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The stellar metallicity and its gradient pose constraints to the formationand evolution of galaxies. This is a study of the metallicity gradient of theLMC, SMC and M33 galaxies derived from their asymptotic giant branch (AGB)stars. The [Fe/H] abundance was derived from the ratio between C- and M-typeAGB stars and its variation analysed as a function of galactocentric distance.Galaxy structure parameters were adopted from the literature. The metallicityof the LMC decreases linearly as -0.047+/-0.003 dex/kpc out to ~8 kpc from thecentre. In the SMC, [Fe/H] has a constant value of ~ -1.25+/-0.01 dex up to ~12 kpc. The gradient of the M33 disc, until ~ 9 kpc, is -0.078+/-0.003 dex/kpcwhile an outer disc/halo, out to ~ 25 kpc, has [Fe/H] ~ -1.7 dex. Themetallicity of the LMC, as traced by different populations, bears the signatureof two major star forming episodes: the first one constituting a thickdisc/halo population and the second one a thin disc and bar due to a closeencounter with the MW and SMC. The [Fe/H] of the recent episode supports an LMCorigin for the Stream. The metallicity of the SMC supports star formation, ~ 3Gyr ago, as triggered by LMC interaction and sustained by the bar in the outerregion of the galaxy. The SMC [Fe/H] agrees with the present-day abundance inthe Bridge and shows no significant gradient. The metallicity of M33 supportsan ``inside-out'' disc formation via accretion of metal poor gas from theinterstellar medium.

The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies