Dissecting the hot bubbles in LMC-N57 with XMM-Newton
  We present a study of the diffuse X-ray emission from the star forming region
LMC-N 57 in the Large Magellanic Cloud (LMC). We use archival XMM-Newton
observations to unveil in detail the distribution of hot bubbles in this
complex. X-ray emission is detected from the central superbubble (SB) DEM L
229, the supernova remnant (SNR) 0532$-$675 and the Wolf-Rayet (WR) bubble DEM
L 231 around the WR star Br 48. Comparison with infrared images unveils the
powerful effect of massive stars in destroying their nurseries. The
distribution of the hot gas in the SNR and the SB display their maxima in
regions in contact with the filamentary cold material detected by IR images.
Our observations do not reveal extended X-ray emission filling DEM L 231,
although several point-like sources are detected in the field of view of this
WR nebula. The X-ray properties of Br 48 are consistent with a binary WN4$+$O
as proposed by other authors. We modeled the X-ray emission from the SB and
found that its X-ray emission can be simply explained by pressure-driven wind
model, that is, there is no need to invoke the presence of a SN explosion as
previously suggested. The pressure calculations of the hot gas confirms that
the dynamical evolution of the SB DEM L 229 is dominated by the stellar winds
from the star cluster LH 76.
