  A new revision of the gamma flux that we expect to detect in Imaging
Atmospheric Cherenkov Telescopes (IACTs) from SUSY dark matter annihilation in
the Draco dSph is presented using the dark matter density profiles compatible
with the latest observations. This revision takes also into account the
important effect of the Point Spread Function (PSF) of the Cherenkov telescope.
We show that this effect is crucial in the way we will observe and interpret a
possible signal profile in the telescope. Given these new considerations, some
light can be shed on the recent signal excess reported by the CACTUS
experiment.
