Astrophys. J., 541, 95-111 (2000/September-3)
Hubble space telescope photometry and Keck spectroscopy of the rich cluster MS 1054-03: morphologies, Butcher-Oemler effect, and the color-magnitude relation at z = 0.83.
VAN DOKKUM P.G., FRANX M., FABRICANT D., ILLINGWORTH G.D. and KELSON D.D.
Abstract (from CDS):
We present a study of 81 I-band selected, spectroscopically confirmed members of the X-ray cluster MS 1054-03 at z=0.83. Redshifts and spectral types were determined from Keck spectroscopy. Morphologies and accurate colors were determined from a large mosaic of HST WFPC2 images in RF606W and IF814W, corresponding to U and B in the rest frame. Early-type galaxies constitute only 44% of this galaxy population. This fraction is much lower than in comparable rich clusters at low redshift. Thirty-nine percent are spiral galaxies, and 17% are mergers. The early-type galaxies follow a tight and well-defined color-magnitude relation, with the exception of a few outliers. The observed scatter is 0.029±0.005 mag in rest frame U-B. Most of the mergers lie close to the CM relation defined by the early-type galaxies. They are bluer by only 0.07±0.02 mag, and the scatter in their colors is 0.07±0.04 mag. Spiral galaxies in MS 1054-03 exhibit a large range in their colors. The bluest spiral galaxies are ∼0.7 mag bluer than the early-type galaxies, but the majority is within ±0.2 mag of the early-type galaxy sequence. The red colors of the mergers and the majority of the spiral galaxies are reflected in the fairly low Butcher-Oemler blue fraction of MS 1054-03: fB=0.22±0.05, similar to intermediate redshift clusters and much lower than previously reported values for clusters at z∼0.8. The slope and scatter of the CM relation of early-type galaxies are roughly constant with redshift, confirming previous studies that were based on ground-based color measurements and very limited membership information. However, the scatter in the combined sample of early-type galaxies and mergers (i.e., the sample of future early-type galaxies) is twice as high as the scatter of the early-type galaxies alone. This is a direct demonstration of the ``progenitor bias'': high-redshift early-type galaxies seem to form a homogeneous, old population because the progenitors of the youngest present-day early-type galaxies are not included in the sample.
galaxies: clusters: individual (MS 1054-03) - Galaxies: Elliptical and Lenticular, cD - Galaxies: Evolution - Galaxies: Structure
Tables 2, 3: [VFK98] NNNN N=85 among (Nos 514-2174), 77 are new. Tables 2, 3: [VFF2000] HES N (Nos 1-2).
p. 100 : 1604+43 = ClG 1603+43 (=ClG J1604+4304)
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