  The accreting millisecond pulsar XTE J1807-294 is studied through a pulse
shape modeling analysis. The model includes blackbody and Comptonized emission
from the one visible hot spot and makes use of the Oblate Schwarzschild
approximation for ray-tracing. We include a scattered light contribution, which
accounts for flux scattered off an equatorial accretion disk to the observer
including time delays in the scattered light. We give limits to mass and radius
for XTE J1807-294 and compare to limits determined for SAX J1808-3658 and XTE
J1814-334 previously determined using similar methods. The resulting allowed
region for mass-radius curves is small but is consistent with a mass-radius
relation with nearly constant radius (~12 km) for masses between 1 and 2.5
solar masses.
