BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies

Jaffé, Yara L.; Smith, Rory; Candlish, Graeme N.; Poggianti, Bianca M.; Sheen, Yun-Kyeong; Verheijen, Marc

doi:10.1093/mnras/stv100

Cited by 238 publications

(337 citation statements)

References 82 publications

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“…A similar plot was already shown in Jaffé et al (2015) but it is presented here again with the much larger spectroscopic sample. A few areas, defined in Jaffé et al (2015), are shown. The 'recent infall' and 'virialized' areas reflect the orbital histories of cluster galaxies, as already discussed in Section 3.1.…”

Section: Distribution Of Red Blue and Hi -Rich Galaxiessupporting

confidence: 80%

“…It is possible that some of these (especially the most massive ones) have been 'mass quenched' (by internal processes such as AGN feedback; see Peng et al 2010), but additional 'environmental quenching' might also be at play, especially for lower mass galaxies. As discussed in Jaffé et al (2015), the abundance of passive galaxies in the cluster outskirts cannot easily be explained by RPS alone (or backsplashing galaxies). However, a more plausible explanation for this effect is that many of these galaxies started to be quenched in a previous environment.…”

Section: Distribution Of Red Blue and Hi -Rich Galaxiesmentioning

confidence: 98%

“…The 'recent infall' and 'virialized' areas reflect the orbital histories of cluster galaxies, as already discussed in Section 3.1. The 'stripping' zone, also defined in Jaffé et al (2015) is the outcome of embedding Gunn & Gott (1972)'s prescription of RPS, together with a model of A963 1's ICM, into dark matter cosmological simulations. Our model predicted gas-rich galaxies to be located in the 'recent infall' region of phase-space, avoiding the 'stripping' and 'virialized' zones.…”

Section: Distribution Of Red Blue and Hi -Rich Galaxiesmentioning

confidence: 99%

“…In Jaffé et al (2015) we concentrated on the more massive cluster Abell 963 (A963 1 hereafter, following previous papers) to study the effect of RPS by the ICM. We compared the location of Hi -detected cluster galaxies in velocity versus position phase-space diagrams with the distribution of dark matter haloes in zoom-in cosmological simulations, and found strong evidence for Hi gas stripping (down to the detection limit of BUDHIES) on first infall into the cluster.…”

Section: Introductionmentioning

confidence: 99%

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

Jaffé

Verheijen

Haines

et al. 2016

Mon. Not. R. Astron. Soc.

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112

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In a hierarchical Universe clusters grow via the accretion of galaxies from the field, groups and even other clusters. As this happens, galaxies can lose their gas reservoirs via different mechanisms, eventually quenching their star formation. We explore the diverse environmental histories of galaxies through a multiwavelength study of the combined effect of ram-pressure stripping and group 'processing' in Abell 963, a massive growing cluster at z = 0.2 from the Blind Ultra Deep Hi Environmental Survey (BUDHIES). We incorporate hundreds of new optical redshifts (giving a total of 566 cluster members), as well as Subaru and XMM-Newton data from LoCuSS, to identify substructures and evaluate galaxy morphology, star formation activity, and Hi content (via Hi deficiencies and stacking) out to 3×R 200 . We find that Abell 963 is being fed by at least seven groups, that contribute to the large number of passive galaxies outside the cluster core. More massive groups have a higher fraction of passive and Hi -poor galaxies, while low-mass groups host younger (often interacting) galaxies. For cluster galaxies not associated with groups we corroborate our previous finding that Hi gas (if any) is significantly stripped via ram-pressure during their first passage through the intracluster medium, and find mild evidence for a starburst associated with this event. In addition, we find an overabundance of morphologically peculiar and/or star-forming galaxies near the cluster core. We speculate that these arise as groups pass through the cluster (post-processing). Our study highlights the importance of environmental quenching and the complexity added by evolving environments.

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Section: Distribution Of Red Blue and Hi -Rich Galaxiessupporting

confidence: 80%

Section: Distribution Of Red Blue and Hi -Rich Galaxiesmentioning

confidence: 98%

Section: Distribution Of Red Blue and Hi -Rich Galaxiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Jaffé

Verheijen

Haines

et al. 2016

Mon. Not. R. Astron. Soc.

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112

111

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“…However, the rather extreme conditions within the gravitational potential of a galaxy cluster can work in the opposite direction as well. The ram pressure from the intracluster medium (ICM) is probably able to strip or evaporate the cold gas reservoir of galaxies (Gunn & Gott 1972;Cowie & Songaila 1977;Giovanelli & Haynes 1985;Chung et al 2009;Jaffé et al 2015) and can strongly affect the fueling of the AGN. Other studies, however, have argued that ram pressure stripping cannot be as effective in transforming blue-sequence galaxies to red (e.g.…”

Section: Introductionmentioning

confidence: 99%

The XXL Survey

Koulouridis

Poggianti

Altiéri

et al. 2016

A&A

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Context. This article belongs to the first series of XXL publications. It presents multifibre spectroscopic observations of three 0.55 deg 2 fields in the XXL Survey, which were selected on the basis of their high density of X-ray-detected clusters. The observations were obtained with the AutoFib2+WYFFOS (AF2) wide-field fibre spectrograph mounted on the 4.2 m William Herschel Telescope. Aims. The paper first describes the scientific rationale, the preparation, the data reduction, and the results of the observations, and then presents a study of active galactic nuclei (AGN) within three superclusters. Methods. To determine the redshift of galaxy clusters and AGN, we assign high priority to a) the brightest cluster galaxies (BCGs), b) the most probable cluster galaxy candidates, and c) the optical counterparts of X-ray point-like sources. We use the outcome of the observations to study the projected (2D) and the spatial (3D) overdensity of AGN in three superclusters. Results. We obtained redshifts for 455 galaxies in total, 56 of which are counterparts of X-ray point-like sources. We were able to determine the redshift of the merging supercluster XLSSC-e, which consists of six individual clusters at z ∼ 0.43, and we confirmed the redshift of supercluster XLSSC-d at z ∼ 0.3. More importantly, we discovered a new supercluster, XLSSC-f, that comprises three galaxy clusters also at z ∼ 0.3. We find a significant 2D overdensity of X-ray point-like sources only around the supercluster XLSSC-f. This result is also supported by the spatial (3D) analysis of XLSSC-f, where we find four AGN with compatible spectroscopic redshifts and possibly one more with compatible photometric redshift. In addition, we find two AGN (3D analysis) at the redshift of XLSSC-e, but no AGN in XLSSC-d. Comparing these findings with the optical galaxy overdensity we conclude that the total number of AGN in the area of the three superclusters significantly exceeds the field expectations. All of the AGN found have luminosities below 7 × 10 42 erg s −1 . Conclusions. The difference in the AGN frequency between the three superclusters cannot be explained by the present study because of small number statistics. Further analysis of a larger number of superclusters within the 50 deg 2 of the XXL is needed before any conclusions on the effect of the supercluster environment on AGN can be reached. Key words. galaxies: active -galaxies: clusters: general -X-rays: galaxies: clusters -galaxies: interactions -galaxies: evolutionlarge-scale structure of Universe Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Based on observations obtained with the William Herschel telescope during semester 13B.The Master Catalogue is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

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