Clustering of CODEX clusters

Show full item record



Permalink

http://hdl.handle.net/10138/328220

Citation

Lindholm , V , Finoguenov , A , Comparat , J , Kirkpatrick , C C , Rykoff , E , Clerc , N , Collins , C , Damsted , S , Chitham , J I & Padilla , N 2021 , ' Clustering of CODEX clusters ' , Astronomy & Astrophysics , vol. 646 , 8 . https://doi.org/10.1051/0004-6361/202038807

Title: Clustering of CODEX clusters
Author: Lindholm, V.; Finoguenov, A.; Comparat, J.; Kirkpatrick, C. C.; Rykoff, E.; Clerc, N.; Collins, C.; Damsted, S.; Chitham, J. Ider; Padilla, N.
Other contributor: University of Helsinki, Helsinki Institute of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics

Date: 2021-01-29
Language: eng
Number of pages: 13
Belongs to series: Astronomy & Astrophysics
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/202038807
URI: http://hdl.handle.net/10138/328220
Abstract: Context. The clustering of galaxy clusters links the spatial nonuniformity of dark matter halos to the growth of the primordial spectrum of perturbations. The amplitude of the clustering signal is widely used to estimate the halo mass of astrophysical objects. The advent of cluster mass calibrations enables using clustering in cosmological studies.Aims. We analyze the autocorrelation function of a large contiguous sample of galaxy clusters, the Constrain Dark Energy with X-ray (CODEX) sample, in which we take particular care of cluster definition. These clusters were X-ray selected using the ROentgen SATellite All-Sky Survey and then identified as galaxy clusters using the code redMaPPer run on the photometry of the Sloan Digital Sky Survey. We develop methods for precisely accounting for the sample selection effects on the clustering and demonstrate their robustness using numerical simulations.Methods. Using the clean CODEX sample, which was obtained by applying a redshift-dependent richness selection, we computed the two-point autocorrelation function of galaxy clusters in the 0.1 Omega m0 = 0.22-0.03+0.04 Omega m 0 = 0 . 22 - 0.03 + 0.04 and S8 = sigma 8(Omega m0/0.3)0.5 = 0.85-0.08+0.10 S 8 = sigma 8 ( Omega m 0 / 0.3 ) 0.5 = 0 . 85 - 0.08 + 0.10 with estimated additional systematic errors of sigma Omega m0=0.02 and sigma S8=0.20. We illustrate the complementarity of clustering constraints by combining them with CODEX cosmological constraints based on the X-ray luminosity function, deriving Omega m0=0.25 +/- 0.01 and sigma (8) = 0.81(-0.02)(+0.01) sigma 8 = 0 . 81 - 0.02 + 0.01 with an estimated additional systematic error of sigma Omega m0=0.07 and sigma sigma 8=0.04. The mass calibration and statistical quality of the mass tracers are the dominant source of uncertainty.
Subject: large-scale structure of Universe
cosmology: observations
galaxies: clusters: general
COLD DARK-MATTER
LARGE-SCALE BIAS
GALAXY CLUSTERS
SPIDERS SPECTROSCOPY
HALO CONCENTRATIONS
MASS CALIBRATION
DENSITY
MODEL
ANISOTROPIES
CONSTRAINTS
115 Astronomy, Space science
Rights:


Files in this item

Total number of downloads: Loading...

Files Size Format View
aa38807_20.pdf 1.092Mb PDF View/Open

This item appears in the following Collection(s)

Show full item record