| | |
| | |
Stat |
Members: 3645 Articles: 2'504'928 Articles rated: 2609
26 April 2024 |
|
| | | |
|
Article overview
| |
|
Scale Invariance of Rich Cluster Abundance: A Possible Test for Models of Structure Formation | Wen Xu
; Li-Zhi Fang
; Xiang-Ping Wu
; | Date: |
27 Jun 1998 | Journal: | Astrophys.J. 508 (1998) 472 | Subject: | astro-ph | Abstract: | We investigate the dependence of cluster abundance $n(>M,r_{cl})$, i.e., the number density of clusters with mass larger than $M$ within radius $r_{cl}$, on scale parameter $r_{cl}$. Using numerical simulations of clusters in the CDM cosmogonic theories, we notice that the abundance of rich clusters shows a simple scale invariance such that $n[>(r_{cl}/r_0)^{alpha}M, r_{cl}]= n(>M,r_0)$, in which the scaling index $alpha$ remains constant in a scale range where halo clustering is fully developed. The abundances of scale $r_{cl}$ clusters identified from IRAS are found basically to follow this scaling, and yield $alpha sim 0.5$ in the range $1.5 < r_{cl} < 4 h^{-1}$Mpc. The scaling gains further supports from independent measurements of the index $alpha$ using samples of X-ray and gravitational lensing mass estimates. We find that all the results agree within error limit as: $alpha sim 0.5 - 0.7$ in the range of $1.5 < r_{cl} < 4 h^{-1}$Mpc. These numbers are in good consistency with the predictions of OCDM ($Omega_M=0.3$) and LCDM ($Omega_M+Omega_{Lambda} =1$), while the standard CDM model has different behavior. The current result seems to favor models with a low mass density. | Source: | arXiv, astro-ph/9806361 | Services: | Forum | Review | PDF | Favorites |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
| News, job offers and information for researchers and scientists:
| |