We present the star formation histories (SFHs) as a function of galactocentric radius of four isolated dwarf galaxies, Cetus, Tucana, LGS-3, and Phoenix. Our results suggest that beyond some distance from the center, there are no significative differences in fundamental properties of these galaxies. In the innermost regions, dwarf galaxies appear

We report on our ongoing project "Statistical studies of HII regions in the nearby extragalaxies". In EWASS 2014 we presented the overview of our detailed study of warm dust in the nearby Galaxy NGC 4321 (M100), which included new relations between the Halpha luminosity and the near-IR luminosity and temperature of some 275 HII regions in M100. In

Several ambitious scientific projects are currently pushing the limits of astrophysical spectroscopy, in terms of wavelength accuracy and long-term stability. These objectives put strong constraints also on the treatment of observational data, requiring dedicated software to be developed as an integral part of the instrument. In this context, a key

Context. Fornax is one of the most massive dwarf spheroidal galaxies in the Local Group. The Fornax field star population is dominated by intermediate age stars but star formation was going on over almost its entire history. It has been proposed that Fornax experienced a minor merger event. Aims: Despite recent progress, only the high metallicity

Aims: We derive the vertical velocities of disk stars in the range of Galactocentric radii of R = 5 - 16 kpc within 2 kpc in height from the Galactic plane. This kinematic information is connected to dynamical aspects in the formation and evolution of the Milky Way, such as the passage of satellites and vertical resonance and determines whether the

We have combined observations of the Antennae galaxies from the radio interferometer ALMA (Atacama Large Millimeter/submillimeter Array) and from the optical interferometer GHαFaS (Galaxy Hα Fabry-Perot System). The two sets of observations have comparable angular and spectral resolutions, enabling us to identify 142 giant molecular clouds (GMCs)