  If dark matter is composed of weakly interacting particles with mass in the
GeV-TeV range, their annihilation or decay may produce gamma rays that could be
detected by gamma-ray telescopes. Observations of dwarf spheroidal satellite
galaxies of the Milky Way (dSphs) benefit from the relatively accurate
predictions of dSph dark matter content to produce robust constraints to the
dark matter properties. The sensitivity of these observations for the search
for dark matter signals can be optimized thanks to the use of advanced
statistical techniques able to exploit the spectral and morphological
peculiarities of the expected signal. In this paper, I review the status of the
dark matter searches from observations of dSphs with the current generation of
gamma-ray telescopes: Fermi-LAT, H.E.S.S, MAGIC, VERITAS and HAWC. I will
describe in detail the general statistical analysis framework used by these
instruments, putting in context the most recent experimental results and
pointing out the most relevant differences among the different particular
implementations. This~will facilitate the comparison of the current and future
results, as well as their eventual integration in a multi-instrument and
multi-target dark matter search.
