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Extending the earlier measurements reported in Hitomi collaboration (2016,Nature, 535, 117), we examine the atmospheric gas motions within the central100~kpc of the Perseus cluster using observations obtained with the Hitomisatellite. After correcting for the point spread function of the telescope andusing optically thin emission lines, we find that the line-of-sight velocitydispersion of the hot gas is remarkably low and mostly uniform. The velocitydispersion reaches maxima of approximately 200~km~s$^{-1}$ toward the centralactive galactic nucleus (AGN) and toward the AGN inflated north-western `ghost'bubble. Elsewhere within the observed region, the velocity dispersion appearsconstant around 100~km~s$^{-1}$. We also detect a velocity gradient with a100~km~s$^{-1}$ amplitude across the cluster core, consistent with large-scalesloshing of the core gas. If the observed gas motions are isotropic, thekinetic pressure support is less than 10\% of the thermal pressure support inthe cluster core. The well-resolved optically thin emission lines have Gaussianshapes, indicating that the turbulent driving scale is likely below 100~kpc,which is consistent with the size of the AGN jet inflated bubbles. We alsoreport the first measurement of the ion temperature in the intracluster medium,which we find to be consistent with the electron temperature. In addition, wepresent a new measurement of the redshift to the brightest cluster galaxyNGC~1275.

Atmospheric gas dynamics in the Perseus cluster observed with Hitomi