10.2. The equation of state of the vacuum
So far, we have assumed that the vacuum energy is exactly
a classical , or
at any rate indistinguishable from
one. This is a highly reasonable prior: there is no reason
for the asymptotic value of any potential to go exactly
to zero, so one always needs to solve the classical cosmological
constant problem - for which probably the only reasonable
explanation is an anthropic one (e.g.
Vilenkin 2001).
Therefore, dynamical provision of
w
pv /
v
- 1
is not needed. Nevertheless, one can readily take an
empirical approach to w (treated as a constant for
a first approach).
Figure 22 shows a simplified approach to this,
plotting the locus on (w,
m) space
that is required for
a given value of h if the location of the main CMB acoustic peak
is known exactly. For
h
0.7, this is
very similar to the locus derived from the SN Hubble diagram
(Garnavich et al. 1998).
The solid circles show the updated 2dFGRS constraint of
mh
= 0.18. In order to match the data with w closer to zero,
m must
increase and h must
decrease. The latter trend means that the HST Hubble constant
sets an upper limit to w of about -0.54
(Percival et al. 2002).
This is very similar to the SNe constraint of
Garnavich et al. (1998),
so the combined limit is already close to w < - 0.8. The vacuum
energy is indeed looking rather similar to
.