Titlebook: Large-Scale Structures in the Universe Observational and Analytical Methods; Proceedings of a Wor W. C. Seitter,H. W. Duerbeck,M. Tacke Con

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Large-Scale Structures in the Universe Observational and Analytical MethodsProceedings of a Wor

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,Large scales — Large numbers — Large efforts: Historical annotations,riefly traced. It is intended to show small portions of the structure on which our present work is built, to provide a background onto which the data and discussions of the workshop can be projected..Section 1 lists some major historical and contemporary large-scale surveys, in two and three dimensi

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The Edinburgh/Durham galaxy survey,nitial catalogue covers some 60 plates and contains approximately 10. galaxies to .. = 20. For each galaxy we store 27 image parameters, including image magnitude, RA, DEC, area, and position angle, enabling the database to be used for a wide range of astronomical applications. Here we discuss our d

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The Muenster Redshift project. Automated analysis of galaxy clustering on Schmidt plates,tive prism Schmidt plates. This contribution describes the role of direct plates in the survey. Methods of analysis and their errors are discussed. Maps of two-dimensional galaxy distributions are presented, including the distributions of different types of galaxies (using ellipticity as a coarse mo

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,A study of galaxies with ,≤0.3 in the ESO/SRC Atlas Field No. 411: Galaxy distribution and luminosi. 411 is dominated by a galaxy supercluster at . = 0.11±0.01, (330±30 ...). The supercluster consists of at least five rich clusters, connected by bridges of galaxies, constituting a filament of length > 20 ..Mpc. Luminosity functions are calculated for the high and low density regions. The fraction

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An application of projected distance cross-correlation for Abell clusters,ance cross-correlation function .. between the Struble and Rood catalogue and the Abell catalogue. The σ-correlation function is determined, the best fit is ..(σ) = σ./σ, where σ. = 2.3Mpc. The spatial cross-correlation function can be derived from ..(σ) by an integral transformation. In our case, w