  Regions of different metallicity have been identified in the Magellanic
Clouds by using the ratio between Asymptotic Giant Branch stars of spectral
type C and M. In the Large Magellanic Cloud the ratio appears to decrease
radially while in the Small Magellanic Cloud (SMC) there is no clear trend,
reflecting either the large extension of the SMC along the line of sight or a
more complex star formation history. The distribution of the C/M ratio is
clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There
is an indication of increasing C/M ratio, thus decreasing metallicity, towards
the Bridge region connecting the two Clouds.
