GASP – XII. The variety of physical processes occurring in a single galaxy group in formation

Vulcani, Benedetta; Poggianti, Bianca M.; Jaffé, Yara L.; Moretti, Alessia; Fritz, J.; Gullieuszik, Marco; Bettoni, D.; Fasano, G.; Tonnesen, Stephanie; McGee, Sean L.

doi:10.1093/mnras/sty2095

Cited by 50 publications

(54 citation statements)

References 152 publications

(161 reference statements)

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“…As galaxies undergo complex encounters, the gas in their CGM, being more diffuse and extended, should be even more susceptible to the effects of gravitational interactions like tidal stripping, or to hydrodynamic interactions. Indeed at low redshifts (z < 0.1), the effects of galaxy interactions within groups and clusters are manifested on the cool neutral hydrogen and molecular gas in the form of tidal streams, plumes, fountains, high-velocity clouds and warped discs (Fraternali et al 2002;Sancisi et al 2008;Mihos et al 2012;Jáchym et al 2014;Ramatsoku et al 2019;Moretti et al 2020), as well as on the ionized gas (Fumagalli et al 2014;Poggianti et al 2017;Vulcani et al 2018;Fossati et al 2019a). Galaxy mergers are also more likely in denser environments, and merger-driven outflows could affect the gas content and distribution in the CGM (Hani et al 2018).…”

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confidence: 99%

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

Dutta

Fumagalli

Fossati

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a study of the metal-enriched cool halo gas traced by Mg ii absorption around 228 galaxies at z ∼ 0.8 − 1.5 within 28 quasar fields from the MUSE Analysis of Gas around Galaxies (MAGG) survey. We observe no significant evolution in the Mg ii equivalent width versus impact parameter relation and in the Mg ii covering fraction compared to surveys at z ≲ 0.5. The stellar mass, along with distance from galaxy centre, appears to be the dominant factor influencing the Mg ii absorption around galaxies. With a sample that is 90% complete down to a star formation rate of ≈0.1 $\rm M_\odot yr^{-1}$PLXINSERT-, and up to impact parameters ≈250 − 350 kpc from quasars, we find that the majority ($67^{+12}_{-15}$% or 14/21) of the Mg ii absorption systems are associated with more than one galaxy. The complex distribution of metals in these richer environments adds substantial scatter to previously-reported correlations. Multiple galaxy associations show on average five times stronger absorption and three times higher covering fraction within twice the virial radius than isolated galaxies. The dependence of Mg ii absorption on galaxy properties disfavours the scenario in which a widespread intra-group medium dominates the observed absorption. This leaves instead gravitational interactions among group members or hydrodynamic interactions of the galaxy haloes with the intra-group medium as favoured mechanisms to explain the observed enhancement in the Mg ii absorption strength and cross section in rich environments.

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confidence: 99%

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

Dutta

Fumagalli

Fossati

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Some of these galaxies display Hi deficiencies as well as Hi morphologies consistent with RPS (Kleiner et al 2021). Finally, evidence for RPS stripping in groups has also been presented in the form of gas disks which are truncated relative to the stellar component, consistent with RPS removing gas from the outside-in (Sengupta et al 2007;Vulcani et al 2018b).…”

Section: Introductionmentioning

confidence: 77%

LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

Roberts,

van Weeren,

McGee

et al. 2021

Preprint

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Ram pressure stripping is a frequently cited mechanism for quenching galaxy star formation in dense environments. Numerous examples of ram pressure stripping in galaxy clusters are present in literature; however, substantially less work has been focused on ram pressure stripping in lower mass groups, the most common galaxy environment in the local Universe. In this work we use the LOFAR Two-metre Sky Survey (LoTSS) to search for jellyfish galaxies (i.e. galaxies with ram pressure stripped tails extending beyond the optical disk) in ∼500 SDSS groups (z < 0.05), making this the most comprehensive search for ram pressure stripping in groups to date. We identify 60 jellyfish galaxies in groups with extended, asymmetric radio continuum tails, which are found across the entire range of group mass from 10 12.5 < M group < 10 14 h −1 M . We compare the group jellyfish galaxies identified in this work with the LoTSS jellyfish galaxies in clusters presented in Roberts et al. (2021b), allowing us to compare the effects of ram pressure stripping across three decades in group/cluster mass. We find that jellyfish galaxies are most commonly found in clusters, with the frequency decreasing towards the lowest mass groups. Both the orientation of observed radio continuum tails, and the positions of group jellyfish galaxies in phase space, suggest that galaxies are stripped more slowly in groups relative to clusters. Finally, we find that the star formation rates of jellyfish galaxies in groups are consistent with 'normal' star-forming group galaxies, which is in contrast to cluster jellyfish galaxies that have clearly enhanced star formation rates. On the whole, there is clear evidence for ongoing ram pressure stripping in galaxy groups (down to very low group masses), though the frequency of jellyfish galaxies and the strength of ram pressure stripping appears smaller in groups than clusters. Differences in the efficiency of ram pressure stripping in groups versus clusters likely contributes to the positive trend between quenched fraction and host halo mass observed in the local Universe.

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“…Jellyfish galaxies appear to exist in a range of environments, from the very dense centers of large clusters to the low-density outskirts (e.g. Vulcani et al 2018a;Gullieuszik et al 2020;Vulcani et al 2021). There is a growing consensus that many jellyfish galaxies have been shaped by ram pressure stripping, i.e.…”

Section: Introductionmentioning

confidence: 99%

GASP XXXVII: The Most Extreme Jellyfish Galaxies Compared to Other Disk Galaxies in Clusters, an HI Study

Luber,

Müller,

van Gorkom

et al. 2022

Preprint

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We present the results of a VLA HI imaging survey aimed at understanding why some galaxies develop long extraplanar Hα tails, becoming extreme jellyfish galaxies. The observations are centered on five extreme jellyfish galaxies, optically selected from the WINGS and OmegaWINGS surveys and confirmed to have long Hα tails through MUSE observations. Each galaxy is located in a different cluster. In the observations there are in total 88 other spiral galaxies within the field of view (40 x40 ) and observed bandwidth (6500 km s −1 ). We detect 13 of these 88 spirals, plus one uncatalogued spiral, with HI masses ranging from 1 to 7 × 10 9 M . Many of these detections have extended HI disks, two show direct evidence for ram pressure stripping, while others are possibly affected by tidal forces and/or ram-pressure stripping. We stack the 75 non-detected spiral galaxies and find an average HI mass of 1.9 × 10 8 M , which given their average stellar mass, implies they are very HI deficient. Comparing the extreme jellyfish galaxies to the other disk galaxies, we find that they have a larger stellar mass than almost all disk galaxies and than all HI detected galaxies, they are at smaller projected distance from the cluster center and at higher relative velocity to the cluster mean than all HI detections and most non-detections. We conclude that the high stellar mass allows extreme jellyfish galaxies to fall deeply into the cluster before being stripped and the surrounding ICM pressure gives rise to their spectacular star-forming tails.

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GASP – XII. The variety of physical processes occurring in a single galaxy group in formation

Cited by 50 publications

References 152 publications

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

MUSE Analysis of Gas around Galaxies (MAGG) – II: metal-enriched halo gas around z ∼ 1 galaxies

LoTSS jellyfish galaxies: II. Ram pressure stripping in groups versus clusters

GASP XXXVII: The Most Extreme Jellyfish Galaxies Compared to Other Disk Galaxies in Clusters, an HI Study

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