Genetic factors in the population of Plati, Greece

One‐thousand, thirty‐eight individuals from Plati, Greece were examined for the following red cell antigens, serum proteins, and red cell enzymes A A1 Ai B H; MNSs Mg Henshaw Nya Mur Vw; CCwcDEeCe; K k Kpa Kpb Jsa Jsb; P1; Lua; Fy1 Fy2; Jka Jkb; Wra; Zt; Vel; Swa; Jensen, Radin, Gerbich, Diego, Gregory, Haptoglobin, Transferrin, Acid phosphatase, Adenylate kinase, Adenosine deaminase, Esterase‐D, Glucose‐6‐phosphate dehydrogenase, Phosphoglucomutase, 6‐Phosphogluconate dehydrogenase, Phosphohexose isomerase, Lactate dehydrogenase, Malate dehydrogenase, and Superoxide dismutase. The results are discussed in detail and compared with other Greek and neighbouring populations. Because of the Plati population's long history of residence in the Cappadocian area of Turkey the data have been compared, whenever possible, with results for that region. Copyright © 1983 Wiley‐Liss, Inc., A Wiley Compan

The Average Mass Profile of Galaxy Clusters

The average mass density profile measured in the CNOC cluster survey is well described with the analytic form rho(r)=A/[r(r+a_rho)^2], as advocated on the basis on n-body simulations by Navarro, Frenk & White. The predicted core radii are a_rho=0.20 (in units of the radius where the mean interior density is 200 times the critical density) for an Omega=0.2 open CDM model, or a_rho=0.26 for a flat Omega=0.2 model, with little dependence on other cosmological parameters for simulations normalized to the observed cluster abundance. The dynamically derived local mass-to-light ratio, which has little radial variation, converts the observed light profile to a mass profile. We find that the scale radius of the mass distribution, 0.20<= a_rho <= 0.30 (depending on modeling details, with a 95% confidence range of 0.12-0.50), is completely consistent with the predicted values. Moreover, the profiles and total masses of the clusters as individuals can be acceptably predicted from the cluster RMS line-of-sight velocity dispersion alone. This is strong support of the hierarchical clustering theory for the formation of galaxy clusters in a cool, collisionless, dark matter dominated universe.Comment: Accepted for publication in ApJLetts. Also available at http://manaslu.astro.utoronto.ca/~carlberg/cnoc/nfw/ave.ps.g

The CNOC Cluster Survey: Omega, sigma\_8, Phi(L,z) Results, and Prospects for Lambda Measurement

Rich galaxy clusters are powerful probes of both cosmological and galaxy evolution parameters. The CNOC cluster survey was primarily designed to distinguish between Omega=1 and Omega~0.2 cosmologies. Projected foreground and background galaxies provide a field sample of comparable size. The results strongly support a low-density universe. The luminous cluster galaxies are about 10-30% fainter, depending on color, than the comparable field galaxies, but otherwise they show a slow and nearly parallel evolution. On the average, there is no excess star formation when galaxies fall into clusters. These data provide the basis for a simple Lambda measurement using the survey's clusters and the field data. The errors in Omega_M, Lambda, sigma_8 and galaxy evolution parameters could be reduced to a few percent with a sample of a few hundred clusters spread over the 0<z<1 range.Comment: to appear in Ringberg Workshop on Large-Scale Structure (ed. D. Hamilton) 14 pages, also available at http://manaslu.astro.utoronto.ca/~carlberg/cnoc/conference/ring2.ps.g

The Omega\_M-Omega\_Lambda Constraint from CNOC Clusters

The CNOC redshift survey of galaxy clusters measures Omega_M from Omega_e(z)= M/L x j/\rho_c which can be applied on a cluster-by-cluster basis. The mass-to-light ratios, M/L, are estimated from rich galaxy clusters, corrected to the field population over the 0.18 to 0.55 redshift range. Since the luminosity density depends on cosmological volumes, the resulting Omega_e(z) has a strong dependence on cosmology which allows us to place the results in the Omega_M-Omega_Lambda plane. The resulting Omega_M declines if Omega_Lambda>0 and we find that Omega_Lambda<1.5.Comment: 4 pages LaTeX. To appear in "Fundamental Parameters in Cosmology," the proceedings of the XXXIIIrd Rencontres de Morion

Omega_M and the CNOC Surveys

The CNOC1 cluster survey measures Omega_M via Oort's method, Omega_M= M/L x j/rho_c, where M/L is the field mass-to-light ratio, j is the field luminosity density and rho_c is the closure density. A wide range of potential systematic effects are explicitly controlled by independently deriving the mean cluster mass profile (finding good agreement with theoretical predictions), the cluster light profile, the redshift evolution of both cluster and field galaxies, the differential evolution between the two, and the field and cluster efficiencies for the conversion of baryons into galaxies. We conclude that Omega_M=0.19+/-0.06 where the errors are objectively evaluated via resampling methods. The redshift evolution of the numbers of clusters per unit co-moving volume over the 0< z < 0.6 range is found to be very slow, as is required for consistency with a low density universe. The evolution of galaxy clustering in the field is compatible with a low density universe, and strongly disfavors models of galaxy evolution that associate low density halos with individual galaxies.Comment: To appear in the 12 th Postdam Cosmology Workshop, "Large Scale Structure: Tracks and Traces", ed. V. Mueller, World Scientific 1998 also available at http://manaslu.astro.utoronto.ca/~carlberg/cnoc/conference/pots.ps.g