The abundances of O, N, S, Cl, Ne, Ar, and Fe in H II regions of the
  Magellanic Clouds
  We use very deep spectra obtained with the Ultraviolet-Visual Echelle
Spectrograph in the Very Large Telescope in order to determine the physical
conditions, the chemical abundances and the iron depletion factors of four H II
regions of the Large Magellanic Cloud and four H II regions of the Small
Magellanic Cloud. The spectral range covered is 3100-10400 $\mathring{A}$ with
a resolution of $\Delta\lambda \sim \lambda / 8800$. We measure the intensity
of up to 200 emission lines in each object. Electron temperature and electron
density are determined using different line intensity ratios. The ionic and
total 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 in
the Magellanic Clouds. Thus, we can derive chemical abundances and depletion
factors and constrain their variations across each galaxy with better accuracy
than previous studies. In particular, we find that the amount of Fe depleted on
to dust grains in the H II regions of the Magellanic Clouds is similar to that
found in Galactic H II regions.
