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An Excess of Mid-Infrared Emission from the Type Iax SN 2014dt

Fox, Ori D. and Johansson, Joel and Kasliwal, Mansi M. and Andrews, Jennifer E. and Bally, John and Bond, Howard E. and Boyer, Martha L. and Gehrz, R. D. and Helou, George and Hsiao, E. Y. and Masci, Frank J. and Parthasarathy, M. and Smith, Nathan and Tinyanont, Samaporn and Van Dyk, Schuyler D. (2016) An Excess of Mid-Infrared Emission from the Type Iax SN 2014dt. Astrophysical Journal Letters, 816 (1). Art. No. 13. ISSN 2041-8205. https://resolver.caltech.edu/CaltechAUTHORS:20151117-084214250

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Abstract

Supernovae Type Iax (SNe Iax) are less energetic and less luminous than typical thermonuclear explosions. A suggested explanation for the observed characteristics of this subclass is a binary progenitor system consisting of a CO white dwarf primary accreting from a helium star companion. A single-degenerate explosion channel might be expected to result in a dense circumstellar medium (CSM), although no evidence for such a CSM has yet been observed for this subclass. Here we present recent Spitzer observations of the SN Iax 2014dt obtained by the SPIRITS program nearly one year post-explosion that reveal a strong mid-IR excess over the expected fluxes of more normal SNe Ia. This excess is consistent with 10^(−5) M_⊙ of newly formed dust, which would be the first time that newly formed dust has been observed to form in a Type Ia. The excess, however, is also consistent with a dusty CSM that was likely formed in pre-explosion mass-loss, thereby suggesting a single degenerate progenitor system. Compared to other SNe Ia that show significant shock interaction (SNe Ia-CSM) and interacting core-collapse events (SNe IIn), this dust shell in SN 2014dt is less massive. We consider the implications that such a pre-existing dust shell has for the progenitor system, including a binary system with a mass donor that is a red giant, a red supergiant, or an asymptotic giant branch star.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/2041-8205/816/1/L13DOIArticle
http://arxiv.org/abs/1510.08070arXivDiscussion Paper
ORCID:
AuthorORCID
Fox, Ori D.0000-0003-2238-1572
Johansson, Joel0000-0001-5975-290X
Kasliwal, Mansi M.0000-0002-5619-4938
Andrews, Jennifer E.0000-0003-0123-0062
Bally, John0000-0001-8135-6612
Bond, Howard E.0000-0003-1377-7145
Boyer, Martha L.0000-0003-4850-9589
Gehrz, R. D.0000-0003-1319-4089
Helou, George0000-0003-3367-3415
Masci, Frank J.0000-0002-8532-9395
Tinyanont, Samaporn0000-0002-1481-4676
Van Dyk, Schuyler D.0000-0001-9038-9950
Additional Information:© 2016. The American Astronomical Society. Received 2015 October 27; accepted 2015 December 17; published 2015 December 30. This work is based on data obtained via Program #11063 with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors thank Ryan Foley for useful discussions. We thank Peter Milne, Jacob Jencson, and Tom Prince for help with observations.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/Caltech11063
Non-Subject Keywords:circumstellar matter; dust, extinction; infrared: stars; supernovae: general; supernovae: individual (SN 2014dt)
Issue or Number:1
Record Number:CaltechAUTHORS:20151117-084214250
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151117-084214250
Official Citation:Ori D. Fox et al 2016 ApJ 816 L13
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:62153
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:17 Nov 2015 18:50
Last Modified:19 Nov 2019 23:07

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