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Abundances and Correlations of Structures Beyond Galaxy Clusters
Astrophysics · Submitted 13 May 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Therefore, the ``universal'' increase of the correlation amplitude with the scale of objects from galaxies, groups, to poor, rich clusters is broken down for structures of $r_{cl} > 3 - 4 h^{-1}$ Mpc.
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We investigated the structures on scales beyond the typical clusters of galaxies. These structures are crucial to understand the cosmic gravitational clustering in the pre-virialized stage, or quasilinear r\`egime. Based on the multi-resolution analysis of the discrete wavelet transformation, we got statistical available ensembles of $r_{cl}$-clusters, i.e. the structures on scale $r_{cl}$, in the range $1 \leq r_{cl} \leq 24 h^{-1}$ Mpc for both N-body simulation and the IRAS 1.2 Jy galaxy survey samples. If the mass-to-light ratio on scales larger than clusters asymptotically reaches a constant, we found that the abundances and correlations of these IRAS $r_{cl}$-clusters to be basically consistent with the predictions of the flat low-density CDM model (LCDM) and the open CDM model (OCDM), except the model-predicted abundance of $r_{cl} = 24 h^{-1}$ Mpc clusters seems to be higher than IRAS data. The standard CDM (SCDM) gives too much power, and too weak correlations on all the scales. For a given $r_{cl}$, the amplitude of two-point correlation function of $r_{cl}$-clusters is increasing with their richness. However, for a given richness (defined by the mean separation of neighbor objects), the clustering strengths of both simulation and observation sample are found to be declining with $r_{cl}$ when $r_{cl}$ is larger than 3 - 4 $h^{-1}$ Mpc. Therefore, the ``universal'' increase of the correlation amplitude with the scale of objects from galaxies, groups, to poor, rich clusters is broken down for structures of $r_{cl} > 3 - 4 h^{-1}$ Mpc. Supercluster should not be a member of the ``universal'' increase family.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We investigated the structures on scales beyond the typical clusters of galaxies. | contribution 0.92 | 0.94 | 0.02 | asserted 0.89 |
| s1 | These structures are crucial to understand the cosmic gravitational clustering in the pre-virialized stage, or quasilinear r\`egime. | background 0.98 | 0.08 | 0.04 | asserted 1.00 |
| s2 | Based on the multi-resolution analysis of the discrete wavelet transformation, we got statistical available ensembles of $r_{cl}$-clusters, i.e. the structures on scale $r_{cl}$, in the range $1 \leq r_{cl} \leq 24 h^{-1}$ Mpc for both N-body simulation and the IRAS 1.2 Jy galaxy survey samples. | method 0.77 | 0.96 | 0.06 | asserted 1.00 |
| s3 | If the mass-to-light ratio on scales larger than clusters asymptotically reaches a constant, we found that the abundances and correlations of these IRAS $r_{cl}$-clusters to be basically consistent with the predictions of the flat low-density CDM model (LCDM) and the open CDM model (OCDM), except the model-predicted abundance of $r_{cl} = 24 h^{-1}$ Mpc clusters seems to be higher than IRAS data. | result 0.98 | 0.95 | 0.41 | asserted 0.56 |
| s4 | The standard CDM (SCDM) gives too much power, and too weak correlations on all the scales. | result 0.96 | 0.71 | 0.08 | asserted 1.00 |
| s5 | For a given $r_{cl}$, the amplitude of two-point correlation function of $r_{cl}$-clusters is increasing with their richness. | result 1.00 | 0.90 | 0.07 | asserted 1.00 |
| s6 | However, for a given richness (defined by the mean separation of neighbor objects), the clustering strengths of both simulation and observation sample are found to be declining with $r_{cl}$ when $r_{cl}$ is larger than 3 - 4 $h^{-1}$ Mpc. | result 1.00 | 0.96 | 0.17 | asserted 1.00 |
| s7 | Therefore, the ``universal'' increase of the correlation amplitude with the scale of objects from galaxies, groups, to poor, rich clusters is broken down for structures of $r_{cl} > 3 - 4 h^{-1}$ Mpc. | interpretation 0.90 | 0.85 | 0.56 | asserted 1.00 |
| s8 | Supercluster should not be a member of the ``universal'' increase family. | interpretation 0.98 | 0.65 | 0.35 | asserted 1.00 |
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Original abstract
We investigated the structures on scales beyond the typical clusters of galaxies. These structures are crucial to understand the cosmic gravitational clustering in the pre-virialized stage, or quasilinear r\`egime. Based on the multi-resolution analysis of the discrete wavelet transformation, we got statistical available ensembles of $r_{cl}$-clusters, i.e. the structures on scale $r_{cl}$, in the range $1 \leq r_{cl} \leq 24 h^{-1}$ Mpc for both N-body simulation and the IRAS 1.2 Jy galaxy survey samples. If the mass-to-light ratio on scales larger than clusters asymptotically reaches a constant, we found that the abundances and correlations of these IRAS $r_{cl}$-clusters to be basically consistent with the predictions of the flat low-density CDM model (LCDM) and the open CDM model (OCDM), except the model-predicted abundance of $r_{cl} = 24 h^{-1}$ Mpc clusters seems to be higher than IRAS data. The standard CDM (SCDM) gives too much power, and too weak correlations on all the scales. For a given $r_{cl}$, the amplitude of two-point correlation function of $r_{cl}$-clusters is increasing with their richness. However, for a given richness (defined by the mean separation of neighbor objects), the clustering strengths of both simulation and observation sample are found to be declining with $r_{cl}$ when $r_{cl}$ is larger than 3 - 4 $h^{-1}$ Mpc. Therefore, the ``universal'' increase of the correlation amplitude with the scale of objects from galaxies, groups, to poor, rich clusters is broken down for structures of $r_{cl} > 3 - 4 h^{-1}$ Mpc. Supercluster should not be a member of the ``universal'' increase family.
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