BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

Jaffé, Yara L.; Verheijen, Marc; Haines, C. P.; Yoon, Hyein; Cybulski, Ryan; Montero-Castaño, María; Smith, Rory; Chung, Aeree; Deshev, Boris; Fernández, Ximena; Gorkom, Jacqueline van; Poggianti, Bianca M.; Yun, Min S.; Finoguenov, A.; Smith, Graham P.; Okabe, Nobuhiko

doi:10.1093/mnras/stw984

Cited by 112 publications

(122 citation statements)

References 99 publications

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“…At small clustocentric radii, combined with low clustocentric velocity, the density of H i detection decreases dramatically, indicating that most galaxies are H i stripped when they settle into the cluster center as virialized. This not only confirms the trend with a clustocentric radius found in a number of nearby clusters (Solanes et al 2001;Boselli & Gavazzi 2006) but also agrees with the findings in a cluster at the z = 0.2 cluster (Jaffé et al 2016). In addition, we confirm that the H i gas in massive galaxies is still detected near the center of the cluster, implying that less massive galaxies get easily stripped in H i.…”

Section: Discussionsupporting

confidence: 90%

“…There are several possible explanations, including (1) merging of subgroups into the main cluster, which may generate non-static ICM (Shibata et al 2001), (2) preprocessing within infalling subgroups and/or filamentary structures (Fujita 2004;Jaffé et al 2016), or (3) backsplashing of galaxies (Gill et al 2005). Hence, in order to study the detailed histories of gas stripping and star formation of galaxies in the cluster environment, it is important to probe not only the current surroundings of galaxies but also which environments galaxies have gone through in the past, i.e.…”

Section: Introductionmentioning

confidence: 99%

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A History of H i Stripping in Virgo: A Phase-space View of VIVA Galaxies

Yoon

Chung

Smith

et al. 2017

ApJ

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We investigate the orbital histories of Virgo galaxies at various stages of H i gas stripping. In particular, we compare the location of galaxies with different H i morphology in phase space. This method is a great tool for tracing the gas stripping histories of galaxies as they fall into the cluster. Most galaxies at the early stage of H i stripping are found in the first infall region of Virgo, while galaxies undergoing active H i stripping mostly appear to be falling in or moving out near the cluster core for the first time. Galaxies with a severely stripped, yet symmetric, H i disks are found in one of two locations. Some are deep inside the cluster, but others are found in the cluster outskirts with low orbital velocities. We suggest that the latter group of galaxies belong to a "backsplash" population. These present the clearest candidates for backsplashed galaxies observationally identified to date. We further investigate the distribution of a large sample of H i-detected galaxies toward Virgo in phase space, confirming that most galaxies are stripped of their gas as they settle into the gravitational potential of the cluster. In addition, we discuss the impact of tidal interactions between galaxies and group preprocessing on the H i properties of the cluster galaxies, and link the associated star formation evolution to the stripping sequence of cluster galaxies.

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Section: Discussionsupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

A History of H i Stripping in Virgo: A Phase-space View of VIVA Galaxies

Yoon

Chung

Smith

et al. 2017

ApJ

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175

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“…The different PPSD of S0 and S galaxies might result from the fact that the morphological evolutionary processes are more effective in the central cluster regions (e.g., Moran et al 2007). In particular, ram-pressure stripping (Gunn & Gott 1972), and/or starbursts induced by tidal compression by the cluster gravitational field, especially while the galaxies are accreted in groups (the so-called 'post-processing'; Bekki 1999;Oemler et al 2009;Vijayaraghavan & Ricker 2013;Stroe et al 2015;Jaffé et al 2016), likely play a relevant role. This compression could drive the rapid consumption of gas funneled into the central galaxy region and the build-up of a central bulge.…”

Section: Discussionmentioning

confidence: 99%

Structural and dynamical modeling of WINGS clusters

Cava

Biviano

Mamon

et al. 2017

A&A

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Context. We study the distribution of galaxies in nearby clusters to shed light on the evolutionary processes at work within clusters and prepare for a full dynamical analysis to be conducted in forthcoming papers of this series. Aims. We use the Wide-field Nearby Galaxy-clusters Survey (WINGS) database complemented with literature data. We assign galaxy membership to individual clusters, then select a sample of 67 clusters with at least 30 spectroscopic members each. 53 of these clusters do not show evidence of substructures in phase-space, as measured by the Dressler-Shectman test, while 14 do. We estimate the virial radii and circular velocities of the 67 clusters by a variety of proxies (velocity dispersion, X-ray temperature, and richness) and use these estimates to build stack samples from these 53 and 14 clusters, that we call 'Reg' and 'Irr' stacks, respectively. We show that our results are robust with regard to the choice of the virial radii and circular velocities used to scale galaxy radii and velocities in the stacking procedure. We determine the number-density and velocity-dispersion profiles of Elliptical (E), S0, and Spiral+Irregular (S) galaxies in the Reg and Irr samples, separately, and fit models to these profiles. Methods. The number density profiles of E, S0, and S galaxies are adequately described by either a Navarro, Frenk, & White (NFW) or a cored King model, both for the Reg and Irr samples, with a slight preference for the NFW model. The spatial distribution concentration increases from the S to the S0 and to the E populations, both in the Reg and the Irr stacks, reflecting the well-known morphology-radius relation. Reg clusters have a more concentrated spatial distribution of E and S0 galaxies than Irr clusters, while the spatial distributions of S galaxies in Reg and Irr clusters have a similar concentration. We propose a new phenomenological model that provides acceptable fits to the velocity dispersion profile of all our galaxy samples. The velocity dispersion profiles become steeper and with a higher normalization from E to S0 to S galaxies. The S0 velocity dispersion profile is close to that of E galaxies in Reg clusters, and intermediate between those of E and S galaxies in Irr clusters. Results. Our results suggest that S galaxies are a recently accreted cluster population, that take ≤ 3 Gyr to evolve into S0 galaxies after accretion, and in doing so modify their phase-space distribution, approaching that of cluster ellipticals. While in Reg clusters this evolutionary process is mostly completed, it is still ongoing in Irr clusters.

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“…The low-density environments are populated primarily by gas-rich, star forming galaxies with late-type morphologies, while the densest parts of the clusters are almost completely devoid of any cold gas or signs of star-formation, and are domThe full table with measured redshifts is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ inated by early-type galaxies (e.g. Dressler 1980;Dressler et al 1997;Solanes et al 2001;Lewis et al 2002;Gómez et al 2003;Jaffé et al 2016). …”

Section: Introductionmentioning

confidence: 99%

Galaxy evolution in merging clusters: The passive core of the “Train Wreck” cluster of galaxies, A 520

Deshev¹,

Finoguenov²,

Verdugo³

et al. 2017

A&A

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Aims. The mergers of galaxy clusters are the most energetic events in the universe after the Big Bang. With the increased availability of multi-object spectroscopy and X-ray data, an ever increasing fraction of local clusters are recognised as exhibiting signs of recent or past merging events on various scales. Our goal is to probe how these mergers affect the evolution and content of their member galaxies. We specifically aim to answer the following questions: Is the quenching of star formation in merging clusters enhanced when compared with relaxed clusters? Is the quenching preceded by a (short-lived) burst of star formation? Methods. We obtained optical spectroscopy of > 400 galaxies in the field of the merging cluster Abell 520. We combine these observations with archival data to obtain a comprehensive picture of the state of star formation in the members of this merging cluster. Finally, we compare these observations with a control sample of ten non-merging clusters at the same redshift from The Arizona Cluster Redshift Survey (ACReS). We split the member galaxies into passive, star forming or recently quenched depending on their spectra. Results. The core of the merger shows a decreased fraction of star forming galaxies compared to clusters in the non-merging sample. This region, dominated by passive galaxies, is extended along the axis of the merger. We find evidence of rapid quenching of the galaxies during the core passage with no signs of a star burst on the time scales of the merger ( 0.4 Gyr). Additionally, we report the tentative discovery of an infalling group along the main filament feeding the merger, currently at ∼2.5 Mpc from the merger centre. This group contains a high fraction of star forming galaxies as well as approximately two thirds of all the recently quenched galaxies in our survey.

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BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

Cited by 112 publications

References 99 publications

A History of H i Stripping in Virgo: A Phase-space View of VIVA Galaxies

A History of H i Stripping in Virgo: A Phase-space View of VIVA Galaxies

Structural and dynamical modeling of WINGS clusters

Galaxy evolution in merging clusters: The passive core of the “Train Wreck” cluster of galaxies, A 520

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