Supernovae in deep Hubble Space Telescope galaxy cluster fields: cluster rates and field counts
Supernovae in deep Hubble Space Telescope galaxy cluster fields: cluster rates and field counts
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哈勃太空望远镜深部星系团场中的超新星：星团率和场计数
DOI：
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
K. Sharon
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文献类型：
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作者：
A. Gal;D. Maoz;K. Sharon
我们已经在哈勃太空望远镜（HST）的9个星系团领域的多个深档案图像中搜索了高红移超新星（SN）候选者。我们探测到六个明显的超新星，21.6I81428.4马格。每深度大约有1个SN（I814>26 mag），双重成像WFPC 2簇场。两个SNe与星系团有关（红移z=0.18和z=0.83），三个可能在星系团以外的星系中（z=0.49，z=0.60和z=0.98），一个z未知。在考虑了观测效率和不确定性（统计和系统）后，我们得出了在富星系团的预测中心内Ia型SNe的比率：SNu在0.18 z0.37星系团中，SNu在0.83 z1.27星系团中（95%置信区间; 1 SNu = 1 SN世纪-1/1010 LB）。结合两个红移箱，平均速率为SNu。上限反对超新星Ia是在集群内介质中观察到的大铁质量的主要来源。我们还将我们观察到的场SNe（即所有类型的非集群SNe）计数与最近的模型预测进行了比较。观测到的场数为N1 SN（I81426等）和1 N3 SNe（I81427等）。这些数字是一些预测的一半。由于这些星等的计数很可能由II型SNe主导，我们的观测可能表明遥远的SNe II的遮蔽，或者没有大的高光度尾部的SN II光度分布。
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 21.6I81428.4 mag. There is roughly 1 SN per deep (I814>26 mag), 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 of rich clusters: SNu in 0.18z0.37 clusters, and SNu in clusters at 0.83z1.27 (95 per cent confidence interval; 1 SNu≡1 SN century−1 per 1010 LB⊙). Combining the two redshift bins, the mean rate is 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 N1 SN with I81426 mag, and 1N3 SNe with I81427 mag. 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.