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Nebular spectra and abundance tomography of the Type Ia supernova SN 2011fe: a normal SN Ia with a stable Fe core

Nebular spectra and abundance tomography of the Type Ia supernova SN 2011fe: a normal SN Ia with a stable Fe core
Nebular spectra and abundance tomography of the Type Ia supernova SN 2011fe: a normal SN Ia with a stable Fe core
A series of optical and one near-infrared nebular spectra covering the first year of the Type Ia supernova SN 2011fe are presented and modelled. The density profile that proved best for the early optical/ultraviolet spectra, ‘?-11fe’, was extended to lower velocities to include the regions that emit at nebular epochs. Model ?-11fe is intermediate between the fast deflagration model W7 and a low-energy delayed-detonation. Good fits to the nebular spectra are obtained if the innermost ejecta are dominated by neutron-rich, stable Fe-group species, which contribute to cooling but not to heating. The correct thermal balance can thus be reached for the strongest [Fe ii] and [Fe iii] lines to be reproduced with the observed ratio. The 56Ni mass thus obtained is ?0.47 ± 0.05?M?. The bulk of 56Ni has an outermost velocity of ?8500 km s?1. The mass of stable iron is ?0.23 ± 0.03?M?. Stable Ni has low abundance, ?10?2?M?. This is sufficient to reproduce an observed emission line near 7400 Å. A sub-Chandrasekhar explosion model with mass 1.02?M? and no central stable Fe does not reproduce the observed line ratios. A mock model where neutron-rich Fe-group species are located above 56Ni following recent suggestions is also shown to yield spectra that are less compatible with the observations. The densities and abundances in the inner layers obtained from the nebular analysis, combined with those of the outer layers previously obtained, are used to compute a synthetic bolometric light curve, which compares favourably with the light curve of SN 2011fe.
0035-8711
2631-2643
Mazzali, P.A.
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Sullivan, M.
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Filippenko, A.V.
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Garnavich, P.M.
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Clubb, K.I.
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Maguire, K.
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Pan, Y.-C.
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Shappee, B.
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Silverman, J.M.
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Benetti, S.
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Hachinger, S.
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Nomoto, K.
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Pian, E.
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Mazzali, P.A.
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Sullivan, M.
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Filippenko, A.V.
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Garnavich, P.M.
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Clubb, K.I.
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Maguire, K.
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Pan, Y.-C.
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Shappee, B.
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Silverman, J.M.
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Benetti, S.
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Hachinger, S.
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Nomoto, K.
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Pian, E.
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Mazzali, P.A., Sullivan, M., Filippenko, A.V., Garnavich, P.M., Clubb, K.I., Maguire, K., Pan, Y.-C., Shappee, B., Silverman, J.M., Benetti, S., Hachinger, S., Nomoto, K. and Pian, E. (2015) Nebular spectra and abundance tomography of the Type Ia supernova SN 2011fe: a normal SN Ia with a stable Fe core. Monthly Notices of the Royal Astronomical Society, 450 (3), 2631-2643. (doi:10.1093/mnras/stv761).

Record type: Article

Abstract

A series of optical and one near-infrared nebular spectra covering the first year of the Type Ia supernova SN 2011fe are presented and modelled. The density profile that proved best for the early optical/ultraviolet spectra, ‘?-11fe’, was extended to lower velocities to include the regions that emit at nebular epochs. Model ?-11fe is intermediate between the fast deflagration model W7 and a low-energy delayed-detonation. Good fits to the nebular spectra are obtained if the innermost ejecta are dominated by neutron-rich, stable Fe-group species, which contribute to cooling but not to heating. The correct thermal balance can thus be reached for the strongest [Fe ii] and [Fe iii] lines to be reproduced with the observed ratio. The 56Ni mass thus obtained is ?0.47 ± 0.05?M?. The bulk of 56Ni has an outermost velocity of ?8500 km s?1. The mass of stable iron is ?0.23 ± 0.03?M?. Stable Ni has low abundance, ?10?2?M?. This is sufficient to reproduce an observed emission line near 7400 Å. A sub-Chandrasekhar explosion model with mass 1.02?M? and no central stable Fe does not reproduce the observed line ratios. A mock model where neutron-rich Fe-group species are located above 56Ni following recent suggestions is also shown to yield spectra that are less compatible with the observations. The densities and abundances in the inner layers obtained from the nebular analysis, combined with those of the outer layers previously obtained, are used to compute a synthetic bolometric light curve, which compares favourably with the light curve of SN 2011fe.

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Accepted/In Press date: 2 April 2015
e-pub ahead of print date: 8 May 2015
Published date: 1 July 2015
Organisations: Astronomy Group

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Local EPrints ID: 394602
URI: https://eprints.soton.ac.uk/id/eprint/394602
ISSN: 0035-8711
PURE UUID: 117918a4-62b8-4508-aeed-f1e81a32a0bf
ORCID for M. Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

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Date deposited: 20 May 2016 15:48
Last modified: 20 Jul 2019 00:40

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Contributors

Author: P.A. Mazzali
Author: M. Sullivan ORCID iD
Author: A.V. Filippenko
Author: P.M. Garnavich
Author: K.I. Clubb
Author: K. Maguire
Author: Y.-C. Pan
Author: B. Shappee
Author: J.M. Silverman
Author: S. Benetti
Author: S. Hachinger
Author: K. Nomoto
Author: E. Pian

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