Francesco Barbera

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We study the evolution of the relation between half-light (effective) radius, r e , and mean surface brightness, < µ > e , known as Kormendy relation, out to redshift z = 0.64 in V-band restframe on the basis of a large sample of spheroidal galaxies (N = 228) belonging to three clusters of galaxies. The present sample constitutes the largest data set for(More)
2DPHOT: a multipurpose environment for the two-dimensional analysis of wide-field images ABSTRACT We describe 2DPHOT, a general purpose analysis environment for source detection and analysis in deep wide-field images. 2DPHOT is an automated tool to obtain both integrated and surface photometry of galaxies in an image, to perform reliable star-galaxy(More)
Color gradients in early-type galaxies contain valuable clues about their formation and evolutionary histories and mechanisms. We examine color gradients in 1,700 early-type galaxies in 159 galaxy clusters spanning a redshift range of 0.05 to 0.2. We find that color gradients strongly depend on the environment where galaxies reside, with steeper color(More)
The management of clinical data is a complex task. Patient related information reported in patient folders is a set of heterogeneous and structured data accessed by different users having different goals (in local or geographical networks). XML language provides a mechanism for describing, manipulating, and visualising structured data in web-based(More)
We present an analysis of star-formation and nuclear activity in galaxies as a function of both luminosity and environment in the fourth data release of the Sloan Digital Sky Survey (SDSS DR4). Using a sample of 27 753 galaxies in the redshift range 0.005 < z < 0.037 that is 90% complete to M r = −18.0 we find that the EW(Hα) distribution is strongly(More)
This paper is aimed at giving an overview of the global properties of the rich cluster of galaxies ABCG 209. This is achieved by complementing the already available data with new medium resolution spectroscopy and NIR photometry which allow us to i) analyse in detail the cluster dynamics, distinguishing among galaxies belonging to different substructures(More)
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