Ram pressure stripping of disc galaxies orbiting in clusters – I. Mass and radius of the remaining gas disc

By Elke Roediger, M. Brüggen. 2007

134 citations recorded by the source corpus.

We present the first 3D hydrodynamical simulations of ram pressure stripping of a disc galaxy orbiting in a galaxy cluster. Along the orbit, the ram pressure that this galaxy experiences varies with time. In this paper, we focus on the evolution of the radius and mass of the remaining gas disc, and compare it with the classical analytical estimate proposed by Gunn & Gott. We find that this simple estimate works well in predicting the evolution of the radius of the remaining gas disc. Only if the ram pressure increases faster than the stripping time-scale, the disc radius remains larger than predicted. However, orbits with such short ram pressure peaks are unlikely to occur in other than compact clusters. Unlike the radius evolution, the mass-loss history for the galaxy is not accurately described by the analytical estimate. Generally, in the simulations the galaxy loses its gas more slowly than predicted.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7f6248e329ef3a8683a2d313e9b8942c0f01bab3

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In Astronomy and Astrophysics

Citations in the corpus

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies (2009, methodology): “Further galaxy-scale numerical simulations for ram-pressure stripping were presented by Quilis et al. (2000), Mori & Burkert (2000), Toniazzo & Schindler (2001), Schulz & Struck (2001), and Roediger & Brüggen (2006, 2007).”
X-ray spectroscopy of the Virgo Cluster out to the virial radius (2011, unknown): “Recent simulations (e.g. Roediger & Brüggen 2007, 2008) show that galaxies can get stripped already at large radii with low ICM densities due to continuous or turbulent/viscous stripping (see Nulsen 1982).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “In fact ram-pressure stripping models indicate that HI can be fully depleted after a transit through the ICM’s core (Roediger & Brüggen 2007).”
GAS STRIPPING IN SIMULATED GALAXIES WITH A MULTIPHASE INTERSTELLAR MEDIUM (2009, methodology): “We will follow Roediger & Brüggen (2007) by naming the initial stage ram pressure pushing and the later stage continuous stripping.”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, background): “…star formation rates (and redder colours) of cluster spirals relative to their field counterparts (e.g., Abadi et al. 1999; Quilis et al. 2000; Vollmer et al. 2001; Okamoto & Nagashima 2003; Mayer et al. 2006; Roediger et al. 2006; Hester 2006; Jachym et al. 2007; Roediger & Brüggen 2006; 2007).”