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Published September 1, 2014 | Submitted + Published
Journal Article Open

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

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.

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.

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Published - MNRAS-2014-Gorbikov-671-7.pdf

Submitted - 1312.0012v3.pdf

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Additional details

Created:
August 20, 2023
Modified:
October 17, 2023