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We present a study of the diffuse X-ray emission from superbubbles N 70 (DEML301) and N 185 (DEM L25) located in the Large Magellanic Cloud, based on datafrom the XMM-Newton Satellite. We obtained spectra and images of these objectsin the soft X-ray energy band. These X-ray spectra were fitted by a thermalplasma model, with temperatures of $2.6 \times 10^{6}$ K and $2.3 \times10^{6}$ K, for N 70 and N 185, respectively. For N 70, images show that X-rayemission comes from the inner regions of the superbubble, when we compare thedistribution of the X-ray and the optical emission; while for N 185, the X-rayemission is partially confined by the optical shell. We suggest that theobserved X-ray emission is caused by shock-heated gas, inside of the opticalshells. We also obtained X-ray luminosities which exceed the values predictedby the standard analytical model. This fact shows that, in addition to thewinds of the interior stars, it is necessary to consider another ingredient inthe description, such as a supernova explosion, as has been proposed inprevious numerical models.

Diffuse X-ray emission from the superbubbles N 70 and N 185 in the Large Magellanic Cloud