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, T.; Vinkó, J.; Könyves-Tóth, R.; Nagy, A. P.; Bostroem, K. A.; Sárneczky, K.; Brown, P. J.; Pejcha, O.; Bódi, A.; Cseh, B.; Csörnyei, G.; Dencs, Z.; Hanyecz, O.; Ignácz, B.; Kalup, C.; Kriskovics, L.; Ordasi, A.; Pál, A.; Seli, B.; Sódor, Á.; Szakáts, R.; Vida, K.; Zsidi, G.; Konkoly Team; Arcavi, I.; Ashall, C.; Burke, J.; Galbany, L.; Hiramatsu, D.; Hosseinzadeh, G.; Hsiao, E. Y.; Howell, D. A.; McCully, C.; Moran, S.; Rho, J.; Sand, D. J.; Shahbandeh, M.; Valenti, S.; Wang, X.; Wheeler, J. C.; Supernova Project, G.

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, T. and Vinkó, J. and Könyves-Tóth, R. and Nagy, A. P. and Bostroem, K. A. and Sárneczky, K. and Brown, P. J. and Pejcha, O. and Bódi, A. and Cseh, B. and Csörnyei, G. and Dencs, Z. and Hanyecz, O. and Ignácz, B. and Kalup, C. and Kriskovics, L. and Ordasi, A. and Pál, A. and Seli, B. and Sódor, Á. and Szakáts, R. and Vida, K. and Zsidi, G. and Konkoly Team and Arcavi, I. and Ashall, C. and Burke, J. and Galbany, L. and Hiramatsu, D. and Hosseinzadeh, G. and Hsiao, E. Y. and Howell, D. A. and McCully, C. and Moran, S. and Rho, J. and Sand, D. J. and Shahbandeh, M. and Valenti, S. and Wang, X. and Wheeler, J. C. and Supernova Project, G.},
  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},
}