A Measurement of the Rate of type-Ia Supernovae at Redshift $z\approx$ 0.1 from the First Season of the SDSS-II Supernova Survey

TL;DR

This paper measures the rate of type Ia supernovae at redshift 0.1 using SDSS-II data, providing a precise rate estimate and insights into its redshift evolution and relation to stellar mass and star formation.

Contribution

It presents the most precise measurement of the SN Ia rate at z~0.1 and constrains its redshift evolution and dependence on stellar mass and star formation.

Findings

SN Ia rate at z~0.1 is approximately 2.93 x 10^{-5} SNe Mpc^{-3} yr^{-1}

SN Ia rate increases with redshift, with a power-law index of 1.5 ± 0.6

The rate correlates with stellar mass density and star formation rate

Abstract

We present a measurement of the rate of type Ia supernovae (SNe Ia) from the first of three seasons of data from the SDSS-II Supernova Survey. For this measurement, we include 17 SNe Ia at redshift $z\le0.12$. Assuming a flat cosmology with $\Omega_m = 0.3=1-\Omega_\Lambda$, we find a volumetric SN Ia rate of $[2.93^{+0.17}_{-0.04}({\rm systematic})^{+0.90}_{-0.71}({\rm statistical})] \times 10^{-5} {\rm SNe} {\rm Mpc}^{-3} h_{70}^3 {\rm year}^{-1}$, 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, $r_V \propto (1+z)^{\beta}$, we obtain a value of $\beta = 1.5 \pm 0.6$, i.e. the SN Ia rate is determined to be an increasing function of redshift at the $\sim 2.5 \sigma$ level. Fitting the results to a model in which the volumetric SN rate, $r_V=A\rho(t)+B\dot \rho(t)$, where $\rho(t)$ is the stellar mass density and $\dot \rho(t)$ is the star formation rate, we find $A = (2.8 \pm 1.2) \times 10^{-14} \mathrm{SNe} \mathrm{M}_{\sun}^{-1} \mathrm{year}^{-1}$, $B = (9.3^{+3.4}_{-3.1})\times 10^{-4} \mathrm{SNe} \mathrm{M}_{\sun}^{-1}$.