  We discuss probability distributions for the cosmological constant Lambda and
the amplitude of primordial density fluctuations Q in models where they both
are anthropic variables. With mild assumptions about the prior probabilities,
the distribution P(Lambda,Q) factorizes into two independent distributions for
the variables Q and $y \propto \Lambda/Q^3$. The distribution for y is largely
model-independent and is in a good agreement with the observed value of y. The
form of P(Q) depends on the origin of density perturbations. If the
perturbations are due to quantum fluctuations of the inflaton, then P(Q) tends
to have an exponential dependence on Q, due to the fact that in such models Q
is correlated with the amount of inflationary expansion. For simple models with
a power-law potential, P(Q) is peaked at very small values of Q, far smaller
than the observed value of 10^{-5}. This problem does not arise in
curvaton-type models, where the inflationary expansion factor is not correlated
with Q.
