Bright globular clusters in NGC 5128: the missing link between young massive clusters and evolved massive objects

Best fit values of the relation between total mass and gas, star and baryon fraction of MUSIC-2 halos for all objects, massive clusters and groups of galaxies.. Best fit values of the

Globular clusters are ideal laboratories for testing theories of stellar evolution, the chemical evolution of the Universe and the dynamics of N-body systems' They are

Finally, experiments with solar [17–34], atmospheric [35–45], reactor [46–50], and long-baseline accelerator [51–59] neutrinos indicate that neutrino flavor change through

A comparison between the radio and X-ray populations in Orion shows that the radio detections so far have been strongly biased to the brighter X-ray stars. This supports the

Relationship between the total cluster stellar mass and the photometric blue fraction for the ALHAMBRA cluster and group sample stacked into different redshift bins. The galaxy

In order to provide a more quantitative estimate of the relative probability of observationally detecting such massive clusters at the indicated redshifts we used n( > M, z) –

By the consistency of the truncation, the metric and dilaton in (3.5), together with the constant-scalar field strengths (3.8), solve the field equations of massive type

Clearly for our choice of cosmological parameters, haloes at these mass scales are more massive in strongly coupled cosmolo- gies but can have similar masses in cosmologies with