tokens: model component, given as with the electron and hydrogen densities n e and n H , respectively, and the filling factor f . We used the ratio of n e ≈ 1.21 n H for the LMC abundance of 0.5 solar ( Sasaki et al. 2011 ). With this, we can estimate the hydrogen density from the normalization with Assuming an ideal gas, the pressure can then be estimated from the temperature of the plasma, which we obtained from the spectral fits: with the X-ray temperature T x and the Boltzmann constant k B . And with the pressure P we can estimate the thermal energy E stored in the plasma with Additionally, the mass of the plasma can be calculated using with the m H and μ being the hydrogen mass and molecular weight of the ionized gas, respectively. We used the spectral fit results of the tessellates for the calculations, as those results cover most of the X-ray spur and the surroundings. The derived values are given in Table 4 . We derived the results for each region individually and then took the average of the resulting map over regions which correspond to the large scale structures in the vicinity. The upper and lower limits were calculated by taking the average of the upper and lower limit map of the respective derived parameter. The volume V was estimated by calculating the area of each tessellate polygon region using the Shapely 7 python package. Multiplied with the depth of the X-ray emitting plasma, we obtain the volume of each region. We varied the depth for the volumes, depending on the region the tessellates are located in, to account for the complex geometry of the ISM. We took the values given by Points et al. (2001) and additionally, we estimated the depth of the 30 Dor region with z = 300 pc based on the extent of the structure. The assumed depth is by far the largest factor of uncertainty in the calculations, however, the order of magnitude should be approximately correct. The thermal energy E and mass M of the plasma was also normalized to the volume in cm 3 . Otherwise we would obtain the total numbers for each tessellate region, which would not be comparable between different regions. We give the results without assuming any specific filling factor, as this parameter is largely unknown to us. Based on the true value of the factor the results could change slightly. If we compare, for example, a filling factor of f = 1 versus f = 0.3, the pressure, hydrogen density and mass would increase by a factor ~ 3 while the thermal energy would decrease by that factor for f = 0.3. To gain further insight into the geometry of the hot plasma, we compared the absorption column from the spectral fits with the column density N H of the H I data. This ratio is a measure how deeply the plasma is embedded inside the X-ray absorbing material ( Maggi et al. 2016 ). A value smaller or close to unity suggests that the plasma is located more to the front and consequently a value larger then unity that the plasma is located to the back. We obtain the column density N H
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