We present two high dynamic range images of the quasar 3C 345 from observations at lambda 18 cm (1990.74) and at lambda 49 cm (1990.72). The simultaneous observations at two wavelengths have made it possible to construct a spectral index map covering the core and the extended jet. At a distance of similar to 15 mas the jet flares out and the emission beyond this is probably due to optically thick self-absorbed synchrotron radiation, while the radiation downstream is due to emission from an adiabatically expanding plasma. We conclude that the flaring out is either due to a standing shock caused by the jet passing into a region of different density, or due to large scale oscillations in a helical jet disrupting the collimated flow. There is a tentative detection of a feature extending perpendicular from the jet in connection with the jet flaring out. We suggest that this either may be the beamed part of a backflow connected to the standing shock and the turbulent region, or a coherent structural part of a wider turbulent flow.

On June 11 and 15, 1985 two packages with balloons have been inserted in the atmosphere of Venus from the Soviet VEGA landing modules. This paper summarizes the pressure, temperature, wind illumination and backscattering data from the balloons.

The traces of a radio jet from the NGC 1275 galaxy nucleus are revealed in position angle (PA) +45° using the data of published observations at 18, 20, and 73 cm wavelengths. The jet has a distorted form and is seen at 6′–7′ distance from the nucleus where its PA=+20°. It is shown that the optical detail situated 7″ north-east from the nucleus of the galaxy is projected exactly on the trace of the radio jet. It is supposed that the radio jet is connected with this optical detail, a group of stars. One may compare theree radio jets in the circumstellar region of the NGC 1275 galaxy: the youngest in PA=149°, the older in PA=−15° and +145° with the centres of star formations in a 6″ circumnuclear region. Their ages differ as the ages of corresponding radio jets.

A global array of 20 radio observatories was used to measure the three-dimensional position and velocity of the two meteorological balloons that were injected into the equatorial region of the Venus atmosphere by the VEGA spacecraft.

The trajectories of the motion of balloons floating freely in the Venusian atmosphere (the Vega project) are measured via VLBI. The balloon in the southern hemisphere moved with an average velocity of 66 m/s. The latitudinal velocity component was equal to 3.4 + or - 0.5 m/s and was directed northward. The velocity of the balloon in the northern hemisphere was equal to 69 m/s and was directed nearly parallel to the equator.

VLBI observations were performed of 21 radio sources which exhibit low frequency variability. The integrated flux densities, variability indices at 0.4 GHz, optical magnitudes, redshifts, spectral indices at 0.4 GHz, and flux intensities with respect to a reference energy flux are provided. The VLBI data were synthesized from observatories located on different continents around the world. All structures were emitted from compact sources with sizes confined to milliarcsc scales. Nearly half displayed core-jet morphologies, while 28 percent had complex structures and 14 percent had either simple structures or were not resolvable. Further observations are proceeding at 400 mHz to confirm the presence of synchrotron electrons and magnetic fields ejected at relativistic speeds along the line of sight, which has the appearance of superluminal velocities.