The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase

Tamás Szalai, József Vinkó, Réka Könyves-Tóth, Andrea P. Nagy, K. Azalee Bostroem, Krisztián Sárneczky, Peter J. Brown, Ondrej Pejcha, Attila Bódi, Borbála Cseh, Géza Csörnyei, Zoltán Dencs, Ottó Hanyecz, Bernadett Ignácz, Csilla Kalup, Levente Kriskovics, András Ordasi, András Pál, Bálint Seli, Ádám SódorRóbert Szakáts, Krisztián Vida, Gabriella Zsidi, Iair Arcavi, Chris Ashall, Jamison Burke, Lluís Galbany, Daichi Hiramatsu, Griffin Hosseinzadeh, Eric Y. Hsiao, D. Andrew Howell, Curtis McCully, Shane Moran, Jeonghee Rho, David J. Sand, Melissa Shahbandeh, Stefano Valenti, Xiaofeng Wang, J. Craig Wheeler

Research output: Contribution to journalArticlepeer-review

25 Scopus citations

Abstract

The nearby SN 2017eaw is a Type II-P ("plateau") supernova (SN) showing early-time, moderate CSM interaction. We present a comprehensive study of this SN, including the analysis of high-quality optical photometry and spectroscopy covering the very early epochs up to the nebular phase, as well as near-ultraviolet and near-infrared spectra and early-time X-ray and radio data. The combined data of SNe 2017eaw and 2004et allow us to get an improved distance to the host galaxy, NGC 6946, of D ∼ 6.85 ± 0.63 Mpc; this fits into recent independent results on the distance of the host and disfavors the previously derived (30% shorter) distances based on SN 2004et. From modeling the nebular spectra and the quasi-bolometric light curve, we estimate the progenitor mass and some basic physical parameters for the explosion and ejecta. Our results agree well with previous reports on a red supergiant progenitor star with a mass of ∼15-16 M o. Our estimation of the pre-explosion mass-loss rate ( yr-1) agrees well with previous results based on the opacity of the dust shell enshrouding the progenitor, but it is orders of magnitude lower than previous estimates based on general light-curve modeling of Type II-P SNe. Combining late-time optical and mid-infrared data, a clear excess at 4.5 μm can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw.

Original languageEnglish (US)
Article number19
JournalAstrophysical Journal
Volume876
Issue number1
DOIs
StatePublished - May 1 2019

Keywords

  • supernovae: general
  • supernovae: individual (SN 2017eaw)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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