The relation between the surface velocity of a pulsating star in the star's inertial frame and the apparent expansion velocity measured by a remote observer has been classically formulated in terms of a projection factor p. This factor depends on the relative limb darkening in continuum and spectral lines and may therefore be a function of

We have selected a sample of 55 kpc-sized flat spectrum radio sources from the JVAS/CLASS1 surveys which contain about 4800 objects. Optical (photometry and spectroscopy) and higher resolution radio follow ups are being carried out. Our sample is characterized by objects dominated by radio emission on kpc scales and splits, morphologically, into

We have extended our evolutionary synthesis models for star forming regions to the γ-ray domain. We obtain the light-curves of γ-ray line emission due to radioactive decay of stellar nucleosynthesis products, such as 26 Al, 60 Fe, or the e- e+ annihilation line as well as the evolution of the kinetic energy from massive stars. We present the

The description of the PESCA instrument control system is presented. The PESCA instrument has been designed and built with the purpose of studying the Solar Energetic Particles and the Anomalous Cosmic Rays from helium to iron in the energy range 1.5-50 MeV/uma and will be part of the Russian PHOTON satellite payload. The instrument comprises two

Over the past 12 years we have been conducting a survey of IRAS (PSC) sources with dust temperatures between 100 and 250 K, which is the temperature of AGB shells after mass loss has ceased. About 1000 PSC sources fulfill this criterion, about half of them identified previously in the literature: most are PNe (49%) and post-AGB stars (27%), but

We test the hypothesis that radio galaxies are a random subset of otherwise normal elliptical galaxies. Starting with the observed optical luminosity functions for elliptical galaxies, we show that the probability of an elliptical forming a radio source is a continuous, increasing function of optical luminosity, proportional to L2+/-0.4. With this