We present measurements of parameters of the 3-dimensional power spectrum of galaxy clustering from 222 square degrees of early imaging data in the Sloan Digital Sky Survey .
The projected galaxy distribution on the sky is expanded over a set of Karhunen-Loève eigenfunctions , which optimize the signal-to-noise ratio in our analysis .
A maximum likelihood analysis is used to estimate parameters that set the shape and amplitude of the 3-dimensional power spectrum .
Our best estimates are \Gamma = 0.188 \pm 0.04 and \sigma _ { 8 L } = 0.915 \pm 0.06 ( statistical errors only ) , for a flat universe with a cosmological constant .
We demonstrate that our measurements contain signal from scales at or beyond the peak of the 3D power spectrum .
We discuss how the results scale with systematic uncertainties , like the radial selection function .
We find that the central values satisfy the analytically estimated scaling relation .
We have also explored the effects of evolutionary corrections , various truncations of the KL basis , seeing , sample size and limiting magnitude .
We find that the impact of most of these uncertainties stay within the 2 \sigma uncertainties of our fiducial result .