The power spectrum of density fluctuations measured from galaxy redshift
surveys provides important constraints on models for the formation of
large-scale structure. I review current results for the 3-D power spectrum and
examine the limitations of current measurements and estimation techniques. 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 describe a new method for estimating the power spectrum
that optimally treats survey data with arbitrary geometry and sampling.Comment: 10 pages, uuencoded compressed postscript. To appear in ``Clustering
in the Universe,'' Proc. of XXXth Moriond Conference, Les Arcs, France, March
11-18, 199
