  Since its launch in 2008, the Fermi Large Area Telescope (LAT) has detected
over 200 -ray pulsars above 100 MeV. This population of pulsars is
characterised by a rich diversity of light curve morphologies. Researchers have
been using both the radio and -ray light curves to constrain the inclination
and observer angles for each of these pulsars. At first, this was done using a
by-eye technique and later via statistical approaches. We have also developed
two novel statistical approaches that place the radio and -ray data on equal
footing despite their disparate relative flux errors. We chose eleven pulsars
from the Second Fermi Pulsar Catalog, both old and young, and applied these new
techniques as well as the by-eye technique to constrain their geometric
parameters using standard pulsar models. We present first results on our
comparison of the best-fit parameters yielded by each of the aforementioned
techniques. This will assist us in determining the utility of our new
statistical approaches, and gauge the overlap of the best-fit parameters (plus
errors) from each of the different methods. Such a statistical fitting approach
will provide the means for further pulsar magnetospheric model development
using light curve data.
