Ram pressure stripping of the multiphase ISM and star formation in the Virgo spiral galaxy NGC 4330

Vollmer, B.; Soida, M.; Braine, J.; Abramson, Anne; Beck, Rainer; Chung, Aeree; Crowl, Hugh H.; Kenney, Jeffrey D. P.; Gorkom, J. H. van

doi:10.1051/0004-6361/201117680

Cited by 68 publications

(81 citation statements)

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“…14-24 and references therein). Recent detailed observations of ongoing gas depletion from galaxies in clusters are presented by the Very Large Array survey of neutral hydrogen (HI) in Virgo galaxies showing long tails of stripped gas behind galaxies, where the gas clumps in the tails are accelerated by ram pressure, leaving behind streams of new stars (22,24). Long tails of HI and ionized gas are observed in galaxies in several nearby clusters, consistent with the description given here (e.g., refs.…”

supporting

confidence: 85%

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Gas loss in simulated galaxies as they fall into clusters

Cen

Pop

Bahcall

2014

Proc. Natl. Acad. Sci. U.S.A.

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We use high-resolution cosmological hydrodynamic galaxy formation simulations to gain insights into how galaxies lose their cold gas at low redshift as they migrate from the field to the highdensity regions of clusters of galaxies. We find that beyond three cluster virial radii, the fraction of gas-rich galaxies is constant, representing the field. Within three cluster-centric radii, the fraction of gas-rich galaxies declines steadily with decreasing radius, reaching <10% near the cluster center. Our results suggest galaxies start to feel the effect of the cluster environment on their gas content well beyond the cluster virial radius. We show that almost all gas-rich galaxies at the cluster virial radius are falling in for the first time at nearly radial orbits. Furthermore, we find that almost no galaxy moving outward at the cluster virial radius is gas-rich (with a gas-to-baryon ratio greater than 1%). These results suggest that galaxies that fall into clusters lose their cold gas within a single radial round-trip.cosmology | observations | large-scale structure of universe | intergalactic medium I t has long been known that the local environment affects galaxy properties. Earlier work (1)(2)(3)(4) showed that the fraction of early-type galaxies increases dramatically toward the central regions of clusters of galaxies, whereas the less-dense regions of the field are dominated by spiral galaxies. Similarly, the "color-density relation" (5-8) indicates that red, old galaxies are found preferentially in overdense environments, and galaxies with bluer, younger stellar populations are more common in the field. This color bimodality is linked to a transition in star formation rates between the low-density field and the high-density regions inside clusters (4, 9). However, we still do not have a complete picture of the process through which blue, late-type, star-forming galaxies in the field transform into red, early-type galaxies when entering a cluster. We know that cold gas in galaxies is spatially extended and often distributed far beyond the optical disks (10). Cosmologically, some of the cold gas that feeds galaxy formation may come from the intergalactic medium (11,12). Observations suggest that neutral hydrogen feeds galaxies and turns into molecular hydrogen at a high column density of ∼10 22 cm −2 (13), within which star formation is observed to occur. Together, these facts suggest that the amount of neutral hydrogen supply may ultimately set the rate of star formation. The environmental dependence of galaxy properties may thus be related to the availability of cold gas in or around galaxies. This expectation is supported by observations of galaxies in different environments, showing the well-known depletion of both cold gas and star formation toward the high-density central regions of clusters; this is likely caused by ram pressure stripping of the cold gas by the hot intracluster medium (plus additional gravitational interactions) in the dense environments (refs. 14-24 and references therein). Recent deta...

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supporting

confidence: 85%

“…Long tails of HI and ionized gas are observed in galaxies in several nearby clusters, consistent with the description given here (e.g., refs. 21,22,[25][26][27].…”

mentioning

confidence: 99%

Gas loss in simulated galaxies as they fall into clusters

Cen

Pop

Bahcall

2014

Proc. Natl. Acad. Sci. U.S.A.

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“…The timestep of interest (26 Myr) is marked by "model". (Vollmer et al 2008b) and NGC 4330 (Vollmer et al 2012a): we assume that the molecular fraction depends linearly on the square root of the gas density f mol = M mol /M tot = ρ/(0.03 M pc −3 ) and the molecular fraction cannot exceed unity. A detailed motivation for this prescription is given in Vollmer et al (2008b).…”

Section: Gas Distributionmentioning

confidence: 99%

“…To calculate the large-scale regular magnetic field for our simulations, we apply the same procedure as Otmianowska-Mazur & Vollmer (2003) and Vollmer et al (2012a). We solve the induction equation:…”

Section: Modelmentioning

confidence: 99%

A dynamical model for the Taffy galaxies UGC 12914/5

Vollmer¹,

Braine²,

Soida³

2012

A&A

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The spectacular head-on collision of the two gas-rich galaxies of the Taffy system, UGC 12914/15, gives us a unique opportunity to study the consequences of a direct ISM-ISM collision. To interpret existing multi-wavelength observations, we made dynamical simulations of the Taffy system including a sticky particle component. To compare simulation snapshots to Hi and CO observations, we assume that the molecular fraction of the gas depends on the square root of the gas volume density. For the comparison of our simulations with observations of polarized radio continuum emission, we calculated the evolution of the 3D large-scale magnetic field for our simulations. The induction equations including the time-dependent gas-velocity fields from the dynamical model were solved for this purpose. Our simulations reproduce the stellar distribution of the primary galaxy, UGC 12914, the prominent Hi and CO gas bridge, the offset between the CO and Hi emission in the bridge, the bridge isovelocity vectors parallel to the bridge, the Hi double-line profiles in the bridge region, the large line-widths (∼200 km s −1 ) in the bridge region, the high field strength of the bridge large-scale regular magnetic field, the projected magnetic field vectors parallel to the bridge and the strong total power radio continuum emission from the bridge. The stellar distribution of the secondary model galaxy is more perturbed than observed. The observed distortion of the Hi envelope of the Taffy system is not reproduced by our simulations which use initially symmetric gas disks. The model allows us to define the bridge region in three dimensions. We estimate the total bridge gas mass (Hi, warm and cold H 2 ) to be 5 to 6× 10 9 M , with a molecular fraction M H 2 /M HI of about unity. Despite the enormous mass of molecular gas in the bridge, very little star formation is present, similar to other systems with extraplanar gas and broad CO lines. The structure of the model gas bridge is bimodal: on kpc-scales there is a dense ( 0.01 M pc −3 ) component with a high velocity dispersion >100 km s −1 and a less dense (∼10 −3 M pc −3 ) component with a smaller, but still high, velocity dispersion ∼50 km s −1 . The synchrotron lifetime of relativistic electrons is only long enough to be consistent with the existence of the radio continuum bridge for the less dense component. On the other hand, only the high-density gas undergoes a high enough mechanical energy input to produce the observed strong emission of warm H 2 . We propose that, despite the high local gas densities, this high input of mechanical energy drives strong turbulence and quenches star formation in the bridge gas except for the giant Hii region near UGC 12915. Our model suggests that we observe this galaxy head-on collision near the time of maximum CO and H 2 emission.

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“…These authors have shown that the molecular gas phase, even in high-density regions, can be removed during the interaction. Whereas detailed multifrequency observations of representative objects in nearby clusters begin to show cases of ongoing molecular gas ram pressure stripping events (Vollmer et al 2008a(Vollmer et al , 2009(Vollmer et al , 2012aSivanandam et al 2010), strong and convincing statistical evidence is still lacking. Since star formation occurs mainly inside molecular clouds, the perturbation of the molecular gas phase in any kind of interaction can have a strong impact on the evolution of the stellar populations of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

et al. 2014

A&A

176

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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Ram pressure stripping of the multiphase ISM and star formation in the Virgo spiral galaxy NGC 4330

Cited by 68 publications

References 31 publications

Gas loss in simulated galaxies as they fall into clusters

Gas loss in simulated galaxies as they fall into clusters

A dynamical model for the Taffy galaxies UGC 12914/5

Cold gas properties of theHerschelReference Survey

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