I present a new method for extracting\ power\ spectra from galaxy\ redshift\ surveys called the pair weight compression method. I then apply the method to determine the\ redshift\ power\ spectrum\ of the\ Las\ Campanas\ Redshift\ Survey\ (LCRS). The measured\ redshift\ power\ spectrum\ has the same shape as that found by Lin et al. (1996b) but is a factor of 2 smaller. Upon expanding the method to include linear\ redshift\ distortions, the method is able to measure real space\ power\ spectra and β. β ≈ Ωm0.6/b where β is the linear\ redshift\ distortion parameter, Ωm is the cosmological density of matter and b is the linear galaxy to mass "bias factor."\ Applying the method to LCRS yields a real space\ power\ spectrum\ that is very similar to the\ redshift\ space\ power\ spectrum. The measured value of β ≈.55+.35-.30\ is larger than, but consistent with, a previous measurement by Matsubara et al. (2000).
N2 -I present a new method for extracting\ power\ spectra from galaxy\ redshift\ surveys called the pair weight compression method. I then apply the method to determine the\ redshift\ power\ spectrum\ of the\ Las\ Campanas\ Redshift\ Survey\ (LCRS). The measured\ redshift\ power\ spectrum\ has the same shape as that found by Lin et al. (1996b) but is a factor of 2 smaller. Upon expanding the method to include linear\ redshift\ distortions, the method is able to measure real space\ power\ spectra and β. β ≈ Ωm0.6/b where β is the linear\ redshift\ distortion parameter, Ωm is the cosmological density of matter and b is the linear galaxy to mass "bias factor."\ Applying the method to LCRS yields a real space\ power\ spectrum\ that is very similar to the\ redshift\ space\ power\ spectrum. The measured value of β ≈.55+.35-.30\ is larger than, but consistent with, a previous measurement by Matsubara et al. (2000).
PB - University of Colorado Boulder PY - 2000 TI - Measurements of the Power Spectrum and Redshift Distortions of the Las Campanas Redshift Survey ER -