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We use very deep spectra obtained with the Ultraviolet-Visual EchelleSpectrograph in the Very Large Telescope in order to determine the physicalconditions, the chemical abundances and the iron depletion factors of four H IIregions of the Large Magellanic Cloud and four H II regions of the SmallMagellanic Cloud. The spectral range covered is 3100-10400 $\mathring{A}$ witha resolution of $\Delta\lambda \sim \lambda / 8800$. We measure the intensityof up to 200 emission lines in each object. Electron temperature and electrondensity are determined using different line intensity ratios. The ionic andtotal abundances are derived using collisionally excited lines for O, N, S, Cl,Ne, Ar, and Fe. The uncertainties are calculated using Monte Carlo simulations.This is the largest available set of high quality spectra for H II regions inthe Magellanic Clouds. Thus, we can derive chemical abundances and depletionfactors and constrain their variations across each galaxy with better accuracythan previous studies. In particular, we find that the amount of Fe depleted onto dust grains in the H II regions of the Magellanic Clouds is similar to thatfound in Galactic H II regions.

The abundances of O, N, S, Cl, Ne, Ar, and Fe in H II regions of the Magellanic Clouds