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Supernova (SN) rates are potentially powerful diagnostics of metal enrichmentand SN physics, particularly in galaxy clusters with their deep,metal-retaining potentials and relatively simple star-formation histories. Wehave carried out a survey for supernovae (SNe) in galaxy clusters, at aredshift range 0.5<z<0.9, using the Advanced Camera for Surveys (ACS) on theHubble Space Telescope. We reimaged a sample of 15 clusters that werepreviously imaged by ACS, thus obtaining two to three epochs per cluster, inwhich we discovered five likely cluster SNe, six possible cluster SNe Ia, twohostless SN candidates, and several background and foreground events. Keckspectra of the host galaxies were obtained to establish cluster membership. Weconducted detailed efficiency simulations, and measured the stellarluminosities of the clusters using Subaru images. We derive a cluster SN rateof 0.35 SNuB +0.17/-0.12 (statistical) \pm0.13 (classification) \pm0.01(systematic) [where SNuB = SNe (100 yr 10^10 L_B_sun)^-1] and 0.112 SNuM+0.055/-0.039 (statistical) \pm0.042 (classification) \pm0.005 (systematic)[where SNuM = SNe (100 yr 10^10 M_sun)^-1]. As in previous measurements ofcluster SN rates, the uncertainties are dominated by small-number statistics.The SN rate in this redshift bin is consistent with the SN rate in clusters atlower redshifts (to within the uncertainties), and shows that there is, atmost, only a slight increase of cluster SN rate with increasing redshift. Thelow and fairly constant SN Ia rate out to z~1 implies that the bulk of the ironmass in clusters was already in place by z~1. The recently observed doubling ofiron abundances in the intracluster medium between z=1 and 0, if real, islikely the result of redistribution of existing iron, rather than newproduction of iron.

The Type Ia Supernova Rate in Redshift 0.5--0.9 Galaxy Clusters