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

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dc.contributor.authorAndrews, Jennifer E.
dc.contributor.authorSand D.J.
dc.contributor.authorValenti S.
dc.contributor.authorSmith, Nathan
dc.contributor.authorDastidar, Raya
dc.contributor.authorSahu D.K.
dc.contributor.authorMisra, Kuntal
dc.contributor.authorSingh, Avinash
dc.contributor.authorHiramatsu D.
dc.contributor.authorBrown P.J.
dc.contributor.authorHosseinzadeh G.
dc.contributor.authorWyatt S.
dc.contributor.authorVinko J.
dc.contributor.authorAnupama G.C.
dc.contributor.authorArcavi I.
dc.contributor.authorAshall, Chris
dc.contributor.authorBenetti S.
dc.contributor.authorBerton, Marco
dc.contributor.authorBostroem K.A.
dc.contributor.authorBulla M.
dc.contributor.authorBurke J.
dc.contributor.authorChen S.
dc.contributor.authorChomiuk L.
dc.contributor.authorCikota A.
dc.contributor.authorCongiu E.
dc.contributor.authorCseh B.
dc.contributor.authorDavis, Scott
dc.contributor.authorElias-Rosa N.
dc.contributor.authorFaran T.
dc.contributor.authorFraser, Morgan
dc.contributor.authorGalbany L.
dc.contributor.authorGall C.
dc.contributor.authorGal-Yam A.
dc.contributor.authorGangopadhyay, Anjasha
dc.contributor.authorGromadzki M.
dc.contributor.authorHaislip J.
dc.contributor.authorHowell D.A.
dc.contributor.authorHsiao E.Y.
dc.contributor.authorInserra C.
dc.contributor.authorKankare E.
dc.contributor.authorKuncarayakti H.
dc.contributor.authorKouprianov V.
dc.contributor.authorKumar, Brajesh
dc.contributor.authorLi, Xue
dc.contributor.authorLin, Han
dc.contributor.authorMaguire K.
dc.contributor.authorMazzali P.
dc.contributor.authorMcCully C.
dc.contributor.authorMilne P.
dc.contributor.authorMo, Jun
dc.contributor.authorMorrell N.
dc.contributor.authorNicholl M.
dc.contributor.authorOchner P.
dc.contributor.authorOlivares F.
dc.contributor.authorPastorello A.
dc.contributor.authorPatat F.
dc.contributor.authorPhillips M.
dc.contributor.authorPignata G.
dc.contributor.authorPrentice S.
dc.contributor.authorReguitti A.
dc.contributor.authorReichart D.E.
dc.contributor.authorRodríguez Ó.
dc.contributor.authorRui, Liming
dc.contributor.authorSanwal, Pankaj
dc.contributor.authorSárneczky K.
dc.contributor.authorShahbandeh M.
dc.contributor.authorSingh, Mridweeka
dc.contributor.authorSmartt S.
dc.contributor.authorStrader J.
dc.contributor.authorStritzinger M.D.
dc.contributor.authorSzakáts R.
dc.contributor.authorTartaglia L.
dc.contributor.authorWang, Huijuan
dc.contributor.authorWang, Lingzhi
dc.contributor.authorWang, Xiaofeng
dc.contributor.authorWheeler J.C.
dc.contributor.authorXiang, Danfeng
dc.contributor.authorYaron O.
dc.contributor.authorYoung D.R.
dc.contributor.authorZhang, Junbo
dc.date.accessioned2024-07-04T19:47:14Z
dc.date.available2024-07-04T19:47:14Z
dc.date.issued2019-11-01
dc.descriptionIndexación: Scopus.
dc.description.abstractWe 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.
dc.description.urihttps://iopscience.iop.org/article/10.3847/1538-4357/ab43e3/pdf
dc.identifier.citationAstrophysical Journal Volume 885, Issue 1 1 November 2019 Article number 43
dc.identifier.doi10.3847/1538-4357/ab43e3
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/58203
dc.language.isoen_US
dc.publisherInstitute of Physics Publishing
dc.rights.licenseATRIBUCIÓN 4.0 INTERNACIONAL
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectSupernovae
dc.subjectSupernovae: General
dc.subjectPhotometry
dc.titleSN 2017gmr: An Energetic Type II-P Supernova with Asymmetries
dc.typeArtículo
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