Knowledge of the supernova (SN) delay time distribution (DTD) - the SN rate versus time that would follow a hypothetical brief burst of star formation - can shed light on SN progenitors and physics. We compile recent measurements of the Type-Ia SN (SN Ia) rate in galaxy clusters at redshifts z=0-1.45. Together with the observed iron-to-stellar mass ratio in clusters, which constrains the time-integrated number of SN Ia events in clusters, we recover the DTD of SNe Ia in cluster environments. The DTD peaks at the shortest time-delay interval we probe, 0<t<2.2 Gyr, with a low tail out to delays of ~10 Gyr, and is remarkably consistent with several recent DTD reconstructions based on different methods, in different environments. We test DTD models from the literature, requiring that they simultaneously reproduce the observed cluster SN rates and the observed iron-to-stellar mass ratios. A power-law DTD of the form t^{-1.2+/-0.3}, extending to a Hubble time, can satisfy both constraints. Shallower power laws, such as t^{-1/2} cannot, assuming a single DTD, and a single star-formation burst (either brief or extended) at high z. This implies 50-85% of SNe Ia explode within 1 Gyr of star formation. DTDs from double-degenerate (DD) models, which generically have ~t^{-1} shapes over a wide range of timescales, match the data, but only if their predictions are scaled up by factors of 5-10. Single degenerate (SD) DTDs always give poor fits to the data, due to a lack of delayed SNe and overall low numbers of SNe. The observations also permit a combination of two SN Ia populations - prompt (e.g. SD) SNe Ia that explode within a few Gyr of star formation, and produce about 60% of the iron mass in clusters, and a DD population that contributes the events seen at z<1.4. Our results support the existence of a DD progenitor channel for SNe Ia, if the overall predicted numbers can be suitably increased.
Integral field spectroscopy of supernova explosion sites: constraining mass and metallicity of the progenitors -- II. Type II-P and II-L supernovae
利用积分场光谱学已经观测到了附近星系中II-P和II-L型超新星的13个爆炸点，使得对爆炸点的空间和光谱研究成为可能。我们利用同时代超新星祖先星的母恒星星族的性质来推导它的金属丰度和初始质量（c.f. Paper I）。母恒星星族的光谱通过强线方法得到金属丰度的估计，并通过与简单的恒星星族（SSP）模型的比较得到年龄。这些金属丰度和年龄参数被采用的祖星。通过与恒星演化模型的比较，利用恒星的年龄或寿命来推导恒星的初始质量。利用这种技术，我们能够确定我们样品中SN祖细胞的金属丰度和初始质量。我们的结果表明，一些II型超新星的祖先可能是质量与SN Ib/c祖先相当的恒星。
