The Power Spectrum of Galaxy Clustering in the Las Campanas Redshift Survey

Abstract

The Las Campanas Redshift Survey (LCRS) contains 23697 galaxies, with an average redshift $z = 0.1$, distributed over six $1.5\arcdeg$ by $80\arcdeg$ slices in the North and South galactic caps. We have computed the power spectrum $P(k)$ for LCRS galaxies over wavelengths $λ= 2π/ k = 5 - 400\ h^{-1}$~Mpc. The LCRS $P(k)$ may be approximated as $\propto k^{-1.8 \pm 0.1}$ for small scales $λ= 5 - 30\ h^{-1}$~Mpc, changing to $\propto k^{1 \pm 1}$ for large scales $λ\approx 200 - 400\ h^{-1}$~Mpc. The overall amplitude corresponds to $σ_8 = 1.0 \pm 0.1$ in redshift space. Comparisons to the power spectra of other redshift surveys will be presented; the LCRS results agree best with those from the combined Center for Astrophysics and Southern Sky redshift surveys. We find evidence for type- dependent clustering differences in the LCRS, such that galaxies brighter than about $M^* - 1$ appear about 50\% more strongly clustered than those fainter, and that a sample of emission galaxies shows 30\% weaker clustering than the full LCRS sample. On large scales $λ\gtrsim 40\ h^{-1}$~Mpc, we have also fit the LCRS results to various linear CDM models, and find that a number of them could meet the constraints set by the LCRS power spectrum, the Hubble constant range $0.5 \lesssim h \lesssim 0.8$, the abundance of galaxy clusters, and the reasonable assumption that LCRS galaxies are roughly unbiased tracers of the mass, relative to the normalization provided by the 4-year COBE DMR data. The possibilites include open CDM or flat non-zero cosmological-constant CDM models with $Ω_0 \approx 0.4-0.6$ and shape parameter $Γ\approx 0.2-0.3$, as well as flat $Ω_0 = 1$ models with massive neutrino density $Ω_ν\approx 0.2-0.3$ or a spectral tilt $n \approx 0.7-0.8$. (abridged)