X-ray spectroscopy of the starburst feedback in 30 Doradus
  X-ray observations provide a potentially powerful tool to study starburst
feedback. The analysis and interpretation of such observations remain
challenging, however, due to various complications, including the
non-isothermality of the diffuse hot plasma and the inhomogeneity of the
foreground absorption. We here illustrate such complications and a way to
mitigate their effects by presenting an X-ray spectroscopy of the 30 Doradus
nebula in the Large Magellanic Clouds, based on a 100 ks Suzaku observation. We
measure the thermal and chemical properties of the hot plasma and
quantitatively confront them with the feedback expected from embedded massive
stars. We find that our spatially resolved measurements can be well reproduced
by a global modeling of the nebula with a log-normal temperature distribution
of the plasma emission measure and a log-normal foreground absorption
distribution. The metal abundances and total mass of the plasma are consistent
with the chemically enriched mass ejection expected from the central OB
association and a ~55% mass-loading from the ambient medium. The total thermal
energy of the plasma is smaller than what is expected from a simple superbubble
model, demonstrating that important channels of energy loss are not accounted
for. Our analysis indeed shows tentative evidence for a diffuse non-thermal
X-ray component, indicating that cosmic-ray acceleration needs to be considered
in such a young starburst region. Finally, we suggest that the log-normal
modeling may be suitable for the X-ray spectral analysis of other giant HII
regions, especially when spatially resolved spectroscopy is not practical.
