AbstractROSAT X-ray observations of the LMC show several X-ray shadows in the ¾ keV and 1.5 keV bands. The ¼ keV band is dominated by emission of the galactic foreground. It is uncertain whether there is additional soft X-ray contribution from the LMC. The so-called HI-L-component is located in front of the HI-D-component and therefore the matter of the L-component accounts for most of the observed X-ray shadows. The ¼ keV ROSAT image of the LMC reveals a slightly fainter X-ray emission region at the position of the eastern part of the HI-L-component. This suggests the existence of a soft X-ray halo in the LMC. Investigations of the X-ray shadows show that also the lower energy end of the ¾ keV band originates partly from this soft X-ray plasma which is located in front of the absorption features. This additional soft X-ray emission, in the lower energy end of the ¾ keV band, is brighter than the typical diffuse galactic emission at the same galactic latitude.