The XXL Survey

Pompei, E.; Adami, C.; Eckert, D.; Gastaldello, F.; Lavoie, S.; Poggianti, Bianca M.; Altiéri, B.; Aliş, Sinan; Baran, N.; Benoist, Christophe; Jaffé, Yara L.; Koulouridis, E.; Maurogordato, S.; Pacaud, F.; Pierre, M.; Sadibekova, T.; Smolčić, Vernesa; Valtchanov, I.

doi:10.1051/0004-6361/201527142

Cited by 24 publications

(23 citation statements)

References 29 publications

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“…Johnston-Hollitt et al 2008;Schirmer et al 2011;Pompei et al 2016;Einasto et al 2015). They are lower than the masses of very rich superclusters such as the Shapley supercluster, the Corona Borealis supercluster, and other very rich superclusters (Reisenegger et al 2000;Proust et al 2006;Ragone et al 2006;Pearson et al 2014;O'Mill et al 2015).…”

Section: Discussion and Summarymentioning

confidence: 96%

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Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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Context. The formation and evolution of the cosmic web is governed by the gravitational attraction of dark matter and antigravity of dark energy (cosmological constant). In the cosmic web, galaxy superclusters or their high-density cores are the largest objects that may collapse at present or during the future evolution. Aims. We study the dynamical state and possible future evolution of galaxy superclusters from the Sloan Great Wall (SGW), the richest galaxy system in the nearby Universe. Methods. We calculated supercluster masses using dynamical masses of galaxy groups and stellar masses of galaxies. We employed normal mixture modelling to study the structure of rich SGW superclusters and search for components (cores) in superclusters. We analysed the radial mass distribution in the high-density cores of superclusters centred approximately at rich clusters and used the spherical collapse model to study their dynamical state. Results. The lower limit of the total mass of the SGW is approximately M = 2.5 × 10 16 h −1 M . Different mass estimators of superclusters agree well, the main uncertainties in masses of superclusters come from missing groups and clusters. We detected three high-density cores in the richest SGW supercluster (SCl 027) and two in the second richest supercluster (SCl 019). They have masses of 1.2−5.9 × 10 15 h −1 M and sizes of up to ≈60 h −1 Mpc. The high-density cores of superclusters are very elongated, flattened perpendicularly to the line of sight. The comparison of the radial mass distribution in the high-density cores with the predictions of spherical collapse model suggests that their central regions with radii smaller than 8 h −1 Mpc and masses of up to M = 2 × 10 15 h −1 M may be collapsing. Conclusions. The rich SGW superclusters with their high-density cores represent dynamically evolving environments for studies of the properties of galaxies and galaxy systems.

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Section: Discussion and Summarymentioning

confidence: 96%

“…We also added 10% of the total mass as the mass of intercluster gas (see e.g. Pompei et al 2016). Total masses of superclusters M g tot (here g stands for both groups and gas) were obtained by summing these mass estimates.…”

Section: Masses Of Superclustersmentioning

confidence: 99%

Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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“…Early studies reported that AGN are less frequent in galaxy clusters than in the field (Osterbrock 1960;Gisler 1978;Dressler et al 1985) and more recent studies support this suggestion (Kauffmann et al 2004;Popesso & Biviano 2006;von der Linden et al 2010;Pimbblet et al 2013). Other studies, however, have found no differences between cluster and field galaxies (e.g.…”

Section: Introductionmentioning

confidence: 93%

“…all five clusters found at z ∼ 0.43 are located within a circle of 4 radius (1.3 h −1 Mpc) and a sixth but uncertain member within 10 . A more detailed analysis of the supercluster and its BCGs is presented in Pompei et al (2016, hereafter Paper VII). Baran et al (2016, hereafter Paper IX) identified several overdensities via a Voronoi Tessellation analysis of optically detected galaxies and presented new radio observations.…”

Section: Agn In Superclustersmentioning

confidence: 99%

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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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The XXL survey: First results and future

et al. 2017

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The XXL survey currently covers two 25 deg2 patches with XMM observations of ∼10 ks. We summarize the scientific results associated with the first release of the XXL dataset, which occurred in mid-2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z < 2) cluster, (z < 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-λ observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters, and the X-ray background. In particular, it will offer a unique opportunity to pinpoint the z > 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions

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The XXL Survey

Cited by 24 publications

References 29 publications

Sloan Great Wall as a complex of superclusters with collapsing cores

Sloan Great Wall as a complex of superclusters with collapsing cores

The XXL Survey

The XXL survey: First results and future

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