Group pre-processing versus cluster ram-pressure stripping: the case of ESO156−G029

Džudžar, Robert; Kilborn, V. A.; Murugeshan, C.; Meurer, G. R.; Sweet, Sarah M.; Putman, Mary E.

doi:10.1093/mnrasl/slz139

Cited by 13 publications

(18 citation statements)

References 55 publications

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“…These groups are: J0258-74, J1026-19, J1250-20, J1408-21 and J1956-50. The only exception to these scenarios is the J0400-52 group as it is infalling into a cluster Džudžar et al (2019b). The rapid H i-removal process, ram-pressure, is expected in the S1 galaxy within J0400-52 once it approaches the cluster centre Džudžar et al (2019b).…”

Section: Discussionmentioning

confidence: 99%

“…Moreover, each of these galaxies have a peculiar morphology that can be connected with an interaction and possible accretion of the H i gas. J0400-51:S1 has visible faint stellar streams in the North, and we discussed in Džudžar et al (2019b) how these may be related to a merger. J1250-20:S1 had clear ongoing multiple interactions and a stellar stream reaching out of a spiral arm (Džudžar et al 2019a) and see Figure H4.…”

Section: H I Distribution In Galaxiesmentioning

confidence: 99%

“…J0400-50:S1 has highly asymmetric H i intensity distribution and disturbed gas kinematics. We presented this galaxy in Džudžar et al (2019b) as an example of being shaped by the group environment as it is falling into a cluster. J1250-20:S1 is interacting with other galaxies in its group (with S2, S3) and it is connected to a stellar stream that contains S6 and S7.…”

Section: Physical Processes In the H I-deficient And H I-excess Galaxiesmentioning

confidence: 99%

“…One Choir group, J0400-51, is infalling into a cluster. Džudžar et al (2019b) proposed that the gas-rich galaxy within this group (ESO156-G029) will be under the effects of ram-pressure once the galaxy approaches closer to the cluster centre. Moreover, we used this galaxy as an example to show that group pre-processing is important in its evolution.…”

Section: Choirs In Context Of Hickson Compact Groups and Their Evolutionmentioning

confidence: 99%

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Environmental processing of galaxies in H i-rich groups

Džudžar

Kilborn

Sweet

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present and explore the resolved atomic hydrogen (H i) content of 13 H i-rich and late-type dominated groups denoted ‘Choirs’. We quantify the H i content of the Choir galaxies with respect to the median of the H i-mass fraction (f$_{\rm {{\small H\,{I}}}}$) of their grandparent Hipass sample. We find that the H i mass fraction of the Choir galaxies is dispersed around the Hipass median in the range -1.4≤Δf$_{\rm {{\small H\,{I}}}}\rm {[dex]}\le$0.7, from H i-excess to H i-deficient galaxy regime. The H i-excess/H i-deficient galaxies contain more/less than 2.5 times their expected H i content with respect to the Hipass median. We show and discuss that the environmental processing in Choirs occurs via tidal stripping and galaxy mergers. Our analysis suggests that tidal stripping contributes to the loss of the H i, while galaxy mergers contribute to the enhancement of the H i. Exploring the mid-infrared properties of Choir galaxies we find possible environmental processing in only nine Choir galaxies, which indicates that environmental processing is more perceptible in the H i content than the mid-infrared properties. Moreover, we find that environmental processing occurs in Choir groups regardless of their global environment, whether they are in isolation or in proximity to the denser structures, such as cosmic web filaments. We explore possible scenarios of the Choirs evolution, taking into account their H i content, velocity dispersion, crossing time and their global environment. We conclude that the most likely evolution for the majority of Choir groups is that they will become more compact as their members undergo multiple H i-rich mergers.

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Section: Discussionmentioning

confidence: 99%

Section: H I Distribution In Galaxiesmentioning

confidence: 99%

Section: Physical Processes In the H I-deficient And H I-excess Galaxiesmentioning

confidence: 99%

Section: Choirs In Context Of Hickson Compact Groups and Their Evolutionmentioning

confidence: 99%

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Environmental processing of galaxies in H i-rich groups

Džudžar

Kilborn

Sweet

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…McGee et al 2009(see, e.q. McGee et al , 2014Aragon Calvo et al 2019;Džudžar et al 2019, and references therein). Alpaslan et al (2016) found that among spiral galaxies in GAMA fields galaxies which lie closer to the filament axes have higher stellar masses and higher star-formation rates than spiral galaxies in the outer parts of filaments.…”

Section: Galaxy Evolution In the Supercluster And In The Cocoonmentioning

confidence: 99%

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Einasto

Deshev

Tenjes

et al. 2020

A&A

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Context. Superclusters of galaxies and their surrounding low-density regions (cocoons) represent dynamically evolving environments in which galaxies and their systems form and evolve. While evolutionary processes of galaxies in dense environments are extensively studied at present, galaxy evolution in low-density regions has received less attention. Aims. We study the properties, connectivity, and galaxy content of groups and filaments in the A2142 supercluster (SCl A2142) cocoon to understand the evolution of the supercluster with its surrounding structures and the galaxies within them. Methods. We calculated the luminosity-density field of SDSS galaxies and traced the SCl A2142 cocoon boundaries by the lowest luminosity-density regions that separate SCl A2142 from other superclusters. We determined galaxy filaments and groups in the cocoon and analysed the connectivity of groups, the high density core (HDC) of the supercluster, and the whole of the supercluster. We compared the distribution and properties of galaxies with different star-formation properties in the supercluster and in the cocoon. Results. The supercluster A2142 and the long filament that is connected to it forms the longest straight structure in the Universe detected so far, with a length of approximately 75 h −1 Mpc. The connectivity of the cluster A2142 and the whole supercluster is C = 6 − 7; poor groups exhibit C = 1 − 2. Long filaments around the supercluster's main body are detached from it at the turnaround region. Among various local and global environmental trends with regard to the properties of galaxies and groups, we find that galaxies with very old stellar populations lie in systems across a wide range of richness from the richest cluster to poorest groups and single galaxies. They lie even at local densities as low as D1 < 1 in the cocoon and up to D1 > 800 in the supercluster. Recently quenched galaxies lie in the cocoon mainly in one region and their properties are different in the cocoon and in the supercluster. The star-formation properties of single galaxies are similar across all environments. Conclusions. The collapsing main body of SCl A2142 with the detached long filaments near it are evidence of an important epoch in the supercluster evolution. There is a need for further studies to explore possible reasons behind the similarities between galaxies with very old stellar populations in extremely different environments, as well as mechanisms for galaxy quenching at very low densities. The presence of long, straight structures in the cosmic web may serve as a test for cosmological models.

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The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

Cortese

Catinella

Smith

2021

Publ. Astron. Soc. Aust.

126

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One of the key open questions in extragalactic astronomy is what stops star formation in galaxies. While it is clear that the cold gas reservoir, which fuels the formation of new stars, must be affected first, how this happens and what are the dominant physical mechanisms involved is still a matter of debate. At least for satellite galaxies, it is generally accepted that internal processes alone cannot be responsible for fully quenching their star formation, but that environment should play an important, if not dominant, role. In nearby clusters, we see examples of cold gas being removed from the star-forming discs of galaxies moving through the intracluster medium, but whether active stripping is widespread and/or necessary to halt star formation in satellites, or quenching is just a consequence of the inability of these galaxies to replenish their cold gas reservoirs, remains unclear. In this work, we review the current status of environmental studies of cold gas in star-forming satellites in the local Universe from an observational perspective, focusing on the evidence for a physical link between cold gas stripping and quenching of the star formation. We find that stripping of cold gas is ubiquitous in satellite galaxies in both group and cluster environments. While hydrodynamical mechanisms such as ram pressure are important, the emerging picture across the full range of dark matter halos and stellar masses is a complex one, where different physical mechanisms may act simultaneously and cannot always be easily separated. Most importantly, we show that stripping does not always lead to full quenching, as only a fraction of the cold gas reservoir might be affected at the first pericentre passage. We argue that this is a key point to reconcile apparent tensions between statistical and detailed analyses of satellite galaxies, as well as disagreements between various estimates of quenching timescales. We conclude by highlighting several outstanding questions where we expect to see substantial progress in the coming decades, thanks to the advent of the Square Kilometre Array and its precursors, as well as the next-generation optical and millimeter facilities.

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Group pre-processing versus cluster ram-pressure stripping: the case of ESO156−G029

Cited by 13 publications

References 55 publications

Environmental processing of galaxies in H i-rich groups

Environmental processing of galaxies in H i-rich groups

Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

The Dawes Review 9: The role of cold gas stripping on the star formation quenching of satellite galaxies

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