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Date and Time of the Query: 2019-07-18 T20:05:12 PDT
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For refcode 2000ApJ...530...62G:
Retrieve 105 NED objects in this reference.
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2000ApJ...530...62G Optical Luminosities and Mass-to-Light Ratios of Nearby Galaxy Clusters Marisa Girardi, Stefano Borgani, Giuliano Giuricin, Fabio Mardirossian, and Marino Mezzetti Received 1999 April 14; accepted 1999 July 28 ABSTRACT We analyze a sample of 105 clusters having virial mass homogeneously estimated and for which galaxy magnitudes are available with a well-defined high degree of completeness. In particular, we consider a subsample of 89 clusters with B_j_-band galaxy magnitudes taken from the COSMOS/UKST Southern Sky Object Catalog. After suitable magnitude corrections and uniform conversions to B_j_ band, we compute cluster luminosities L_Bj_ within several clustercentric distances, 0.5, 1.0, 1.5 h^-1^ Mpc and within the virialization radius R_vir_. In particular, we use the luminosity function and background counts estimated by Lumsden et al. on the Edinburgh/Durham Southern Galaxy Catalog, which is the well-calibrated part of the COSMOS catalog. We analyze the effect of several uncertainties connected to photometric data, fore/background removal, and extrapolation below the completeness limit of the photometry, in order to assess the robustness of our cluster luminosity estimates. We draw our results on the relations between luminosity and dynamical quantities from the COSMOS sample by considering mass and luminosities determined within the virialization radius. We find a very good correlation between cluster luminosity, L_Bj_, and galaxy velocity dispersion, {sigma}_v_, with L_Bj_ is proportional to {sigma}_v_^2.1-2.3^. Our estimate of the typical value for the mass-to-light ratio is M/L_Bj_ ~ 250 h M_sun_/L_sun_. We do not find any correlation of M/L_Bj_ with cluster morphologies, i.e., Rood- Sastry and Bautz-Morgan types, and only a weak significant correlation with cluster richness. We find that mass has a slight, but significant, tendency to increase faster than the luminosity does, M is proportional to L_Bj_^1.2-1.3^. We verify the robustness of this relation against a number of possible systematics. We verify that this increasing trend of M/L with cluster mass cannot be entirely due to a higher spiral fraction in poorer clusters, thus suggesting that a similar result would also be found by using R-band galaxy magnitudes. Subject headings: cosmology: observations-galaxies: clusters: general- galaxies: fundamental parameters-galaxies: photometry
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