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PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

Pian, E. and Mazzali, P. A. and Moriya, T. J. and Rubin, A. and Gal-Yam, A. and Arcavi, I. and Ben-Ami, S. and Blagorodnova, N. and Bufano, F. and Filippenko, A. V. and Kasliwal, M. and Kulkarni, S. R. and Lunnan, R. and Manulis, I. and Matheson, T. and Nugent, P. E. and Ofek, E. and Perley, D. A. and Prentice, S. J. 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. https://resolver.caltech.edu/CaltechAUTHORS:20201030-124833319

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Abstract

The hydrogen-poor supernova (SN) 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 December 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 M_⊙ carbon–oxygen core evolved from a progenitor of main-sequence mass 25–40 M_⊙, that liberated a kinetic energy E_k ≈ 4 × 10⁵¹ erg, expelled ∼8 M_⊙ of ejecta, and synthesized ∼0.5 M_⊙ of ⁵⁶Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (≳ 15 000 km s⁻¹). 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 × 10⁵⁰ erg), less than 2 per cent 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 SNe in luminosity, although it has a lower energy and a lower E_k/M_(ej) ratio.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/staa2191DOIArticle
https://arxiv.org/abs/2007.13144arXivDiscussion Paper
https://wiserep.weizmann.ac.ilRelated ItemData
ORCID:
AuthorORCID
Pian, E.0000-0001-8646-4858
Mazzali, P. A.0000-0001-6876-8284
Moriya, T. J.0000-0003-1169-1954
Rubin, A.0000-0003-4557-0632
Gal-Yam, A.0000-0002-3653-5598
Arcavi, I.0000-0001-7090-4898
Ben-Ami, S.0000-0001-6760-3074
Blagorodnova, N.0000-0003-0901-1606
Bufano, F.0000-0002-3429-2481
Filippenko, A. V.0000-0003-3460-0103
Kasliwal, M.0000-0002-5619-4938
Kulkarni, S. R.0000-0001-5390-8563
Lunnan, R.0000-0001-9454-4639
Matheson, T.0000-0001-6685-0479
Nugent, P. E.0000-0002-3389-0586
Ofek, E.0000-0002-6786-8774
Perley, D. A.0000-0001-8472-1996
Prentice, S. J.0000-0003-0486-6242
Yaron, O.0000-0002-0301-8017
Additional Information:© 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 July 21. Received 2020 July 21; in original form 2020 June 2. Published: 27 July 2020. We are grateful to Y. Cao, J. Bloom, and J. M. Silverman for their assistance with data acquisition and reduction. EP thanks the Weizmann Institute for Science (WIS, Rehovot, Israel), the National Astronomical Observatory of Japan, the Astrophysics Research Institute of Liverpool John Moores University, and the Munich Institute for Astrophysics and Particle Physics (MIAPP) for hospitality and support, and acknowledges fruitful conversations and exchanges with the participants of MIAPP programs ‘The Physics of Supernovae’ (2016) and ‘Superluminous Supernovae in the Next Decade’ (2017). TJM is supported by the grants-in-aid for Scientific Research of the Japan Society for the Promotion of Science (JP17H02864 and JP18K13585). AG-Y’s research is supported by the European Union (EU) via European Research Council (ERC) grant 725161, the Israeli Science Foundation (ISF)Gravitational Waves (GW) Excellence Center, an Israeli Ministry of Science space infrastructure grant, and Binational Science Foundation (BSF)/Transformative and GIF grants, as well as by the Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Paul and Tina Gardner, Yeda-Sela, and the WIS-CIT joint research grant; AG-Y is also the recipient of the Helen and Martin Kimmel Award for Innovative Investigation. IA is a Canadian Institute for Advanced Research Azrieli Global Scholar in the Gravity and the Extreme Universe Program and acknowledges support from that program, from the ERC under the EU's Horizon 2020 research and innovation program (grant agreement number 852097), from the ISF (grant numbers 2108/18 and 2752/19), from the United States - Israel BSF, and from the Israeli Council for Higher Education Alon Fellowship. AVF is grateful for financial assistance from U.S. National Science Foundation (NSF) grant AST-1211916, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (U.C. Berkeley). This research was supported by the Italian Ministry for Research (MIUR) with Progetto di ricerca di Rilevante Interesse Nazionale (PRIN) 2010/2011, Istituto Nazionale di Astrofisica (INAF, PRIN 2011 and 2014), by Scuola Normale Superiore, and by the National Astronomical Observatory of Japan Research Coordination Committee, NINS, grant numbers 19FS-0506 and 19FS-0507. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the U.S. NSF. This research has made use of the National Aeronautics and Space Administration (NASA)/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based on observations taken at the ESO VLT under program 090.D-0440, Keck, Palomar, and Kitt Peak National Observatories. This paper is dedicated to the memory of our friend and colleague Adi Pauldrach. Data Availability: The photometric and spectroscopic data presented in this article are publicly available via the Weizmann Interactive Supernova Data Repository (Yaron & Gal-Yam 2012), at https://wiserep.weizmann.ac.il.
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
Weizmann Institute of ScienceUNSPECIFIED
National Astronomical Observatory of JapanUNSPECIFIED
Astrophysics Research InstituteUNSPECIFIED
Munich Institute for Astro- and Particle Physics (MIAPP)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17H02864
Japan Society for the Promotion of Science (JSPS)JP18K13585
European Research Council (ERC)725161
Israeli Ministry of ScienceUNSPECIFIED
Binational Science Foundation (USA-Israel)UNSPECIFIED
German-Israeli Foundation for Research and DevelopmentUNSPECIFIED
Benoziyo Endowment Fund for the Advancement of ScienceUNSPECIFIED
Deloro Institute for Advanced Research in Space and OpticsUNSPECIFIED
Veronika A. Rabl Physics Discretionary FundUNSPECIFIED
Paul and Tina GardnerUNSPECIFIED
Yeda-SelaUNSPECIFIED
Helen and Martin Kimmel AwardUNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
European Research Council (ERC)852097
Israel Science Foundation2108/18
Israel Science Foundation2752/19
Council for Higher Education (Israel)UNSPECIFIED
NSFAST-1211916
TABASGO FoundationUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
Miller Institute for Basic Research in ScienceUNSPECIFIED
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)UNSPECIFIED
Progetto di ricerca di Rilevante Interesse Nazionale (PRIN)2010/2011
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Scuola Normale SuperioreUNSPECIFIED
National Institutes of Natural Sciences of Japan19FS-0506
National Institutes of Natural Sciences of Japan19FS-0507
NASA/JPL/CaltechUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:radiative transfer – stars: massive – galaxies: star formation – transients: supernovae
Issue or Number:3
Record Number:CaltechAUTHORS:20201030-124833319
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20201030-124833319
Official Citation:E Pian, P A Mazzali, T J Moriya, A Rubin, A Gal-Yam, I Arcavi, S Ben-Ami, N Blagorodnova, F Bufano, A V Filippenko, M Kasliwal, S R Kulkarni, R Lunnan, I Manulis, T Matheson, P E Nugent, E Ofek, D A Perley, S J Prentice, O Yaron, PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses, Monthly Notices of the Royal Astronomical Society, Volume 497, Issue 3, September 2020, Pages 3542–3556, https://doi.org/10.1093/mnras/staa2191
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:106362
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:30 Oct 2020 21:43
Last Modified:30 Oct 2020 21:43

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