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The Power Spectrum of Galaxy Clustering in the Las Campanas Redshift Survey | | Huan Lin
; Robert P. Kirshner
; Stephen A. Shectman
; Stephen D. Landy
; Augustus Oemler
; Douglas L. Tucker
; Paul L. Schechter
; | | Date: |
10 Jun 1996 | | Subject: | astro-ph | | Abstract: | The Las Campanas Redshift Survey (LCRS) contains 23697 galaxies, with an average redshift $z = 0.1$, distributed over six $1.5arcdeg$ by $80arcdeg$ slices in the North and South galactic caps. We have computed the power spectrum $P(k)$ for LCRS galaxies over wavelengths $lambda = 2pi / k = 5 - 400 h^{-1}$~Mpc. The LCRS $P(k)$ may be approximated as $propto k^{-1.8 pm 0.1}$ for small scales $lambda = 5 - 30 h^{-1}$~Mpc, changing to $propto k^{1 pm 1}$ for large scales $lambda approx 200 - 400 h^{-1}$~Mpc. The overall amplitude corresponds to $sigma_8 = 1.0 pm 0.1$ 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 50more strongly clustered than those fainter, and that a sample of emission galaxies shows 30weaker clustering than the full LCRS sample. On large scales $lambda gtrsim 40 h^{-1}$~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 $Omega_0 approx 0.4-0.6$ and shape parameter $Gamma approx 0.2-0.3$, as well as flat $Omega_0 = 1$ models with massive neutrino density $Omega_
u approx 0.2-0.3$ or a spectral tilt $n approx 0.7-0.8$. (abridged) | | Source: | arXiv, astro-ph/9606055 | | Services: | Forum | Review | PDF | Favorites | |
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