We have analyzed the radial distribution of old stars in a sample of 218 nearby face-on disks, using deep 3.6 μm images from the Spitzer Survey of Stellar Structure in Galaxies. In particular, we have studied the structural properties of those disks with a broken or down-bending profile. We find that, on average, disks with a genuine single

By making use of Herschel PACS Evolutionary Probe observations of the COSMOS and Extended Groth Strip fields, we have estimated the dependence of the clustering properties of FIR-selected sources on their 100 μm fluxes. Our analysis shows a tendency for the clustering strength to decrease with limiting fluxes. By assuming a power-law slope with γ =

The First Billion Years is one of the largest and most comprehensive cosmological, hydrodynamical simulation of the early Universe to date. It studies the formation of the first proto-galaxies down to redshift 6, and provides the path of the evolution from proto-galaxies to the observed galaxy population at redshift 4. It also provides predictions

We present a study of galaxy sizes in the local Universe as a function of galaxy environment, comparing clusters and the general field. Galaxies with radii and masses comparable to high-z massive and compact galaxies represent 4.4% of all galaxies more massive than 3 × 1010M⊙ in the field. Such galaxies are 3 times more frequent in clusters than in

We study the global efficiency of star formation in high-resolution hydrodynamical simulations of gas discs embedded in isolated early-type and spiral galaxies. Despite using a universal local law to form stars in the simulations, we find that the early-type galaxies are offset from the spirals on the large-scale Kennicutt relation, and form stars

We present the results of a new search for variable stars in the Local Group dwarf galaxy Leo A, based on deep photometry from the Advanced Camera for Surveys onboard the Hubble Space Telescope. We detected 166 bona fide variables in our field, of which about 60 per cent are new discoveries and 33 candidate variables. Of the confirmed variables, we