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We present first results of a long term study: Searching for OB--type runawaystars inside supernova remnants (SNRs). We identified spectral types andmeasured radial velocities (RV) by optical spectroscopic observations and wefound an early type runaway star inside SNR S147. HD 37424 is a B0.5V type starwith a peculiar velocity of 74$\pm$8 km s$^{-1}$. Tracing back the pasttrajectories via Monte Carlo simulations, we found that HD 37424 was located atthe same position as the central compact object, PSR J0538+2817, $30\!\pm\!4$kyr ago. This position is only $\sim$4 arcmin away from the geometrical centerof the SNR. So, we suggest that HD 37424 was the pre--supernova binarycompanion to the progenitor of the pulsar and the SNR. We found a distance of1333$^{+103}_{-112}$ pc to the SNR. The zero age main sequence progenitor massshould be greater than 13 $M_\odot$. The age is $30\pm4$ kyr and the totalvisual absorption towards the center is 1.28$\pm$0.06 mag. For differentprogenitor masses, we calculated the pre--supernova binary parameters. TheRoche Lobe radii suggest that it was an interacting binary in the late stagesof the progenitor.

Discovery of an OB Runaway Star Inside SNR S147