  Based on its Hipparcos proper motion, we propose that the high-mass X-ray
binary HD153919/4U1700-37 originates in the OB association Sco OB1. At a
distance of 1.9 kpc the space velocity of 4U1700-37 with respect to Sco OB1 is
75 km/s. This runaway velocity indicates that the progenitor of the compact
X-ray source lost about 7 Msun during the (assumed symmetric) supernova
explosion. The system's kinematical age is about 2 +/- 0.5 million years which
marks the date of the supernova explosion forming the compact object. The
present age of Sco OB1 is <8 Myr; its suggested core, NGC 6231, seems to be
somewhat younger (~5 Myr). If HD153919/4U1700-37 was born as a member of Sco
OB1, this implies that the initially most massive star in the system terminated
its evolution within <6 million years, corresponding to an initial mass >30
Msun. With these parameters the evolution of the binary system can be
constrained.
