Other
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........21l&link_type=abstract
Thesis (PH.D.)--HARVARD UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-11, Section: B, page: 6171.
Other
17
Galaxies, Luminosity, Clustering
Scientific paper
Analyses of the luminosity and clustering properties of galaxies in the Las Campanas Redshift Survey (LCRS) are presented. Chapter I describes details of the survey and presents the data. The sample consists of 23697 galaxies, with average redshift z = 0.1, distributed over six 1.5 ^circ x 80^circ slices in the North and South galactic caps. Maps of the galaxy distribution reveal a rich network of filaments, clusters, voids, and walls, with the largest structures having sizes 50-100 h^{-1} Mpc. The combination of the survey's large sample size, volume, and depth argues that the LCRS may currently represent the best chance for a fair sample of the nearby universe. In Chapter II we compute the Gunn-r band galaxy luminosity function, and find that it may be fit by a Schechter function with M^* = -20.29 +/- 0.02 + 5 log h, alpha = -0.70 +/- 0.05, and phi^* = 0.019 +/- 0.001 h^3 Mpc^{ -3}. We split the sample by (OII) 3727 equivalent width W_lambda, and show that the faint end of the luminosity function is dominated by galaxies with W_lambda >= 5 A. We also compare our luminosity function to that from previous surveys, and discuss some implications of our results for the faint galaxy count data. Chapter III presents the galaxy power spectrum P(k), which may be approximated as ~ k^{-1.8+/- 0.1} for small scales lambda = 2pi/k = 5 - 30 h^{-1} Mpc, changing to ~ k^{1+/- 1} for large scales lambda ~ 200 - 400 h^{-1 } Mpc, with overall amplitude sigma _ 8 = 1.0 +/- 0.1 in redshift space. We compare our results to that from previous surveys and find good agreement with the CfA2 + SSRS2 sample. We also find type-dependent clustering differences, specifically a 50% stronger clustering for galaxies brighter than M ^* - 1 and a 30% weaker clustering for emission galaxies. The LCRS P(k) lies in between that of a standard Omega h = 0.5, b = 1.5, cold dark matter (CDM) N-body model and an unbiased Omega h = 0.2 model. On large scales lambda _sp{~}> 60 h^{-1} Mpc, the LCRS P(k) may be fit by a linear CDM model with Omega h = 0.36.. Finally, Chapter IV analyzes redshift-space distortions in the galaxy correlation function zeta. On small scales an exponential pairwise velocity distribution describes the data well, and we obtain a galaxy pairwise peculiar velocity dispersion sigma 12 = 452 +/- 60 km s ^{-1} at separation <1 h^{-1} Mpc. Our sigma12 is in between the classical value of 340 km s^ {-1} from the CfA1 survey and the recent higher value of 540 km s^{-1} from the much larger CfA2 + SSRS2 sample, over which the LCRS volume is another factor of two bigger. On larger scales, separations {~}30 h^{-1} Mpc, we use linear theory to estimate Omega^{0.6 }/b = 0.5 +/- 0.25, consistent with results from similar analyses of other surveys, but again the LCRS provides an independent result, valid over deeper redshifts than previously explored.
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