Relativistic Electrons & Magnetic Fields in Clusters of Galaxies

RXTE and BeppoSAX observations have yielded evidence for the presence of a secondary power-law spectral component in the spectra of several clusters of galaxies. This emission in clusters with extended regions of radio emission is likely to be by relativistic electrons that are Compton scattered by the CMB. The radio and non-thermal (NT) X-ray measurements yield the values of the volume-averaged magnetic field and electron energy density in the cluster extragalactic environment. These directly deduced quantities provide a tangible basis for the study of NT phenomena in clusters.Comment: 3 pages, 1 figure, to be published in proceedings of the 10th Marcel Grossmann meetin

The Sunyaev-Zeldovich Effect: Current Status and Future Prospects

The detailed spectral and spatial characteristics of the signature imprinted on the cosmic microwave background (CMB) radiation by Compton scattering of the radiation by electrons in the hot gas in clusters of galaxies - the Sunyaev-Zeldovich (S-Z) effect - are of great astrophysical and cosmological significance. In recent years observations of the effect have improved tremendously; high signal-to-noise images of the effect (at low microwave frequencies) can now be obtained by interferometric arrays. In the near future, high frequency measurements of the effect will be made with ground based and balloon-borne telescopes equipped with bolometeric arrays. Towards the end of the decade the PLANCK satellite will carry out an extensive S-Z survey over a wide frequency range. Along with the improved observational capabilities, the theoretical description of the effect, and its use as a precise cosmological probe, have been considerably advanced. In this review, I briefly discuss the nature and significance of the effect, its exact theoretical description, the current observational status, and prospects for the near future.Comment: Invited review, proceedings of the 9th Marcel Grossmann Meeting; 10 pages, 4 figure

Neutrino Mass from SZ Surveys

The expected sensitivity of cluster SZ number counts to neutrino mass in the sub-eV range is assessed. We find that from the ongoing {\it Planck}/SZ measurements the (total) neutrino mass can be determined at a (1-sigma) precision of 0.06 eV, if the mass is in the range 0.1-0.3 eV, and the survey detection limit is set at the 5-sigma significance level. The mass uncertainty is predicted to be lower by a factor ~2/3, if a similar survey is conducted by a cosmic-variance-limited experiment, a level comparable to that projected if CMB lensing extraction is accomplished with the same experiment. At present, the main uncertainty in modeling cluster statistical measures reflects the difficulty in determining the mass function at the high-mass end.Comment: 8 pages, Proceedings of the 13th Marcel Grossmann Meetin

High-energy emission from star-forming galaxies

Adopting the convection-diffusion model for energetic electron and proton propagation, and accounting for all the relevant hadronic and leptonic processes, the steady-state energy distributions of these particles in the starburst galaxies M82 and NGC253 can be determined with a detailed numerical treatment. The electron distribution is directly normalized by the measured synchrotron radio emission from the central starburst region; a commonly expected theoretical relation is then used to normalize the proton spectrum in this region, and a radial profile is assumed for the magnetic field. The resulting radiative yields of electrons and protons are calculated: the predicted >100MeV and >100GeV fluxes are in agreement with the corresponding quantities measured with the orbiting Fermi telescope and the ground-based VERITAS and HESS Cherenkov telescopes. The cosmic-ray energy densities in central regions of starburst galaxies, as inferred from the radio and gamma-ray measurements of (respectively) non-thermal synchrotron and neutral-pion-decay emission, are U=O(100) eV/cm3, i.e. at least an order of magnitude larger than near the Galactic center and in other non-very-actively star-forming galaxies. These very different energy density levels reflect a similar disparity in the respective supernova rates in the two environments. A L(gamma) ~ SFR^(1.4) relationship is then predicted, in agreement with preliminary observational evidence.Comment: Invited talk at SciNeGHE2010 (8th Wotkshop on Science with the New Generation of High Energy Gamma-ray Experiments): Gamma-ray Astrophysics in the Multimessenger Context (Trieste, Sept.8-10, 2010

Evolution of the gas mass fraction in galaxy clusters

The mass fraction of hot gas in clusters is a basic quantity whose level and dependence on the cluster mass and redshift are intimately linked to all cluster X-ray and SZ measures. Modeling the evolution of the gas fraction is clearly a necessary ingredient in the description of the hierarchical growth of clusters through mergers of subclumps and mass accretion on the one hand, and the dispersal of gas from the cluster galaxies by tidal interactions, galactic winds, and ram pressure stripping on the other hand. A reasonably complete description of this evolution can only be given by very detailed hydrodynamical simulations, which are, however, resource-intensive, and difficult to implement in the mapping of parameter space. A much more practical approach is the use of semi-analytic modeling that can be easily implemented to explore a wide range of parameters. We present first results from a simple model that describes the build up of the gas mass fraction in clusters by following the overall impact of the above processes during the merger and accretion history of each cluster in the ensemble. Acceptable ranges for model parameters are deduced through comparison with results of X-ray observations. Basic implications of our work for modeling cluster statistical properties, and the use of these properties in joint cosmological data analyses, are discussed.Comment: 10 pages, 6 figures, updated to match MNRAS accepted versio