Corsi, A. and Ofek, E. O. and Kulkarni, S. R. and Kasliwal, M. M. and Quimby, R. M. (2011) PTF 10bzf (SN 2010ah): A Broad-Line Ic Supernova Discovered by the Palomar Transient Factory. Astrophysical Journal, 741 (2). Art. No. 76. ISSN 0004-637X http://resolver.caltech.edu/CaltechAUTHORS:20120123-115808955
- Published Version
See Usage Policy.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20120123-115808955
We present the discovery and follow-up observations of a broad-line Type Ic supernova (SN), PTF 10bzf (SN 2010ah), detected by the Palomar Transient Factory (PTF) on 2010 February 23. The SN distance is ≅218 Mpc, greater than GRB 980425/SN 1998bw and GRB 060218/SN 2006aj, but smaller than the other SNe firmly associated with gamma-ray bursts (GRBs). We conducted a multi-wavelength follow-up campaign with Palomar 48 inch, Palomar 60 inch, Gemini-N, Keck, Wise, Swift, the Allen Telescope Array, Combined Array for Research in Millimeter-wave Astronomy, Westerbork Synthesis Radio Telescope, and Expanded Very Large Array. Here we compare the properties of PTF 10bzf with those of SN 1998bw and other broad-line SNe. The optical luminosity and spectral properties of PTF 10bzf suggest that this SN is intermediate, in kinetic energy and amount of ^(56)Ni, between non-GRB-associated SNe like 2002ap or 1997ef, and GRB-associated SNe like 1998bw. No X-ray or radio counterpart to PTF 10bzf was detected. X-ray upper limits allow us to exclude the presence of an underlying X-ray afterglow as luminous as that of other SN-associated GRBs such as GRB 030329 or GRB 031203. Early-time radio upper limits do not show evidence for mildly relativistic ejecta. Late-time radio upper limits rule out the presence of an underlying off-axis GRB, with energy and wind density similar to the SN-associated GRB 030329 and GRB 031203. Finally, by performing a search for a GRB in the time window and at the position of PTF 10bzf, we find that no GRB in the interplanetary network catalog could be associated with this SN.
|Additional Information:||© 2011 The American Astronomical Society. Received 2011 January 21; accepted 2011 August 7; published 2011 October 19. PTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and Berkeley. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. E.O.O. is supported by an Einstein Fellowship and NASA grants. D.P. is supported by an Einstein fellowship. The Weizmann Institute PTF partnership is supported in part by grants from the Israeli Science Foundation (ISF) to A.G. Joint work by the Weizmann and Caltech groups is supported by a grant from the Binational Science Foundation (BSF) to A.G. and S.R.K. A.G. acknowledges further support from an EU/FP7 Marie Curie IRG fellowship and a research grant from the Peter and Patricia Gruber Awards. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnología e Innovaciόn Productiva (Argentina). The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. LAIWO, a wide-angle camera operating on the 1 m telescope at the Wise Observatory, Israel, was built at the Max Planck Institute for Astronomy (MPIA) in Heidelberg, Germany, with financial support from the MPIA, and grants from the German Israeli Science Foundation for Research and Development, and from the Israel Science Foundation. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation. We are grateful to IPN collaborators S. Golenetskii, R. Aptekar, E. Mazets, D. Frederiks, and T. Cline for the Konus data; to M. Briggs and C. Meegan for the Fermi data; to T. Takahashi, Y. Terada, M. Tashiro, Y. Fukazawa, T. Murakami, M. Ohno, and K. Makishima for the Suzaku data; to S. Barthelmy, N. Gehrels, H. Krimm, and D. Palmer for the Swift data; to D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, C. Fellows, K. Harshman, and R. Starr for the Odyssey data; and to A. von Kienlin and X. Zhang for the INTEGRAL data. K.H. acknowledges support from the following NASA sources: NNX09AV61G (Suzaku), NNX10AI23G (Swift), NNX10AU34G (Fermi), and NNX07AR71G (MESSENGER). S.B.C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. A.C. and S.R.K. acknowledge partial support from NASA/Swift Guest Investigator Program Cycle 7 (NNH10ZDA001N).|
|Subject Keywords:||gamma-ray burst: general; radiation mechanisms: non-thermal; supernovae: general; supernovae: individual (PTF 10bzf)|
|Official Citation:||PTF 10bzf (SN 2010ah): A Broad-line Ic Supernova Discovered by the Palomar Transient Factory A. Corsi et al. 2011 ApJ 741 76|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||24 Jan 2012 15:58|
|Last Modified:||26 Dec 2012 14:43|
Repository Staff Only: item control page