Structure of the Coma cluster of galaxies

Details Structure of the Coma cluster of galaxies Structure of the Coma cluster of galaxies

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985phdt........21s&link_type=abstract

Ph.D. Thesis California Univ., Berkeley.

Astronomy and Astrophysics

Astronomy

3

Galactic Clusters, Galactic Structure, Spatial Distribution, Astronomy, Density (Number/Volume), Luminosity

Scientific paper

This study is based primarily upon a sample of 1722 galaxies in the Coma cluster observed by Abell. Researchers compare Abell's observations of the inner part of the Coma cluster (within 75 arc-min) with those of several other observers, and prepare a catalogue of observations from several observers. They test the distribution of galaxies for irregularities, finding marginal evidence that there are some clumps of galaxies in certain regions and magnitude ranges. However, they find that axially symmetric bumps in the radial density distribution of galaxies are not significant. They then fit the projected spatial distribution of galaxies in order to determine the core radius. They find that the value of the core radius is larger than that found by most previous authors, and it increases with increasing galaxy magnitude. This finding implies that a degree of mass segregation exists in the cluster. Finally, they determined the spatial luminosity density at the center of the cluster. They then discuss the impact of the inclusion of non-members on the analysis. They discuss different methods of determining membership in the cluster and correcting for the effect of nonmembers upon the observations. They find that the clumped nature of the background makes it difficult to determine the membership of the cluster by a smooth subtraction of background galaxies. However, the uncertain background subtraction is not the reason for the increase in the core radius with magnitude.

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