We present 2.2 micron maps of selected areas of the Galactic Plane, taken with the 1.5 m. Sánchez-Magro telescope on the island of Tenerife. A model of the galactic stellar distribution has been developed and the derived stellar surface densities are compared with the observations. The results are in good agreement with the experimental data and suggest remarkable differences between
the luminosity functions for the disk and the spheroid components. The extinction toward the galactic centre shows an abrupt increase when compared with other galactic directions. We note also that a
better fit is obtained when the 5 Kpc ring is included in the model, but cannot infer from our data the existence of a thick disk.
The galactic plane has been sampled at 5´ spacing between l = 38° and J = 1-0 line of 13CO with the 2.5 m telescope of the Bordeaux Observatory. An automatic analysis of the data gives 181 clouds with masses ranging from a few solar msses to a few 10^5 M. Two spirals at liast can be fitted to our data.
The present-day mass function (PDMF) of field stars in the solar neighborhood is discussed. Major uncertainties in the derivation exist, in partlcular the luminosity-mass relation and the bolometric corrections. Consequently, It is not clear whether the PDMF turns over at very low masses (M < 0.3 Mq), and the slope at the
high-mass end (M > 10 Mq) is more uncertain than usually assumed. The reality of two features in the PDMF (at M = 1.2 Mq and M = 3 Mq respectively) is an open question. Next, the concept of a bimodal IMF is critically examined. Both Gůsten and Mezger's (1983) and Larson's (1986) bimodal models may run into problems. If the effects of high-mass stars prevent low-mass stars from forming, the term "biassed IMF" is a better
description of the situation than "bimodal IMF". The IMF is probably not universal; reported IMF variations in open clusters and globular clusters are unlikely to be spurious. Finally the physics of the IMF is discussed. The. fact that the mass of a star in the making depends on many random-valued (multlplicative) input parameters
suggests a stochastic rather than a deterministic approach for the origin of the IMF.
31 UV spectra obtained with tne LWR camera of the lUE satellite in the period 1978-83 were analysed. Changes of Mg II h and k emissions are evident but there is no evident correlation between emission intensity of Mg II and orbital or photometric phase. Using three various methods of analysis of possible periodicity in variation of Mg II h and k emission intensities we have found reál chanes in
h + k fluxes with period equal to the half of the orbital one, 0.5 Porb = 10.2606. We interpret this effect as evidence of direct influence of tidal inxeraction of secondary component on the chromospheric structure of the primary. Evident minimum of the Mg II h and k intensity is observed when the tides are on the line of sight and maximum when both tidal bulges are visible. Difference between maximum and minimum of total flux of k line is equal to about 20%, while the shape of the profile is practically unchanged.
The abundance of the objects with splitted nuclei among the candidates - the members of tight systems can be explained by the existence of bright HII regions in their central parts and also by the existence of dust lanes in their nuclear regions. 270 objects out of our lists are listed in IRAS catalogue.