TY - JOUR
T1 - The XXL Survey
T2 - XXV. Cosmological analysis of the C1 cluster number counts
AU - Pacaud, F.
AU - Pierre, M.
AU - Melin, J. B.
AU - Adami, C.
AU - Evrard, A. E.
AU - Galli, S.
AU - Gastaldello, F.
AU - Maughan, B. J.
AU - Sereno, M.
AU - Alis, S.
AU - Altieri, B.
AU - Birkinshaw, M.
AU - Chiappetti, L.
AU - Faccioli, L.
AU - Giles, P. A.
AU - Horellou, C.
AU - Iovino, A.
AU - Koulouridis, E.
AU - Le Fèvre, J. P.
AU - Lidman, C.
AU - Lieu, M.
AU - Maurogordato, S.
AU - Moscardini, L.
AU - Plionis, M.
AU - Poggianti, B. M.
AU - Pompei, E.
AU - Sadibekova, T.
AU - Valtchanov, I.
AU - Willis, J. P.
PY - 2018/12
Y1 - 2018/12
N2 - Context. We present an estimation of cosmological parameters with clusters of galaxies. Aims. We constrain the Ωm, σ8, and w parameters from a stand-alone sample of X-ray clusters detected in the 50 deg2 XMM-XXL survey with a well-defined selection function. Methods. We analyse the redshift distribution of a sample comprising 178 high signal-to-noise ratio clusters out to a redshift of unity. The cluster sample scaling relations are determined in a self-consistent manner. Results. In a lambda cold dark matter (ΛCDM) model, the cosmology favoured by the XXL clusters compares well with results derived from the Planck Sunyaev-Zel'dovich clusters for a totally different sample (mass/redshift range, selection biases, and scaling relations). However, with this preliminary sample and current mass calibration uncertainty, we find no inconsistency with the Planck CMB cosmology. If we relax the w parameter, the Planck CMB uncertainties increase by a factor of ~10 and become comparable with those from XXL clusters. Combining the two probes allows us to put constraints on Ωm = 0.316 ± 0.060, σ8 = 0.814 ± 0.054, and w = -1.02 ± 0.20. Conclusions. This first self-consistent cosmological analysis of a sample of serendipitous XMM clusters already provides interesting insights into the constraining power of the XXL survey. Subsequent analysis will use a larger sample extending to lower confidence detections and include additional observable information, potentially improving posterior uncertainties by roughly a factor of 3.
AB - Context. We present an estimation of cosmological parameters with clusters of galaxies. Aims. We constrain the Ωm, σ8, and w parameters from a stand-alone sample of X-ray clusters detected in the 50 deg2 XMM-XXL survey with a well-defined selection function. Methods. We analyse the redshift distribution of a sample comprising 178 high signal-to-noise ratio clusters out to a redshift of unity. The cluster sample scaling relations are determined in a self-consistent manner. Results. In a lambda cold dark matter (ΛCDM) model, the cosmology favoured by the XXL clusters compares well with results derived from the Planck Sunyaev-Zel'dovich clusters for a totally different sample (mass/redshift range, selection biases, and scaling relations). However, with this preliminary sample and current mass calibration uncertainty, we find no inconsistency with the Planck CMB cosmology. If we relax the w parameter, the Planck CMB uncertainties increase by a factor of ~10 and become comparable with those from XXL clusters. Combining the two probes allows us to put constraints on Ωm = 0.316 ± 0.060, σ8 = 0.814 ± 0.054, and w = -1.02 ± 0.20. Conclusions. This first self-consistent cosmological analysis of a sample of serendipitous XMM clusters already provides interesting insights into the constraining power of the XXL survey. Subsequent analysis will use a larger sample extending to lower confidence detections and include additional observable information, potentially improving posterior uncertainties by roughly a factor of 3.
KW - Cosmological parameters
KW - Galaxies: clusters: intracluster medium
KW - Large-scale structure of Universe
KW - Surveys
KW - X-rays: galaxies: clusters
UR - http://www.scopus.com/inward/record.url?scp=85057331959&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201834022
DO - 10.1051/0004-6361/201834022
M3 - Review article (Academic Journal)
AN - SCOPUS:85057331959
SN - 0004-6361
VL - 620
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A10
ER -