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The rise and fall of the Type Ib supernova iPTF13bvn - Not a massive Wolf-Rayet star

Fremling, C. and Sollerman, J. and Taddia, F. and Ergon, M. and Valenti, S. and Arcavi, I. and Ben-Ami, S. and Cao, Y. and Cenko, S. B. and Filippenko, A. V. and Gal-Yam, A. and Howell, D. A. (2014) The rise and fall of the Type Ib supernova iPTF13bvn - Not a massive Wolf-Rayet star. Astronomy and Astrophysics, 565 . Art. No. A114. ISSN 0004-6361.

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Context. We investigate iPTF13bvn, a core-collapse (CC) supernova (SN) in the nearby spiral galaxy NGC 5806. This object was discovered by the intermediate Palomar Transient Factory (iPTF) very close to the estimated explosion date and was classified as a stripped-envelope CC SN, likely of Type Ib. Furthermore, a possible progenitor detection in pre-explosion Hubble Space Telescope (HST) images was reported, making this the only SN Ib with such an identification. Based on the luminosity and color of the progenitor candidate, as well as on early-time spectra and photometry of the SN, it was argued that the progenitor candidate is consistent with a single, massive Wolf-Rayet (WR) star. Aims. We aim to confirm the progenitor detection, to robustly classify the SN using additional spectroscopy, and to investigate if our follow-up photometric and spectroscopic data on iPTF13bvn are consistent with a single-star WR progenitor scenario. Methods. We present a large set of observational data, consisting of multi-band light curves (UBVRI, g′r′i′z′) and optical spectra. We perform standard spectral line analysis to track the evolution of the SN ejecta. We also construct a bolometric light curve and perform hydrodynamical calculations to model this light curve to constrain the synthesized radioactive nickel mass and the total ejecta mass of the SN. Late-time photometry is analyzed to constrain the amount of oxygen. Furthermore, image registration of pre- and post-explosion HST images is performed. Results. Our HST astrometry confirms the location of the progenitor candidate of iPTF13bvn, and follow-up spectra securely classify this as a SN Ib. We use our hydrodynamical model to fit the observed bolometric light curve, estimating the total ejecta mass to be 1.9 M⊙ and the radioactive nickel mass to be 0.05 M⊙. The model fit requires the nickel synthesized in the explosion to be highly mixed out in the ejecta. We also find that the late-time nebular r′-band luminosity is not consistent with predictions based on the expected oxygen nucleosynthesis in very massive stars. Conclusions. We find that our bolometric light curve of iPTF13bvn is not consistent with the previously proposed single massive WR-star progenitor scenario. The total ejecta mass and, in particular, the late-time oxygen emission are both significantly lower than what would be expected from a single WR progenitor with a main-sequence mass of at least 30 M⊙.

Item Type:Article
Related URLs:
URLURL TypeDescription DOIArticle Paper
Fremling, C.0000-0002-4223-103X
Sollerman, J.0000-0003-1546-6615
Taddia, F.0000-0002-2387-6801
Valenti, S.0000-0001-8818-0795
Arcavi, I.0000-0001-7090-4898
Ben-Ami, S.0000-0001-6760-3074
Cao, Y.0000-0002-8036-8491
Cenko, S. B.0000-0003-1673-970X
Filippenko, A. V.0000-0003-3460-0103
Gal-Yam, A.0000-0002-3653-5598
Howell, D. A.0000-0003-4253-656X
Additional Information:© 2014 ESO. Article published by EDP Sciences. Received 26 March 2014; Accepted 16 April 2014. Published online 20 May 2014. The Oskar Klein Centre is funded by the Swedish Research Council. This work is partially based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. Some of the data presented herein were obtained at theW.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. A. G.-Y. is supported by the EU/FP7 via ERC grant 307260, “The Quantum Universe” I-Core program by the Israeli Committee for planning and budgeting, by ISF, GIF, and Minerva grants, and by the Kimmel award. A. V. F.’s group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST- 1211916, and NASA grants AR-12623 and AR-12850 from the Space Telescope Science Institute (which is operated by AURA, Inc., under NASA contract NAS 5-26555). We extend our thanks to the following people for their various contributions to this work: Shri Kulkarni, Mansi M. Kasliwal, Ofer Yaron, Paul Vreeswijk, Daniel Perley, Joel Johansson, Anders Jerkstrand, Kelsey Clubb, Ori Fox, Patrick Kelly, Barak Zackay, Adam Waszczak, Donald O’Sullivan, and Thomas Augusteijn.
Group:Palomar Transient Factory
Funding AgencyGrant Number
Swedish Research CouncilUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
European Research Council (ERC)307260
Israeli Committee I-Core ProgramUNSPECIFIED
Israel Science FoundationUNSPECIFIED
German-Israeli Foundation for Research and DevelopmentUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
NASANAS 5-26555
Subject Keywords:supernovae: general / supernovae: individual: iPTF13bvn
Record Number:CaltechAUTHORS:20140703-105004666
Persistent URL:
Official Citation:The rise and fall of the Type Ib supernova iPTF13bvn C. Fremling, J. Sollerman, F. Taddia, M. Ergon, S. Valenti, I. Arcavi, S. Ben-Ami, Y. Cao, S. B. Cenko, A. V. Filippenko, A. Gal-Yam, D. A. Howell A&A 565 A114 (2014) DOI: 10.1051/0004-6361/201423884
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46813
Deposited By: Tony Diaz
Deposited On:07 Jul 2014 16:04
Last Modified:21 Nov 2019 23:20

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