  The power spectrum of density fluctuations measured from galaxy redshift
surveys provides important constraints on models for the formation of
large-scale structure. I present new results for a redshift sample of 15,000
galaxies, and review the limitations of current measurements. To span the
decade of wavelength between the scales probed by galaxy surveys and COBE,
measure the detailed shape of the power spectrum, and accurately examine the
dependence of clustering on galaxy species, we require deeper samples with
carefully controlled selection criteria and improved techniques for power
spectrum estimation. I review plans for the Sloan Digital Sky Survey and
describe a new method for estimating the power spectrum that optimally treats
survey data with arbitrary geometry and sampling.
