Pian, E, Mazzali, PA, Moriya, TJ, Rubin, A, Gal-Yam, A, Arcavi, I, Ben-Ami, S, Blagorodnova, N, Bufano, M, Filippenko, AV, Kasliwal, M, Kulkarni, SR, Lunnan, R, Manulis, I, Matheson, T, Nugent, PE, Ofek, E, Perley, DA, Prentice, SJ and Yaron, O (2020) PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses. Monthly Notices of the Royal Astronomical Society, 497 (3). pp. 3542-3556. ISSN 0035-8711

Preview

Text PTF11rka an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses.pdf - Published Version Download (1MB) | Preview

Abstract

The hydrogen-poor supernova PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 Dec. 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the R_PTF filter band, and maximum in this band was reached ~30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ~10 Msun carbon-oxygen core evolved from a progenitor of main-sequence mass 25--40 Msun, that liberated a kinetic energy (KE) ~ 4 x 10^{51} erg, expelled ~8 Msun of ejecta (Mej), and synthesised ~0.5 Msun of 56Nichel. The photospheric spectra of PTF11rka are characterised by narrow absorption lines that point to suppression of the highest ejecta velocities ~>15,000 km/s. This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (~5 x 10^50 erg), less than 2% of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst supernovae (GRB-SNe) in luminosity, although it has a lower energy and a lower KE/Mej ratio.

Item Type:	Article
Additional Information:	This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords:	astro-ph.HE; astro-ph.HE
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press
Related URLs:	Author
Date Deposited:	30 Jul 2020 10:20
Last Modified:	10 Sep 2021 11:15
DOI or ID number:	10.1093/mnras/staa2191
URI:	https://researchonline.ljmu.ac.uk/id/eprint/13415

View Item