Mass and Light distributions in Clusters of Galaxies - Henry A ...
Mass and Light distributions in Clusters of Galaxies - Henry A ...
Mass and Light distributions in Clusters of Galaxies - Henry A ...
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Chapter 3<br />
Detailed Cluster <strong>Mass</strong> <strong>and</strong><br />
<strong>Light</strong> Pr<strong>of</strong>iles <strong>of</strong> A1703, A370<br />
& RXJ1347-11 from Deep<br />
Subaru Imag<strong>in</strong>g<br />
A version <strong>of</strong> this chapter has been published as Medez<strong>in</strong>ski, E., Broadhurst,<br />
T., Umetsu, K., Oguri, M., Rephaeli, Y., & Benítez, N. 2010, MNRAS, 405,<br />
257.<br />
3.1 Introduction<br />
Galaxy <strong>Clusters</strong> are the largest virialised objects whose properties reflect the<br />
<strong>in</strong>itial spectrum <strong>of</strong> density perturbations <strong>and</strong> the evolutionary history <strong>of</strong> dark<br />
matter (DM) <strong>and</strong> baryons. Wide rang<strong>in</strong>g observations provide a wealth <strong>of</strong><br />
<strong>in</strong>formation for exam<strong>in</strong><strong>in</strong>g the relation between dark <strong>and</strong> visible matter <strong>and</strong><br />
their radial pr<strong>of</strong>iles. Unlike galaxies, where substantial cool<strong>in</strong>g is predicted to<br />
have concentrated baryons <strong>in</strong> the centers <strong>of</strong> DM halos, clusters are observed<br />
to cool relatively <strong>in</strong>efficiently via thermal emission so that the gas rema<strong>in</strong>s<br />
close to the virial temperature, mak<strong>in</strong>g cluster mass pr<strong>of</strong>iles easy to <strong>in</strong>terpret,<br />
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