  The nearby dwarf irregular galaxies the Large and Small Magellanic Clouds
have metallicities of about half and a fifth solar, respectively, which offers
the unique opportunity to study astrophysical processes as a function of
metallicity. Masers in the outflows from evolved stars allow to measure the
wind speed, vital to derive mass-loss rates and test wind driving mechanisms.
The metallicity dependence of the wind speed in particular allows us to make
inferences about dust formation and mass loss in the early Universe. I will
review past surveys for circumstellar OH, water, and SiO masers in the
Magellanic Clouds (and provide a literature review of interstellar masers). I
will then discuss the way these measurements have influenced our understanding
of mass loss, and end with outlining the prospects for future surveys for OH
masers in the Magellanic Clouds.
