Infall time estimation from projected radius and line-of-sight velocity is capped at roughly 2.5 Gyr by orbital overlap, making a simple linear partition as accurate as any method.
Measuring the mass profile of galaxy clusters beyond their virial radius
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abstract
Traditional estimators of the mass of galaxy clusters assume that the cluster components (galaxies, intracluster medium, and dark matter) are in dynamical equilibrium. Two additional estimators, that do not require this assumption, were proposed in the 1990s: gravitational lensing and the caustic technique. With these methods, we can measure the cluster mass within radii much larger than the virial radius. In the caustic technique, the mass measurement is only based on the celestial coordinates and redshifts of the galaxies in the cluster field of view; therefore, unlike lensing, it can be, in principle, applied to clusters at any redshift. Here, we review the origin, the basics and the performance of the caustic method.
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Estimating infall times of galaxies around clusters: how accurately can it be done with observational data?
Infall time estimation from projected radius and line-of-sight velocity is capped at roughly 2.5 Gyr by orbital overlap, making a simple linear partition as accurate as any method.