The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function

F. Pacaud; N. Clerc; P. A. Giles; C. Adami; T. Sadibekova; M. Pierre; B. J. Maughan; M. Lieu; J. P. Le Fèvre; S. Alis; B. Altieri; F. Ardila; I. Baldry; C. Benoist; M. Birkinshaw; L. Chiappetti; J. Démoclès; D. Eckert; A. E. Evrard; L. Faccioli; F. Gastaldello; L. Guennou; C. Horellou; A. Iovino; E. Koulouridis; V. Le Brun; C. Lidman; J. Liske; S. Maurogordato; F. Menanteau; M. Owers; B. Poggianti; D. Pomarède; E. Pompei; T. J. Ponman; D. Rapetti; T. H. Reiprich; G. P. Smith; R. Tuffs; P. Valageas; I. Valtchanov; J. P. Willis; F. Ziparo

doi:10.1051/0004-6361/201526891

The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function

F. Pacaud, N. Clerc, P. A. Giles, C. Adami, T. Sadibekova, M. Pierre, B. J. Maughan, M. Lieu, J. P. Le Fèvre, S. Alis, B. Altieri, F. Ardila, I. Baldry, C. Benoist, M. Birkinshaw, L. Chiappetti, J. Démoclès, D. Eckert, A. E. Evrard, L. FaccioliF. Gastaldello, L. Guennou, C. Horellou, A. Iovino, E. Koulouridis, V. Le Brun, C. Lidman, J. Liske, S. Maurogordato, F. Menanteau, M. Owers, B. Poggianti, D. Pomarède, E. Pompei, T. J. Ponman, D. Rapetti, T. H. Reiprich, G. P. Smith, R. Tuffs, P. Valageas, I. Valtchanov, J. P. Willis, F. Ziparo

Research output: Contribution to journal › Review article › peer-review

Abstract

Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ∼2 at a sensitivity of ∼10^-14 erg s^-1 cm^-2 in the [0.5-2] keV band. Aims. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10^-14 erg s^-1 cm^-2 on the source flux within a 1' aperture. Methods. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results. The bright cluster sample consists of systems with masses between M₅₀₀ = 7 × 10¹³ and 3 × 10¹⁴ M_⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ₈ and/or Ω_M appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ∼1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters.

Original language	English (US)
Article number	A2
Journal	Astronomy and Astrophysics
Volume	592
DOIs	https://doi.org/10.1051/0004-6361/201526891
State	Published - 2016

Keywords

Cosmological parameters
Galaxies: clusters: intracluster medium
Large-scale structure of Universe
Surveys
X-rays: galaxies: clusters

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Online availability

10.1051/0004-6361/201526891

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Pacaud, F., Clerc, N., Giles, P. A., Adami, C., Sadibekova, T., Pierre, M., Maughan, B. J., Lieu, M., Le Fèvre, J. P., Alis, S., Altieri, B., Ardila, F., Baldry, I., Benoist, C., Birkinshaw, M., Chiappetti, L., Démoclès, J., Eckert, D., Evrard, A. E., ... Ziparo, F. (2016). The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function. Astronomy and Astrophysics, 592, Article A2. https://doi.org/10.1051/0004-6361/201526891

Pacaud, F, Clerc, N, Giles, PA, Adami, C, Sadibekova, T, Pierre, M, Maughan, BJ, Lieu, M, Le Fèvre, JP, Alis, S, Altieri, B, Ardila, F, Baldry, I, Benoist, C, Birkinshaw, M, Chiappetti, L, Démoclès, J, Eckert, D, Evrard, AE, Faccioli, L, Gastaldello, F, Guennou, L, Horellou, C, Iovino, A, Koulouridis, E, Le Brun, V, Lidman, C, Liske, J, Maurogordato, S, Menanteau, F, Owers, M, Poggianti, B, Pomarède, D, Pompei, E, Ponman, TJ, Rapetti, D, Reiprich, TH, Smith, GP, Tuffs, R, Valageas, P, Valtchanov, I, Willis, JP & Ziparo, F 2016, 'The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function', Astronomy and Astrophysics, vol. 592, A2. https://doi.org/10.1051/0004-6361/201526891

@article{0938b29a341947678731d96eed90c46f,

title = "The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function",

abstract = "Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ∼2 at a sensitivity of ∼10-14 erg s-1 cm-2 in the [0.5-2] keV band. Aims. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10-14 erg s-1 cm-2 on the source flux within a 1' aperture. Methods. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results. The bright cluster sample consists of systems with masses between M500 = 7 × 1013 and 3 × 1014 M⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ∼1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters.",

keywords = "Cosmological parameters, Galaxies: clusters: intracluster medium, Large-scale structure of Universe, Surveys, X-rays: galaxies: clusters",

author = "F. Pacaud and N. Clerc and Giles, {P. A.} and C. Adami and T. Sadibekova and M. Pierre and Maughan, {B. J.} and M. Lieu and {Le F{\`e}vre}, {J. P.} and S. Alis and B. Altieri and F. Ardila and I. Baldry and C. Benoist and M. Birkinshaw and L. Chiappetti and J. D{\'e}mocl{\`e}s and D. Eckert and Evrard, {A. E.} and L. Faccioli and F. Gastaldello and L. Guennou and C. Horellou and A. Iovino and E. Koulouridis and {Le Brun}, V. and C. Lidman and J. Liske and S. Maurogordato and F. Menanteau and M. Owers and B. Poggianti and D. Pomar{\`e}de and E. Pompei and Ponman, {T. J.} and D. Rapetti and Reiprich, {T. H.} and Smith, {G. P.} and R. Tuffs and P. Valageas and I. Valtchanov and Willis, {J. P.} and F. Ziparo",

note = "Publisher Copyright: {\textcopyright} ESO, 2016.",

year = "2016",

doi = "10.1051/0004-6361/201526891",

language = "English (US)",

volume = "592",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - The XXL Survey

T2 - II. the bright cluster sample: Catalogue and luminosity function

AU - Pacaud, F.

AU - Clerc, N.

AU - Giles, P. A.

AU - Adami, C.

AU - Sadibekova, T.

AU - Pierre, M.

AU - Maughan, B. J.

AU - Lieu, M.

AU - Le Fèvre, J. P.

AU - Alis, S.

AU - Altieri, B.

AU - Ardila, F.

AU - Baldry, I.

AU - Benoist, C.

AU - Birkinshaw, M.

AU - Chiappetti, L.

AU - Démoclès, J.

AU - Eckert, D.

AU - Evrard, A. E.

AU - Faccioli, L.

AU - Gastaldello, F.

AU - Guennou, L.

AU - Horellou, C.

AU - Iovino, A.

AU - Koulouridis, E.

AU - Le Brun, V.

AU - Lidman, C.

AU - Liske, J.

AU - Maurogordato, S.

AU - Menanteau, F.

AU - Owers, M.

AU - Poggianti, B.

AU - Pomarède, D.

AU - Pompei, E.

AU - Ponman, T. J.

AU - Rapetti, D.

AU - Reiprich, T. H.

AU - Smith, G. P.

AU - Tuffs, R.

AU - Valageas, P.

AU - Valtchanov, I.

AU - Willis, J. P.

AU - Ziparo, F.

PY - 2016

Y1 - 2016

N2 - Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ∼2 at a sensitivity of ∼10-14 erg s-1 cm-2 in the [0.5-2] keV band. Aims. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10-14 erg s-1 cm-2 on the source flux within a 1' aperture. Methods. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results. The bright cluster sample consists of systems with masses between M500 = 7 × 1013 and 3 × 1014 M⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ∼1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters.

AB - Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ∼2 at a sensitivity of ∼10-14 erg s-1 cm-2 in the [0.5-2] keV band. Aims. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10-14 erg s-1 cm-2 on the source flux within a 1' aperture. Methods. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results. The bright cluster sample consists of systems with masses between M500 = 7 × 1013 and 3 × 1014 M⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ∼1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters.

KW - Cosmological parameters

KW - Galaxies: clusters: intracluster medium

KW - Large-scale structure of Universe

KW - Surveys

KW - X-rays: galaxies: clusters

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UR - http://www.scopus.com/inward/citedby.url?scp=84975514127&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201526891

DO - 10.1051/0004-6361/201526891

M3 - Review article

AN - SCOPUS:84975514127

SN - 0004-6361

VL - 592

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A2

ER -

The XXL Survey: II. the bright cluster sample: Catalogue and luminosity function

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