We derive atmospheric parameters and lithium abundances for 671 stars and include our measurements in a literature compilation of 1381 dwarf and subgiant stars. First, a "lithium desert" in the effective temperature (T eff) versus lithium abundance (A Li) plane is observed such that no stars with T eff ~= 6075 K and A Li ~= 1.8 are found. We

We present a new estimate of the lithium abundance in the atmosphere of the brown dwarf LP944-20. Our analysis is based on a self-consistent analysis of low-, intermediate- and high-resolution optical and near-infrared spectra. We obtain logN(Li) = 3.25 +/- 0.25 using fits of our synthetic spectra to the LiI resonance line doublet profiles observed

High-resolution spectra (range 655-675 nm) are presented of the pre-main sequence triple system UX Tau. Favorable seeing conditions allowed detection of the spectra of the faintest component, where detection of the H-alpha and the Li-I 670.7 nm feature are reported. An estimate of effective temperature, luminosity, and mass leads to the conclusion

Models of galaxy formation predict that gas accretion from the cosmic web is a primary driver of star formation over cosmic history. Except in very dense environments where galaxy mergers are also important, model galaxies feed from cold streams of gas from the web that penetrate their dark matter halos. Although these predictions are unambiguous

The LOFT mission concept is one of four candidates selected by ESA for the M3 launch opportunity as Medium Size missions of the Cosmic Vision programme. The launch window is currently planned for between 2022 and 2024. LOFT is designed to exploit the diagnostics of rapid X-ray flux and spectral variability that directly probe the motion of matter

The dissolution of fullerene C60 in oleum (fuming sulphuric acid 20 % free SO3) was followed simultaneously with ESR (Electron Spin Resonance) and NIR (Near Infrared Spectroscopy). It is shown that the intensity of the ESR signal associated to the formation of C60 radical cation (C60+•) follows the same kinetics as the NIR absoption band at about