| We present estimates of cosmological parameters from the application of the linear Karhunen-Loeve (KL) transform technique to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey (SDSS) galaxy redshifts. We use O mh and fb = O b/Om to describe the shape of the power spectrum, sL8g 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 Omh = 0.26+0.08-0.06 , fb = 0.27+0.08-0.13 , sL8g = 0.97+0.05-0.05 , and beta = 0.45+0.12-0.12 . When we take a prior on Ob from the Wilkinson Microwave Anisotropy Probe (WMAP) results, we find O mh = 0.21+0.03-0.03 , which is in excellent agreement with other measurements. Thus we have reasonably measured the gross shape of the power spectrum, but some degeneracy remains between Omh and fb because the baryon oscillations were not resolved given the survey window function at the time.; This work also describes methods for processing data within science archive databases, specifically the SDSS Catalog Archive Server (CAS), in order to prepare well-characterized samples of data that are free of survey artifacts for sensitive studies of galaxy clustering. Advanced spatial indexing systems are used to improve performance and describe the complex interactions of spherical geometric objects that describe the geometry of the survey. We also generate and use Monte Carlo random points on a cluster of database servers. These methods are combined to compress the galaxy redshift data for the first step in the linear KL algorithm. |
