| © CAMBRIDGE UNIVERSITY PRESS 1999
| |
The observed mass function (MF), n( > M), of clusters of galaxies, which describes the number density of clusters above a threshold mass M, can be used as a critical test of theories of structure formation in the universe. The richest, most massive clusters are thought to form from rare high peaks in the initial mass-density fluctuations; poorer clusters and groups form from smaller, more common fluctuations. Bahcall and Cen (1993) determined the MF of clusters of galaxies using both optical and X-ray observations of clusters. Their MF is presented in Figure 5. The function is well fit by the analytic expression
| (50) |
with M* = (1.8 ± 0.3) ×
1014h-1
M
,
(where the mass M represents the cluster mass within
1.5h-1 Mpc radius).
|
Figure 5. Cluster mass functions from observations and from CDM dimulations (Bahcall and Cen 1992). |
The observed cluster mass function is compared in
Figure 5 with expectations from different
cold-dark-matter cosmologies using large-scale simulations
(Bahcall and Cen 1992).
The comparison shows that the cluster MF is indeed a
powerful discriminant among models. The standard CDM model
(
m = 1)
cannot reproduce the observed MF for any bias parameter; when
normalized to the COBE microwave background fluctuations on large
scales, this model produces too many massive clusters, unseen by the
observations. A low-density CDM model on the other hand, with
m ~
0.2-0.3 (with or without a cosmological constant),
appears to fit well the observed cluster MF
(Fig. 5).