The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase
| Autor: | Iair Arcavi, Zoltán Dencs, Curtis McCully, A. Ordasi, Lluís Galbany, Ádám Sódor, Tamás Szalai, O. Hanyecz, A. Bódi, Global Supernova, Daichi Hiramatsu, J. Craig Wheeler, Jamison Burke, Róbert Szakáts, Krisztián Sárneczky, R. Konyves-Toth, Konkoly team, G. Csörnyei, Peter de Nully Brown, Ondrej Pejcha, David J. Sand, D. Andrew Howell, Stefano Valenti, Chris Ashall, B. Cseh, Griffin Hosseinzadeh, András Pál, S. Moran, Jeonghee Rho, Melissa Shahbandeh, Bálint Seli, L. Kriskovics, Csilla Kalup, G. Zsidi, K. Vida, Bernadett Ignácz, Jozsef Vinko, Xiaofeng Wang, Andrea Nagy, K. Azalee Bostroem, Eric Hsiao |
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| Rok vydání: | 2019 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics 010504 meteorology & atmospheric sciences FOS: Physical sciences Astronomy and Astrophysics Astrophysics 01 natural sciences Supernova Space and Planetary Science Phase (matter) 0103 physical sciences Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics 0105 earth and related environmental sciences |
| Zdroj: | The Astrophysical Journal. 876:19 |
| ISSN: | 1538-4357 |
| Popis: | 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 |
| Databáze: | OpenAIRE |
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