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The SRG/eROSITA All-Sky Survey
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-12 , DOI: 10.1051/0004-6361/202348843 R. Seppi , J. Comparat , V. Ghirardini , C. Garrel , E. Artis , A. G. Sánchez , A. Liu , N. Clerc , E. Bulbul , S. Grandis , M. Kluge , T. H. Reiprich , A. Merloni , X. Zhang , Y. E. Bahar , S. Shreeram , J. Sanders , M. Ramos-Ceja , M. Krumpe
Astronomy & Astrophysics ( IF 5.4 ) Pub Date : 2024-06-12 , DOI: 10.1051/0004-6361/202348843 R. Seppi , J. Comparat , V. Ghirardini , C. Garrel , E. Artis , A. G. Sánchez , A. Liu , N. Clerc , E. Bulbul , S. Grandis , M. Kluge , T. H. Reiprich , A. Merloni , X. Zhang , Y. E. Bahar , S. Shreeram , J. Sanders , M. Ramos-Ceja , M. Krumpe
Context. The spatial distribution of galaxy clusters provides a reliable tracer of the large-scale distribution of matter in the Universe. The clustering signal depends on intrinsic cluster properties and cosmological parameters.Aims. The ability of eROSITA on board Spectrum-Roentgen-Gamma (SRG) to discover galaxy clusters allows the association of extended X-ray emission with dark matter haloes to be probed. We measured the projected two-point correlation function to study the occupation of dark matter haloes by clusters and groups detected by the first eROSITA all-sky survey (eRASS1).Methods. We created five volume-limited samples probing clusters with different redshifts and X-ray luminosity values. We interpreted the correlation function with halo occupation distribution (HOD) and halo abundance matching (HAM) models. We simultaneously fit the cosmological parameters and halo bias of a flux-limited sample of 6493 clusters with purity > 96%.Results. We obtained a detailed view of the halo occupation for eRASS1 clusters. The fainter population at low redshift (S0: erg s−1, 0.1 < z < 0.2) is the least biased compared to dark matter, with b = 2.95 ± 0.21. The brightest clusters up to higher redshift (S4: erg s−1, 0.1 < z < 0.6) exhibit a higher bias b = 4.34 ± 0.62. Satellite groups are rare, with a satellite fraction < 14.9% (8.1) for the S0 (S4) sample. We combined the HOD prediction with a HAM procedure to constrain the scaling relation between LX and mass in a new way, and find a scatter of ⟨σLx⟩ = 0.36. We obtain cosmological constraints for the physical cold dark matter density and an average halo bias .Conclusions. We modelled the clustering of galaxy clusters with a HOD approach for the first time, paving the way for future studies combining eROSITA with 4MOST, SDSS, Euclid, Rubin, and DESI to unravel the cluster distribution in the Universe.
中文翻译：
SRG/eROSITA 全天巡天
语境。星系团的空间分布为宇宙中物质的大规模分布提供了可靠的示踪剂。聚类信号取决于内在的聚类特性和宇宙学参数。目的。光谱伦琴伽玛 (SRG) 上的 eROSITA 能够发现星系团，从而可以探测扩展 X 射线发射与暗物质晕的关联。我们测量了投影的两点相关函数，以研究首次 eROSITA 全天空巡天 (eRASS1) 检测到的星团和群对暗物质晕的占据。方法。我们创建了五个具有不同红移和 X 射线光度值的体积有限的样本探测簇。我们用光环占据分布（HOD）和光环丰度匹配（HAM）模型解释了相关函数。我们同时拟合了纯度 > 96% 的 6493 个星团的通量限制样本的宇宙学参数和光晕偏差。结果。我们获得了 eRASS1 簇晕占据的详细视图。低红移处较暗的群体（S0：erg s −1, 0.1 < z < 0.2) is the least biased compared to dark matter, with b = 2.95 ± 0.21. The brightest clusters up to higher redshift (S4: erg s−1, 0.1 < z < 0.6) exhibit a higher bias b = 4.34 ± 0.62. Satellite groups are rare, with a satellite fraction < 14.9% (8.1) for the S0 (S4) sample. We combined the HOD prediction with a HAM procedure to constrain the scaling relation between LX and mass in a new way, and find a scatter of ⟨σLx⟩ = 0.36. We obtain cosmological constraints for the physical cold dark matter density and an average halo bias .Conclusions. We modelled the clustering of galaxy clusters with a HOD approach for the first time, paving the way for future studies combining eROSITA with 4MOST, SDSS, Euclid, Rubin, and DESI to unravel the cluster distribution in the Universe.
更新日期：2024-06-12
中文翻译：
SRG/eROSITA 全天巡天
语境。星系团的空间分布为宇宙中物质的大规模分布提供了可靠的示踪剂。聚类信号取决于内在的聚类特性和宇宙学参数。目的。光谱伦琴伽玛 (SRG) 上的 eROSITA 能够发现星系团，从而可以探测扩展 X 射线发射与暗物质晕的关联。我们测量了投影的两点相关函数，以研究首次 eROSITA 全天空巡天 (eRASS1) 检测到的星团和群对暗物质晕的占据。方法。我们创建了五个具有不同红移和 X 射线光度值的体积有限的样本探测簇。我们用光环占据分布（HOD）和光环丰度匹配（HAM）模型解释了相关函数。我们同时拟合了纯度 > 96% 的 6493 个星团的通量限制样本的宇宙学参数和光晕偏差。结果。我们获得了 eRASS1 簇晕占据的详细视图。低红移处较暗的群体（S0：erg s −1, 0.1 < z < 0.2) is the least biased compared to dark matter, with b = 2.95 ± 0.21. The brightest clusters up to higher redshift (S4: erg s−1, 0.1 < z < 0.6) exhibit a higher bias b = 4.34 ± 0.62. Satellite groups are rare, with a satellite fraction < 14.9% (8.1) for the S0 (S4) sample. We combined the HOD prediction with a HAM procedure to constrain the scaling relation between LX and mass in a new way, and find a scatter of ⟨σLx⟩ = 0.36. We obtain cosmological constraints for the physical cold dark matter density and an average halo bias .Conclusions. We modelled the clustering of galaxy clusters with a HOD approach for the first time, paving the way for future studies combining eROSITA with 4MOST, SDSS, Euclid, Rubin, and DESI to unravel the cluster distribution in the Universe.
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