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

Röediger, E.; Brüggen, M.

doi:10.1111/j.1365-2966.2007.12241.x

Cited by 168 publications

(176 citation statements)

References 25 publications

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“…Boselli et al 2008a,b), or making spirals gas deficient (e.g. Abadi et al 1999;Roediger & Brüggen 2007), with stellar populations in agreement with observations ).…”

Section: Introductionsupporting

confidence: 53%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boissier

Boselli

Duc

et al. 2012

A&A

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Context. Several galaxies in the Virgo cluster are known to have large H i gas tails related to a recent ram-pressure stripping event. The Virgo cluster has been extensively observed at 1539 Å in the far-ultraviolet for the GALEX Ultraviolet Virgo Cluster Survey (GUViCS), and in the optical for the Next Generation Virgo Survey (NGVS), allowing a study of the stellar emission potentially associated with the gas tails of 8 cluster members. On the theoretical side, models of ram-pressure stripping events have started to include the physics of star formation. Aims. We aim to provide quantitative constraints on the amount of star formation taking place in the ram-pressure stripped gas, mainly on the basis of the far-UV emission found in the GUViCS images in relation with the gas content of the tails. Methods. We have performed three comparisons of the young stars emission with the gas column density: visual, pixel-by-pixel, and global. We have compared our results to other observational and theoretical studies. Results. We find that the level of star formation taking place in the gas stripped from galaxies by ram-pressure is low with respect to the available amount of gas. Star formation is lower by at least a factor 10 compared to the predictions of the Schmidt Law as determined in regular spiral galaxy disks. It is also lower than measured in dwarfs galaxies and the outer regions of spirals, and than predicted by some numerical simulations. We provide constraints on the star formation efficiency in the ram-pressure stripped gas tails, and compare these with current models.

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“…Boselli et al 2008a,b), or making spirals gas deficient (e.g. Abadi et al 1999;Roediger & Brüggen 2007), with stellar populations in agreement with observations ).…”

Section: Introductionsupporting

confidence: 53%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boissier

Boselli

Duc

et al. 2012

A&A

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“…To answer this question we first compare the gas depletion timescales determined in this work to other representative timescales for the evolution of galaxies in clusters. The typical crossing of a cluster such as Virgo is ∼1.7 Gyr (Boselli & Gavazzi 2006), while the timescale necessary to strip gas from a galaxy via ram pressure is of the order of ∼100−200 Myr (Vollmer et al 2004(Vollmer et al , 2008a(Vollmer et al , 2009(Vollmer et al , 2012aRoediger & Bruggen 2007;Crowl & Kenney 2008). This stripping process only removes a fraction of the total gas from massive objects, while it has dramatic effects in dwarfs, where the star formation process is completely stopped (Boselli et al 2008a).…”

Section: Implications On the Star Formation History Of Cluster Galaxiesmentioning

confidence: 99%

“…The simulations of Tonnesen et al (2007) done using a single phase component of the ISM show that the gas is totally removed on timescales ≥1 Gyr. Timescales of the order of 1.5 Gyr are also obtained using 3D hydrodynamical simulations by Roediger & Bruggen (2007) for a substantial reduction of the total gas content of the perturbed galaxy via ram pressure. These hydrodynamical simulations based on a single and homogeneous gas phase for the ISM, however, generally underestimate the efficiency of ram pressure stripping (Tonnesen & Bryan 2009).…”

Section: Implications On the Star Formation History Of Cluster Galaxiesmentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

et al. 2014

A&A

177

250

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The Herschel Reference Survey is a complete volume-limited, K-band-selected sample of nearby objects including Virgo cluster and isolated objects. Using a recent compilation of Hi and CO data for this sample we study the effects of the cluster environment on the molecular gas content of spiral galaxies. With the subsample of unperturbed field galaxies, we first identify the stellar mass as the scaling variable that traces the total molecular gas mass of galaxies better. We show that, on average, Hi-deficient galaxies are significantly offset (4σ) from the M(H 2 ) vs. M star relation for Hi-normal galaxies. We use the M(H 2 ) vs. M star scaling relation to define the H 2 -deficiency parameter as the difference, on logarithmic scale, between the expected and observed molecular gas mass for a galaxy of given stellar mass. The H 2 -deficiency parameter shows a weak and scattered relation with the Hi-deficiency parameter, here taken as a proxy for galaxy interactions with the surrounding cluster environment. We also show that, as for the atomic gas, the extent of the molecular disc decreases with increasing Hi-deficiency. All together, these results show that cluster galaxies have, on average, a lower molecular gas content than similar objects in the field. Our analysis indicates that ram pressure stripping is the physical process responsible for this molecular gas deficiency. The slope of the H 2 − de f vs. Hi − de f relation is less than unity, while the D(Hi)/D(i) vs. Hi − de f relation is steeper than the D(CO)/D(i) vs. Hi − de f relation, thereby indicating that the molecular gas is removed less efficiently than the atomic gas. This result can be understood if the atomic gas is distributed on a relatively flat disc that is more extended than the stellar disc. It is thus less anchored to the gravitational potential well of the galaxy than the molecular gas phase, which is distributed on an exponential disc with a scalelength r CO 0.2r 24.5 (g). There is a clear trend between the NUV-i colour index, which is a proxy for the specific star formation activity, and the H 2 -deficiency parameter, which suggests that molecular gas removal quenches the activity of star formation. This causes galaxies migrate from the blue cloud to the green valley and, eventually, to the red sequence. The total gas-consumption timescale of gas deficient cluster galaxies is comparable to that of isolated, unperturbed systems. The total gas depletion timescale determined by considering the recycled fraction is τ gas,R 3.0−3.3 Gyr, which is significantly larger than the typical timescale for total gas removal in a ram pressure stripping process, indicated by recent hydrodynamical simulations to be τ RP 1.5 Gyr. The comparison of these timescales suggests that ram pressure, rather than a simple stop of the infall of pristine gas from the halo, will be the dominant process driving the future evolution of these cluster galaxies.

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“…When the ram-pressure is greater than the anchoring force of the galaxy, the diffuse ISM will be stripped ( Jaffé et al 2015). Some models predict that Hi can be fully depleted after a single transit through the ICM's core (Roediger & Brüggen 2007). It is also possible that only the diffuse hot halo gas can be ram-pressure stripped or thermally evaporated (Bekki, Couch & Shioya 2002).…”

Section: Introductionmentioning

confidence: 99%

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

Jaffé

Verheijen

Haines

et al. 2016

Mon. Not. R. Astron. Soc.

114

111

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In a hierarchical Universe clusters grow via the accretion of galaxies from the field, groups and even other clusters. As this happens, galaxies can lose their gas reservoirs via different mechanisms, eventually quenching their star formation. We explore the diverse environmental histories of galaxies through a multiwavelength study of the combined effect of ram-pressure stripping and group 'processing' in Abell 963, a massive growing cluster at z = 0.2 from the Blind Ultra Deep Hi Environmental Survey (BUDHIES). We incorporate hundreds of new optical redshifts (giving a total of 566 cluster members), as well as Subaru and XMM-Newton data from LoCuSS, to identify substructures and evaluate galaxy morphology, star formation activity, and Hi content (via Hi deficiencies and stacking) out to 3×R 200 . We find that Abell 963 is being fed by at least seven groups, that contribute to the large number of passive galaxies outside the cluster core. More massive groups have a higher fraction of passive and Hi -poor galaxies, while low-mass groups host younger (often interacting) galaxies. For cluster galaxies not associated with groups we corroborate our previous finding that Hi gas (if any) is significantly stripped via ram-pressure during their first passage through the intracluster medium, and find mild evidence for a starburst associated with this event. In addition, we find an overabundance of morphologically peculiar and/or star-forming galaxies near the cluster core. We speculate that these arise as groups pass through the cluster (post-processing). Our study highlights the importance of environmental quenching and the complexity added by evolving environments.

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

Cited by 168 publications

References 25 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Cold gas properties of theHerschelReference Survey

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

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