We still do not know if PAHs (or other carbon dominated elements)
 exist in environments as deficient in metal as in the case of the
 SMC. From the ultraviolet observations, the SMC mean extinction
 curve shows a very weak bump at 0.22 microns compared to the
 galactic curve. The LMC curve is intermediate between the SMC and
 Milky Way curves. This observational fact is thought to be related
 to the underabundance of carbon in the interstellar dust in these
 irregular galaxies compared to the solar neighborhood. From the
 IRAS observations on the SMC one observes a very weak mid-infrared
 (12 and 25 microns) emission. There seems to be a tight
 correlation between the ratio nu*I(12 microns) to far-infrared
 and the abundance O/H, which suggests that the weakness of the
 12 microns emission is due to a metallicity effect.
 The search of the PAH features in the Magellanic Clouds will
 permit a more quantitative analysis in the frame of models
 accounting for the underabundance of carbon in the dust grain
 population.
 The principal goals of this proposal are:
 1) the detection of the near infrared features at 7.7 and 11.3
    microns.
 2) a sensitive photometry over a broad range of wavelengths to
    constrain the models of grain population (composition and
    size distribution).
 3) measuring occasional contribution of line emissions in the far
    infrared.
 4) comparison between the far infrared emission and HI
    distribution.