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Michael, additional, Wu, Xiuqin, additional, Xin, Bo, additional, Yoachim, Peter, additional, and Zhan, Hu, additional
!["z\leq]("eq-00001.gif")
z [?] 0.12. Assuming a flat cosmology with !["\Omega]("eq-00002.gif")
Om = 0.3 = 1 [?] OL, we find a volumetric SN Ia rate of !["[]("eq-00003.gif")
[ 2.93+ 0.17[?]0.04(systematic)+ 0.90[?]0.71(statistical) ] x 10[?]5 SNe Mpc [?]3 h370 yr [?]1, at a volume-weighted mean redshift of 0.09. This result is consistent with previous measurements of the SN Ia rate in a similar redshift range. The systematic errors are well controlled, resulting in the most precise measurement of the SN Ia rate in this redshift range. We use a maximum likelihood method to fit SN rate models to the SDSS-II Supernova Survey data in combination with other rate measurements, thereby constraining models for the redshift evolution of the SN Ia rate. Fitting the combined data to a simple power-law evolution of the volumetric SN Ia rate, !["r_{V}\propto]("eq-00004.gif")
rV [?] (1 + z)b, we obtain a value of !["\beta]("eq-00005.gif")
b = 1.5 +- 0.6, i.e., the SN Ia rate is determined to be an increasing function of redshift at the ~2.5 s level. Fitting the results to a model in which the volumetric SN rate is rV = Ar(t) + Br(t) !["r_{V}=A\rho]("eq-00006.gif")
!["\rho]("eq-00007.gif")
r (t) is the stellar mass density and r(t) !["\dot{\rho]("eq-00008.gif")
!["A=(2.8\pm]("eq-00009.gif")
A = (2.8 +- 1.2) x 10[?]14 SNe M[?]1 yr [?]1, !["B=(9.3^{+3.4}_{-3.1})]("eq-00010.gif")
B = (9.3+ 3.4[?]3.1) x 10[?]4 SNe M[?]1.