Speaker
Description
We investigate the diffuse X-ray emission around the HII region LHA 120-N11, one of the most active star-forming regions in the Large Magellanic Cloud (LMC). Using data from the eROSITA telescope on the Spectrum-Roentgen-Gamma (SRG) mission, we defined four spectral extraction regions based on the morphology of the X-ray emission to determine the physical properties of the hot diffuse X-ray emission. We also compared HI, CO, and Hα line emission data with the properties of the diffuse X-ray emission. Our results show that the X-ray emission in all four regions can be modeled by absorbed thermal plasma (vapec) with temperatures of kT ∼0.2 keV and kT 0.8–1.0 keV. The comparison of the X-ray absorption column density with the hydrogen column density suggests that the X-ray dark lane north of N11 is caused by absorption by HI and CO clouds. Evaluating the energy budget of the thermal plasma, we found that in the superbubble region, encompassing OB associations LH9, LH10, LH11, and LH13, the observed X-ray energy can be explained by heating from high-mass stars. In the surrounding regions, the energy indicated by the X-ray emission suggests additional heating caused by shocks from cloud–cloud collisions.
