Supernova 2013fc in a circumnuclear ring of a luminous infrared galaxy: the big brother of SN 1998S

作者：Kangas T; Mattila S; Kankare E; Lundqvist P; Vaeisaenen P; Childress M; Pignata G; McCully C; Valenti S; Vinko J; Pastorello A; Elias Rosa N; Fraser M; Gal Yam A; Kotak R; Kotilainen J K; Smartt S J; Galbany L; Harmanen J; Howell D A; Inserra C; Marion G H; Quimby R M; Silverman J M; Szalai T; Wheeler J C; Ashall C; Benetti S; Romero Canizales C; Smith K W; Sullivan M; Takats K; Young D R

来源：Monthly Notices of the Royal Astronomical Society, 2016, 456(1): 323-346.

DOI：10.1093/mnras/stv2567

• supernovae
• general-supernovae
• individual
• 2013fc-galaxies
• starburst

We present photometric and spectroscopic observations of SN 2013fc, a bright type II supernova (SN) in a circumnuclear star-forming ring in the luminous infrared galaxy ESO 154-G010, observed as part of the Public ESO Spectroscopic Survey of Transient Objects. SN 2013fc is both photometrically and spectroscopically similar to the well-studied type IIn SN 1998S and to the bright type II-L SN 1979C. It exhibits an initial linear decline, followed by a short plateau phase and a tail phase with a decline too fast for Co-56 decay with full. gamma-ray trapping. Initially, the spectrum was blue and featureless. Later on, a strong broad (similar to 8000 km s(-1)) H alpha emission profile became prominent. We apply a STARLIGHT stellar population model fit to the SN location (observed when the SN had faded) to estimate a high extinction of A(V) = 2.9 +/- 0.2 mag and an age of 10(+ 3) (- 2) Myr for the underlying cluster. We compare the SN to SNe 1998S and 1979C and discuss its possible progenitor star considering the similarities to these events. With a peak brightness of B = - 20.46 +/- 0.21 mag, SN 2013fc is 0.9 mag brighter than SN 1998S and of comparable brightness to SN 1979C. We suggest that SN 2013fc was consistent with a massive red supergiant (RSG) progenitor. Recent mass loss probably due to a strong RSG wind created the circumstellar matter illuminated through its interaction with the SN ejecta. We also observe a near- infrared excess, possibly due to newly condensed dust.

• 出版日期2016-2-11