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Detection of Circumstellar Material in a Normal Type Ia Supernova

Patat, F. and Chandra, P. and Chevalier, R. and Justham, S. and Podsiadlowski, Ph. and Wolf, C. and Gal-Yam, A. and Pasquini, L. and Crawford, I. A. and Mazzali, P. A. and Pauldrach, A. W. A. and Nomoto, K. and Benetti, S. and Cappellaro, E. and Elias-Rosa, N. and Hillebrandt, W. and Leonard, D. C. and Pastorello, A. and Renzini, A. and Sabbadin, F. and Simon, J. D. and Turatto, M. (2007) Detection of Circumstellar Material in a Normal Type Ia Supernova. Science, 317 (5840). pp. 924-926. ISSN 0036-8075. https://resolver.caltech.edu/CaltechAUTHORS:20141114-104814192

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Abstract

Type Ia supernovae are important cosmological distance indicators. Each of these bright supernovae supposedly results from the thermonuclear explosion of a white dwarf star that, after accreting material from a companion star, exceeds some mass limit, but the true nature of the progenitor star system remains controversial. Here we report the spectroscopic detection of circumstellar material in a normal type Ia supernova explosion. The expansion velocities, densities, and dimensions of the circumstellar envelope indicate that this material was ejected from the progenitor system. In particular, the relatively low expansion velocities suggest that the white dwarf was accreting material from a companion star that was in the red-giant phase at the time of the explosion.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1126/science.1143005DOIArticle
http://www.sciencemag.org/content/317/5840/924PublisherArticle
http://www.sciencemag.org/content/317/5840/924/suppl/DC1PublisherSupporting Online Material
https://arxiv.org/abs/0707.2793arXivDiscussion Paper
ORCID:
AuthorORCID
Patat, F.0000-0002-0537-3573
Wolf, C.0000-0002-4569-016X
Gal-Yam, A.0000-0002-3653-5598
Mazzali, P. A.0000-0001-6876-8284
Nomoto, K.0000-0001-9553-0685
Benetti, S.0000-0002-3256-0016
Cappellaro, E.0000-0001-5008-8619
Elias-Rosa, N.0000-0002-1381-9125
Renzini, A.0000-0002-7093-7355
Additional Information:© 2007 American Association for the Advancement of Science. Received 26 March 2007; accepted 29 June 2007 Published online 12 July 2007. We thank K. Krisciunas for providing information about the photometric evolution of SN 2006X. We acknowledge K. Steenbrugge, F. Primas, W. M. Wood-Vasey, R. Corradi, G. J. Ferland, P. van Hoof, F. Bresolin, and C. Stockdale for useful discussions. We particularly thank M. F. Bode for sharing some results on RS Ophiuchi before publication. This work is based on observations made with ESO telescopes at Paranal Observatory, obtained under run IDs 276.D-5048, 277.D-5003, and 277.D-5013. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. This work made use of the Very Large Array telescope of the National Radio Astronomy Observatory (NRAO), which is operated by Associated Universities, Incorporated, under a cooperative agreement with NSF. P.C. is a Jansky Fellow of the NRAO.
Issue or Number:5840
Record Number:CaltechAUTHORS:20141114-104814192
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20141114-104814192
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:51767
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:14 Nov 2014 18:56
Last Modified:09 Mar 2020 13:19

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