Krisciunas, Kevin and Marion, G. H. and Suntzeff, Nicholas B. and Blanc, Guillaume and Bufano, Filomena and Candia, Pablo and Cartier, Regis and Elias-Rosa, Nancy and Espinoza, Juan and Gonzalez, David and Gonzalez, Luis and Gonzalez, Sergio and Gooding, Samuel D. and Hamuy, Mario and Knox, Ethan A. and Milne, Peter A. and Morrell, Nidia and Phillips, Mark M. and Stritzinger , Maximilian and Thomas-Osip, Joanna (2009) The Fast Declining Type Ia Supernova 2003gs, and Evidence for a Significant Dispersion in Near-Infrared Absolute Magnitudes of Fast Decliners at Maximum Light. Astronomical Journal, 138 (6). pp. 1584-1596. ISSN 0004-6256 http://resolver.caltech.edu/CaltechAUTHORS:20091224-084803741
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We obtained optical photometry of SN 2003gs on 49 nights, from 2 to 494 days after T(B_(max)). We also obtained near-IR photometry on 21 nights. SN 2003gs was the first fast declining Type Ia SN that has been well observed since SN 1999by. While it was subluminous in optical bands compared to more slowly declining Type Ia SNe, it was not subluminous at maximum light in the near-IR bands. There appears to be a bimodal distribution in the near-IR absolute magnitudes of Type Ia SNe at maximum light. Those that peak in the near-IR after T(B_(max)) are subluminous in the all bands. Those that peak in the near-IR prior to T(B_(max)), such as SN 2003gs, have effectively the same near-IR absolute magnitudes at maximum light regardless of the decline rate Δm_(15)(B). Near-IR spectral evidence suggests that opacities in the outer layers of SN 2003gs are reduced much earlier than for normal Type Ia SNe. That may allow γ rays that power the luminosity to escape more rapidly and accelerate the decline rate. This conclusion is consistent with the photometric behavior of SN 2003gs in the IR, which indicates a faster than normal decline from approximately normal peak brightness.
|Additional Information:||© 2009 The American Astronomical Society. Received 2009 June 10; accepted 2009 September 19; published 2009 October 27. We thank Rubina Kotak for access to IR spectra of SN 2003gs ahead of publication and for calculating the bolometric light curve of SN 2003gs. E.A.K. was supported by the REU program of the National Science Foundation. We particularly thank the Carnegie Supernova Project for access to data prior to publication. We thank Jose Luis Prieto for his BVRI light-curve fitting templates. We thank Peter Hoeflich for useful discussions relating to the “late and faint” effect. We made use of the NASA/IPAC Extragalactic Database (NED), data of the Two Micron All Sky Survey, and SIMBAD, operated at CDS, Strasbourg, France. Most of the optical and IR photometry was obtained with the CTIO 1.3 m telescope, which is operated by the SMARTS consortium. Without the rapid response made possible by SMARTS, this valuable data set would not have been obtained. M.H. and R.C. acknowledge support provided by FONDECYT through grant 1060808, the Millennium Center for Supernova Science through grant P06-045-F, Centro de Astrof´ısica FONDAP 15010003, Center of Excellence in Astrophysics and Associated Technologies (PFB 06). R.C. was supported by CONICYT through Programa Nacional de Becas de Postgrado grant D-2108082. Some of the infrared data in Table 5 were obtained as part of the European Supernova Collaboration (ESC).|
|Subject Keywords:||supernovae: individual (SN 2003gs); techniques: photometric|
|Official Citation:||The Fast Declining Type Ia Supernova 2003gs, and Evidence for a Significant Dispersion in Near-Infrared Absolute Magnitudes of Fast Decliners at Maximum Light Kevin Krisciunas, G. H. Marion, Nicholas B. Suntzeff, Guillaume Blanc, Filomena Bufano, Pablo Candia, Regis Cartier, Nancy Elias-Rosa, Juan Espinoza, David Gonzalez, Luis Gonzalez, Sergio Gonzalez, Samuel D. Gooding, Mario Hamuy, Ethan A. Knox, Peter A. Milne, Nidia Morrell, Mark M. Phillips, Maximilian Stritzinger, and Joanna Thomas-Osip 2009 The Astronomical Journal 138 1584-1596 doi: 10.1088/0004-6256/138/6/1584|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||05 Jan 2010 17:08|
|Last Modified:||26 Dec 2012 11:39|
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