  We present estimates of cosmological parameters from the application of the
Karhunen-Loeve transform to the analysis of the 3D power spectrum of density
fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Omega_m*h
and f_b = Omega_b/Omega_m to describe the shape of the power spectrum, sigma8
for the (linearly extrapolated) normalization, and beta to parametrize linear
theory redshift space distortions. On scales k < 0.16 h/Mpc, our maximum
likelihood values are Omega_m*h = 0.264 +/-0.043, f_b = 0.286 +/- 0.065, sigma8
= 0.966 +/- 0.048, and beta = 0.45 +/- 0.12. When we take a prior on Omega_b
from WMAP, we find Omega_m*h = 0.207 +/- 0.030, which is in excellent agreement
with WMAP and 2dF. This indicates that we have reasonably measured the gross
shape of the power spectrum but we have difficulty breaking the degeneracy
between Omega_m*h and f_b because the baryon oscillations are not resolved in
the current spectroscopic survey window function.
