Large Scale Structures in the Universe. Cluster Analysis of Faint Galaxies in the Direction of HERCULES Void

Details Large Scale Structures in the Universe. Cluster Analysis of Faint Galaxies in the Direction of HERCULES Void Large Scale Structures in the Universe. Cluster Analysis of Faint Galaxies in the Direction of HERCULES Void

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006vopc.conf..285p&link_type=abstract

Virtual Observatory: Plate Content Digitization, Archive Mining and Image Sequence Processing, iAstro workshop, Sofia, Bulgaria,

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Ca. 1850 faint galaxies in the wide range of magnitudes 13m <= B <= 21m and effective surface brightness 16 μ_eff(B) <= 24 mag arcsec^-2 are detected in a field of one square degree centered at 1600+18 (1950) (Hercules void). Their coordinates (2000), magnitudes m(B), diameters, position angles surface brightness and some morphological parameters are studied using cluster analysis technique. Nearest and Furthest neighbor, Centroid, Median, Group, K means and Wards methods were used to determine the substructures in the distribution of faint galaxies. The distance metric in all the cases is squared Euclidean distance. The groups of Low surface brightness galaxies galaxies as well as the ones with high Surface Brightness were detected in such manner in the direction of the void. Edge on galaxies are not selected because of bias effects of the discrimination between stars and galaxies. Distribution of the concentration index (a parameter describing morphology of the object) was used to separate spiral and elliptical galaxies.

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