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The quiescent progenitors of four Type II-P/L supernovae

Johnson, Samson A. and Kochanek, C. S. and Adams, S. M. (2018) The quiescent progenitors of four Type II-P/L supernovae. Monthly Notices of the Royal Astronomical Society, 480 (2). pp. 1696-1704. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20181205-163501897

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Abstract

We present Large Binocular Telescope difference imaging data for the final years of four Type II-P/L supernovae progenitors. For all four, we find no significant evidence for stochastic or steady variability in the U, B, V, or R bands. Our limits constrain variability to no more than roughly 5–10per cent of the expected R-band luminosities of the progenitors. These limits are comparable to the observed variability of red supergiants in the Magellanic Clouds. Based on these four events, the probability of a Type II-P/L progenitor having an extended outburst after Oxygen ignition is <37 per cent at 90 per cent confidence. Our observations cannot exclude short outbursts in which the progenitor returns to within ∼10 per cent of its quiescent flux on the time-scale of months with no dust formation.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty1966DOIArticle
https://arxiv.org/abs/1712.03957arXivDiscussion Paper
ORCID:
AuthorORCID
Johnson, Samson A.0000-0001-9397-4768
Adams, S. M.0000-0001-5855-5939
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices) Accepted 2018 July 19. Received 2018 July 19; in original form 2017 December 11. We thank the referee for their comments and suggestions that helped clarify our work. We thank K. Stanek for discussions on RSG variability, and T. Sukhbold for providing models on SNe progenitors. CSK is supported by National Science Foundation (NSF) grants AST-1515876 and AST-1515927. This work is based on observations made with the Large Binocular Telescope (LBT). The LBT is an international collaboration among institutions in the United States, Italy, and Germany. The LBT Corporation partners are: the University of Arizona on behalf of the Arizona university system; the Istituto Nazionale di Astro. 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. The All-Sky Automated Survey for Supernovae (ASAS-SN) is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University (OSU), NSF grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, and the Chinese Academy of Sciences South America Center for Astronomy (CASSACA).
Funders:
Funding AgencyGrant Number
NSFAST-1515876
NSFAST-1515927
NASA/JPL/CaltechUNSPECIFIED
Gordon and Betty Moore FoundationGBMF5490
Mt. Cuba Astronomical FoundationUNSPECIFIED
Center for Cosmology and AstroParticle Physics (CCAPP)UNSPECIFIED
Chinese Academy of Sciences South America Center for Astronomy (CASSACA)UNSPECIFIED
Subject Keywords:stars: massive, supernovae: general, supernovae: individual: SN 2013am, SN 2013ej, ASASSN-2016fq, SN 2017eaw
Record Number:CaltechAUTHORS:20181205-163501897
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20181205-163501897
Official Citation:Samson A Johnson, C S Kochanek, S M Adams; The quiescent progenitors of four Type II-P/L supernovae, Monthly Notices of the Royal Astronomical Society, Volume 480, Issue 2, 21 October 2018, Pages 1696–1704, https://doi.org/10.1093/mnras/sty1966
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:91529
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:06 Dec 2018 15:43
Last Modified:06 Dec 2018 15:43

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