3.2 Galaxy Power-Spectrum
The power-spectrum (PS) of galaxies in redshift space has been
computed for a number of optical (e.g.,
Park et al. 1992,
Park et al. 1994,
da Costa et al. 1994b,
Lin et al. 1996b)
and infrared surveys
(Fisher et al. 1993).
The redshift-space PS estimates roughly
follow a power-law P (k) kn with a
slope ranging from n ~
-2 on small scales (
30
h-1 Mpc) to n ~ -1.1 on
intermediate scales (30 h-1 <
< 120
h-1 Mpc). For nearby samples,
such as the combined CfA2-SSRS2, one finds that the PS continues to
rise on scales up to ~ 200 h-1 Mpc. This result has been
confirmed by similar analysis of other optical and infrared-selected
samples, all showing essentially the same shape, while differences in
the amplitude can be ascribed to the relative bias between optically
and infrared-selected galaxies or between galaxies of different
luminosities. These earlier results have been confirmed by the PS
computed from the LCRS which shows good agreement with previous
calculations on scales
100 h-1 Mpc. On larger scales, the LCRS
PS shows a change in slope and strongly suggests that it has detected
the turnover. A good fit for the observed PS in redshift space,
satisfying the constraints implied by COBE, can be obtained with a
open or flat nonzero cosmological constant CDM model with a shape
parameter
=
h = 0.2 with no
bias. However, several other
models are equally viable
(da Costa et
al. 1994b,
Lin et al. 1996b).