Cosmological constraints from the abundance, weak lensing, and clustering of galaxy clusters: Application to the SDSS

被引:21
作者
Fumagalli, A. [1 ,2 ,3 ,4 ]
Costanzi, M. [1 ,2 ,3 ]
Saro, A. [1 ,2 ,3 ,5 ,6 ]
Castro, T. [2 ,3 ,5 ,6 ]
Borgani, S. [1 ,2 ,3 ,5 ,6 ]
机构
[1] Univ Trieste, Dipartimento Fis, Sez Astron, Via Tiepolo 11, I-34131 Trieste, Italy
[2] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy
[3] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy
[4] Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany
[5] INFN Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy
[6] ICSC Ctr Nazl Ric High Performance Comp Big Data &, Via Magnanelli 2, Bologna, Italy
基金
欧洲研究理事会;
关键词
galaxies: clusters: general; cosmological parameters; large-scale structure of Universe; LARGE-SCALE BIAS; MASS-RICHNESS RELATION; DARK ENERGY; NUMBER COUNTS; CALIBRATION; IMPACT; VARIANCE; SAMPLE; COVARIANCE; GENERATION;
D O I
10.1051/0004-6361/202348296
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. The clustering of galaxy clusters is a powerful cosmological tool. When it is combined with other cosmological observables, it can help to resolve parameter degeneracies and improve constraints, especially on Omega(m) and sigma(8). We aim to demonstrate its potential in constraining cosmological parameters and scaling relations when combined with cluster counts and weak-lensing mass information. As a case study, we use the redMaPPer cluster catalog derived from the Sloan Digital Sky Survey (SDSS). Methods. We extended a previous analysis of the number counts and weak-lensing signal by the two-point correlation function. We derived cosmological and scaling relation posteriors for all possible combinations of the three observables to assess their constraining power, parameter degeneracies, and possible internal tensions. Results. We find no evidence for tensions between the three data sets we analyzed. We demonstrate that the constraining power of the sample can be greatly improved by including the clustering statistics because this can break the Omega(m) - sigma(8) degeneracy that is characteristic of cluster abundance studies. In particular, for a flat Lambda CDM model with massive neutrinos, we obtain Omega(m) = 0.28 +/- 0.03 and sigma(8) = 0.82 +/- 0.05, which is an improvement of 33% and 50% compared to the posteriors derived by combining cluster abundance and weak-lensing analyses. Our results are consistent with cosmological posteriors from other cluster surveys, and also with Planck results for the cosmic microwave background (CMB) and DES-Y3 galaxy clustering and weak-lensing analysis.
引用
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页数:16
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