Study of the resonant scattering in the Perseus cluster core with ASTRO-H SXS

Resonance lines from cores of galaxy clusters have significant optical depth, as predicted by Gilfanov, Sunyaev & Churazov (1987). We can constrain turbulence velocity from the level of suppression of the resonance lines, providing a good measure of dynamical condition of gas. The Soft X-ray Spectrometer (SXS) onboard ASTRO-H is a high-resolution spectrometer and capable of separating resonance lines from other line components. It is important to estimate the flux contamination due to the point spread function (PSF) of the X-ray telescope ~1.5’. Zhuravleva et al. (2013) constructed spectral models for the Perseus cluster which took into account modifications of line fluxes and shapes due to the resonant scattering effect as well as by radial variations of density, temperature and abundances of heavy elements. Line broadening by small-scale motions were also included. We performed simulation of these models by taking into account the pixel layout of SXS and PSF effect. The suppression of resonance line from H-like Fe will enable us to constrain gas velocities below 300 km/sec.