Details

Autor(en) / Beteiligte

• 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

Titel

The Type II-P Supernova 2017eaw: From Explosion to the Nebular Phase

Ist Teil von

• The Astrophysical journal, 2019-05, Vol.876 (1), p.19

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2019

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• 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 ∼ 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 ∼15-16 M . Our estimation of the pre-explosion mass-loss rate ( 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 m can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw.