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The Exceptionally Luminous Type Ia Supernova 2007if

Yuan, F. and Quimby, R. M. and Wheeler, J. C. and Vinkό, J. and Chatzopoulos, E. and Akerlof, C. W. and Kulkarni, S. and Miller, J. M. and McKay, T. A. and Aharonian, F. (2010) The Exceptionally Luminous Type Ia Supernova 2007if. Astrophysical Journal, 715 (2). pp. 1338-1343. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20100614-140415579

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Abstract

SN 2007if was the third over-luminous Type Ia supernova (SN Ia) detected after 2003fg and 2006gz. We present the photometric and spectroscopic observations of the SN and its host by ROTSE-III, HET, and Keck. From the H_α line identified in the host spectra, we determine a redshift of 0.0736. At this distance, the SN reached an absolute magnitude of –20.4, brighter than any other SNe Ia ever observed. If the source of luminosity is radioactive decay, a large amount of radioactive nickel (~1.5 M_☉) is required to power the peak luminosity, more than can be produced realistically in a Chandrasekhar mass progenitor. Low expansion velocity, similar to that of 2003fg, is also measured around the maximum light. The observations may suggest that SN 2007if was from a massive white dwarf progenitor, plausibly exploding with mass well beyond 1.4 M_☉. Alternatively, we investigate circumstellar interaction that may contribute to the excess luminosity.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/715/2/1338DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/715/2/1338PublisherUNSPECIFIED
ORCID:
AuthorORCID
Quimby, R. M.0000-0001-9171-5236
Kulkarni, S.0000-0001-5390-8563
Additional Information:© 2010 The American Astronomical Society. Received 2009 December 22; accepted 2010 April 13; published 2010 May 10. The authors gratefully acknowledge M. Kasliwal for the data taken at Keck, and C. S. Peters and J. R. Thorstensen for the data taken at the 2.4 m Hiltner telescope. Special thanks to the McDonald Observatory staff and the H.E.S.S. staff, especially David Doss and Toni Hanke. We also thank the staff of Hobby- Eberly Telescope for their support. F.Y. is supported by the NASA Swift Guest Investigator grants NNX-08AN25G. J.C.W. is supported in part by NSF AST-0707769. ROTSE-III has been supported by NASA grant NNX-08AV63G, NSF grant PHY- 0801007, the Australian Research Council, the University of New South Wales, the University of Texas, and the University of Michigan. The authors thank the anonymous referee for the valuable comments.
Funders:
Funding AgencyGrant Number
NASANNX-08AN25G
NSFAST-0707769
NASANNX-08AV63G
NSFPHY-0801007
Australian Research CouncilUNSPECIFIED
University of New South WalesUNSPECIFIED
University of TexasUNSPECIFIED
University of MichiganUNSPECIFIED
Subject Keywords:supernovae: individual (SN 2007if)
Issue or Number:2
Classification Code:PACS: 97.60.Bw; 97.10.Ri; 97.10.Fy; 95.85.Kr
Record Number:CaltechAUTHORS:20100614-140415579
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20100614-140415579
Official Citation:F. Yuan et al 2010 ApJ 715 1338 doi: 10.1088/0004-637X/715/2/1338
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18670
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:14 Jun 2010 21:50
Last Modified:03 Oct 2019 01:46

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