ISOCAM will be used to survey selected regions of the Small
 and Large Magellanic Clouds in order to detect evolved stars
 with mass loss. These stars will be primarily identified by
 their observed infrared colors. The sources detected will
 also be compared with ground-based spectroscopic and near-ir
 surveys of the same fields. The populations in the two
 galaxies will be compared to see whether the sizes of the
 detected excesses are proportional to metal abundance,
 which would imply roughly constant mass-loss rates for
 similar stars in the two galaxies. If the mass loss rates are
 not similar, or source densities are very different
 the data set should be large enough to look for other
 effects that may explain the differences, for example
 effects related to the different C to M star ratios in the
 LMC and SMC.