CaltechAUTHORS
  A Caltech Library Service

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Gorbikov, Evgeny and Gal-Yam, Avishay and Ofek, Eran O. and Vreeswijk, Paul M. and Nugent, Peter E. and Chotard, Nicolas and Kulkarni, Shrinivas R. and Cao, Yi and De Cia, Annalisa and Yaron, Ofer and Tal, David and Arcavi, Iair and Kasliwal, Mansi M. and Cenko, S. Bradley and Sullivan, Mark and Chen, Juncheng (2014) iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion. Monthly Notices of the Royal Astronomical Society, 443 (1). pp. 671-677. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20140904-153832373

[img]
Preview
PDF - Published Version
See Usage Policy.

1343Kb
[img]
Preview
PDF - Submitted Version
See Usage Policy.

1669Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20140904-153832373

Abstract

We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova (SN) iPTF13beo. Detected by the intermediate Palomar Transient Factory ∼3 h after the estimated first light, iPTF13beo is the youngest and the most distant (∼430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo R-band light curve exhibits a double-peak structure separated by ∼9 d, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He i and Si ii features with full width at half-maximum ≈2000–5000 km s^(−1) and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of ∼0.1 M_⊙ over a time-scale of couple of weeks prior to the SN explosion.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://mnras.oxfordjournals.org/content/443/1/671.abstractPublisherArticle
http://dx.doi.org/10.1093/mnras/stu1184DOIArticle
http://arxiv.org/abs/1312.0012arXivDiscussion Paper
ORCID:
AuthorORCID
Gal-Yam, Avishay0000-0002-3653-5598
Ofek, Eran O.0000-0002-6786-8774
Nugent, Peter E.0000-0002-3389-0586
Kulkarni, Shrinivas R.0000-0001-5390-8563
Cao, Yi0000-0002-8036-8491
De Cia, Annalisa0000-0003-2082-1626
Arcavi, Iair 0000-0001-7090-4898
Kasliwal, Mansi M.0000-0002-5619-4938
Cenko, S. Bradley0000-0003-1673-970X
Additional Information:© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 June 9. Received 2014 June 8; in original form 2013 November 28. First published online July 15, 2014. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. 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. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. EOO is incumbent of the Arye Dissentshik career development chair and is grateful to support by a grant from the Israeli Ministry of Science and the I-CORE Programme of the Planning and Budgeting Committee and The Israel Science Foundation (grant no. 1829/12). AG-Y acknowledges support by the EU/FP7 via ERC grant no. 307260, ISF, BSF, Minerva and GIF grants, the ‘Quantum Universe’ I-Core programme funded by the ISF and the Israeli Planning and Budgeting Committee, and the Kimmel award. Observations obtained with the SuperNova Integral Field Spectrograph on the University of Hawaii 2.2-m telescope as part of the Nearby Supernova Factory II project, a scientific collaboration between the Centre de Recherche Astronomique de Lyon, Institut de Physique Nucléaire de Lyon, Laboratoire de Physique Nucléaire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and Centre de Physique des Particules de Marseille. NC acknowledges support from the Lyon Institute of Origins under grant ANR-10-LABX-66. We would like to express our gratitude to the anonymous referee for the valuable comments, that helped to improve this paper.
Group:IPTF
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Ministry of Science (Israel)UNSPECIFIED
Israel Science Foundation1829/12
European Research Council (ERC)307260
Binational Science Foundation (USA-Israel)UNSPECIFIED
MinervaUNSPECIFIED
German-Israeli Foundation for Research and DevelopmentUNSPECIFIED
Israeli Planning and Budgeting CommitteeUNSPECIFIED
Kimmel AwardUNSPECIFIED
Lyon Institute of OriginsANR-10-LABX-66
Subject Keywords:supernovae: general supernovae: individual: iPTF13beo stars: winds, outflows stars: Wolf–Rayet
Record Number:CaltechAUTHORS:20140904-153832373
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140904-153832373
Official Citation:Evgeny Gorbikov, Avishay Gal-Yam, Eran O. Ofek, Paul M. Vreeswijk, Peter E. Nugent, Nicolas Chotard, Shrinivas R. Kulkarni, Yi Cao, Annalisa De Cia, Ofer Yaron, David Tal, Iair Arcavi, Mansi M. Kasliwal, S. Bradley Cenko, Mark Sullivan, and Juncheng Chen iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion MNRAS (September 1, 2014) Vol. 443 671-677 doi:10.1093/mnras/stu1184 First published online July 15, 2014
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:49257
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:05 Sep 2014 23:02
Last Modified:27 Oct 2017 03:31

Repository Staff Only: item control page