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The late-time light curve of the Type Ia supernova SN 2011fe

The late-time light curve of the Type Ia supernova SN 2011fe
The late-time light curve of the Type Ia supernova SN 2011fe
We present late-time optical $R$-band imaging data from the Palomar Transient Factory (PTF) for the nearby type Ia supernova SN 2011fe. The stacked PTF light curve provides densely sampled coverage down to $R\simeq22$ mag over 200 to 620 days past explosion. Combining with literature data, we estimate the pseudo-bolometric light curve for this event from 200 to 1600 days after explosion, and constrain the likely near-infrared contribution. This light curve shows a smooth decline consistent with radioactive decay, except over ~450 to ~600 days where the light curve appears to decrease faster than expected based on the radioactive isotopes presumed to be present, before flattening at around 600 days. We model the 200-1600d pseudo-bolometric light curve with the luminosity generated by the radioactive decay chains of $^{56}$Ni, $^{57}$Ni and $^{55}$Co, and find it is not consistent with models that have full positron trapping and no infrared catastrophe (IRC); some additional energy escape other than optical/near-IR photons is required. However, the light curve is consistent with models that allow for positron escape (reaching 75% by day 500) and/or an IRC (with 85% of the flux emerging in non-optical wavelengths by day 600). The presence of the $^{57}$Ni decay chain is robustly detected, but the $^{55}$Co decay chain is not formally required, with an upper mass limit estimated at 0.014 M$_{\odot}$. The measurement of the $^{57}$Ni/$^{56}$Ni mass ratio is subject to significant systematic uncertainties, but all of our fits require a high ratio >0.031 (>1.3 in solar abundances).
0035-8711
3798-3812
Dimitriadis, G.
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Sullivan, M.
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Kerzendorf, W.
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Ruiter, A. J.
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Seitenzahl, I. R.
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Taubenberger, S.
a81f550f-8713-4f0a-9205-34ae5078f88d
Doran, G. B.
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Gal-Yam, A.
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Laher, R. R.
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Maguire, K.
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Nugent, P.
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Ofek, E. O.
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Surace, J.
5ed4d52a-2b90-4b0f-ba42-13045011a993
Dimitriadis, G.
b8c45fce-1e15-408b-b698-41681f516860
Sullivan, M.
2f31f9fa-8e79-4b35-98e2-0cb38f503850
Kerzendorf, W.
07cd846e-6835-498d-ba25-11a7c5891fc5
Ruiter, A. J.
985ec08e-67e2-4f21-872c-6e204fb970f4
Seitenzahl, I. R.
c74fa47c-3d3e-4d19-87e1-04c65bc54eb8
Taubenberger, S.
a81f550f-8713-4f0a-9205-34ae5078f88d
Doran, G. B.
bb3a030a-e66b-49b8-985e-8d172cc329b3
Gal-Yam, A.
32060b88-6fbc-42cc-9ec3-1de2842aa0e5
Laher, R. R.
4489e67f-8929-44f1-af59-c2f150f799b8
Maguire, K.
94dfab90-b220-454f-8d2a-4ab4ffe27c65
Nugent, P.
0b012273-c3a5-4319-ac63-d0d3e15f8f61
Ofek, E. O.
85a83718-89bf-46d7-84b7-e33dcea29a25
Surace, J.
5ed4d52a-2b90-4b0f-ba42-13045011a993

Dimitriadis, G., Sullivan, M., Kerzendorf, W., Ruiter, A. J., Seitenzahl, I. R., Taubenberger, S., Doran, G. B., Gal-Yam, A., Laher, R. R., Maguire, K., Nugent, P., Ofek, E. O. and Surace, J. (2017) The late-time light curve of the Type Ia supernova SN 2011fe. Monthly Notices of the Royal Astronomical Society, 468 (4), 3798-3812. (doi:10.1093/mnras/stx683).

Record type: Article

Abstract

We present late-time optical $R$-band imaging data from the Palomar Transient Factory (PTF) for the nearby type Ia supernova SN 2011fe. The stacked PTF light curve provides densely sampled coverage down to $R\simeq22$ mag over 200 to 620 days past explosion. Combining with literature data, we estimate the pseudo-bolometric light curve for this event from 200 to 1600 days after explosion, and constrain the likely near-infrared contribution. This light curve shows a smooth decline consistent with radioactive decay, except over ~450 to ~600 days where the light curve appears to decrease faster than expected based on the radioactive isotopes presumed to be present, before flattening at around 600 days. We model the 200-1600d pseudo-bolometric light curve with the luminosity generated by the radioactive decay chains of $^{56}$Ni, $^{57}$Ni and $^{55}$Co, and find it is not consistent with models that have full positron trapping and no infrared catastrophe (IRC); some additional energy escape other than optical/near-IR photons is required. However, the light curve is consistent with models that allow for positron escape (reaching 75% by day 500) and/or an IRC (with 85% of the flux emerging in non-optical wavelengths by day 600). The presence of the $^{57}$Ni decay chain is robustly detected, but the $^{55}$Co decay chain is not formally required, with an upper mass limit estimated at 0.014 M$_{\odot}$. The measurement of the $^{57}$Ni/$^{56}$Ni mass ratio is subject to significant systematic uncertainties, but all of our fits require a high ratio >0.031 (>1.3 in solar abundances).

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More information

Accepted/In Press date: 16 March 2016
e-pub ahead of print date: 22 March 2017
Published date: 22 March 2017
Organisations: Astronomy Group, Physics & Astronomy

Identifiers

Local EPrints ID: 408292
URI: https://eprints.soton.ac.uk/id/eprint/408292
ISSN: 0035-8711
PURE UUID: 75c6174a-1d3d-4c97-93c0-c0c05ef61691
ORCID for M. Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

Catalogue record

Date deposited: 19 May 2017 04:02
Last modified: 20 Jul 2019 00:40

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