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Spectral models for early time SN 2011fe observations

Spectral models for early time SN 2011fe observations
Spectral models for early time SN 2011fe observations
We use observed UV through near-IR spectra to examine whether SN 2011fe can be understood in the framework of Branch-normal Type Ia supernovae (SNe Ia) and to examine its individual peculiarities. As a benchmark, we use a delayed-detonation model with a progenitor metallicity of Z?/20. We study the sensitivity of features to variations in progenitor metallicity, the outer density profile, and the distribution of radioactive nickel. The effect of metallicity variations in the progenitor have a relatively small effect on the synthetic spectra. We also find that the abundance stratification of SN 2011fe resembles closely that of a delayed-detonation model with a transition density that has been fit to other Branch-normal SNe Ia. At early times, the model photosphere is formed in material with velocities that are too high, indicating that the photosphere recedes too slowly or that SN 2011fe has a lower specific energy in the outer ?0.1 M? than does the model. We discuss several explanations for the discrepancies. Finally, we examine variations in both the spectral energy distribution and in the colours due to variations in the progenitor metallicity, which suggests that colours are only weak indicators for the progenitor metallicity, in the particular explosion model that we have studied. We do find that the flux in the U band is significantly higher at maximum light in the solar metallicity model than in the lower metallicity model and the lower metallicity model much better matches the observed spectrum.
0035-8711
2549-2556
Baron, E.
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Hoeflich, P.
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Friesen, Brian
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Sullivan, M.
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Hsiao, E.
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Ellis, R.S.
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Gal-Yam, A.
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Howell, D.A.
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Nugent, P.E.
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Dominguez, I.
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Krisciunas, K.
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Phillips, M.M.
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Suntzeff, N.
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Wang, L.
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Thomas, R.C.
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Baron, E.
94502a84-e3b0-41bc-a9c2-c1a308a8b559
Hoeflich, P.
34054d2f-21d8-4856-ae26-38709b8bd7bb
Friesen, Brian
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Sullivan, M.
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Hsiao, E.
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Ellis, R.S.
bf153fc2-2ab9-495b-913c-2f849ad42225
Gal-Yam, A.
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Howell, D.A.
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Nugent, P.E.
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Dominguez, I.
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Krisciunas, K.
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Phillips, M.M.
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Suntzeff, N.
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Wang, L.
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Thomas, R.C.
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Baron, E., Hoeflich, P., Friesen, Brian, Sullivan, M., Hsiao, E., Ellis, R.S., Gal-Yam, A., Howell, D.A., Nugent, P.E., Dominguez, I., Krisciunas, K., Phillips, M.M., Suntzeff, N., Wang, L. and Thomas, R.C. (2015) Spectral models for early time SN 2011fe observations. Monthly Notices of the Royal Astronomical Society, 454 (3), 2549-2556. (doi:10.1093/mnras/stv1951).

Record type: Article

Abstract

We use observed UV through near-IR spectra to examine whether SN 2011fe can be understood in the framework of Branch-normal Type Ia supernovae (SNe Ia) and to examine its individual peculiarities. As a benchmark, we use a delayed-detonation model with a progenitor metallicity of Z?/20. We study the sensitivity of features to variations in progenitor metallicity, the outer density profile, and the distribution of radioactive nickel. The effect of metallicity variations in the progenitor have a relatively small effect on the synthetic spectra. We also find that the abundance stratification of SN 2011fe resembles closely that of a delayed-detonation model with a transition density that has been fit to other Branch-normal SNe Ia. At early times, the model photosphere is formed in material with velocities that are too high, indicating that the photosphere recedes too slowly or that SN 2011fe has a lower specific energy in the outer ?0.1 M? than does the model. We discuss several explanations for the discrepancies. Finally, we examine variations in both the spectral energy distribution and in the colours due to variations in the progenitor metallicity, which suggests that colours are only weak indicators for the progenitor metallicity, in the particular explosion model that we have studied. We do find that the flux in the U band is significantly higher at maximum light in the solar metallicity model than in the lower metallicity model and the lower metallicity model much better matches the observed spectrum.

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1508.04774v3.pdf - Accepted Manuscript
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Accepted/In Press date: 20 August 2015
e-pub ahead of print date: 13 October 2015
Published date: 11 December 2015
Organisations: Astronomy Group

Identifiers

Local EPrints ID: 394622
URI: https://eprints.soton.ac.uk/id/eprint/394622
ISSN: 0035-8711
PURE UUID: 795593e6-3de1-40c7-ab79-58e6228712de
ORCID for M. Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

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Date deposited: 23 May 2016 08:01
Last modified: 20 Jul 2019 00:40

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Contributors

Author: E. Baron
Author: P. Hoeflich
Author: Brian Friesen
Author: M. Sullivan ORCID iD
Author: E. Hsiao
Author: R.S. Ellis
Author: A. Gal-Yam
Author: D.A. Howell
Author: P.E. Nugent
Author: I. Dominguez
Author: K. Krisciunas
Author: M.M. Phillips
Author: N. Suntzeff
Author: L. Wang
Author: R.C. Thomas

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