Galaxy interactions II High density environments

As we have identified, at a comparable spatial resolution, stellar clumps and GMCs in the same high-redshift galaxy, it is tempting to estimate the efficiency of star formation in

of Hubble type, and galaxy stellar mass, M ?. The goals are: 1) to characterize in detail the radial structure of stellar population properties of galaxies in the local universe; 2)

Next we study the evolution of the total mass density profiles of the main galaxy clusters in the dataset to find how stable is their mass distribution across their

To cross-validate the aforementioned analyses of pretest1 posttest1 scores with respect to idea development of the participants in the control and experimental groups,

The circularized stellar mass density profiles for the galaxies in our sample, comparing them with similar mass SDSS ETGs and the massive compact galaxies in Szomoru et al..

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

An example of projected stellar mass density for the disk, spheroid, and galaxy stellar particles is given in Figure 2 for G-1536, as well as the position of the radial cut we use

As a means to probe the possible fractal structure of the galaxy distribution we have studied the scaling of the num- ber density and angular correlation function of galaxies