  We analyse the structure and kinematics of ionized gas in the vicinity of the
ultraluminous X-ray source (ULX) HoII X-1 in the Holmberg II galaxy using
observational data obtained with a scanning Fabry-Perot interferometer in the
H$\alpha$, [SII] and [OIII] emission lines at the Russian 6-m telescope.
Decomposition of the line profiles allows us to identify the broad component of
emission lines caused by the ULX action. We found evidence of an expanding
superbubble around the young star cluster located in the studied region. We
conclude that the blue-shifted 'arc' around the ULX observed in the
line-of-sight velocity field may correspond to a bow shock caused by the ULX
movement from that nearby young star cluster. If this interpretation is
correct, it will be the first kinematic evidence of ULX's escape from their
parent star clusters.
