A simulation-calibrated power law between intracluster light and total mass is used to estimate cluster mass profiles; it works for deep Euclid data of Perseus but fails on shallower Hubble Frontier Fields clusters.
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The intracluster light as an estimator of the cluster mass profile
A simulation-calibrated power law between intracluster light and total mass is used to estimate cluster mass profiles; it works for deep Euclid data of Perseus but fails on shallower Hubble Frontier Fields clusters.