  We explore the emission properties of a dissipative pulsar magnetosphere
model introduced by Kalapotharakos et al. (2014), comparing its high energy
light curves and spectra, due to curvature radiation, with data collected by
the Fermi LAT. The magnetosphere structure is assumed to be near the force-free
solution. The accelerating electric field, inside the light-cylinder, is
assumed to be negligible, while outside the light-cylinder it rescales with a
finite conductivity ({\sigma}). In our approach we calculate the corresponding
high energy emission by integrating the trajectories of test particles that
originate from the stellar surface, taking into account both the accelerating
electric field components and the radiation reaction forces. First we explore
the parameter space assuming different value sets for the stellar magnetic
field, stellar period, and conductivity. We show that the general properties of
the model are in a good agreement with observed emission characteristics of
young {\gamma}-ray pulsars, including features of the phase resolved spectra.
Second we find model parameters that fit each pulsar belonging to a group of
eight bright pulsars that have a published phase-resolved spectrum. The
{\sigma} values that best describe each of the pulsars in this group show an
increase with the spin-down rate $(\dot{E})$ and a decrease with the pulsar
age, expected if pair cascades are providing the magnetospheric conductivity.
Finally, we explore the limits of our analysis and suggest future directions
for improving such models.
