We present the discovery of a companion near the deuterium-burning mass limit located at a very wide distance, at an angular separation of 4.6''+/-0.1'' (projected distance of ~ 670 AU) from UScoCTIO 108, a brown dwarf of the very young Upper Scorpius association. Optical and near-infrared photometry and spectroscopy confirm the cool nature of both

Aims:The “bright” High Frequency Peakers (HFPs) sample is a mixture of blazars and intrinsically small and young radio sources. We investigate the polarimetric characteristics of 45 High Frequency Peakers, from the “bright” HFP sample, in order to have a deeper knowledge of the nature of each object, and to construct a sample made of genuine young

We present simultaneous high time resolution (1-10 Hz) X-ray and optical observations of the persistent LMXBs Sco X-1 and V801 Ara( = 4U 1636-536). In the case of Sco X-1 we find that the Bowen/HeII emission lags the X-ray light-curves with a light travel time of ~11-16 s which is consistent with reprocessing in the donor star. We also present the

New z-band (F850LP, denoted z850 hereafter) imaging was obtained with the ACS camera onboard HST in November 2004 (AC114) and July 2005 (Abell 1835). The 3.6, 4.5, 5.8, and 8.0{mu}m images were obtained using the Infrared Array Camera (IRAC), while the 24{mu}m images were obtained using the Multi-band Imaging Photometer for Spitzer (MIPS), both

We present near-infrared (H- and K-band) integral-field observations of the circumnuclear star formation rings in five nearby spiral galaxies. The data, obtained at the Very Large Telescope with the SINFONI spectrograph, are used to construct maps of various emission lines that reveal the individual star forming regions ("hot spots") delineating

We propose to continue a northern sky program using high resolution, moderate S/N spectra to discover the chemically oldest stars - ultra metal-poor dwarfs and giants drawn from the Hamburg/ESO and SEGUE surveys. With these data we seek to (1) discover more stars with [Fe/H] -4.0 (only three of which are known and all of which our group has