Optical follow-up observations of PTF10qts, a luminous broad-lined Type Ic supernova found by the Palomar Transient Factory

Creators: Walker, E. S.; Mazzali, P. A.; Pian, E.; Hurley, K.; Arcavi, I.; Cenko, S. B.; Gal-Yam, A.; Horesh, A.; Kasliwal, M.; Poznanski, D.; Silverman, J. M.; Sullivan, M.; Bloom, J. S.; Filippenko, A. V.; Kulkarni, S. R.; Nugent, P. E.; Ofek, E.; Barthelmy, S.; Boynton, W.; Goldsten, J.; Golenetskii, S.; Ohno, M.; Tashiro, M. S.; Yamaoka, K.; Zhang, X. L.

Abstract

We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The SN was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907. We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is M_bol = −18.51 ± 0.2 mag, comparable to that of SN 1998bw (M_bol = −18.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SNe Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNe Ic-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely an ∼20 M_⊙ star.

Additional Information

© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 May 19. Received 2014 May 19; in original form 2014 March 10. First published online June 27, 2014. We acknowledge financial contributions from contract ASI I/016/07/0 (COFIS), ASI I/088/06/0, and PRIN INAF 2009 and 2011. PTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and UC Berkeley. Collaborative work between AG and PAM is supported by a Minerva grant. The Weizmann PTF membership is supported by the ISF via grants to AG. Joint work of AG and SRK is supported by a BSF grant. AG also acknowledges support by grants from the GIF, EU/FP7 via ERC grant 307260, 'The Quantum Universe', I-CORE programme by the Israeli Committee for planning and budgeting, the Kimmel award, and the Lord Sieff of Brimpton Fund. AVF's group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. 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). We thank the very helpful staffs of the various observatories (Palomar, Lick, KNPO, TNG, Keck) at which data were obtained. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of theW. M. Keck Foundation. M. T. Kandrashoff and J. Rex assisted with the Lick observations. We are grateful to the following contributors to the IPN for support and sharing their data: I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, C. Fellows, K. Harshman, and R. Starr (for the Odyssey team), R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and D. Svinkin (for the Konus-Wind team), A. von Kienlin and A. Rau (for the INTEGRAL team), T. Takahashi, M. Ohno, Y. Hanabata, Y. Fukazawa, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima (for the Suzaku team), T. Cline, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer (for the Swift team), and V. Connaughton, M. S. Briggs, and C. Meegan (for the Fermi GBM team). KH acknowledges NASA support for the IPN under the following grants: NNX10AI23G (Swift), NNX09AV61G (Suzaku), NNX09AU03G (Fermi), and NNX09AR28G (INTEGRAL).

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Published - MNRAS-2014-Walker-2768-79.pdf

Submitted - 1405.5237v1.pdf

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