Cosmological Constraints on Ωm and σ8 from Cluster Abundances Using the GalWCat19 Optical-spectroscopic SDSS Catalog

被引：39
作者：
Abdullah, Mohamed H. [1 ,2 ]
Klypin, Anatoly [3 ,4 ]
Wilson, Gillian [1 ]
机构：
[1] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA
[2] Natl Res Inst Astron & Geophys, Dept Astron, Helwan 11421, Egypt
[3] New Mexico State Univ, Astron Dept, Las Cruces, NM 88001 USA
[4] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA
来源：
ASTROPHYSICAL JOURNAL | 2020年 / 901卷 / 02期
基金：
美国国家科学基金会;
关键词：
Cosmological parameters; Galaxy clusters; Cosmological models; Galaxy cluster counts; Large-scale structure of the universe; HALO MASS FUNCTION; GALAXY CLUSTERS; RECONSTRUCTION PROJECT; VELOCITY DISPERSIONS; SCALING RELATIONS; DARK ENERGY; SAMPLE; PARAMETERS; PROFILES; IMPACT;
D O I：
10.3847/1538-4357/aba619
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We derive cosmological constraints on the matter density, Wm, and the amplitude of fluctuations, s8, using GalWCat19, a catalog of 1800 galaxy clusters we identified in the Sloan Digital Sky Survey-DR13 spectroscopic data set using our GalWeight technique to determine cluster membership. By analyzing a subsample of 756 clusters in a redshift range of 0.045 <= z <= 0.125 and virial masses of M >= 0.8 x 10(14) h(-1) M-circle dot with mean redshift of z = 0.085, we obtain Omega(m) = -0.310(-0.027)(+0.023) +/- 0.041 (systematic) and sigma(8) = 0.810(-0.036)(+0.031) +/- 0.035 (systematic), with a cluster normalization relation of sigma(8) = 0.43 Omega(-0.55)(m). There are several unique aspects to our approach: we use the largest spectroscopic data set currently available, and we assign membership using the GalWeight technique, which we have shown to be very effective at simultaneously maximizing the number of bona fide cluster members while minimizing the number of contaminating interlopers. Moreover, rather than employing scaling relations, we calculate cluster masses individually using the virial mass estimator. Since GalWCat19 is a low-redshift cluster catalog we do not need to make any assumptions about evolution either in cosmological parameters or in the properties of the clusters themselves. Our constraints on Omega(m) and sigma(8). are consistent and very competitive with those obtained from non-cluster abundance cosmological probes such as cosmic microwave background, baryonic acoustic oscillation (BAO), and supernovae. The joint analysis of our cluster data with Planck18+BAO+Pantheon gives Omega(m) = 0.315(-0.011)(+0.013) and sigma(8) = 0.810(-0.010)(+0.011).
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页数：14
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