Ram pressure stripping of disc galaxies orbiting in clusters. II. Galactic wakes
E. Roediger, M. Brueggen (Jacobs University Bremen)

TL;DR
This study uses 3D hydrodynamical simulations to analyze the properties of gas tails formed by ram pressure stripping of disc galaxies in clusters, revealing dependencies on galaxy mass loss and orbital parameters.
Contribution
It provides detailed insights into the morphology, turbulence, and local deposition of stripped gas, and compares simulation results with observations, highlighting the need for additional physics.
Findings
Galactic wakes exhibit flaring width dependent on gas disc orientation.
Stripped gas tails can extend up to 40 kpc at certain sensitivities.
Simulated tails match some observed HI tails but differ in velocity width.
Abstract
We present 3D hydrodynamical simulations of ram pressure stripping of a disc galaxy orbiting in a galaxy cluster. In this paper, we focus on the properties of the galaxies' tails of stripped gas. The galactic wakes show a flaring width, where the flaring angle depends on the gas disc's cross-section with respect to the galaxy's direction of motion. The velocity in the wakes shows a significant turbulent component of a few 100 km/s. The stripped gas is deposited in the cluster rather locally, i.e. within ~150 kpc from where it was stripped. We demonstrate that the most important quantity governing the tail density, length and gas mass distribution along the orbit is the galaxy's mass loss per orbital length. This in turn depends on the ram pressure as well as the galaxy's orbital velocity. For a sensitivity limit of ~10^19 cm^-2 in projected gas density, we find typical tail lengths of…
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