Other
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt........11t&link_type=abstract
PhD Dissertation, Yale Univ. New Haven, CT United States
Other
18
Galactic Clusters, Galaxies, Red Shift, Galactic Structure, Galactic Evolution, Quantitative Analysis, Autocorrelation, Spatial Distribution, Extraterrestrial Matter, Astronomical Models, Dark Matter, Astronomical Catalogs
Scientific paper
The Las Campanas Deep Redshift Survey (LCDRS) is a survey of the galaxy distribution, out to a redshift of 0.2, which will eventually cover approx. 1000 square degrees over the Northern and Southern galactic Caps in alternating 1.5 deg- thick slices. The goals of the LCDRS are to sample a large enough volume of the nearby Universe in order to constrain the scale of the largest features in the galaxy distribution, and to use this sample for the accurate measurement of galaxy clustering on a wide variety of scales. Upon completion, 25,000 - 30,000 galaxy redshifts will have been compiled. This dissertation describes results obtained by the analysis of the first approx. 5,400 reduced redshifts. Three main topics are discussed. First, the distribution of galaxies in the LCDRS is examined. Although visual inspection of the slices indicates an upper limit of approx. 100 h-1 Mpc to the scale of high- contrast features, quantitative study of the galaxy distribution suggests the presence of low-contrast density gradients on scales comparable to the LCDRS volume itself. The galaxy-galaxy spatial autocorrelation function is also determined; it shows more power on large scales than is compatible for a standard cold dark matter (CDM) model, although it is consistent with results expected from an open CDM model. Second, a group catalog is extracted from the nearly complete LCDRS -6 deg Slice, and its properties are compared with those of other group and cluster catalogs. A group-group spatial autocorrelation function is determined, and its amplitude is compared with the correlation amplitudes for other galaxy, group, and cluster catalogs. Finally, galaxy segregation is studied as a function of color. Overall, evidence from both visual impressions and quantitative tests points toward color-segregation only on scales on the order of or less than the width of a typical void wall (less than 10-20 h-l Mpc). Arguments are made for galaxy evolution as a major driver of color-segregation, with primordial effects playing at most a minor role in the observed color-environment effects.
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