학술논문
The Type II-P Supernova 2017eaw: from explosion to the nebular phase
Document Type
Working Paper
Author
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; 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
Source
Subject
Language
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 ($\dot{M} \sim3 \times 10^{-7} -$ $1\times 10^{-6} M_{\odot}$ 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.
Comment: 34 pages, 19 figures, 7 tables; accepted for publication in ApJ
Comment: 34 pages, 19 figures, 7 tables; accepted for publication in ApJ