The Delay Times of Type Ia Supernova

Abstract

The delay time distribution of Type Ia supernovae (the time-dependent rate of supernovae resulting from a burst of star formation) has been measured using different techniques and in different environments. Here, we study in detail the distribution for field galaxies, using the SDSS DR7 Stripe 82 supernova sample. We improve a technique we introduced earlier, which is based on galaxy color and luminosity, and is insensitive to details of the star formation history, to include the normalization. Assuming a power-law dependence of the supernova rate with time, DTD(t) = A(t/1 Gyr) s , we find a power-law index s = −1.34 +0.19 −0.17 and a normalization log A = −12.15 +0.10 −0.13 dex(M −1 yr −1 ), corresponding to a number of type Ia supernovae integrated over a Hubble time of P E = 0.004 +0.002 −0.001 M −1 . We also implement a method used by Maoz and collaborators, which is based on star formation history reconstruction, and find that this gives a consistent result for the slope, but a lower, marginally inconsistent normalization. With our normalization, the distribution for field galaxies is made consistent with that derived for cluster galaxies. Comparing the inferred distribution with predictions from different evolutionary scenarios for type Ia supernovae, we find that our results are intermediate between the various predictions and do not yet constraint the evolutionary path leading to SNe Ia.

The radial distribution of supernovae compared to star formation tracers

“…According to Nomoto & Leung (2018) companions within the mass range can generate the high accretion rates required for a Type Ia SN to occur and also explain the observed delay time distribution (the rate of SNe arising over time from an instantaneous burst of star formation) of Type Ia SNe (e.g. Totani et al 2008;Maoz, Sharon & Gal-Yam 2010;Heringer, Pritchet & van Kerkwijk 2019). If correct, the SD model, together with the lack of agreement with UV fluxes, suggests the secondary stars of progenitor systems are predominately in the lower portion of the proposed M ∼ 0.7-6 M range.…”

Common envelope to explosion delay time of Type Ia supernovae

“…Friedmann & Maoz (2018) consider t i = 0.04 Gyr and find a SN Ia efficiency, i.e., number of SNe Ia per formed stellar mass to be n Ia ≃ 0.003 − 0.008M −1 ⊙ . Heringer, Pritchet, & van Kerkwijk (2019) have t i = 0.1 Gyr and find n Ia ≃ 0.003 − 0.006M −1 ⊙ . To proceed I take here t i = 0.05 Gyr.…”

The Physics of Star Cluster Formation and Evolution

“…For a normal stellar population, type Ia supernovae appear from about 100 Myr after a star formation event at a rate characterised by the delay time distribution (Heringer et al, 2019):…”