The majority of massive stars is part of a multiple system. After the core collapse supernova (SN) of the more massive component the formed neutron star is ejected by the SN kick whereas the companion star either remains within the system and is gravitationally bounded to the neutron star, or is ejected with a spatial velocity comparable to its former orbital velocity. Such stars with a large peculiar space velocity are called runaway stars.

We present our observational studies of the supernova remnants G74.0-8.5, G119.5+10.2 and G184.6-5.8. The focus of this project lies on the detection of low mass runaway stars. We analyze the spectra of a number of candidates and discuss their possibility of being the former companions of the SN progenitor stars.