Large-Scale Clustering of Galaxies in the CFA Survey

Details Large-Scale Clustering of Galaxies in the CFA Survey Large-Scale Clustering of Galaxies in the CFA Survey

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pkas....7....9p&link_type=abstract

Publications of the Korean Astronomical Society, vol.7, no.1, p.9-17

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Scientific paper

The power spectrum of the galaxy distribution is accuarately measured up to wavelengths over 100h-1 Mpc from the CfA 1 and 2 catalogs. We find that our results agree with power spectra calculated by others from smaller samples of optical, radio and infrared galaxies. The power spectrum of an open CDM model (Omega h = 0.2 and delta8 = 1; see below for definitions) best approximates the observed power spectrum. The power spectrum of the standard CDM model(Omega h = 0.5 and delta8 = 1) is inconsistent with the observed one at the 99% confidence level. Our best estimation of the corresponding correlation function in real space is Xi(r) = (r/6.2h-1 Mpc)^-1.8 for r < 20h-1 Mpc.

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