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| * |
The first imaging
observations of
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clusters of
galaxies with Einstein
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confirmed
predictions that the cooling
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time of gas at
the core of the
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intracluster
media of many clusters
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should be less
than the Hubble time,
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requiring the
presence of a cooling
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flow.
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| * |
One expected the
presence of copious
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soft X-ray line
emission from these
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cluster cores,
incompatible with the
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background
temperature of the cluster.
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| * |
Canizares et al.
detected O K-shell and
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Fe L-shell line
emission, indicative of a
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range of
temperatures, with the FPCS
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for M87 in the
Virgo cluster.
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