VLA H<scp>i</scp>Observations of Gas Stripping in the Virgo Cluster Spiral NGC 4522

Kenney, Jeffrey D. P.; Gorkom, J. H. van; Vollmer, B.

doi:10.1086/420805

Cited by 340 publications

(474 citation statements)

References 70 publications

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“…A wide range of numerical simulations and observations demonstrate that ram pressure in clusters is sufficient to strip part of the gas from galaxies. The stellar disk, on the other hand, is not disturbed by the ICM, leaving galaxies with a truncated atomic gas (H i) disk (Chung et al 2008;Kronberger et al 2008;Boselli & Gavazzi 2006;Quilis et al 2000;Kenney et al 2004).…”

Section: Influence Of Environmentmentioning

confidence: 99%

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Bösch

Böhm

Wolf

et al. 2013

A&A

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Aims. We present spectroscopic observations of 182 disk galaxies (96 in the cluster and 86 in the field environment) in the region of the Abell 901/902 multiple cluster system, which is located at a redshift of z ∼ 0.165. We estimate dynamical parameters of the four subclusters and analyse the kinematics of spiral galaxies, searching for indications of ram-pressure stripping. Furthermore, we focus on dusty red galaxies as a possible intermediate stage in the transformation of field galaxies to lenticulars when falling into the cluster. Methods. We obtained multi-object slit spectroscopy using the VLT instrument VIMOS. We carried out a redshift analysis, determined velocity dispersions using biweight statistics, and detected possible substructures with the Dressler-Shectman test. We exploited rotation curves from emission lines to analyse distortions in the gaseous disk of a galaxy, as well as HST/ACS images to quantify the morphological distortions of the stellar disk. Results. The presence of substructures and non-Gaussian redshift distributions indicate that the cluster system is dynamically young and not in a virialised state. We find evidence of two important galaxy populations. Morphologically distorted galaxies are probably subject to increased tidal interactions. They show pronounced rotation-curve asymmetries at intermediate cluster-centric radii and low rest-frame peculiar velocities. Morphologically undistorted galaxies show the strongest rotation-curve asymmetries at high rest-frame velocities and low cluster-centric radii. Supposedly, this group is strongly affected by ram-pressure stripping due to interaction with the intra-cluster medium. Among the morphologically undistorted galaxies, dusty red galaxies have particularly strong rotation-curve asymmetries, suggesting that ram pressure is an important factor in these galaxies. Furthermore, dusty red galaxies have on average a bulge-to-total ratio that is higher by a factor of two than cluster blue-cloud and field galaxies. The fraction of kinematically distorted galaxies is 75% higher in the cluster than in the field environment. This difference mainly stems from morphologically undistorted galaxies, indicating a cluster-specific interaction process that only affects the gas kinematics but not the stellar morphology. Also the ratio between gas and stellar scale length is reduced for cluster galaxies compared to the field sample. Both findings could be explained best by ram-pressure effects. Conclusions. Ram-pressure stripping seems to be an important interaction process in the multiple cluster system A901/902. Dusty red galaxies might be a crucial element in understanding the transformation of field disk galaxies into cluster lenticular galaxies.

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Section: Influence Of Environmentmentioning

confidence: 99%

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Bösch

Böhm

Wolf

et al. 2013

A&A

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“…While good examples of ram pressure stripping are known among the Virgo spiral galaxies (e.g., Kenney et al 2004;Chung et al 2007Chung et al , 2009Abramson et al 2011), none of these galaxies is completely gas stripped and none has such a luminous UV tail, or linear parallel stellar streams, or fireballs as IC3418. There are already known examples of one-sided tails of young stars extending from more massive galaxies in more distant, richer clusters (Cortese et al 2007;Yoshida et al 2008;Smith et al 2010;Sun et al 2010;Woudt et al 2008), where the ram pressure can be 1 to 2 orders of magnitude stronger than in Virgo, but IC3418 is by far the closest such galaxy known.…”

Section: Introductionmentioning

confidence: 99%

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Jáchym¹,

Kenney²,

Růžička³

et al. 2013

A&A

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We present IRAM 30m sensitive upper limits on CO emission in the ram pressure stripped dwarf Virgo galaxy IC3418 and in a few positions covering H ii regions in its prominent 17 kpc UV/Hα gas-stripped tail. In the central few arcseconds of the galaxy, we report a possible marginal detection of about 1 × 10 6 M ⊙ of molecular gas (assuming a Galactic CO-to-H 2 conversion factor) that could correspond to a surviving nuclear gas reservoir. We estimate that there is less molecular gas in the main body of IC3418, by at least a factor of 20, than would be expected from the pre-quenching UV-based star formation rate assuming the typical gas depletion timescale of 2 Gyr. Given the lack of star formation in the main body, we think the H 2 -deficiency is real, although some of it may also arise from a higher CO-to-H 2 factor typical in low-metallicity, low-mass galaxies. The presence of H ii regions in the tail of IC3418 suggests that there must be some dense gas; however, only upper limits of < 1 × 10 6 M ⊙ were found in the three observed points in the outer tail. This yields an upper limit on the molecular gas content of the whole tail < 1 × 10 7 M ⊙ , which is an amount similar to the estimates from the observed star formation rate over the tail. We also present strong upper limits on the X-ray emission of the stripped gas in IC3418 from a new Chandra observation. The measured X-ray luminosity of the IC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxy in a more distant cluster with a prominent ram pressure stripped tail. Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to a low gas content in the tail associated with its advanced evolutionary state and/or due to a rather low thermal pressure of the surrounding intra-cluster medium.

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“…The spectacular example of N4522 in the Virgo cluster has been recently published by Kenney, van Gorkom & Vollmer (2004) and is reproduced in Figure 2. The small gas disk is clearly offset from the stellar disk and seems to be bend and swept away from the plane, interpreted to be the result of ram-pressure stripping.…”

Section: Some Phenomena Observed In Himentioning

confidence: 96%

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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VLA HiObservations of Gas Stripping in the Virgo Cluster Spiral NGC 4522

Cited by 340 publications

References 70 publications

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC 3418

Galaxy evolution in dense environments: a concise HI perspective

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