts, Róbert (2019) SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries. ASTROPHYSICAL JOURNAL, 885 (1). ISSN 1538-4357

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Abstract

We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discover through the first 180 days. SN 2017gmr does not show signs of narrow high-ionization emission lines in the early optical spectra, yet th optical light-curve evolution suggests that an extra energy source fro circumstellar medium (CSM) interaction must be present for at least days after explosion. Modeling of the early light curve indicates a ∼50 R ☉ progenitor radius, consistent with a rather compact re supergiant, and late-time luminosities indicate that up to 0.130 ± 0.02 M ☉ of 56Ni are present, if the light curve i solely powered by radioactive decay, although the 56Ni mas may be lower if CSM interaction contributes to the post-platea luminosity. Prominent multipeaked emission lines of Hα and [O I] emerg after day 154, as a result of either an asymmetric explosion o asymmetries in the CSM. The lack of narrow lines within the first 2 day of explosion in the likely presence of CSM interaction may be an exampl of close, dense, asymmetric CSM that is quickly enveloped by th spherical supernova ejecta

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