The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey

Details The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey

2010-01-19

arxiv.org/abs/1001.3428v2

Astrophys.J.712:350-366,2010

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

42 pages, 15 figures, accepted to ApJ for publication in March 2010, v711 issue

Scientific paper

10.1088/0004-637X/712/1/350

We analyze the rise and fall times of type Ia supernova (SN Ia) light curves discovered by the SDSS-II Supernova Survey. From a set of 391 light curves k-corrected to the rest frame B and V bands, we find a smaller dispersion in the rising portion of the light curve compared to the decline. This is in qualitative agreement with computer models which predict that variations in radioactive nickel yield have less impact on the rise than on the spread of the decline rates. The differences we find in the rise and fall properties suggest that a single 'stretch' correction to the light curve phase does not properly model the range of SN Ia light curve shapes. We select a subset of 105 light curves well-observed in both rise and fall portions of the light curves and develop a '2-stretch' fit algorithm which estimates the rise and fall times independently. We find the average time from explosion to B-band peak brightness is 17.38 +/- 0.17 days. Our average rise time is shorter than the 19.5 days found in previous studies; this reflects both the different light curve template used and the application of the 2-stretch algorithm. We find that slow declining events tend to have fast rise times, but that the distribution of rise minus fall time is broad and single-peaked. This distribution is in contrast to the bimodality in this parameter that was first suggested by Strovink (2007) from an analysis of a small set of local SNe Ia. We divide the SDSS-II sample in half based on the rise minus fall value, tr-tf <= 2 days and tr-tf>2 days, to search for differences in their host galaxy properties and Hubble residuals; we find no difference in host galaxy properties or Hubble residuals in our sample.

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