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|Title:||Spectroscopy of the Type Ia supernova 2011fe past 1000d||Authors:||Taubenberger, S.
ELIAS DE LA ROSA, NANCY DEL CARMEN
Kerzendorf, W. E.
Ruiter, A. J.
Seitenzahl, I. R.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||448||First Page:||L48||Abstract:||In this Letter we present an optical spectrum of SN 2011fe taken 1034 d after the explosion, several hundred days later than any other spectrum of a Type Ia supernova (disregarding light-echo spectra and Local Group remnants). The spectrum is still dominated by broad emission features, with no trace of a light echo or interaction of the supernova ejecta with surrounding interstellar material. Comparing this extremely late spectrum to an earlier one taken 331 d after the explosion, we find that the most prominent feature at 331 d - [Fe III] emission around 4700 Å - has entirely faded away, suggesting a significant change in the ionization state. Instead, [Fe II] lines are probably responsible for most of the emission at 1034 d. An emission feature at 6300-6400 Å has newly developed at 1034 d, which we tentatively identify with Fe I λ6359, [Fe I] λλ6231, 6394 or [O I] λλ6300, 6364. Interestingly, the features in the 1034 d spectrum seem to be collectively redshifted, a phenomenon that we currently have no convincing explanation for. We discuss the implications of our findings for explosion models, but conclude that sophisticated spectral modelling is required for any firm statement.||Acknowledgments:||Observations were carried out using the GTC, installed in the Spanish Observatorio del Roque de los Muchachos, on the island of La Palma, and the LBT at Mt Graham, AZ. The authors are grateful to the LBT-Italy consortium for making these ground-breaking DDT observations possible, and would like to thank the telescope operators at LBT, and the support astronomers at GTC, for their commitment. We are also grateful to our referee, Jeffrey Silverman, for his careful reading of the manuscript and his helpful comments. ST is supported by the Transregional Collaborative Research Centre TRR 33 ‘The Dark Universe’ of the DFG. NER acknowledges support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 26751 (AstroFIt). SH is supported by an ARCHES award. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project no. CE110001020, and by ARC Laureate Grant FL0992131. SB, EC, AP and MT are partially supported by PRIN-INAF 2011 with the project ‘Transient Universe: from ESO Large to PESSTO’.||URI:||http://hdl.handle.net/20.500.12386/24141||URL:||https://academic.oup.com/mnrasl/article/448/1/L48/2891006||ISSN:||0035-8711||DOI:||10.1093/mnrasl/slu201||Bibcode ADS:||2015MNRAS.448L..48T||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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|2015MNRAS.448L..48T_postprint.pdf||2015MNRAS.448L..48T||424.42 kB||Adobe PDF||View/Open|
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