head 1.1; access; symbols; locks http:1.1; strict; comment @# @; expand @b@; 1.1 date 2005.03.24.11.24.51; author PaoloPadovani; state Exp; branches; next ; desc @none @ 1.1 log @none @ text @ࡱ> 02/ bjbj " lXXXX d>      $ l..pCppppppb rTx `^XN"\Y0jSpSp Proposed AVO SRM The Formation and Evolution of Galaxy Clusters Science Issues Clusters of galaxies are the largest entities in the Universe that are in gravitational equilibrium. Their formation and evolution hold keys to fundamental questions is cosmology, large scale structure formation, the formation and evolution of galaxies, the reionization of the Universe, and the origins of metallicities in the intergalactic medium. Clusters of galaxies and their intracluster media also act as crucial test beds for examining the evolution of AGNs and collimated outflows as well as for examining the details of galaxy encounters and galaxy stripping by dense gas. Some fundamental questions that could be addressed by a Science Reference Mission are: What is the necessary environment for the formation of rich clusters? Are they already in place when the first density fluctuations begin to appear? Or do they form at later epochs? Do clusters only occur at the intersections of cosmic filaments? Do clusters always form from subassemblies of small groups? Is there a distribution in the epoch of formation of clusters? Why? When does the ICM form? When does it first reach virial equilibrium? What is the origin of the ICM? What is the frequency of cluster-cluster interactions as a function of epoch? What is the role of AGN in the evolution of clusters? As a function of epoch? What is the role of AGN in the evolution of the ICM? When does the presence of dark matter first become significant in the evolution of clusters? How does the galaxy population in clusters evolve as a function of epoch? Some Strategies for implementation of an SRM A multiwavelength, multi-institutional approach will be the most effective in addressing this very large topic. In addition, extensive comparisons between large-scale databases and very detailed theoretical simulation datasets will be needed. X-ray data from all archives will be essential in looking for the first signatures of the ICM and its evolution, including its metallicity, as a function of redshift. Moreover, x-ray data may be of some use in characterizing AGN in clusters that are at lower redhshift. Radio data are invaluable in detecting the first onset of AGN activity out to large redshifts. The presence of AGN indicates that at least one galaxy has formed a massive central black hole at that epoch, and finding this at large redshift is extremely important. Moreover, the increasing awareness that radio sources may have a significant role in influencing the evolution of the ICM and perhaps other cluster features makes it imperative to have much more complete radio data. In addition, the superposition of radio, optical and x-ray data immediately gives a wealth of information about the AGN-ICM interaction. Hence image archives at these wavelengths, together with superposition tools such as Aladin will be essential. Optical and IR data archives will of course be central in determining redshifts, morphologies of clusters and galaxies as a function of redhshift, metallicities, emission line signatures, indicators of interactions, etc. Theoretical simulations are now able to address the entire range of physics involved, from the first formation of large scale structure through the dynamical interactions of galaxies and clusters, the evolution of the ICM, cluster mergers with ICM, the injection of energy and mass from AGN, galaxy stripping, etc. Hence extensive use of present and future theoretical simulation databases will be essential to the success of this SRM. 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