Ram pressure stripping in the Virgo Cluster

Verdugo, Celia; Combes, F.; Dasyra, K. M.; Salomé, P.; Braine, J.

doi:10.1051/0004-6361/201526551

Cited by 50 publications

(64 citation statements)

References 60 publications

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“…2) In Moretti et al (2018b) we presented APEX CO(2-1) data for four of the galaxies presented in this paper and found large amounts of molecular gas (several 10 9 M ) in the tails of these galaxies. Molecular gas was also found in the tails of 3 other jellyfishes in the literature (Jáchym et al , 2017Verdugo et al 2015). The CO observed in the tails is the smoking gun of the presence of cold, molecular gas where new stars can be born.…”

Section: In-situ Star Formation In the Tailsmentioning

confidence: 87%

GASP XIII. Star formation in gas outside galaxies

Poggianti

Gullieuszik

Tonnesen

et al. 2018

Monthly Notices of the Royal Astronomical Society

119

169

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Based on MUSE data from the GASP survey, we study the Hα-emitting extraplanar tails of 16 cluster galaxies at z ∼ 0.05 undergoing ram pressure stripping. We demonstrate that the dominating ionization mechanism of this gas (between 64% and 94% of the Hα emission in the tails depending on the diagnostic diagram used) is photoionization by young massive stars due to ongoing star formation (SF) taking place in the stripped tails. This SF occurs in dynamically quite cold HII clumps with a median Hα velocity dispersion σ = 27 km s −1 . We study the characteristics of over 500 star-forming clumps in the tails and find median values of Hα luminosity L Hα = 4 × 10 38 erg s −1 , dust extinction A V = 0.5 mag, star formation rate SFR= 0.003 M yr −1 , ionized gas density n e = 52 cm −3 , ionized gas mass M gas = 4 × 10 4 M , and stellar mass M * = 3 × 10 6 M . The tail clumps follow scaling relations (M gas − M * , L Hα − σ, SFR-M gas ) similar to disk clumps, and their stellar masses are comparable to Ultra Compact Dwarfs and Globular Clusters. The diffuse gas component in the tails is ionized by a combination of SF and composite/LINER-like emission likely due to thermal conduction or turbulence. The stellar photoionization component of the diffuse gas can be due either to leakage of ionizing photons from the HII clumps with an average escape fraction of 18%, or lower luminosity HII regions that we cannot individually identify.

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Section: In-situ Star Formation In the Tailsmentioning

confidence: 87%

GASP XIII. Star formation in gas outside galaxies

Poggianti

Gullieuszik

Tonnesen

et al. 2018

Monthly Notices of the Royal Astronomical Society

119

169

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“…We will investigate the relative contribution of old stars, presumably stripped from the interacting galaxies, and the in situ intracluster star formation. While we expect that the first contribution will be dominant, the second seems to have been observed in Virgo (Verdugo et al 2015).…”

Section: Introductionmentioning

confidence: 84%

The XXL Survey

Adami

Pompei

Sadibekova

et al. 2016

A&A

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Aims. Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies and their subsequent dispersal into the intracluster medium. Gas hydrodynamical effects can additionally strip gas and dust from galaxies; both gas and stars contribute to intracluster light (ICL). The properties of the ICL can therefore help constrain the physical processes at work in clusters by serving as a fossil record of the interaction history. Methods. The present study is designed to characterise this ICL for the first time in a ∼10 14 M and z ∼ 0.53 cluster of galaxies from imaging and spectroscopic points of view. By applying a wavelet-based method to CFHT Megacam and WIRCAM images, we detect significant quantities of diffuse light and are able to constrain their spectral energy distributions. These sources were then spectroscopically characterised with ESO Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data. MUSE data were also used to compute redshifts of 24 cluster galaxies and search for cluster substructures.Results. An atypically large amount of ICL, equivalent in i to the emission from two brightest cluster galaxies, has been detected in this cluster. Part of the detected diffuse light has a very weak optical stellar component and apparently consists mainly of gas emission, while other diffuse light sources are clearly dominated by old stars. Furthermore, emission lines were detected in several places of diffuse light. Our spectral analysis shows that this emission likely originates from low-excitation parameter gas. Globally, the stellar contribution to the ICL is about 2.3 × 10 9 yr old even though the ICL is not currently forming a large number of stars. On the other hand, the contribution of the gas emission to the ICL in the optical is much greater than the stellar contribution in some regions, but the gas density is likely too low to form stars. These observations favour ram pressure stripping, turbulent viscous stripping, or supernovae winds as the origin of the large amount of intracluster light. Since the cluster appears not to be in a major merging phase, we conclude that ram pressure stripping is the most plausible process that generates the observed ICL sources. Conclusions. This is one of the first times that we are able to spectroscopically study diffuse light in such a distant and massive cluster, and it demonstrates the potential of MUSE observations for such studies.

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“…On the other hand, several processes have been proved to strip the gas from galaxies in dense environments, as confirmed by the detection of molecular gas in tidal tails (e.g. Kenney & Koopmann 1999;Braine et al 2000;Verdugo et al 2015). Quilis et al (2000) and Abadi et al (1999), among other authors, claimed that ram pressure and viscous stripping are very effective at removing the disk gas in a relatively short timescale.…”

Section: Fcc 170: In the Core Of The Fornax Clustermentioning

confidence: 94%

The Fornax 3D project: Unveiling the thick disk origin in FCC 170; possible signs of accretion

Pinna

Falcón-Barroso

Martig

et al. 2019

A&A

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We present and discuss the stellar kinematics and populations of the S0 galaxy FCC 170 (NGC 1381) in the Fornax cluster, using deep MUSE data from the Fornax 3D survey. We show the maps of the first four moments of the stellar line-of-sight velocity distribution and of the mass-weighted mean stellar age, metallicity and [Mg/Fe] abundance ratio. The high-quality MUSE stellar kinematic measurements unveil the structure of this massive galaxy: a nuclear disk, a bar seen as a boxy bulge with a clear higher-velocitydispersion X shape, a fast-rotating and flaring thin disk and a slower rotating thick disk. Whereas their overall old age makes it difficult to discuss differences in the formation epoch between these components, we find a clear-cut distinction between metal-rich and less [Mg/Fe]-enhanced populations in the thin-disk, boxy-bulge and nuclear disk, and more metal-poor and [Mg/Fe]-enhanced stars in the thick disk. Located in the densest region of the Fornax cluster, where signs of tidal stripping have been recently found, the evolution of FCC 170 might have been seriously affected by its environment. We discuss the possibility of its "pre-processing" in a subgroup before falling into the present-day cluster, which would have shaped this galaxy a long time ago. The thick disk displays a composite star formation history, as a significant fraction of younger stars co-exist with the main older thick-disk population. The former sub-population is characterized by even lower-metallicity and higher-[Mg/Fe] values, suggesting that these stars formed later and faster in a less chemically evolved satellite, which was subsequently accreted. Finally, we discuss evidence that metal-rich and less [Mg/Fe]-enhanced stars were brought in the outer parts of the thick disk by the flaring of the thin disk.

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Ram pressure stripping in the Virgo Cluster

Cited by 50 publications

References 60 publications

GASP XIII. Star formation in gas outside galaxies

GASP XIII. Star formation in gas outside galaxies

The XXL Survey

The Fornax 3D project: Unveiling the thick disk origin in FCC 170; possible signs of accretion

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