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We present the results of our survey of 1612 MHz circumstellar OH maseremission from asymptotic giant branch (AGB) stars and red supergiants (RSGs) inthe Large Magellanic Cloud. We have discovered four new circumstellar masersources in the LMC, and increased the number of reliable wind speeds from IRstars in the LMC from 5 to 13. Using our new wind speeds, as well as those fromGalactic sources, we have derived an updated relation for dust driven winds:$v_{exp} \propto Z L^{0.4}$. We compare the sub-solar metallicity LMC OH/IRstars with carefully selected samples of more metal-rich OH/IR stars, also atknown distances, in the Galactic Centre and Galactic Bulge. For 8 of the Bulgestars we derive pulsation periods for the first time, using near-IR photometryfrom the VVV survey. We have modeled our LMC OH/IR stars and developed anempirical method of deriving gas-to-dust ratios and mass loss rates by scalingthe models to the results from maser profiles. We have done this also forsamples in the Galactic Centre and Bulge and derived a new mass lossprescription that includes luminosity, pulsation period, and gas-to-dust ratio$\dot{M} = 1.06^{+3.5}_{-0.8} \rm{ \cdot}10^{-5}\,(L/10^4\,\rm{L}_\odot)^{0.9\pm0.1}(P/500\,\rm{d})^{0.75\pm0.3}(r_{gd}/200)^{-0.03\pm0.07}\,\rm{M_{\odot}}\, yr^{-1}$. The tightestcorrelation is found between mass loss rate and luminosity. We find that thegas-to-dust ratio has little effect on the mass loss of oxygen-rich AGB starsand RSGs within the Galaxy and the LMC. This suggests that mass loss ofoxygen-rich AGB stars and RSGs is (nearly) independent of metallicity between ahalf and twice solar.

The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity