In the last years, photometric and spectroscopic evidence has demonstrated that many, maybe all the Globular Clusters (GC) host multiple stellar populations. High-resolution spectroscopy has established that, while most GCs are mono-metallic with no significant abundance spread in s-elements, in all the globulars studied to date the presence of

Blue Compact Dwarf (BCD) galaxies are metal-poor and gas-rich systems undergoing intense, spatially extended star-forming activity. These galaxies offer a unique opportunity to investigate dwarf galaxy formation and evolution, and probe violent star formation and its implications on the chemical, dynamical and structural properties of low-mass

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We are carrying out a detailed 2D spectroscopic study of the central 210×130 pc of the blue compact dwarf (BCD) galaxy NGC 5253. This contribution presents the ionization conditions and chemical abundance patterns for the different kinematic components of the ionized gas detected in our previous work. All the kinematic components present an excess

Magnetohydrodynamic (MHD) wave activity is ubiquitous in the solar atmosphere. MHD seismology aims to determine difficult to measure physical parameters in solar atmospheric magnetic and plasma structures by a combination of observed and theoretical properties of MHD waves and oscillations. This technique, similar to seismology or helio-seismology

We present an analysis of near-IR images, obtained with the instrument PANIC at the Baade telescope (Las Campanas), of the star-forming regions associated with the sources IRAS 12272-6240 and IRAS 17149-3916, selected from the southern sky survey of sub-mm cores of Beltran et al. (2006). We identify two young clusters associated with each one of