We present some results from a new 2D spectrograph, SAURON (Bacon et al. 2001; de Zeeuw et al. 2002). Each SAURON, exposure provides stellar as well as gaseous kinematics and absorption line strength in the wavelength range (4800-5200 Å), covering an area of (33"x41"). We have observed a sample of 24 early-type spiral galaxies, and have obtained

We present high-time-resolution multicolour observations of the quiescent soft X-ray transient V404 Cyg obtained with ULTRACAM. Superimposed on the ellipsoidal modulation of the secondary star are large flares on time-scales of a few hours, as well as several distinct rapid flares on time-scales of tens of minutes. The rapid flares, most of which

All the projects of the Extremely Large Telescopes (ELTs) are based on segmented primary mirrors. This idea, solving the problem of producing single mirrors having diameter larger than 8m, introduces the needs for an accurate co-phasing of the various segments. The paper presents some laboratory measurements aimed to investigate the use of the

We investigate the nuclear and global structure of early-type galaxies, and the apparent disparity between the Nuker and Sersic models for radial light profiles. We show that the so-called "power-law" galaxies in fact have Sersic r1/n profiles over their entire observed radial range. Consequently, only three (Sersic-profile) parameters are required

We have compiled and studied photometric and spectroscopic data published in the literature of several star-forming regions and young open clusters (Orion, Taurus, IC 348, Sco-Cen complex, Chamaeleon I, TW Hydrae association, σ Orionis cluster, IC 2391, α Persei cluster, and the Pleiades). Our goal was to seek the definition of a simple empirical

Recent star count surveys of areas around globular star clusters have shown strong evidence of tidal tails stretching out many degrees beyond the cluster tidal radius. These tails are believed to be cluster stars which have escaped due to tidal shocking after passages through the disk of the Galaxy. Although the statistical star counts indicate and