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iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia, F. and Fremling, C. and Sollerman, J. and Corsi, A. and Gal-Yam, A. and Karamehmetoglu, E. and Lunnan, R. and Bue, B. and Ergon, M. and Kasliwal, M. and Vreeswijk, P. M. and Wozniak, P. R. (2016) iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor. Astronomy and Astrophysics, 592 . Art .No. A89. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20161117-112958640

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Abstract

Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H- (and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (~10−15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (~30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star. Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission. Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (~10 M_⊙) and strong ^(56)Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended (≳500 R_⊙), low-mass (≳0.045 M_⊙) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. Conclusions. The large ejecta mass and the presence of H- and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive (≳35 M_⊙) WR star that experienced strong mass loss.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201628703DOIArticle
http://www.aanda.org/articles/aa/full_html/2016/08/aa28703-16/aa28703-16.htmlPublisherArticle
ORCID:
AuthorORCID
Fremling, C.0000-0002-4223-103X
Sollerman, J.0000-0003-1546-6615
Corsi, A.0000-0001-8104-3536
Gal-Yam, A.0000-0002-3653-5598
Lunnan, R.0000-0001-9454-4639
Kasliwal, M.0000-0002-5619-4938
Additional Information:© 2016 ESO. Received: 13 April 2016. Accepted: 31 May 2016. We gratefully acknowledge the support from the Knut and Alice Wallenberg Foundation. This work is partly 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. This work is partly based on observations made with DOLoRes@TNG. This paper made use of Lowell Observatory’s Discovery Channel Telescope (DCT). Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The Large Monolithic Imager (LMI) on DCT was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). LANL participation in iPTF was funded by the US Department of Energy as part of the Laboratory Directed Research and Development program. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank N. Blagorodnova, E. Bellm, Y. Cao, G. Duggan, S. Kulkarni, J. Jencson, P. Nugent, for their precious help with the observations of iPTF15dtg and contribution to iPTF. We thank L. Yan for her comments on the paper. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the intermediate Palomar Transient Factory (iPTF) project, a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. A. Corsi acknowledges support from NSF CAREER Award #1455090.
Group:IPTF, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Knut and Alice Wallenberg FoundationUNSPECIFIED
Discovery CommunicationsUNSPECIFIED
NSFAST-1005313
Department of Energy (DOE)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
NSFAST-1455090
Subject Keywords:supernovae: general
Record Number:CaltechAUTHORS:20161117-112958640
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20161117-112958640
Official Citation:iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor F. Taddia, C. Fremling, J. Sollerman, A. Corsi, A. Gal-Yam, E. Karamehmetoglu, R. Lunnan, B. Bue, M. Ergon, M. Kasliwal, P. M. Vreeswijk and P. R. Wozniak A&A, 592 (2016) A89 DOI: http://dx.doi.org/10.1051/0004-6361/201628703
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72121
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:17 Nov 2016 19:58
Last Modified:27 Oct 2017 22:37

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