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Date and Time of the Query: 2019-07-21 T14:07:30 PDT
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For refcode 1991ApJ...375...15O:
Retrieve 43 NED objects in this reference.
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1991ApJ...375...15O FUNDAMENTAL PARAMETERS OF BRIGHTEST CLUSTER GALAXIES WILLIAM R. OEGERLE Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 AND JOHN G. HOESSEL Washburn Observatory, University of Wisconsin-Madison, Department of Astronomy, 475 North Charter Street, Madison, WI 53706 Received 1990 July 30; accepted 1990 December 17 ABSTRACT We have obtained photometry and spectroscopy of a sample of brightest cluster galaxies in order to determine the relationships between scale length, surface brightness, velocity dispersion, and line strength, and to make comparisons with the relations determined for lower luminosity elliptical galaxies. We have computed the velocity dispersions for 32 brightest cluster galaxies, which when supplemented by additional data from the literature, give us a sample of 43 galaxies. CCD surface photometry of these galaxies produced characteristic scale lengths and surface brightnesses. We find that the relation between log r_e_, log {sigma}, and mean surface brightness reported by Dressler et al. for lower luminosity ellipticals also describes the relation for brightest cluster galaxies fairly well. There is a slight curvature in the fundamental plane at the high luminosity end, apparently due to the fact that the velocity dispersions of BCGs increase more slowly with luminosity than those for lower luminosity ellipticals. We derive the fundamental plane solutions for BCGs in r_e_ - {sigma} - <{mu}>_e_ space, which can be used as a distance indicator with a predicted error of ~21% per galaxy. The r_e_ - <{mu}>_e_ relation for BCGs is also a good distance indicator (distance errors of ~25% per galaxy) and has the advantage of not requiring knowledge of the velocity dispersion. We find only a weak correlation between the Na D 5893 line strength (metallicity) and velocity dispersion for BCGs, in contrast to the significant correlation between these quantities reported for lower luminosity ellipticals. Finally, we find that the mean mass-to-light ratio for BCGs is a factor of ~2 greater than for the lower luminosity ellipticals in the Virgo and Coma sample of Dressler et al., consistent with the correlation M/L ~ L^1/4^. By observing BCGs at higher redshift (i.e., z~0.5), the fundamental plane solutions can be used to determine the change in surface brightness due to stellar evolution with an accuracy of ~25% and to place limits on q_0_. Subject headings: galaxies: clustering - galaxies: internal motions - galaxies: photometry
Retrieve 43 NED objects in this reference.
Please click here for ADS abstract

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