Non-hydrostatic Gas in the Core of the Relaxed Galaxy Cluster A1795

Chandra data on A1795 reveal a mild edge-like discontinuity in the gas density and temperature in the southern sector of the cluster at r = 60 h−1 kpc. The gas inside the edge is 1.3–1.5 times denser and cooler than outside, while the pressure is continuous, indicating that this is a “cold front”, the surface of contact between two moving gases. The continuity of the pressure indicates that the current relative velocity of the gases is near zero, making the edge appear to be in hydrostatic equilibrium. However, a total mass profile derived from the data in this sector under the equilibrium assumption, exhibits an unphysical jump by a factor of 2, with the mass inside the edge being lower. We propose that the cooler gas is “sloshing” in the cluster gravitational potential well and is now near the point of maximum displacement, where it has zero velocity but nonzero centripetal acceleration. The distribution of this non-hydrostatic gas should reflect the reduced gravity force in the accelerating reference frame, resulting in the apparent mass discontinuity. Assuming that the gas outside the edge is hydrostatic, the acceleration of the moving gas can be estimated from the mass jump, a ∼ 800 h km s−1 (108 yr)−1. The gravitational potential energy of this gas available for dissipation is about half of its current thermal energy. The length of the cool filament extending from the cD galaxy (Fabian et al.) may give the amplitude of the gas sloshing, 30 − 40 h−1 kpc. Such gas bulk motion might be caused by a disturbance of the central gravitational potential by past subcluster infall. Subject headings: Galaxies: clusters: individual (A1795) — intergalactic medium — X-rays: galaxies