We recently discovered an unresolved radio source coincident with the ultraluminous X-ray source (ULX) IC 342 X-1. The radio emission and hard X-ray spectrum of the source suggest that it is a compact object accreting in the X-ray hard/radio loud state. This enables use of the fundamental plane relation, found valid for stellar to supermassive

Images of asteroid (596) Scheila have been acquired at various dates after the discovery of the 2010 outburst. Assuming a short-duration event scenario, as suggested by the quick vanishing of the dust tail brightness with time, and numerically integrating the equation of motion of individual particles ejected from the surface, we have developed a

Multi-object spectroscopic observations of A545 were carried out at the TNG telescope in October 2009. We used DOLORES/MOS with the LR-B Grism 1, yielding a dispersion of 187Å/mm. We used the new 2048x2048pixels E2V CCD, with a pixel size of 13.5um. In total, we observed 4 MOS masks for a total of 142 slits. We acquired three exposures of 1200s for

Multi-object spectroscopic observations of A2345 were carried out at the TNG telescope in August 2008. We used DOLORES/MOS with the LR-B Grism 1, yielding a dispersion of 187Å/mm. We used the new E2V CCD, a matrix of 2048x2048 pixels with a pixel size of 13.5um. In total we observed four MOS masks for a total of 147 slits. Total exposure times were

We used the CLUMPY torus models and a Bayesian approach to fit the infrared spectral energy distributions and ground-based high angular resolution mid-infrared spectroscopy of 13 nearby Seyfert galaxies. This allowed us to put tight constraints on torus model parameters such as the viewing angle i, the radial thickness of the torus Y, the angular

We investigate the column density distribution function of neutral hydrogen at redshift z = 3 using a cosmological simulation of galaxy formation from the OverWhelmingly Large Simulations project. The base simulation includes gravity, hydrodynamics, star formation, supernovae feedback, stellar winds, chemodynamics, and element-by-element cooling in