Observations of the high energy sky , mainly with the INTEGRAL satellite , have raised new questions about the formation and evolution of High Mass X-ray Binaries ( HMXBs ) .
The number of detected HMXBs of different types is now high enough to allow us to carry out a statistical analysis of their distribution in the Milky Way .
For the first time , we derive the distance and absorption of a sample of HMXBs using a Spectral Energy Distribution fitting procedure , and we examine the correlation with the distribution of Star Forming Complexes ( SFCs ) in the Galaxy .
We show that HMXBs are clustered with SFCs with a typical cluster size of 0.3 \pm 0.05 kpc and a characteristic distance between clusters of 1.7 \pm 0.3 kpc .
Furthermore , we present an investigation of the expected offset between the position of spiral arms and HMXBs , allowing us to constrain age and migration distance due to supernova kick for some sources .
These new methods will allow us to assess the influence of the environment on these high energy objects with unprecedented reliability .