The star formation history (SFH) of the Pegasus dIr, a likely Local Group member at 0.95 Mpc from the Milky Way, is investigated. We characterize the SFH by two basic functions: the star formation rate, psi (t), and the chemical enrichment law, Z(t). It has been derived by comparing the color-magnitude diagram of the resolved stars in Pegasus, with

We derive the relative distances to the Virgo, Fornax and Coma clusters of galaxies by applying the D_n-sigma and the Fundamental Plane (FP) relations to the data of the homogeneous samples of early-type galaxies studied by Caon et al., Lucey et al. and Jorgensen et al. The two distance indicators give consistent results, the relative distance

The number of minor bodies in the Solar System is continuing to increase. More than 30,000 asteroids have been discovered by 1996, and about 7,000 have been catalogued. About 855 comets had known orbits by 1994. The number of known planetary satellites reached 60 (1996). All these minor bodies require improved astrometry, also more accurate

We present a detailed analysis of the cosmic microwave background (CMB) structure in the Tenerife Dec.=+40 deg data. The effect of local atmospheric contributions on the derived fluctuation amplitude is considered, resulting in an improved separation of the intrinsic CMB signal from noise. Our analysis demonstrates the existence of common structure

A high-resolution study of fragment-fragment-$gamma$ triple coincident measurements of the symmetric-mass fission exit-channel from the ^{28}Si+^{28}Si reaction has been performed at the VIVITRON Tandem facility by using the EUROGAM Phase II $gamma$-ray spectrometer. The bombarding energy E_{lab}(^{28}Si) = 111.6 MeV has been chosen to populate a

We have modelled the spectral energy distributions of the 13 Hubble Deep Field (HDF) galaxies reliably detected by the Infrared Space Observatory (ISO). For two galaxies the emission detected by ISO is consistent with being starlight or the infrared `cirrus' in the galaxies. For the remaining 11 galaxies there is a clear mid-infrared excess, which