Jeremy S. Sanders
Abstract
High-spectral resolution observations of clusters of galaxies are a powerful tool to understand the physical processes taking place in these massive objects. Their hot multi-million-degree X-ray emitting cluster atmospheres, containing most of the baryons in these systems, are enriched to around 1/3 of the solar metallicity. Therefore, cluster spectra host a variety of spectral lines, in particular, the Fe-L complex around 1 keV typically emitted from cooler systems and Fe-K at 6.7 keV seen from more massive clusters. The line ratios and continuum are sensitive probes of the temperature distribution of the gas, while the strength of lines compared to the continuum measures metallicity. With sufficient spectral resolution, the velocity structure can be obtained from line widths and shifts in position. Using detailed modelling, we can then understand better processes such as feedback from active galactic nuclei, mergers and enrichment, that are taking place in clusters.