Measuring Ω_M in the Near-Infrared

Details Measuring Ω_M in the Near-Infrared Measuring Ω_M in the Near-Infrared

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..342h&link_type=abstract

NOAO Proposal ID #1999A-0342

Astronomy and Astrophysics

Astrophysics

Scientific paper

The CNOC1 cluster redshift survey has determined the mass density of the universe Ω_M to +/-30% statistical uncertainty. A dominant possible source of systematic error in this measurement is any differential redshift evolution between cluster and field galaxies. Existing g- and r-band observations suggest that any such evolution is small, but it is important to verify this using near-infrared light which more closely traces galaxy mass and is much less affected by different star formation histories. Thus we propose H-band imaging of all 15 CNOC1 clusters (1sq arcdeg) plus 0.4sq arcdeg of the CNOC2 field galaxy redshift survey to obtain H-band luminosities for 1100 cluster and > 1100 field galaxies with existing redshifts. These data will provide the most precise measurements ever made of the H-band galaxy luminosity function at z=0.2-0.55 in clusters and the field. Simple, direct tests of differential evolution in the H band will constrain possible systematic errors in Ω_M, help determine the astrophysics of galaxy evolution using the largest available homogeneous cluster and field galaxy redshift samples, and serve as a benchmark for higher-z cluster studies in the 8m era.

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