In chapter 2, a brief theoretical introduction to the fundamentals of aperture synthesis is given, followed by a discussion of the SHEVE operation and the reduction path that SHEVE data takes.
In chapters 3 to 8, the observations of the radio sources are described in order of their right ascension. In chapter 3, the first multi epoch and multi frequency VLBI imaging observations of the low red shift FR II type radio galaxy PKS 0518-458 (Pictor A) are described and related to sub-arcsecond optical imaging observations from the Hubble Space Telescope (HST).
In chapter 4, multi epoch and multi frequency SHEVE observations of the radio galaxy PKS 0521-365 are described. Prompted by the identification of PKS 0521-365 by EGRET, an extensive comparison of the VLBI properties of EGRET-identified sources with the VLBI properties of similar radio sources not identified by EGRET has been made. Observations of PKS 1514-241, another of the low red shift sources, has been used in this study. Results from the comparison are also given in chapter 4.
In chapter 5, the most extensive VLBI observations of the closest active radio galaxy, PKS 1322-427 (Centaurus A, NGC 5128), are described. Multi frequency and multi epoch observations are described, as well as VLBI observations which utilised the SHEVE array in conjunction with the VLBA.
In chapter 6, SHEVE observations of the Galactic X-ray and radio source GRO J1655-40 are presented.
In chapter 7, the first VLBI imaging observations of the unusual low red shift radio galaxy PKS 1718-649 (NGC 6328) are discussed. A consideration of multi frequency data from optical to radio wavelengths, from the sub-pc-scale to the kpc-scale, show that this source is probably the lowest red shift example of a GHz Peaked-Spectrum radio source.
In chapter 8, the first VLBI imaging observations of the low red shift radio galaxy PKS 2152-699 are discussed. The relationships between the pc-scale radio source and the kpc-scale radio and optical structure of the galaxy are discussed and a model to explain the relationships is developed and presented.
Finally, in chapter 9, a summary of the properties of the Southern Hemisphere component of the ``Whole-Sky'' sample is given as well as a brief literature review of the properties of the Northern Hemisphere sources in the sample. Thus, for the first time, a ``Whole-Sky'' sample of nearby, bright, and compact radio sources is assembled and its VLBI properties described.