We discuss the use of the spectral range near 7570 Å to determine the Mg isotopic ratios in carbon stars using the B'2 Sigma +-X 2 Sigma + system of the MgH molecule. We also compare with the spectral range near 5140 Å that has been commonly used in normal stars (oxygen-rich stars). The region near 5140 Å is not the better choice for carbon stars

We discuss abundances of alpha -elements in the ultra-metal-poor giants CS29498-043 and CS22949-037. The abundance of oxygen has been derived from measurements of the oxygen triplet at 7771-5 Å in high resolution and high S/N ratio near-IR spectra obtained with KeckI/HIRES. A detailed non-LTE analysis of Fe lines has been carried to provide more

We present new deep color-magnitude diagrams (CMD) at two galactocentric distances, and Ca II triplet spectroscopy, of the Local Group dSph galaxy Fornax, obtained with the VLT and FORS1. These data are being used to reliably derive the star formation and chemical enrichment histories of this galaxy, and preliminary results are presented here: we

We demonstrate a strong correlation between supermassive black hole (SMBH) mass and the global structure of ellipticals and bulges: more centrally concentrated bulges and ellipticals (higher Sérsic index n) host higher-mass black holes. This correlation is as good as that previously found between SMBH mass and central velocity dispersion, with

Lipid bilayers are key components of biomembranes; they are self-assembled two-dimensional structures, primarily serving as barriers to the leakage of cell's contents. Lipid bilayers are typically charged in aqueous solution and may electrostatically interact with each other and with their environment. In this work, we investigate electrostatics of

DQ white dwarfs have Teff values below 13000 K and are characterized by the presence of trace amounts of carbon in their helium-rich atmospheres. The wide range of surface carbon abundances they exhibit could be reflecting the existence of hydrogen-deficient white dwarfs with a variety of evolutionary history and formation processes. The aim of