Resonant scattering in the Perseus Cluster: spectral model for constraining gas motions with Astro-H

X-ray spectra from cores of galaxy clusters can be strongly distorted by resonant scattering of line photons, aecting metal abundance and gas velocity measurements. We introduce simulated spectral models that take into account the resonant scattering eect, radial variations of thermodynamic properties of the hot gas, projection eects and small-scale isotropic gas motions. The key feature of the models is that all these eects are treated self-consistently for the whole spectrum, rather than for individual lines. The model spectra are publicly available and can be used for direct comparison with observed projected spectra. Comparison with the existing XMM-Newton and Chandra data of the Perseus Cluster shows that even though there is no strong evidence for the resonant scattering in Perseus, the low energy resolution of the X-ray CCDs is not sucient to robustly distinguish spectral distortions due to the resonant scattering, dierent metal abundance proles and dierent levels of gas turbulence. Future AstroH data will resolve most of the problems we are facing with CCDs. With the help of our models, the resonant scattering analysis can be done self-consistently using the whole spectral information, constraining the level of gas turbulence already with a 100 ks observation with Astro-H.