MOND dynamical mass in groups and clusters
Hierarchical inference of the relationship between Concentration and Mass in Galaxy Groups and Clusters
... population mass should be the clus- ter mass function that describes the number density of clusters of a given mass and redshift ...Massive clusters form from rare, dense peaks in the ...
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Exploring Galaxy Clusters and Groups with Cosmological Simulations
... stellar mass function to Illus- tris (see ...stellar mass buildup in massive ...stellar mass buildup of massive galaxies, thereby allowing the radio-mode to operate on a much shorter duty ...produce ...
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Clusters Setup. Groups of interconnected rectangular tables.
... Setup Groups of interconnected rectangular tables. Benefits: Groups of three rectangular tables, configured to maximize working sessions, collaboration and group participation with the ...
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The FABLE simulations: A feedback model for galaxies, groups and clusters
... galaxies, groups, and ...stellar mass function together with the stellar and gas mass fractions of local groups and clusters across a wide range of halo ...of groups and ...
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Characterization of extended emission from groups and clusters of galaxies
... Galaxy clusters o ffer a unique probe to study the matter distribution over a wide range of redshifts, allowing us to test di fferent cosmological models independently of other methods, such as supernovae type Ia ...
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Towards a realistic population of simulated galaxy groups and clusters
... We compare the properties of the simulated galaxy groups and clusters to a wide range of observational data, such as X-ray luminosity and temperature, gas mass fractions, entropy and den[r] ...
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Simulations of the Dynamical. Evolution of Compact Groups and. Poor Clusters. by Paul W. Bode
... the mass is in galaxies and their halos; this group merged completely in 4 ...cross-sections, dynamical friction, and other physical ...his groups underwent two mergers in a median time of ...model). ...
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Observability of intermittent radio sources in galaxy groups and clusters
... halo mass of 3 × 10 12 M , and one that is a hundred times more massive, with isothermal intergalactic medium/intracluster medium (ICM) gas in hydrostatic equilibrium with the dark matter ...
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The XXL Survey : XXII The XXL North spectrophotometric sample and galaxy stellar mass function in X ray detected groups and clusters
... the mass regime between the adopted and the proper mass ...the mass function in each of these sub-bins to be the same as that in the first ...the mass range between the adopted mass ...
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Unveiling the dynamical state of massive clusters through the ICL fraction
... galaxy clusters with clearly defined dynamical states and HST-like observational char- acteristics is necessary to improve our statistical significance, we have shown that the ICL fraction colors, measured ...
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Generalizing MOND to explain the missing mass in galaxy clusters
... of clusters and invoking new tests of the law, such as gravitational lensing and dynamics of objects that lie within galaxy ...lower MOND ac- celeration scale in galaxies compared to galaxy clusters ...
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The dynamical evolution of very low mass binaries in open clusters
... in clusters, dynamical evo- lution can significantly alter any initial binary population, preferentially destroying wide ...the dynamical evolution of initially differ- ent VLMB distributions in ...
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A dynamical definition of quasibound molecular clusters
... Recognising the precise moment of cluster breakage is important when we analyse the quasi-continuous cluster trajectory, illustrated in Figure 2, obtained by repeatedly repairing the system. In intervals around the ...
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The Formation and Dynamical Evolution of Young Star Clusters
... star clusters, including embedded systems, young massive clusters, and ...and dynamical evolution of these clusters using a combination of simulations and theoretical ...The dynamical ...
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Dynamical formation of millisecond pulsars in globular clusters
... Apart from the radio luminosity functions, the X-ray emission properties of the MSPs in the GCs are also found to be very different from those in the Galactic field. While the MSPs in the Galactic field generally require ...
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Line profiles of cores within clusters II Signatures of dynamical collapse during high mass star formation
... The N 2 H + line still exhibits non-Gaussianity. Table 3 shows the mean intensity peak of the lines from all viewing angles when the central protostar has mass 0.5 M and 5.0 M . The peak intensity of HCO + (1–0) ...
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The early dynamical evolution of cool, clumpy star clusters
... ‘core phase’, the massive star multiple system is in the cen- tre of the cluster (but the individual stars are too close to resolve in this image). Fig. 6(b) shows the cluster 0.7 Myr later. Most of the massive stars ...
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MLG vs MOND
... baryonic mass (see Figure ...luminous mass, the edge-star’s dynamics is seen proportional to the galactic luminous mass (see ...luminous mass [2]. MOND by far solved the mystery of ...
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The effect of the dynamical state of clusters on gas expulsion and infant mortality
... Indeed, in such a scenario there is no reason to as- sume that the initial spacial distribution of the stars and gas should be very similar. Stars will form in dense knots which may not match the large scale mass ...
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Biases in the estimation of velocity dispersions and dynamical masses for galaxy clusters
... objects, for a fixed integration time. Therefore, cluster samples contain only a fraction of the brightest galaxy members, which are also the most massive. In order to simulate this effect, we mimicked observational ...
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