Spectral energy distributions for galaxies in high redshift clusters. I - Methods and application to three clusters with Z = 0.22-0.31

Details Spectral energy distributions for galaxies in high redshift clusters. I - Methods and application to three clusters with Z = 0.22-0.31 Spectral energy distributions for galaxies in high redshift clusters. I - Methods and application to three clusters with Z = 0.22-0.31

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.205.1287c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 205, Dec. 1983, p. 1287-1312. Research supported by the

Astronomy and Astrophysics

Astronomy

49

Galactic Clusters, Galactic Evolution, Red Shift, Spectral Energy Distribution, Spectrophotometry, Bandpass Filters, Charge Coupled Devices, Colorimetry, Error Analysis, Interstellar Extinction, Luminosity

Scientific paper

Using CCDs and a range of intermediate band filters, three moderate redshift (z = 0.22-0.31) clusters were imaged and low-resolution spectral energy distributions for about 50 galaxies per cluster to a limit of R(f) = 21 were derived. The average flux distributions are in good agreement with those expected from published K-corrections and local knowledge of the color-luminosity relation for early-type galaxies; the brightest members do not appear to be anomalous. Some blue galaxies are found: their average spectral energy distribution approximates to an Sbc galaxy at the cluster redshift. At the longest wavelength studied (860 nm) some galaxies are significantly redder than the cluster average; the nature of these objects remains unclear but they do appear to be cluster members. The important question of whether there is any evolution in the early-type population depends sensitively on corrections made for foreground reddening and for the color-luminosity relations. With some uncertainties there is room for a small amount of evolution consistent with previous estimates. At higher redshifts where evolutionary effects are expected to be larger the technique will be a powerful way to study large galaxy samples at known epochs.

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