Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters

By Ian G. McCarthy, Carlos S. Frenk, A. Font, C. Lacey, Richard G. Bower, N. L. Mitchell, M. Balogh, Tom Theuns Icc, Durham, Waterloo and 1 more. 2007

298 citations recorded by the source corpus.

We use a large suite of carefully controlled full hydrodynamic simulations to study the ram pressure stripping of the hot gaseous haloes of galaxies as they fall into massive groups and clusters. The sensitivity of the results to the orbit, total galaxy mass, and galaxy structural properties is explored. For typical structural and orbital parameters, we find that ∼30 per cent of the initial hot galactic halo gas can remain in place after 10 Gyr. We propose a physically simple analytic model that describes the stripping seen in the simulations remarkably well. The model is analogous to the original formulation of Gunn & Gott, except that it is appropriate for the case of a spherical (hot) gas distribution (as opposed to a face-on cold disc) and takes into account that stripping is not instantaneous but occurs on a characteristic time-scale. The model reproduces the results of the simulations to within ≈10 per cent at almost all times for all the orbits, mass ratios, and galaxy structural properties we have explored. The one exception involves unlikely systems where the orbit of the galaxy is highly non-radial and its mass exceeds about 10 per cent of the group or cluster into which it is falling (in which case the model underpredicts the stripping following pericentric passage). The proposed model has several interesting applications, including modelling the ram pressure stripping of both observed and cosmologically simulated galaxies and as a way to improve present semi-analytic models of galaxy formation. One immediate consequence is that the colours and morphologies of satellite galaxies in groups and clusters will differ significantly from those predicted with the standard assumption of complete stripping of the hot coronae.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3bbef028e928c1535a5596822d6fb50a052a10a5

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Citations in the corpus

The colours of satellite galaxies in groups and clusters (2008, methodology): “In the present study, we have improved the treatment of stripping by implementing the model of McCarthy et al. (2008) (which has been shown to match simulations of ram pressure stripping to high accuracy) into the GALFORM semi-analytic model for galaxy formation.”
Cold gas stripping in satellite galaxies: from pairs to clusters (2016, methodology): “…that neither implementation of GP14 used in this work accounts for ram-pressure stripping of the cold gas, a process known to dominate in larger haloes (i.e. galaxy clusters; Boselli et al. 2006; Tonnesen, Bryan & van Gorkom 2007; McCarthy et al. 2008; Chung et al. 2009; Cortese et al. 2010, 2011).”
THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, background): “…can be important as very weak ram pressure (2–3 orders of magnitude weaker than in cluster cores) can cause “strangulation” or “starvation” via stripping of the galaxy’s hot gas halo, thereby shutting off a potential fuel source for subsequent star formation (see McCarthy et al. 2008; Bekki 2009).”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “…predictions of starvation models, in which infalling galaxies are stripped of their diffuse gaseous halos as they pass through the ICM, preventing further gas accretion onto the galaxies from the surrounding inter-galactic medium (Larson et al. 1980; Bekki et al. 2002; McCarthy et al. 2008).”
Why does the environmental influence on group and cluster galaxies extend beyond the virial radius (2012, methodology): “…present (although a larger number is required before the z= 0 specific star formation rates converge, see Section 3 for further discussion), while McCarthy et al. (2008) have shown that t e stripping of hot gas is converged when there are a similar number of hot gas particles present initially.”
The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, background): “Detailed hydrodynamical simulations, however, indicate that the stripping of the hot gas is not instantaneous and may even not be complete after as much as 10 Gyr (e.g. Balsara, Livio & O’Dea 1994; Mori & Burkert 2000; Bekki, Couch & Shioya 2002; Kawata & Mulchaey 2008; McCarthy et al. 2008).”
The Sydney-AAO Multi-object Integral field spectrograph (2011, background): “Simulations suggest that this process can be efficient at removing halo gas, even in small and/or compact groups (Bekki 2009; McCarthy et al. 2008), but there is little direct experimental evidence that this is the case.”
Galaxy formation theory (2010, methodology): “This initial estimate has been revised and calibrated more accurately using numerical simulations (Abadi et al. 1999; McCarthy et al. 2008).”
Galaxy evolution in groups and clusters: star formation rates, red sequence fractions and the persistent bimodality (2011, background): “…as well as loss of existing extended hot gas via heating/evaporation, tidal stripping or ram-pressure stripping (Larson, Tinsley & Caldwell 1980; Balogh, Navarro & Morris 2000; Kawata & Mulchaey 2008; McCarthy et al. 2008), causing SFR in the disc to decline on a cold gas consumption time-scale.”
The dark side of galaxy colour (2013, background): “…2012, and references therein), “strangulation” (Larson et al. 1980; Diemand et al. 2007; Kawata & Mulchaey 2008), ram-pressure stripping (Gunn & Gott 1972; Abadi et al. 1999; McCarthy et al. 2008), “harassment” (Moore et al. 1998), and intra-host mergers (Makino & Hut 1997; Wetzel et al. 2009a,b).”
Substructures in hydrodynamical cluster simulations (2008, background): “The efficiency of gas stripping from substructures also depends strongly on cluster-centric distance (see Gunn & Gott 1972; McCarthy et al. 2008), hence we expect radial variations in the relative content of baryons in subhalos, which we analyse in this section.”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “…find that, if any stripping occurs, it often only does so in the central, most dense and high-pressure regions of massive halos (Weinmann et al. 2006a,b; Wang et al. 2007; Yang et al. 2009; Weinmann et al. 2009a; van den Bosch et al. 2008; Kang & van den Bosch 2008; McCarthy et al. 2008).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “McCarthy et al. (2008) found that for satellite galaxies with typical structural and orbital parameters, up to 30% of the initial hot halo gas can remain in place for up to 10 Gyr.”
Ultraviolet tails and trails in cluster galaxies: a sample of candidate gaseous stripping events in Coma (2010, background): “…to loss of stellar mass through tidal stripping, removal of cold gas from their disks by ram-pressure stripping (e.g. Gunn & Gott 1972; Quilis, Moore & Bower 2000), and stripping of hot gas from their halos by the same mechanism (e.g. Larson, Tinsley & Caldwell 1980; McCarthy et al. 2008).”
The environmental history of group and cluster galaxies in a Λ cold dark matter universe (2011, background): “In recent studies, a more gradual stripping of the hot gas reservoir has been assumed (Kang & van den Bosch 2008; Font et al. 2008; Weinmann et al. 2010; Guo et al. 2011), following results from numerical simulations (McCarthy et al. 2008, but see also Saro et al. 2010).”
The accretion of galaxies into groups and clusters (2009, background): “Journal compilation C© 2009 RAS, MNRAS 400, 937–950 Downloaded from https://academic.oup.com/mnras/article-abstract/400/2/937/1018927 by guest on 26 July 2018 of galaxies falling into more massive haloes is removed according to a prescription of McCarthy et al. (2008b).”
THE ERA OF STAR FORMATION IN GALAXY CLUSTERS (2013, background): “1 Gyr in high-redshift clusters) ram pressure stripping removes of order half of the cool gas from the galaxy disks (McCarthy et al. 2008).”