Showing papers on "Mass segregation published in 1979"

Core radii and mass segregation in clusters of galaxies

Abstract: Isothermal models are fitted to recent data on the Coma and CA 0340-538 clusters. Series of models are obtained for various magnitude limits. In both clusters it is found that the derived core radii are significantly dependent on those limits: They increase by about a factor of 2 when the magnitude increases from about M/sub asterisk/ (the magnitude at the ''knee'' of the luminosity function) to 2--4 magnitudes fainter. The influence on the models of the assumed background, cluster centers, halo, and ring size is investigated. The core radii do not seem very dependent on these parameters. These results seem to imply that more mass segregation than is usually recognized is present, at least in some clusters. Additionally, the Coma cluster shows a narrow density peak centered somewhere within 0.1 Mpc of NGC 4874, and about 0.15 Mpc in radius, which is present essentially at all magnitude levels. The central density is about 1.5--2 times the value predicted by the model. This feature may indicate the presence of a dynamically separated subunit.

Clusters of galaxies compared withN-body simulations: Masses and mass segregation

Abstract: With three virially stableN-body simulations of Wielen, we show that use of the expression for the total mass derived from averaged quantities (velocity dispersion and mean harmonic radius) yields an overestimate of the mass by as much as a factor of 2–3, and use of the heaviest mass sample gives an underestimate by a factor of 2–3 The estimate of the mass using mass weighted quantities (ie, derived from the customary definition of kinetic and potential energies) yields a better value irrespective of mass sample as applied to late time intervals of the models (≥three two-body relaxation times) The uncertainty is at most ∼50% This suggests that it is better to employ the mass weighted expression for the mass when determining cluster masses The virial ratio, which is a ratio of the mass weighted/averaged expression for the potential energy, is found to vary between 1 and 2 We conclude that ratios for observed clusters ∼4–10 cannot be explained even by the imprecision of the expression for the mass using averaged quantities, and certainly implies the presence of unseen matter Total masses via customary application of the virial theorem are calculated for 39 clusters, and total masses for 12 clusters are calculated by a variant of the usual application The distribution of cluster masses is also presented and briefly discussed Mass segregation in Wielen's models is studied in terms of the binding energy per unit mass of the ‘heavy’ sample compared with the ‘light’ sample The general absence of mass segregation in relaxed clusters and the large virial discrepancies are attributed to a population of many low-mass objects that may constitute the bulk mass of clusters of galaxies

Clusters of galaxies compared with n-body

Abstract: With three virially stable N-body simulations of Wielen, we show that use of the expres- sion for the total mass derived from averaged quantities (velocity dispersion and mean harmonic radius) yields an overestimate of the mass by as much as a factor of 2-3, and use of the heaviest mass sample gives an underestimate by a factor of 2-3. The estimate of the mass using mass weighted quantities (i.e., derived from the customary definition of kinetic and potential energies) yields a better value irrespective of mass sample as applied to late timeintervals of the models(> three two-body relaxation times). The uncertainty is at most N 50~oo. This suggests that it is better to employ the mass weighted expression for the mass when determining cluster masses. The virial ratio, which is a ratio of the mass weighted/averaged expression for the potential energy, is found to vary between 1 and 2. We conclude that ratios for observed clusters ~ 4-10 cannot be explained even by the imprecision of the expression for the mass using averaged quantities, and certainly implies the presence of unseen matter. Total masses via customary application of the virial theorem are calculated for 39 clusters, and total masses for 12 clusters are calculated by a variant of the usual application. The distribution of cluster masses is also presented and briefly discussed. Mass segregation in Wielen's models is studied in terms of the binding energy per unit mass of the 'heavy' sample compared with the 'light' sample. The general absence of mass segregation in relaxed clusters and the large virial discrepancies are attributed to a population of many low-mass objects that may constitute the bulk mass of clusters of galaxies.