Conference

The XMM Cluster Survey (XCS) is a serendipitous galaxy cluster survey being conducted using publicly available X-ray data from the XMM-Newton Science Archive. One of the primary aims of the XCS is to determine the form of the evolution of the cluster gas - knowledge of which is crucial for the use of X- ray or SZ selected clusters in constraining cosmological parameters - through measuring the X-ray scaling relations using a large, well characterised cluster sample spanning ~7 Gyr in lookback time. I will present an update on the status of the survey, discuss the expected cosmological constraints, and briefly describe some recent results from galaxy evolution studies conducted under the umbrella of the XCS project.

We build simple, 'top-down', models for the gas density and temperature profiles for clusters of galaxies based on current high precision XRay observations so as to 'exactly' satisfy observed XRay scaling relation between temperature and mass. The gas is assumed to be in hydrostatic equilibrium along with a component of non-thermal pressure due to dispersion and the gas fraction reaches universal value only at or beyond the virial radius. For these models, we calculate the Sunyaev-Zel'dovich Effect (SZE) scaling relations. We show that all the predicted SZE scaling relations between the integrated SZE flux and the gas temperature, the gas mass, the total mass, as well as, the gas fraction are in excellent agreement with recent SZE observations by Bonamente etal (2008). The consistency between the global properties of clusters detected in X-Ray's and in SZE hints that we are looking at the same population of clusters as a whole. Implications for SZE power spectrum, SZE flux-M200 scaling relation and number counts are discussed

"Taking gravitational potential wells from a dark matter simulation, and assuming a polytropic equation of state and hydrostatic equilibrium, one can predict the state of the hot gas in clusters of galaxies. With reasonable values for star formation efficiency, energy input, and nonthermal pressure support, these model clusters can reproduce observed X-ray trends of gas temperature and gas mass fraction with cluster mass, as well as observed entropy and pressure profiles. Normalizing to X-ray observations is a vital step in using such models to predict the SZ signal. "

The observed thermal properties of the ICM shows much greater dispersion than expected if the gas was subject only to shock-heating by mergers and during infall. This diversity can be best understood as a byproduct of AGN feedback occurring in galaxies destined to become cluster members, both before and after cluster formation. Theoretical considerations suggest that the level of preheating ought to vary from one proto-cluster region to another. The entropy profiles of roughly 50% of the clusters with long central cooling times require that the gas be "preheated" to high entropy. Gas density profiles in such systems form hot central cores. Clusters with gas that isn't preheated to sufficiently high values forms peaked density profiles. I will show how variable preheating explain the various observed X-ray/X-ray correlations and discuss some of its implications for SZ studies. I will also present optical results that shed new light on the fate of the cold gas in cooling-unstable clusters, and propose observations tests of the "AGN preheating" aspect of the picture.

Scaling relations among galaxy cluster observables, which will become available in large future samples of galaxy clusters, could be used to constrain not only cluster structure,but also cosmology. I will discuss the utility of this approach, employing a physically motivated parametric model to describe cluster structure, and applying it to the expected relation between the Sunyaev-Zel’dovich decrement (S_{\nu}) and the emission–weighted X–ray temperature (Tew). With a suitable choice of fiducial parameter values, the cluster model satisfies several existing observational constraints. A Fisher matrix is employed to estimate the joint errors on cosmological and cluster structure parameters from a measurement of S_{\nu} vs. Tew in a future survey. I will also compare the cosmology constraints from the scaling relation to those expected from the number counts (dN/dz) of the same clusters.

The growing fascination with unconventional pairing is driven in part by continuing discoveries of exotic superconductors. The first of these, superfluid 3He, was found by Osheroff, Richardson, and Lee in 1971. This was followed soon thereafter by superconductivity in the heavy fermion compound, UPt3. And then an explosion of interest accompanied the observation of superconductivity in cuprates, Sr2RuO4, and organic materials. The newest discoveries are sperconducting compounds of FeAs. These systems have been demonstrated (or in some cases it is just suspected) that they have pairing condensates with non-zero angular momentum, L= 1, 2, and even 3. But all of them have the common hallmark of a high degree of sensitivity to impurities. In this talk I will discuss impurity effects in the best known of these unconventionally paired systems, 3He, a paradigm for the other unconventional superconductors. Impurity scattering is deftly controlled in superfluid 3He by imbibing it into high porosity silica aerogel. We can understand the suppression of its superfluid state (the transition temperature), the effect on its order parameter (the pairing energy), the appearance of quasiparticle bound states (gaplessness), and possibly new phases, in the context of current theory. I will discuss experiments from many laboratories and their theoretical interpretation leading to the topical question of the day, “Can anisotropic scattering stabilize new anisotropic states?”