SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries
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Fecha
2019-11-01
Profesor/a Guía
Facultad/escuela
Idioma
en_US
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ISSN de la revista
Título del volumen
Editor
Institute of Physics Publishing
Nombre de Curso
Licencia CC
ATRIBUCIÓN 4.0 INTERNACIONAL
Licencia CC
https://creativecommons.org/licenses/by/4.0/deed.es
Resumen
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.
Notas
Indexación: Scopus.
Palabras clave
Supernovae, Supernovae: General, Photometry
Citación
Astrophysical Journal Volume 885, Issue 1 1 November 2019 Article number 43
DOI
10.3847/1538-4357/ab43e3