We present two XMM-Newton observations of Jupiter, which were carried out in April and November 2003 for 110 and 250 ks (or 3 and 7 planet rotations) respectively. X-ray images taken with XMM-Newton EPIC CCD cameras show prominent emission, essentially all confined to the 0.2 - 2.0 keV band, from Jupiter's auroral spots; their spectra can be

We report on ESO-VLT near-IR adaptive optics imaging of one radio-loud (PKS 0113-283) and two radio quiet (Q 0045-3337 and Q 0101-337) quasars at z > 2. In the first case we are able to resolve the QSO and find that it is hosted by an elliptical of absolute magnitude MK = -27.6. For the other two objects no extended emission has been unambiguously

We present Very Small Array (VSA) observations (centred on ~34 GHz) on scales ~20 arcmin towards a complete, X-ray flux-limited sample of seven clusters at redshift z 0.1. Four of the clusters have significant Sunyaev-Zel'dovich (SZ) detections in the presence of cosmic microwave background (CMB) primordial anisotropy. For all seven, we use a

The present paper is a progress report on our work towards estimating the energy emission involved in the many Gamma-Ray Bursts for which no redshift has been actually measured. Once such an estimate is obtained, we can try to extend the E peak rest-Eiso relation found by Amati et al.(Astron. Astrophys., 390 (2002) 81) to those events. Following

We present a wide field V-band imaging survey of approximately 1 deg2 (~7.2~h-275 Mpc2) in the direction of the nearby cluster of galaxies Abell 2151 (the Hercules Cluster). The data are used to construct the luminosity function (LF) down to MV ≈ -14.85, thus allowing us to study the dwarf galaxy population in A2151 for the first time. The obtained

We explore the formation and evolution of hydrogen-deficient post-AGB white dwarfs. To this end, we compute the complete evolution of an initially 2.7 ~M&sun; star from the zero-age main sequence through the thermally pulsing and mass-loss phases to the white dwarf stage. Particular attention is given to the chemical abundance changes during the