  Pulsar radio emission and its polarization are observed to evolve with
frequency. This frequency dependence is key to the emission mechanism and the
structure of the radio beam. With the new Ultra-Wideband receiver (UWL) on the
Parkes radio telescope we are able, for the first time, to observe how pulsar
profiles evolve over a broad continuous bandwidth of 700-4000 MHz. We describe
here a technique for processing broadband polarimetric observations to
establish a meaningful alignment and visualize the data across the band. We
apply this to observations of PSRs J1056-6258 and J1359-6038, chosen due to
previously unresolved questions about the frequency evolution of their
emission. Application of our technique reveals that it is possible to align the
polarization position angle (PA) across a broad frequency range when
constrained to applying only corrections for dispersion and Faraday rotation to
do so. However, this does not correspond to aligned intensity profiles for
these two sources. We find that it is possible to convert these misalignments
into emission height range estimates that are consistent with published and
simulated values, suggesting that they can be attributed to relativistic
effects in the magnetosphere. We discuss this work in the context of the radio
beam structure and prepare the ground for a wider study of pulsar emission
using broadband polarimetric data.
