Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..86..419m&link_type=abstract
Astrophysics and Space Science, vol. 86, no. 2, Sept. 1982, p. 419-435
Astronomy and Astrophysics
Astrophysics
2
Galactic Clusters, Galactic Structure, Monte Carlo Method, Astronomical Models, Ellipticity, Spatial Distribution
Scientific paper
The positions, magnitudes, orientations and shapes of spherical supercluster cell galaxies are simulated by means of the Monte Carlo technique described by MacGillivray et al (1982), for different galaxy three-dimensional alignment schemes. Projected galaxy properties are examined. The simulation technique is also used to examine the properties of galaxies in clusters formed at the intersections of adjacent cells, with results that may furnish clues for interpreting the nature of observed galaxy geometric properties in rich clusters and that are presently used for a preliminary comparison with observational data. The comparison indicates that observational results could be understood if clusters were the node points between cells, although observed galaxy properties cannot be produced unambiguously by the adiabatic mechanism for galaxy formation. Model fields are compared with a field obtained from COSMOS measurements of a deep photograph, yielding results which indicate that the observed distribution of faint galaxies on photographic plates can only be represented by a model involving second-order clustering of galaxies. The exact nature of such clustering cannot, however, be unambiguously determined from the two-dimensional distributions. Uniformly-populated supercluster and cellular models are able to statistically represent the observed projected distribution of galaxies.
Dodd Robert J.
MacGillivray Harvey T.
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