The Type II-P Supernova 2017eaw: from explosion to the nebular phase

• Published in: arXiv.org
• Main Authors: 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, Krisztián Vida, Zsidi, Gabriella, Arcavi, Iair, Ashall, Chris, Burke, Jamison, Galbany, Lluís, Hiramatsu, Daichi, Griffin Hosseinzadeh, Hsiao, Eric Y, Howell, D Andrew, McCully, Curtis, Moran, Shane, Rho, Jeonghee, Sand, David J, Shahbandeh, Melissa, Valenti, Stefano, Wang, Xiaofeng, Wheeler, J Craig
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 21.03.2019
• Subjects: Bolometers; Dust; Ejecta; Explosions; Galaxies; Infrared spectra; Light curve; Modelling; Near infrared radiation; Photometry; Physical properties; Physics - High Energy Astrophysical Phenomena; Spectrum analysis
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1903.09048

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.