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Optical and near-infrared observations of SN 2013dx associated with GRB 130702A

Toy, V. L. and Perley, D. A. and Bellm, E. and Cao, Y. and Kulkarni, S. R. and Singer, L. (2016) Optical and near-infrared observations of SN 2013dx associated with GRB 130702A. Astrophysical Journal, 818 (1). Art. No. 79. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20151207-131630440

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Abstract

We present optical and near-infrared (NIR) light curves and optical spectra of SN 2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB 130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is measured to be E_(yiso)=6.4_(-1.0)^(+1.3) x 10^(50) erg (1 keV to 10 MeV in the rest frame), placing it intermediate between low-luminosity GRBs like GRB 980425/SN 1998bw and the broader cosmological population. We compare the observed g'r'i'z' light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves ~20% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined SNe Ic, both associated with (SN 2006aj and SN 1998bw) and lacking (SN 1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric velocities around peak of ~ 21,000 km s^(−1). We construct a quasi-bolometric g'r'i'z'yJ) light curve for SN 2013dx, only the fifth GRB-associated SN with extensive NIR coverage and the third with a bolometric light curve extending beyond Δt > 40 days. Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a ^(56)Ni mass of M_(Ni)= 0.37 ± 0.01 M_☉, an ejecta mass of M_(ej) = 3.1 ± 0.1 M_☉, and a kinetic energy of E_K = 8.2 ± 0.43 x 10^(51) erg (statistical uncertainties only), consistent with previous GRB-associated supernovae. When considering the ensemble population of GRB-associated supernovae, we find no correlation between the mass of synthesized 56Ni and high-energy properties, despite clear predictions from numerical simulations that M_(Ni) should correlate with the degree of asymmetry. On the other hand, M_(Ni) clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1508.00575arXivDiscussion Paper
http://dx.doi.org/10.3847/0004-637X/818/1/79DOIArticle
http://iopscience.iop.org/article/10.3847/0004-637X/818/1/79PublisherArticle
ORCID:
AuthorORCID
Perley, D. A.0000-0001-8472-1996
Bellm, E.0000-0001-8018-5348
Cao, Y.0000-0002-8036-8491
Kulkarni, S. R.0000-0001-5390-8563
Singer, L.0000-0001-9898-5597
Additional Information:© 2016. The American Astronomical Society. Received 2015 July 30; accepted 2015 December 22; published 2016 February 9. We gratefully acknowledge S. Schulze, F. Olivares E., A. Melandri, M. Modjaz, Y. Liu, and E. Pian for generously sharing their raw data, which significantly improved the analysis for this paper. We also thank J. Lyman, M. Modjaz, R. Thomas, and the anonymous referee for useful feedback on the manuscript. This work was supported by the National Aeronautics and Space Administration (NASA) Headquarters under the NASA Earth and Space Science Fellowship Program (Grant NNX12AL70H to V.T.). V.T. and S.V. were partially supported by NSF/ATI grant 1207785. The research of A.V.F.ʼs group at UC Berkeley has been funded by (NSF) grant AST-1211916, Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and the Christopher R. Redlich Fund. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A.G.Y. is supported by the EU/ FP7 via ERC grant no. 307260, the Quantum universe I-Core program by the Israeli Committee for planning and budgeting and the ISF; by Minerva and ISF grants; by the Weizmann-UK “making connections” program; and by Kimmel and ARCHES awards. A.C. acknowledges support from the NASA-Swift GI program via grants 13-SWIFT13-0030 and 14-SWIFT14-0024. E.T. acknowledges support for this project under the Fermi Guest Investigator Program. The work of D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We also acknowledge the help of K. Markey, E. Alduena, A. Alduena, and S. Kuo from Walden School for their help with the Palomar observations on 2013 July 8. We thank the RATIR project team and the staff of the Observatorio Astronómico Nacional on Sierra San Pedro Mártir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonóma de México, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector and hardware and software support from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronómico Nacional on Sierra San Pedro Mártir, and the operation of both are funded through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants INFR- 2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IG100414, and UC MEXUS-CONACyT grant CN 09-283. These results made use of Lowell Observatoryʼs Discovery Channel Telescope. Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the NSF (AST-1005313). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. 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. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. This publication also uses data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, and the U.S. Department of Energy Office of Science. The SDSS-III website is http:// www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
Group:Palomar Transient Factory
Funders:
Funding AgencyGrant Number
NASAUNSPECIFIED
NASA Earth and Space Science Fellowship ProgramNNX12AL70H
NSFATI-1207785
NSFAST-1211916
Gary and Cynthia BengierUNSPECIFIED
Richard and Rhoda Goldman FundUNSPECIFIED
TABASGO FoundationUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
NSF Astronomy and Astrophysics Postdoctoral FellowshipAST-1302771
European Research Council (ERC)307260
Quantum Universe I-Core programUNSPECIFIED
Israeli Committee for planning and budgetingUNSPECIFIED
MINERVA (Israel)UNSPECIFIED
Weizmann-UKUNSPECIFIED
Kimmel AwardUNSPECIFIED
NASA13-SWIFT13-0030
NASA14-SWIFT14-0024
NASA/JPL/CaltechUNSPECIFIED
NASANNX09AH71G
NASANNX09AT02G
NASANNX10AI27G
NASANNX12AE66G
Consejo Nacional de Ciencia y Tecnología (CONACyT)INFR-2009-01-122785
Consejo Nacional de Ciencia y Tecnología (CONACyT)CB-2008-101958
UNAM PAPIITIG100414
Consejo Nacional de Ciencia y Tecnología (CONACyT)CN 09-283
Discovery CommunicationsUNSPECIFIED
NSFAST-1005313
W. M. Keck FoundationUNSPECIFIED
Israel Science FoundationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
ARCHES AwardUNSPECIFIED
Subject Keywords:gamma-ray burst: individual (GRB 130702A) – supernovae: individual (SN 2013dx)
Issue or Number:1
Record Number:CaltechAUTHORS:20151207-131630440
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151207-131630440
Official Citation:V. L. Toy et al 2016 ApJ 818 79
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62656
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:08 Dec 2015 21:33
Last Modified:03 Oct 2019 09:21

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