  In current models for jets of AGNs and their emission a shortcoming in the
description and understanding of the connection between the largest and
smallest scales exists. In this work we present a spatially resolved SSC model
extended to parsec scales, which opens the possibility of probing the
connections between the radio and high energy properties. We simulate an
environment that leads to Fermi-I acceleration of leptonic particles and
includes the full time dependence of this process. Omitting the restriction of
a finite downstream region, we find that the spectral energy distribution (SED)
produced by the accelerated particles strongly depends on their radial
confinement behind the shock. The requirement, for both the restriction of high
energy emission to a small region around the shock and the production of a flat
radio spectrum, is an initial linear increase of the radius immediately behind
the shock, which then slows down with increasing distance from the shock. A
good representation of the data for the Blazar \textit{Mkn501} is achieved by a
parameterized log-function. The prediction for the shape of the radio blob is
given by the flux distribution with respect to shock distance.
