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dc.contributor.authorSharon, Keren
dc.contributor.authorGal-Yam, Avishay
dc.contributor.authorMaoz, Dan
dc.contributor.authorFilippenko, Alexei V.
dc.contributor.authorFoley, Ryan J.
dc.contributor.authorSilverman, Jeffrey M.
dc.contributor.authorEbeling, Harald
dc.contributor.authorMa, Cheng-Jiun
dc.contributor.authorOfek, Eran O.
dc.contributor.authorKneib, Jean-Paul
dc.contributor.authorDonahue, Megan
dc.contributor.authorEllis, Richard S.
dc.contributor.authorFreedman, Wendy L.
dc.contributor.authorKirshner, Robert P.
dc.contributor.authorMulchaey, John S.
dc.contributor.authorSarajedini, Vicki L.
dc.contributor.authorVoit, G. Mark
dc.date.accessioned2019-09-25T14:12:06Z
dc.date.issued2010
dc.identifier.citationSharon, Keren, Avishay Gal-Yam, Dan Maoz, Alexei V. Filippenko, Ryan J. Foley, Jeffrey M. Silverman, Harald Ebeling, et al. 2010. “THE TYPE Ia SUPERNOVA RATE IN REDSHIFT 0.5-0.9 GALAXY CLUSTERS.” The Astrophysical Journal 718 (2): 876–93. https://doi.org/10.1088/0004-637x/718/2/876.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41399765*
dc.description.abstractSupernova (SN) rates are potentially powerful diagnostics of metal enrichment and SN physics, particularly in galaxy clusters with their deep, metal-retaining potentials and relatively simple star formation histories. We have carried out a survey for SNe in galaxy clusters, at a redshift range of 0.5 < z < 0.9, using the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. We reimaged a sample of 15 clusters that were previously imaged by ACS, thus obtaining two to three epochs per cluster in which we discovered five likely cluster SNe, six possible cluster Type Ia supernovae, two hostless SN candidates, and several background and foreground events. Keck spectra of the host galaxies were obtained to establish cluster membership. We conducted detailed efficiency simulations, and measured the stellar luminosities of the clusters using Subaru images. We derive a cluster SN rate of 0.35SNu(B-0.12)(+0.17) (statistical) +/- 0.13(classification) +/- 0.01(systematic) (where SNu(B) = SNe (100 yr 10(10) L(B,circle dot))(-1)) and 0.112SNu(M-0.039)(+0.055)(statistical) +/- 0.042(classification) +/- 0.005(systematic) (where SNu(M) = SNe (100 yr 10(10) M(circle dot))(-1)). As in previous measurements of cluster 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 at lower redshifts (to within the uncertainties), and shows that there is, at most, only a slight increase of cluster SN rate with increasing redshift. The low and fairly constant SN Ia rate out to z approximate to 1 implies that the bulk of the iron mass in clusters was already in place by z approximate to 1. The recently observed doubling of iron abundances in the intracluster medium between z = 1 and 0, if real, is likely to be the result of redistribution of existing iron, rather than new production of iron.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleThe Type Ia Supernova Rate in Redshift 0.5-0.9 Galaxy Clusters
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorKirshner, Robert P.::0f07c3b6230f5e5a42326bcba12a1795::600
dc.date.available2019-09-25T14:12:06Z
dash.workflow.comments1Science Serial ID 98639
dc.identifier.doi10.1088/0004-637X/718/2/876
dash.source.volume718;2
dash.source.page876-893


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