Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...286..106l&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 1, 1984, p. 106-115. Research supported by the Smithsonian Astrop
Astronomy and Astrophysics
Astrophysics
18
Astronomical Photometry, Galactic Clusters, Galactic Evolution, Galactic Structure, Magnitude, Radii, Astronomical Photography, Brightness Distribution, Data Reduction, Electrophotometry, Elliptical Galaxies, Spectrum Analysis, Surface Properties
Scientific paper
To investigate theoretical predictions for the dynamical evolution of first-ranked galaxies, a quantitative study of their properties, as a function of cluster morphology, has been carried out using photographic plates obtained with the Palomar 48 inch (1.2 m) Schmidt telescope. Surface brightness profiles to radii of several hundred kpc for 35 first-ranked cluster galaxies have been analyzed. The dispersion in the metric magnitudes of first-ranked galaxies is quite small (about 0.4 mag), which is consistent with the results of Kristian, Sandage, and Westphal (1978) as well as those of Hoessel, Gunn, and Thuan (1980) and the recent work of Schneider, Gunn, and Hoessel (1983). For the cD (supergiant elliptical) galaxy sample, the mean metric magnitude is about 0.5 mag brighter than for the non-cD galaxies. The mean de Vaucouleurs effective radius for the cD galaxy sample is 80 percent larger than that of the non-cD sample. The relation between de Vaucouleurs effective radius and magnitude determined in the present study for first-ranked galaxies, log r(e) equal to about -0.26 M + constant is consistent with the relations found for fainter galaxies by Strom and Strom (1978) as well as Wirth (1982). The residuals in radius from the mean radius-magnitude relation for first-ranked galaxies do not correlate with the Bautz-Morgan (1970) type of the cluster.
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