Ram Pressure Stripping and Galaxy Orbits: The Case of the Virgo Cluster

Vollmer, B.; Cayatte, V.; Balkowski, C.; Duschl, W. J.

doi:10.1086/323368

Cited by 414 publications

(713 citation statements)

References 62 publications

(99 reference statements)

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“…Observations also suggest that late-type galaxies have slightly more radial orbits than early-type galaxies (58)(59)(60)(61), consistent with the results presented here. Our results indicate that gasbearing galaxies in clusters outside 0.25 r vir should have been accreted within a time frame that is shorter than the cluster dynamical time, because otherwise they would have lost their gas.…”

Section: Resultssupporting

confidence: 89%

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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Section: Resultssupporting

confidence: 89%

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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“…To simulate these effects, the column density of those clouds that are located in regions with a local density below a threshold ρ lim is made to decrease exponentially with time as Σ = Σ 0 exp (−t/t 2 ), where t 2 = 50 Myr. This corresponds approximately to the timescale of saturated evaporation (Vollmer et al 2001). The threshold gas density is fixed at ρ lim = 10 −2 cm −3 , and the parameters t 2 and ρ lim are chosen such that the H properties of NGC 4254 are reproduced.…”

Section: Tidal Interaction and Ram Pressurementioning

confidence: 99%

NGC 4254: a spiral galaxy entering the Virgo cluster

Vollmer

Huchtmeier

Driel

2005

A&A

Self Cite

100

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Abstract. Deep Effelsberg H spectra of the one-armed, bright Virgo cluster spiral galaxy NGC 4254 are presented. Five different positions were observed in the 21 cm H line with the Effelsberg 100-m telescope: one in the center and 4 located one HPBW to the NE, NW, SW, and SE, respectively, from the galaxy center. The spectra are compared to existing deep VLA observations, and the single dish and interferometric H data are used to constrain a dynamical model which includes the effects of ram pressure. The peculiar, one-armed spiral pattern of NGC 4254 and its distorted and kinematically perturbed atomic gas distribution can be explained by a close and rapid encounter ∼280 Myr ago with another massive Virgo galaxy, followed by ram pressure stripping that is ongoing. The stripping occurs almost face-on, since the angle between the disk and the orbital plane is 70 • . The galaxy with which NGC 4254 had its encounter is tentatively identified as the lenticular NGC 4262.

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“…This process is expected to be the main mechanism through which the infalling gas is heated up and virialized into the main dark-matter halo (Gunn & Gott 1972;Heinz et al 2003;Roediger et al 2015;Vollmer et al 2001) and it is believed to be key to the evolution of the cluster galaxy population by quenching rapidly the star formation activity in clusters (Bahé & McCarthy 2015;Roediger & Brüggen 2008). Recent observational evidence suggest that thermal conduction in the ICM is strongly inhibited (e.g.…”

Section: Introductionmentioning

confidence: 99%

The XMM cluster outskirts project (X‐COP)

et al. 2017

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Galaxy clusters are thought to grow hierarchically through the continuous merging and accretion of smaller structures across cosmic time. In the Local Universe, these phenomena are still active in the outer regions of massive clusters (R > R500), where the matter distribution is expected to become clumpy and asymmetric because of the presence of accreting structures. We present the XMM-Newton Cluster Outskirts Project (X-COP), which targets the outer regions of a sample of 13 massive clusters (M500 > 3 × 10 14 M ) in the redshift range 0.04-0.1 at uniform depth. The sample was selected based on the signal-to-noise ratio in the Planck Sunyaev-Zeldovich (SZ) survey with the aim of combining high-quality X-ray and SZ constraints throughout the entire cluster volume. Our observing strategy allows us to reach a sensitivity of 3 × 10 −16 ergs cm −2 s −1 arcmin −2 in the [0.5-2.0] keV range thanks to a good control of systematic uncertainties. The combination of depth and field of view achieved in X-COP will allow us to pursue the following main goals: i) measure the distribution of entropy and thermal energy to an unprecedented level of precision; ii) assess the presence of non-thermal pressure support in cluster outskirts; iii) study the occurrence and mass distribution of infalling gas clumps. We illustrate the capabilities of the program with a pilot study on the cluster Abell 2142.

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Ram Pressure Stripping and Galaxy Orbits: The Case of the Virgo Cluster

Cited by 414 publications

References 62 publications

Gas loss in simulated galaxies as they fall into clusters

Gas loss in simulated galaxies as they fall into clusters

NGC 4254: a spiral galaxy entering the Virgo cluster

The XMM cluster outskirts project (X‐COP)

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