Multiwavelength analysis of the X-ray spur and southeast of the Large
  Magellanic Cloud
  Aims: The giant HII region 30 Doradus (30 Dor) located in the eastern part of
the Large Magellanic Cloud is one of the most active star-forming regions in
the Local Group. Studies of HI data have revealed two large gas structures
which must have collided with each other in the region around 30 Dor. In X-rays
there is extended emission ($\sim 1$ kpc) south of 30 Dor called the X-ray
spur, which appears to be anticorrelated with the HI gas. We study the
properties of the hot interstellar medium (ISM) in the X-ray spur and
investigate its origin including related interactions in the ISM. Methods: We
analyzed new and archival XMM-Newton data of the X-ray spur and its
surroundings to determine the properties of the hot diffuse plasma. We created
detailed plasma property maps by utilizing the Voronoi tessellation algorithm.
We also studied HI and CO data, as well as optical line emission data of
H$\alpha$ and [SII], and compared them to the results of the X-ray spectral
analysis. Results: We find evidence of two hot plasma components with
temperatures of $kT_1 \sim 0.2$ keV and $kT_2 \sim 0.5-0.9$ keV, with the
hotter component being much more pronounced near 30 Dor and the X-ray spur. In
30 Dor, the plasma has most likely been heated by massive stellar winds and
supernova remnants. In the X-ray spur, we find no evidence of heating by stars.
Instead, the X-ray spur must have been compressed and heated by the collision
of the HI gas.
