The supernova CSS121015:004244+132827: a clue for understanding superluminous supernovae
- Creators
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Benetti, S.
- Drake, A. J.
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Djorgovski, S. G.
Abstract
We present optical photometry and spectra of the superluminous Type II/IIn supernova (SN) CSS121015:004244+132827 (z = 0.2868) spanning epochs from −30 d (rest frame) to more than 200 d after maximum. CSS121015 is one of the more luminous SNe ever found and one of the best observed. The photometric evolution is characterized by a relatively fast rise to maximum (∼40 d in the SN rest frame), and by a linear post-maximum decline. The light curve shows no sign of a break to an exponential tail. A broad Hα is first detected at ∼+40 d (rest frame). Narrow, barely resolved Balmer and [O III] 5007 Å lines, with decreasing strength, are visible along the entire spectral evolution. The spectra are very similar to other superluminous supernovae (SLSNe) with hydrogen in their spectrum, and also to SN 2005gj, sometimes considered Type Ia interacting with H-rich circumstellar medium. The spectra are also similar to a subsample of H-deficient SLSNe. We propose that the properties of CSS121015 are consistent with the interaction of the ejecta with a massive, extended, opaque shell, lost by the progenitor decades before the final explosion, although a magnetar-powered model cannot be excluded. Based on the similarity of CSS121015 with other SLSNe (with and without H), we suggest that the shocked-shell scenario should be seriously considered as a plausible model for both types of SLSN.
Additional Information
© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 March 17. Received 2014 March 17; in original form 2013 October 4. We thank the anonymous referee for very useful comments and suggestions. SB, EC, AP, LT and MT are partially supported by the PRIN-INAF 2011 with the project Transient Universe: from ESO Large to PESSTOÓ. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no. [291222] (PI: SJS) and EU/FP7-ERC grant no. [307260] (PI: AG-Y). AG-Y is also supported by 'The Quantum UniverseÓ I-Core programme by the Israeli Committee for planning and funding and the ISF, a GIF grant, and the Kimmel award'. NER and AMG acknowledge financial support by the MICINN grant AYA2011-24704/ESP, and by the ESF EUROCORES Program EuroGENESIS (MINECO grants EUI2009-04170). NER acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251. The CRTS survey is supported by the US National Science Foundation under grant AST-1313422. This work is partially based on observations collected at (1) the European Organisation for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO, (the PESSTO survey) ESO programme 188.D-3003; (2) the Copernico 1.82 m Telescope operated by INAF – Osservatorio Astronomico di Padova at Asiago; (3) the 3.6 m Italian Telescopio Nazionale Galileo operated by the Fundaciόn Galileo Galilei – INAF on the island of La Palma; (4) the 4.3 m William Herschel Telescope operated by the Isaac Newton Group of Telescope; (5) the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof'sica de Canarias, in the island of La Palma; (6) the Liverpool Telescope, which 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; (6) the Faulkes Telescope Project, which is an educational and research arm of the Las Cumbres Observatory Global Telescope Network (LCOGTN); (7) the Large Binocular Telescope (LBT), which is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam and Heidelberg University; the Ohio State University; the Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia. 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. We thank R. Kotak for taking the WHT+intermediate dispersion spectrograph and imaging system (ISIS) spectrum of 2012 November 20.Attached Files
Published - MNRAS-2014-Benetti-289-303.pdf
Submitted - 1310.1311v3.pdf
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Additional details
- Eprint ID
- 46398
- Resolver ID
- CaltechAUTHORS:20140620-110505377
- Istituto Nazionale di Astrofisica (INAF)
- 291222
- European Research Council (ERC)
- 307260
- European Research Council (ERC)
- Quantum UniverseÓ I-Core programme
- Israeli Committee for Planning and Funding
- Israel Science Foundation
- German-Israeli Foundation for Research and Development
- Kimmel Award
- AYA2011-24704/ESP
- MICINN
- EUI2009-04170
- ESF EUDOCORES Progam EuroGENESIS (MINECO)
- 267251
- European Research Council (ERC)
- AST-1313422
- NSF
- Science and Technology Facilities Council (STFC)
- NASA/JPL/Caltech
- Created
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2014-06-20Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field