1996A&AS..120C.239G

GRO J1655-40 was observed with the ROSAT HRI on two occasions: ones (in August 1994) between the first and the second outbursts in 1994, and ones between a soft and a hard X-ray outburst (in March 1995). The first observation allowed to improve the X-ray position, thus confirming the optical and radio identification. In addition, a distance of d≃3kpc is derived using the dust scattering halo. The combination with radio measurements suggests that the X-ray emission originated in an accretion disk or corona rather then in a jet. The results of the second ROSAT observation and the comparison with earlier TTM observations suggest that the X-rays at this epoch were emitted from an accretion disk.