The supernova CSS121015: 004244+132827: A clue for understanding superluminous supernovae

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/101136

Title:	The supernova CSS121015: 004244+132827: A clue for understanding superluminous supernovae
Authors:	陳婷琬;Benetti, S.;Nicholl, M.;Cappellaro, E.;Pastorello, A.;Smartt, S. J.;Elias-Rosa, N.;Drake, A. J.;Tomasella, L.;Turatto, M.;Harutyunyan, A.;Taubenberger, S.;Hachinger, S.;Morales-Garoffolo, A.;Chen, T.-W.;Djorgovski, S. G.;Fraser, M.;Gal-Yam, A.;Inserra, C.;Mazzali, P.;Pumo, M. L.;Sollerman, J.;Valenti, S.;Young, D. R.;Dennefeld, M.;Le Guillou, L.;Fleury, M.;Léget, P.-F.
Contributors:	理學院天文研究所
Keywords:	Astrophysics;Hydrogen;Luminosity;Sciences of the Universe;Spectrum analysis;Star & galaxy formation;Supernovae;supernovae: general;supernovae: individual: CSS121015: 004244+132827
Date:	2014-01-01
Issue Date:	2026-04-21 14:25:10 (UTC+8)
Publisher:	Oxford University Press;London: Oxford University Press
Abstract:	摘要： 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. 其他題名： Mon. Not. R. Astron. Soc 出版者： London: Oxford University Press 出版日期： 2014-06-11 出處： Monthly notices of the Royal Astronomical Society, 2014-06, Vol.441 (1), p.289-303 資源來源： Alma/SFX Local Collection 版權： 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014 版權： Copyright Oxford University Press, UK Jun 11, 2014 版權： licence_http://creativecommons.org/publicdomain/zero 識別號： ISSN: 0035-8711 識別號： ISSN: 1365-2966 識別號： ISSN: 1365-8711 識別號： EISSN: 1365-2966 識別號： DOI: 10.1093/mnras/stu538
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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