2002MNRAS.332...37G

We have searched for high-redshift supernova (SN) candidates in multiple deep Hubble Space Telescope (HST) archival images of nine galaxy cluster fields. We detect six apparent SNe, with 21.6≤I₈₁₄≤28.4mag. There is roughly 1 SN per deep (I₈₁₄>26mag), doubly-imaged WFPC2 cluster field. Two SNe are associated with cluster galaxies (at redshifts z =0.18 and z =0.83), three are probably in galaxies not in the clusters (at z =0.49, z =0.60, and z =0.98), and one is at unknown z. After accounting for observational efficiencies and uncertainties (statistical and systematic) we derive the rate of type Ia SNe within the projected central 500h^–1₅₀kpc of rich clusters: R=0.20^+0.84-0.19_h50_² SNu in 0.18≤z≤0.37 clusters, and R=0.41^+1.23_–0.39h₅₀² SNu in clusters at 0.83≤z ≤1.27 (95 per cent confidence interval; 1 SNu≡1 SN.century^–1 per 10¹⁰ L_B☉). Combining the two redshift bins, the mean rate is R_z=0.41=0.30^+0.58_–0.28h₅₀² SNu. The upper bounds argue against SNe Ia being the dominant source of the large iron mass observed in the intracluster medium. We also compare our observed counts of field SNe (i.e. non-cluster SNe of all types) to recent model predictions. The observed field count is N ≤1 SN with I₈₁₄≤26mag, and 1≤N ≤3 SNe with I₈₁₄≤27mag. These counts are half of some of the predictions. Since the counts at these magnitudes are likely dominated by type II SNe, our observations may suggest obscuration of distant SNe II, or a SN II luminosity distribution devoid of a large high-luminosity tail.