Complexes of triggered star formation in supergiant shell of Holmberg II
  We report a detailed analysis of all regions of current star formation in the
walls of the supergiant HI shell (SGS) in the galaxy Holmberg II based on
observations with a scanning Fabry-Perot interferometer at the 6-m SAO RAS
telescope. We compare the structure and kinematics of ionized gas with that of
atomic hydrogen and with the stellar population of the SGS. Our deep H$\alpha$
images and archival images taken by the HST demonstrate that current star
formation episodes are larger and more complicated than previously thought:
they represent unified star-forming complexes with sizes of several hundred pc
rather than 'chains' of separate bright nebulae in the walls of the SGS. The
fact that we are dealing with unified complexes is evidenced by identified
faint shell-like structures of ionized and neutral gas which connect several
distinct bright HII regions. Formation of such complexes is due to the feedback
of stars with very inhomogeneous ambient gas in the walls of the SGS. The
arguments supporting an idea about the triggering of star formation in SGS by
the HI supershells collision are presented. We also found a faint ionized
supershell inside the HI SGS expanding with a velocity of no greater than 10-15
km/s. Five OB stars located inside the inner supershell are sufficient to
account for its radiation, although a possibility of leakage of ionizing
photons from bright HII regions is not ruled out as well.
