Mathematics – Logic
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop...83r&link_type=abstract
Spitzer Proposal ID #83
Mathematics
Logic
Scientific paper
Use of Massive Clusters as Cosmological LensesG. RiekeMassive galaxy clusters lens the part of the universe behind them D roughly speaking, the lensing action is strongest at twice the distance of the cluster. The effectiveness of the lensing is greatest for the most massive clusters. Although MIPS can observe to confusion limits at 24, 70, and 160mm, the advantage provided by lensing is that galaxies that normally would be below the confusion limit are amplified and can be detected individually. Hence, Massive clusters can be identified by their strong xray emission. This program concentrates on x-ray luminous clusters in the range 0.2 < z < 0.4, also selected to be in regions of very low infrared cirrus.Evolution of Galaxies and Lensing in ClustersKelly & G. RiekeWe have a number of goals for this survey. At low redshifts, we will scan map the clusters, measuring the brightnesses and colors of individual galaxies and checking to see if there is detectable emission from the intracluster medium. In addition, we will look at the properties of the cluster as a whole by determining the luminosity function and the total far-infrared flux, both globally and as a function of location in the cluster. At modest redshifts of 0.2-0.4 we will measure brightness distributions, fluxes for the brightest individual galaxies, and the brightnesses of the clusters as a whole. In this range, we will also use the data as a lensing cluster survey. Because of the very non-linear relation between redshift, z, and distance, the result is that clusters at z ~ 0.3 are effective at lensing from 1 < z < 2, approximately. Use of lensing can extend the MIPS deep surveys in depth by the lensing amplification factor, which typically is 3 to 5. At redshifts greater than 0.75, we will be studying the early history of the clusters. At all of these redshift ranges, we have used x-ray luminosity as a means to select massive clusters and hence we have a homogeneous sample ranging from nearby to z > 1.
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