A1 Refereed original research article in a scientific journal
The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase
Authors: Szalai T, Vinko J, Konyves-Toth R, Nagy AP, Bostroem KA, Sarneczky K, Brown PJ, Pejcha O, Bodi A, Cseh B, Csornyei G, Dencs Z, Hanyecz O, Ignacz B, Kalup C, Kriskovics L, Ordasi A, Pal A, Seli B, Sodor A, Szakats R, Vida K, Zsidi G, Arcavi I, Ashall C, Burke J, Galbany L, Hiramatsu D, Hosseinzadeh G, Hsiao EY, Howell DA, McCully C, Moran S, Rho J, Sand DJ, Shahbandeh M, Valenti S, Wang XF, Wheeler JC
Publisher: IOP PUBLISHING LTD
Publication year: 2019
Journal:: Astrophysical Journal
Journal name in source: ASTROPHYSICAL JOURNAL
Journal acronym: ASTROPHYS J
Article number: ARTN 19
Volume: 876
Issue: 1
Number of pages: 24
ISSN: 0004-637X
eISSN: 1538-4357
DOI: https://doi.org/10.3847/1538-4357/ab12d0
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/40677752
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 similar to 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 similar to 15-16 M-circle dot. Our estimation of the pre-explosion mass-loss rate ((M)over dot similar to 3 x 10(-7)-1 x 10(-6)M(circle dot) 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 mu m can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw.
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