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Using the PACS and SPIRE spectrometers on-board the Herschel SpaceObservatory, we obtained spectra of two red supergiants (RSGs) in the LargeMagellanic Cloud (LMC). Multiple rotational CO emission lines (J=6-5 to 15-14)and 15 H2O lines were detected from IRAS 05280-6910, and one CO line wasdetected from WOH G64. This is the first time CO rotational lines have beendetected from evolved stars in the LMC. Their CO line intensities are as strongas those of the Galactic RSG, VY CMa. Modelling the CO lines and the spectralenergy distribution results in an estimated mass-loss rate for IRAS 05280-6910of 3x10^-4 Msun per yr. The model assumes a gas-to-dust ratio and a CO-to-H2abundance ratio is estimated from the Galactic values scaled by the LMCmetallicity ([Fe/H]~-0.3), i.e., that the CO-to-dust ratio is constant forGalactic and LMC metallicities within the uncertainties of the model. The keyfactor determining the CO line intensities and the mass-loss rate found to bethe stellar luminosity.

The mass-loss rates of red supergiants at low metallicity: Detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud