HST Photometry and Keck Spectroscopy of the Rich Cluster MS1054-03: Morphologies, Butcher-Oemler Effect and the Color-Magnitude Relation at z=0.83

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dc.creatorvan Dokkum, Pieter G.
dc.creatorFranx, Marijn
dc.creatorFabricant, Daniel
dc.creatorIllingworth, Garth D.
dc.creatorKelson, Daniel D.
dc.date2000-02-28
dc.date.accessioned2026-07-07T11:45:56Z
dc.date.available2026-07-07T11:45:56Z
dc.descriptionWe present a study of 81 I selected, spectroscopically-confirmed members of the X-ray cluster MS1054-03 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 F606W and F814W. Early-type galaxies constitute only 44% of this galaxy population. 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 magnitudes in restframe 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 magnitudes, and the scatter in their colors is 0.07 +- 0.04 magnitudes. Spiral galaxies in MS1054-03 exhibit a large range in their colors. The bluest spiral galaxies are 0.7 magnitudes bluer than the early-type galaxies, but the majority is within +- 0.2 magnitudes 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 MS1054-03: f_B=0.22 +- 0.05. 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 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.
dc.descriptionAccepted for publication in the ApJ. At http://astro.caltech.edu/~pgd/cm1054/ color figures can be obtained
dc.identifierhttps://arxiv.org/abs/astro-ph/0002507
dc.identifierhttp://arxiv.org/abs/astro-ph/0002507
dc.identifierAstrophys.J.541:95-111,2000
dc.identifierdoi:10.1086/309402
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/202050
dc.subjectAstrophysics
dc.titleHST Photometry and Keck Spectroscopy of the Rich Cluster MS1054-03: Morphologies, Butcher-Oemler Effect and the Color-Magnitude Relation at z=0.83
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