The XMM-Newton view of the DEM L36 superbubble in the Large Magellanic Cloud

Massive star-forming regions are important laboratories for our understanding of stellar feedback mechanisms in galaxies. They often contain superbubbles, which are large cavities of hot, shock-heated gas powered by massive stellar winds and subsequent supernovae. We present the first multi-wavelength analysis of the superbubble in the Large Magellanic Cloud. We characterise its physical properties for a comparison to model predictions. Additionally, we compare the superbubble with other Galactic and Magellanic Cloud superbubbles. We used data from , supplemented by data from the Magellanic Cloud Emission Line Survey, the Dark Energy Camera Magellanic Cloud Emission Line Survey, the Space Telescope, and the Australia Telescope Compact Array. We performed a multi-wavelength morphological analysis to understand the shape and structure of the superbubble and an X-ray spectral analysis to derive the physical parameters of the hot gas. XMM-Newton Spitzer We find significant X-ray emission in that is dominated by a central bubble region mostly confined by a thin Hα filamentary shell. This has two distinct blowout regions to the east and west, with a possible smaller blowout in the south. The spectral analysis shows that the X-ray emission is well fit with a thermal plasma model in collisional ionisation equilibrium with a temperature of kT=0.17 (0.16-0.18) keV and an unabsorbed luminosity L_ X (0.5-7.0 ) keV =3.62 erg s 10^ 35 -1 . Unlike in other Large Magellanic Cloud superbubbles, no clear powering cluster lies at the centre, although relatively small clusters near the edge likely supply the mechanical input at the present epoch. We used photometric data of these clusters to estimate the cluster masses, ages, and mechanical inputs for a comparison with the energy stored in the superbubble. These clusters have supplied more energy over their lifetime than is currently observed in the superbubble, which is indicative of the so-called growth rate discrepancy problem. The superbubble was probably initially shaped by a central massive stellar population that has since dispersed and largely lost to supernovae, with smaller clusters at the edges of the swept-up shell that currently supply the energy input.