Ram pressure stripping of spiral galaxies in clusters

Abadi, Mario G.; Moore, Ben; Bower, Richard G.

doi:10.1046/j.1365-8711.1999.02715.x

Cited by 705 publications

(762 citation statements)

References 47 publications

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“…There is no accretion onto subhaloes or their descendents. This prescription models the physical phenomenon of strangulation through ram-pressure and tidal stripping (Gunn & Gott 1972;Abadi et al 1999;Peng et al 2015). It is also imposed because a halo may become a subhalo, evade detection by the halo finder as it passes through the centre of its host, reappear as a subhalo one or two timesteps later, and finally be identified as a halo again when it comes out on the other side ("backsplash haloes").…”

Section: Accretionmentioning

confidence: 99%

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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GalICS 2.0 is a new semianalytic code to model the formation and evolution of galaxies in a cosmological context. N-body simulations based on a Planck cosmology are used to construct halo merger trees, track subhaloes, compute spins and measure concentrations. The accretion of gas onto galaxies and the morphological evolution of galaxies are modelled with prescriptions derived from hydrodynamic simulations. Star formation and stellar feedback are described with phenomenological models (as in other semianalytic codes). GalICS 2.0 computes rotation speeds from the gravitational potential of the dark matter, the disc and the central bulge. As the rotation speed depends not only on the virial velocity but also on the ratio of baryons to dark matter within a galaxy, our calculation predicts a different Tully-Fisher relation from models in which v rot ∝ v vir . This is why GalICS 2.0 is able to reproduce the galaxy stellar mass function and the Tully-Fisher relation simultaneously. Our results are also in agreement with halo masses from weak lensing and satellite kinematics, gas fractions, the relation between star formation rate (SFR) and stellar mass, the evolution of the cosmic SFR density, bulge-to-disc ratios, disc sizes and the Faber-Jackson relation.

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Section: Accretionmentioning

confidence: 99%

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…With an isothermal SPH gas model, Abadi et al (1999) show that the HI gas is effectively stripped in the core of rich clusters, for disks oriented perpendicular to the wind. Galaxies can lose 80% of their gas, the final disk being restricted to 4kpc radius, in a time-scale of 10 7 yrs.…”

Section: Ram Pressure and Icm-ism Interactionsmentioning

confidence: 98%

Efficiency of Stripping Mechanisms

Combes

2004

Symp. - Int. Astron. Union

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Abstract. There are several physical processes to remove gas from galaxies in clusters, with subsequent starvation and star formation quenching: tidal interactions between galaxies, or tidal stripping from the cluster potential itself, interactions with the hot intra-cluster medium (ICM) through ram pressure, turbulent or viscous stripping, or also outflows from star formation of nuclear activity, We review the observational evidence for all processes, and numerical simulations of galaxies in clusters which support the respective mechanisms. This allows to compare their relative efficiencies, all along cluster formation.

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“…Once an infalling galaxy encounters the hot ICM, the cold gas may be removed by ram-pressure, and turbulent and viscous stripping (e.g. Schulz & Struck 2001;Abadi et al 1999), provided the ICM is sufficiently dense and the galaxy moves fast enough. Ram-pressure may also compress the cold gas clouds, triggering enhanced star formation.…”

Section: Physical Processesmentioning

confidence: 99%

Galaxy evolution in dense environments: a concise HI perspective

Verheijen¹

2004

IAU

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Abstract. Observing the neutral hydrogen in galaxy clusters provides crucial insights in the physical processes that influence the evolution of gas-rich galaxies as they migrate from the lower-density filaments through the cluster outskirts into to the higher-density central regions. The morphology-density relation, the Butcher-Oemler effect, and the observed HI deficiencies in the central regions of galaxy clusters suggest that infalling galaxies experience a strong transformation of their morphologies, star formation rates, and gas content. The physical mechanisms that trigger and govern these transformations may depend strongly on environment. This contribution aims to illustrate that the morphological and kinematic characteristics of the cold gas provide a sensitive tool to determine which mechanisms dominate in which environments. Motivation for observing the cold gasHydrogen is the most abundant primordial baryonic matter in the Universe out of which the visible galaxies and galaxy clusters have formed. Observations of the distribution and kinematics of cold neutral hydrogen at the epoch of galaxy formation, and during their subsequent evolution, provide one of the most direct windows on the physical processes involved. Numerous studies indicate that the pace of a galaxy's evolution, like its growth by mass accretion, the rate at which it forms stars, the frequency of tidal interactions and the occurrence of minor or major mergers, depends significantly on its local and global environment. In particular the environment encountered in the outskirts of galaxy clusters is very favorable to rapid evolution and transformation of galaxies as they fall in along the lower-density filaments into the higher-density cluster cores. Such infalling galaxies encounter an increased local galaxy density, which results in more frequent tidal interactions, and they may be confronted with a hot Intra-Cluster Medium (ICM) as they approach the cluster core. This change of environment can have a dramatic impact on a galaxy's morphology, its gas content and its star formation rate. This is also implied by the well-known morphology-density relation combined with the notion that clusters continue to accrete galaxies from the surrounding large scale structure in which they are embedded. Consequently, infalling galaxies must experience a significant transformation on a relatively short time scale, which is also suggested by the ButcherOemler effect and the interpretation that the blue galaxies in the outskirts of galaxy clusters experience a period of vigorous star formation which can end abruptly once all the cold gas is consumed or removed. These galaxies eventually find themselves in the cluster core as gas-poor systems with a passively evolving stellar population.The presence of cold gas in galaxies is a prerequisite for star formation, and the amount and distribution of cold gas regulates the duration and intensity of star formation periods. The removal of this cold gas reservoir from infalling galaxies is a crucial element in t...

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Ram pressure stripping of spiral galaxies in clusters

Cited by 705 publications

References 47 publications

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Efficiency of Stripping Mechanisms

Galaxy evolution in dense environments: a concise HI perspective

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