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

Article

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

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

ApJ 876, 19 (2019)

doi ↗ arXiv:1903.09048 ↗

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 ☉. Our estimation of the pre-explosion mass-loss rate (\dot{M}∼ 3× {10}-7{--}1× {10}-6{M}ȯ 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.

Institute authors

Pejcha, Ondřej

Supported by

Primus/17/SCI/17 — Teorie a pozorování astronomických tranzientů: supernovy z hmotných hvězd a splynutí hvězd

BibTeX

@article{UTF718,
  author        = {Szalai, Tamás and Vinkó, József and Könyves-Tóth, Réka and Nagy, Andrea P. and Bostroem, K. Azalee and Sárneczky, Krisztián and Brown, Peter J. and Pejcha, Ondrej and Bódi, Attila and Cseh, Borbála and Csörnyei, Géza and Dencs, Zoltán and Hanyecz, Ottó and Ignácz, Bernadett and Kalup, Csilla and Kriskovics, Levente and Ordasi, András and Pál, András and Seli, Bálint and Sódor, Ádám Szakáts, Róbert and Vida, Krisztián and Zsidi, Gabriella and Konkoly Team and Arcavi, Iair and Ashall, Chris and Burke, Jamison and Galbany, Lluís and Hiramatsu, Daichi and Hosseinzadeh, Griffin and Hsiao, Eric Y. and Howell, D. Andrew and McCully, Curtis and Moran, Shane and Rho, Jeonghee and Sand, David J. and Shahbandeh, Melissa and Valenti, Stefano and Wang, Xiaofeng and Wheeler, J. Craig and Supernova Project, Global},
  title         = {{The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase}},
  journal       = {ApJ},
  volume        = {876},
  pages         = {19},
  year          = {2019},
  doi           = {10.3847/1538-4357/ab12d0},
  eprint        = {1903.09048},
  archivePrefix = {arXiv},
}