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

Walker, E. S. and Mazzali, P. A. and Pian, E. and Hurley, K. and Arcavi, I. and Cenko, S. B. and Gal-Yam, A. and Horesh, A. and Kasliwal, M. and Poznanski, D. and Silverman, J. M. and Sullivan, M. and Bloom, J. S. and Filippenko, A. V. and Kulkarni, S. R. and Nugent, P. E. and Ofek, E. and Barthelmy, S. and Boynton, W. and Goldsten, J. and Golenetskii, S. and Ohno, M. and Tashiro, M. S. and Yamaoka, K. and Zhang, X. L. (2014) Optical follow-up observations of PTF10qts, a luminous broad-lined Type Ic supernova found by the Palomar Transient Factory. Monthly Notices of the Royal Astronomical Society, 442 (3). pp. 2768-2779. ISSN 0035-8711.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Arcavi, I.0000-0001-7090-4898
Cenko, S. B.0000-0003-1673-970X
Gal-Yam, A.0000-0002-3653-5598
Kasliwal, M.0000-0002-5619-4938
Filippenko, A. V.0000-0003-3460-0103
Kulkarni, S. R.0000-0001-5390-8563
Nugent, P. E.0000-0002-3389-0586
Ofek, E.0000-0002-6786-8774
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).
Funding AgencyGrant Number
Agenzia Spaziale Italiana (ASI)I/016/07/0
Agenzia Spaziale Italiana (ASI)I/088/06/0
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Binational Science Foundation (USA-Israel)UNSPECIFIED
German-Israeli Foundation for Research and DevelopmentUNSPECIFIED
European Research Council (ERC)307260
I-CORE Program of the Planning and Budgeting CommitteeUNSPECIFIED
Lord Sieff of Brimpton FundUNSPECIFIED
Gary and Cynthia BengierUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
Richard and Rhoda Goldman FundUNSPECIFIED
NSF Astronomy and Astrophysics FellowshipAST-1302771
Ministry of Science (Israel)UNSPECIFIED
Israel Science Foundation1829/12
Subject Keywords:supernovae: general; supernovae: individual: PTF10qts
Record Number:CaltechAUTHORS:20140828-084958848
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Official Citation:Walker, E. S., Mazzali, P. A., Pian, E., Hurley, K., Arcavi, I., Cenko, S. B., . . . Zhang, X. L.-. (2014). Optical follow-up observations of PTF10qts, a luminous broad-lined Type Ic supernova found by the Palomar Transient Factory. Monthly Notices of the Royal Astronomical Society, 442(3), 2768-2779. doi: 10.1093/mnras/stu1017
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:49013
Deposited By: Jason Perez
Deposited On:28 Aug 2014 20:12
Last Modified:27 Oct 2017 03:33

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