  Gamma-Ray Bursts (GRBs) are widely thought to originate from collimated jets
of material moving at relativistic velocities. Emission from such a jet should
be visible even when viewed from outside the angle of collimation. I summarize
recent work on the special relativistic transformation of the burst quantities
Eiso and Epeak as a function of viewing angle, where Eiso is the
isotropic-equivalent energy of the burst and Epeak is the peak of the burst
spectrum in the power nu F_nu. The formulae resulting from this work serve as
input for a Monte Carlo population synthesis method, with which I investigate
the importance of off-jet relativistic kinematics as an explanation for a class
of GRBs termed "X-ray Flashes" (XRFs). I do this in the context of several
top-hat shaped variable opening-angle jet models. I find that such models
predict a large population of off-jet bursts that are observable and that lie
away from the Epeak ~ Eiso^(1/2) relation. The predicted burst populations are
not seen in current datasets. I investigate the effect of the bulk gamma value
upon the properties of this population of off-jet bursts, as well as the effect
of including an Omega0-Egamma correlation to jointly fit the Epeak ~ Eiso^(1/2)
and Epeak ~ Egamma^(beta) relations, where Omega0 is the opening solid angle of
the GRB jet. I find that the XRFs seen by HETE-2 and BeppoSAX cannot be easily
explained as classical GRBs viewed off-jet. I also find that an inverse
correlation between gamma and Omega0 has the effect of greatly reducing the
visibility of off-jet events. Therefore, unless gamma > 300 for all bursts or
unless there is a strong inverse correlation between gamma and Omega0, top-hat
variable opening-angle jet models produce a significant population of bursts
away from the Epeak ~ Eiso^(1/2) and Epeak ~ Egamma^(beta) relations.
