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

Dimitriadis, G. and Sullivan, M. and Kerzendorf, W. and Ruiter, A. J. and Seitenzahl, I. R. and Taubenberger, S. and Doran, G. B. and Gal-Yam, A. and Laher, R. R. and Maguire, K. and Nugent, P. and 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). pp. 3798-3812. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20170629-102443070

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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 ≃ 22 mag over 200–620 d past explosion. Combining with literature data, we estimate the pseudo-bolometric light curve for this event from 200 to 1600 d after explosion, and constrain the likely near-infrared (Near-IR) contribution. This light curve shows a smooth decline consistent with radioactive decay, except over ∼450 to ∼600 d where the light curve appears to decrease faster than expected based on the radioactive isotopes presumed to be present, before flattening at around 600 d. We model the 200–1600 d 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 per cent by day 500) and/or an IRC (with 85 per cent 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⊙. 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).


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx683DOIArticle
https://arxiv.org/abs/1701.07267arXivDiscussion Paper
ORCID:
AuthorORCID
Sullivan, M.0000-0001-9053-4820
Taubenberger, S.0000-0002-4265-1958
Gal-Yam, A.0000-0002-3653-5598
Laher, R. R.0000-0003-2451-5482
Maguire, K.0000-0002-9770-3508
Nugent, P.0000-0002-3389-0586
Ofek, E. O.0000-0002-6786-8774
Surace, J.0000-0001-7291-0087
Additional Information:© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 March 16. Received 2017 January 23; in original form 2016 October 14. Published: 22 March 2017. The authors thank Claes Fransson and Anders Jerkstrand for helpful discussions regarding the infrared catastrophe and its theoretical implications. We acknowledge support from EU/FP7-ERC grant no. [615929] and the Weizmann–UK ‘Making Connections’ program. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence ‘Origin and Structure of the Universe’. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This study is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 091.D-0764, 092.D-0632 and 096.D-0627 and also based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs #13737 and #14166. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Funders:
Funding AgencyGrant Number
European Research Council (ERC)615929
Weizmann-UKUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
NASANAS 5-26555
Subject Keywords:supernovae: general – supernovae: individual: SN 2011fe
Issue or Number:4
Record Number:CaltechAUTHORS:20170629-102443070
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170629-102443070
Official Citation:G. Dimitriadis, M. Sullivan, W. Kerzendorf, A. J. Ruiter, I. R. Seitenzahl, S. Taubenberger, G. B. Doran, A. Gal-Yam, R. R. Laher, K. Maguire, P. Nugent, E. O. Ofek, J. Surace; The late-time light curve of the Type Ia supernova SN 2011fe. Mon Not R Astron Soc 2017; 468 (4): 3798-3812. doi: 10.1093/mnras/stx683
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78690
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:29 Jun 2017 23:39
Last Modified:19 Nov 2019 23:16

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