The faint nebulosity CM24=PP85 listed by Parsamian and Petrosian (1979) was observed at infrared (1-10 pm) and radio (6 cm and CO line) wavelengths in the vicinity of the CO "hot spot" reported by Torrelles et al. (1983). The radio continuum (6 cm) emission from a spherically symmetrical HIl region was detected with the Very Large Array. Its

The initial orientation of 74 active regions (ARs) as measured in high resolution pictures. As previous works by the author (Garcia de la Rosa, 1984) suggest a different behavior between large and small active regions, the sample has been divided into those two classes, whose dividing line is roughly set at 5 x 10 to the 21st Mx in the magnetic

We obtained at the Coude Echelle Spectrometer (CES) attached to the 1.4m CAT telescope of the European Southern Observatory ,high resolution (R=1O0000),high signal to noise (S/N=30-20O) spectra of the Ca II H and k,H alpha and Ca II infrared triplet lines on a sample of southern late-type dwarfs also observed with lUE for the Mg II h and k lines

B-magnitudes have been compiled from the literature for 3C 345, covering a period from 1965 to 1980, 905 values in all. Since the last major study of the light-curve of this object (Barbieri et al., 1977), new and also revised data have been presented, which extend the light-curve and improve the temporal resolution. A compilation of the

A model of the galactic stellar distribution has been developed and the surface stellar densities in the near infrared are compared with observations along the galactic plane between l = 0° and l = 10°. The model, based on data taken from the literature, is in reasonable agreement with the observational results. However, the mass distribution