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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 Sódor
; Róbert 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
; | | Date: |
21 Mar 2019 | | Abstract: | The nearby SN 2017eaw is a Type II-P (’’plateau’) supernova 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-UV 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, as $D sim 6.85$ $pm 0.63$ Mpc; this fits in 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 the ejecta. Our
results agree well with previous reports on a RSG progenitor star with a mass
of $sim15-16$ M$_odot$. Our estimation on the pre-explosion mass-loss rate
($dot{M} sim3 imes 10^{-7} -$ $1 imes 10^{-6} M_{odot}$ 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. | | Source: | arXiv, 1903.9048 | | Services: | Forum | Review | PDF | Favorites | |
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