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For refcode 1996ApJ...471..694A:
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Copyright by American Astronomical Society. Reproduced by permission
1996ApJ...471..694A GALAXY EVOLUTION IN ABELL 2390 R. G. ABRAHAM Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA UK; and Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, Victona, BC V8X 4M6, Canada; abraham@ast.cam.ac.uX TAMMY A. SMECKER-HANE AND J. B. HUTCHINGS Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC V8X 4M6, Canada; smecker@carina.ps.uci.edu, hutchngs@dao.nrc.ca R. G. CARLBERG AND H. K. C. YEE Department of Astronomy, University of Toronto, Toronto, Ontario M5S 1A7, Canada; carlberg@moonray.astro.utoronto.ca, hyee@makalu.astro.utoronto.ca ERICA ELLINGSON CASA, University of Colorado, Boulder, Colorado 80309-0389; e.elling@pisco.colorado.edu AND SIMON MORRIS, J. B. OKE, AND MICHAEL RIGLER Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 W. Saanich Road, Victoria, BC V8X 4M6, Canada; simon@dao.nrc.ca, oke@dao.nrc.ca, mrigler@raicrosoft.com Received 1995 September 25; accepted 1996 May 17 ABSTRACT The galaxy population in the intermediate-redshift (z = 0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46' x 7' (6 h^-1^ Mpc x 1 h^-1^ Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4 h^-1^ Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3 h^-1^ Mpc in radius. Radial gradients in galaxy g - r color, 4000 A break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8 Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only <~ 5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one sub-component on the west side of the cluster, which is likely to be infalling at the epoch of observation. Subject headings: galaxies: clusters: individual (Abell 2390) - galaxies: distances and redshifts - galaxies: photometry - galaxies: stellar content
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