Abstract: On large scales, the clustering of galaxies is dependent on cosmological parameters. In this talk, I will discuss one method of quantizing this clustering which is the angular power spectrum, calculated using quadratic estimation of the maximum likelihood function, and its application to the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) galaxies. To apply this method to discrete galaxies, we pixelize the sky using HEALpix and perform Karhunen-Loeve Compression, which is a transformation of pixelized overdensities into a signal-to-noise eigenmode basis. I will present the results of the angular power spectrum analysis of all galaxies in the SDSS DR7 North Galactic Cap ellipse from magnitudes 18-21, as well as a volume-limited sample of galaxies from 0.0<z<0.4 split by type, and the cosmological parameters we have obtained by fitting these observed angular power spectra to the projection of theoretical linear power spectra.