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|Title:||A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw||Authors:||Gall, E. E. E.
Smartt, S. J.
Anderson, J. P.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||582||First Page:||A3||Abstract:||We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P. Appendices are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201525868/olm">http://www.aanda.org||Acknowledgments:||We are grateful to T. Faran, A. Filippenko, and D. Poznanski for making the light curve data of SNe 2000dc, 2001cy, 2001do, 2001fa, 2003hf, 2005dq available to us prior to publication, and to N. Elias-Rosa for providing the spectra of SN 2009hd in digital form. R.K. acknowledges funding from STFC (ST/L000709/1). S.J.S. acknowledges funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement number 291222. S.B. is partially supported by the PRIN-INAF 2014 with the project “Transient Universe: unveiling new types of stellar explosions with PESSTO”. M.F. is supported by the European Union FP7 programme through ERC grant number 320360 to G. Gilmore. S.G. acknowledges support from CONICYT through FONDECYT grant 3130680 and from the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. K.M. is supported by a Marie Curie Intra-European Fellowship, within the 7th European Community Framework Programme (FP7). This work is based (in part) on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects) ESO programme 188.D-3003, 191.D-0935. This work utilizes data from the 40-inch ESO Schmidt Telescope at the La Silla Observatory in Chile with the large area QUEST camera built at Yale University and Indiana University. 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. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/ . The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. This research has made use of the CfA Supernova Archive, which is funded in part by the National Science Foundation through grant AST 0907903.||URI:||http://hdl.handle.net/20.500.12386/24118||URL:||https://www.aanda.org/articles/aa/abs/2015/10/aa25868-15/aa25868-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201525868||Bibcode ADS:||2015A&A...582A...3G||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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