Between Oct 1999 and Jun 2001 Chandra observed M31 on a nearly monthly schedule. These observations allowed the discovery of 14 X-ray transients, a few of which were followed up with HST in an attempt to find contemporaneous optical counterparts. The transient most luminous in X-rays shows a possible U ~23 counterpart in HST imaging. The ratio of

We present the first light curves in the infrared J and K filters of VV UMa and analyze them, together with a new set of BVR light curves obtained in different runs from 1997 to 2000. Based on the spectra of VV UMa and standard stars in the region 8440-8870 Å, we classify the primary component of the binary as a type A1.5-2 V star. Evidence of

We have derived beryllium abundances in a wide sample of stars hosting planets, with spectral types in the range F7V-K0V, aimed at studying in detail the effects of the presence of planets on the structure and evolution of the associated stars. Predictions from current models are compared with the derived abundances and suggestions are provided to

We present terminal velocities of M 33 B-supergiants, obtained from STIS HST spectra as part of our programme to investigate the Wind Momentum - Luminosity Relationship (WLR) in the Local Group. Terminal velocities are derived from their N V, C Iv, and Si Iv resonance lines in UV spectra. Comparing with IUE spectra of Galactic B-supergiants we

We present the first results from an X-ray and optical survey of a sample of radio jets in active galactic nuclei with Chandra and the Hubble Space Telescope (HST). We focus here on the first six sources observed in X-ray, in four of which a bright X-ray jet was detected for the first time. In three out of the four cases, optical emission from the

We measured the bar pattern speed, Ωp , of the SB0 galaxy NGC 1023 using the Tremaine-Weinberg method with stellar-absorption slit spectroscopy. The morphology and kinematics of the Hi gas outside NGC 1023 suggest it suffered a tidal interaction, sometime in the past, with one of its dwarf companions. At present, however, the optical disc is