Summary: Clusters of Galaxies and the High Redshift Universe Observed in X-Rays

By S. Borgani. 2001

269 citations recorded by the source corpus.

This Meeting featured the recent advancements in our understanding of galaxy clusters and the distant Universe, achieved by the past and new generation of X-ray satellites. I summarize here the main themes that have been discussed: (a) Clusters of galaxies as probes of cosmological models; (b) The physics of cosmic baryons trapped within the potential wells of galaxy clusters; (c) The origin of the cosmic X-ray background and the nature of the contributing sources.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1781de59b8bf966aeca85df78126cc2228b6e632

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Citations in the corpus

The Distribution of Metallicity in the Intergalactic Medium at z ~ 2.5: O VI and C IV Absorption in the Spectra of Seven QSOs (2003, background): “The models match observations of the UV and hard X-ray backgrounds at low redshift, within errors (Haardt & Madau 2001).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “Photoheating and cooling are implemented as described in Wiersma et al. (2009a), including contributions from 11 elements in the presence of a spatially uniform, time evolving UV background of the form calculated by Haardt & Madau (2001).”
The case for AGN feedback in galaxy groups (2009, methodology): “…within pre-computed tables (generated with CLOUDY) that contain cooling rates as a function of density, temperature, and redshift calculated in the presence of the cosmic microwave background and photoionisation from a Haardt & Madau (2001) ionising UV/X-Ray background (see Wiersma et al. 2009a).”
On the evolution of the H i column density distribution in cosmological simulations (2012, methodology): “…ionization rates and the small-scale structure of the absorbers, has been found to have no significant impact on the simulated HI CDDF (Pontzen et al. 2008; McQuinn & Switzer 2010; Altay et al. 2011). c© 0000 RAS, MNRAS 000, 000–000 on Haardt & Madau (2001) together with Haardt & Madau (2012).”