GAS STRIPPING IN SIMULATED GALAXIES WITH A MULTIPHASE INTERSTELLAR MEDIUM

By S. Tonnesen, Greg L. Bryan. 2009

150 citations recorded by the source corpus.

Cluster galaxies moving through the intracluster medium (ICM) are expected to lose some of their interstellar medium (ISM) through ISM–ICM interactions. We perform high-resolution (40 pc) three-dimensional hydrodynamical simulations of a galaxy undergoing ram pressure stripping, including radiative cooling, in order to investigate stripping of a multiphase medium. The clumpy, multiphase ISM is self-consistently produced by the inclusion of radiative cooling, and spans six orders of magnitude in gas density. We find no large variations in the amount of gas lost whether or not cooling is involved, although the gas in the multiphase galaxy is stripped more quickly and to a smaller radius. We also see significant differences in the morphology of the stripped disks. This occurs because the multiphase medium naturally includes high-density clouds set inside regions of lower density. We find that the lower density gas is stripped quickly from any radius of the galaxy, and the higher density gas can then be ablated. If high-density clouds survive, through interaction with the ICM, they lose enough angular momentum to drift toward the center of the galaxy where they are no longer stripped. Finally, we find that low ram pressure values compress gas into high-density clouds that could lead to enhanced star formation, while high ram pressure leads to a smaller amount of high-density gas.

View Paper: https://www.semanticscholar.org/paper/2e42aa3dc882518d40378e09761f53008de07e5d

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Citations in the corpus

• MORPHOLOGICAL QUENCHING OF STAR FORMATION: MAKING EARLY-TYPE GALAXIES RED (2009, background): “Such processes include (i) a cluster environment in which the cold gas is stripped and no cold gas can be found in the neighborhood (but see Tonnesen & Bryan 2009; Salome et al. 2008; Revaz et al. 2008), (ii) heating by virial shocks of gas infalling in a massive dark matter halo (Birnboim & Dekel…”
• The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies (2012, methodology): “This value is purely an approximation given that the stripping radius found in galaxy models varies depending on the model ingredients and are often around 11−15 kpc in a galaxy with semimajor axis of 25 kpc (Kronberger et al. 2008; Tonnesen & Bryan 2009).”
• Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “Idealized simulations of ram pressure stripping at high resolution that model a multiphase medium find that clumps with the density of molecular clouds are able to survive certain low-ram pressure circumstances and that lower density gas is stripped more easily (Tonnesen & Bryan 2009).”
• Cold gas stripping in satellite galaxies: from pairs to clusters (2016, background): “Until relatively recently, much of the success in this area came from non-cosmological, high-resolution simulations of well-resolved galaxies (e.g. Marcolini, Brighenti & D’Ercole 2003; Mayer et al. 2006, 2007; Bekki 2009; Tonnesen & Bryan 2009, 2010).”
• A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “…GALAXY CLASSIFICATION Vol. 00 Still, many authors argue that ram-pressure stripping is not the whole – or even the main – story, because it is difficult to strip dense central gas in giant galaxies (Farouki & Shapiro 1980; Abadi et al. 1999; Quilis et al. 2000; Tonnesen & Bryan 2009).”
• ISM properties in hydrodynamic galaxy simulations: turbulence cascades, cloud formation, role of gravity and feedback (2010, background): “Journal compilation C© 2010 RAS, MNRAS 409, 1088–1099 2009; see also Tonnesen & Bryan 2009 on the effect of ram pressure on a cloudy ISM).”
• BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “Recent simulations (see Roediger 2009, for a review) have further supported the idea that this happens via ram-pressure stripping and gravitational interactions (e.g. Vollmer et al. 2001; Vollmer 2003; Tonnesen & Bryan 2009; Kapferer et al. 2009).”
• The ATLAS3D project – IV. The molecular gas content of early-type galaxies (2011, background): “Tonnesen & Bryan (2009) also mention that the angular momentum transfer to the non-rotating cluster gas can gradually drive the remaining molecular gas towards the centre of its host galaxy.”