Our present work introduces important advances with respect to previous astrometric studies, carried out over radio source pairs separated by smaller angular distances. We have consistently modeled the parameters involved in an astrometric VLBI observation, in order to reproduce the differential phase observed for radio sources separated by almost 7o on the sky. We have demonstrated the possibility of phase-connection over these angular distances at 8.4 GHz, even at an epoch of a maximum in the solar activity. After the phase-connection we have corrected the effects of the extended structure of the radio source and of the ionosphere. This last correction is one of the main technical achievements of this thesis: it is possible to remove the ionospheric contribution with independent measurements of the ionosphere total electron content obtained at Global Positioning Systems (GPS) sites the VLBI observing stations.
The triangular geometry introduces constraints in parameter space that allow a better estimation of the angular separations among the radio sources. It is possible to test the consistency of the astrometric results through the Sky-Closure, defined as the circular sum of the angular separations of the three radio sources, determined pairwise and independently. In our case it is consistent with zero, and verifies satisfactorily the data process followed.
The comparison of the measurements of the separations of the pair 1928+738/2007+777 (1991 data) with previous measurements (data from 1985 and 1988), carried out with the same technique, allows us to register adequately the absolute position of 1928+738 relative to 2007+777. We estimate the proper motion of components in 1928+738, and also identify the position of the radio source core. We confirm the superluminal motion of the components of 1928+738. The comparison of our results with those obtained by Eubanks (USNO) from group delay measurements (without structure correction) show the incorrectness of the latter.
We also include succinctly in this PhD my colaboration in the work on the radio supernova SN 1993J, in galaxy M81. We have discovered a shell-like structure of the radio emission of SN 1993J which exploded on March 1993. We have also elaborated a movie of its evolution, by monitoring the shell structure for different epochs, and determined the deceleration of its expansion.
