Titlebook: Soft X-Ray Emission from Clusters of Galaxies and Related Phenomena; Richard Lieu,Jonathan Mittaz Conference proceedings 2004 Springer Sci

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The Ism from the Soft X-ray Background Perspective been seen as it has been about detections. High resolution spectra of the local SXRB have been observed, but are inconsistent with current thermal emission models. An excess over the extrapolation of the high-energy (most clearly visible at . 1.5 keV) extragalactic power law down to ¾ keV has been

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Soft X-Ray Excess Emission in Three Clusters of Galaxies Observed with XMM-Newtona large fraction of the current epoch’s bayons located in a warm-hot intergalactic medium (WHIM). However, the derived densities are too high in the cluster cores, compared to WHIM simulations, and thus more theoretical work is needed to fully understand the origin of the observed soft X-ray excess.

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The Fuse Survey of High Velocity O VI in the Vicinity of the Milky Wayous galaxy formation scenarios. Additional spectroscopic data in the coming years will help to determine the ionization properties of the high velocity clouds and discriminate between the multiple types of high velocity O VI features found in this study.

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The Cluster Abell 85 and its X-ray Filament Revisited by Chandra and XMM-NewtonV. This is significantly lower than the ambient cluster medium, but is significantly higher than anticipated for a gas in a weakly bound extended filament. It is not clear whether this is a filament of diffuse emission or a chain of several groups of galaxies.

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0067-0057 the recent launch of new missions such as XMM-Newton and FUSE, we are beginning to answer some of the complex issues regarding the phenomenon. This conference proceedings is an attempt to bring together the latest research results and covers both observational and theoretical work on the CSE and rel

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Hard X-Ray Excesses in Clusters of Galaxies and Their Non-Thermal OriginThe first part of the paper reports all the results obtained by . observations concerning the search for non-thermal components in the spectra of clusters of galaxies, while the origin of the hard X-ray excesses detected in Coma, A2256 and, at lower confidence level, in A754 is discussed in the second part.