  The structure and kinematics of ionized gas in the star-forming region in the
BCD galaxy VIIZw403 (UGC6456) are analyzed using observations with the SCORPIO
focal reducer on the 6-m Special Astrophysical Observatory telescope in three
modes: direct imaging (in the H-alpha, [OIII], and [SII] lines), long-slit
spectroscopy, and spectroscopy with a scanning Fabry-Perot interferometer. In
addition to the previously known bright HII regions and the faint giant ring
that surrounds the entire star-forming region, many new faint diffuse and arc
structures have been detected. Fine structure of the giant ring has been
revealed. We do not confirm the previously detected expansion of the bright
shells around young stellar associations with a velocity of 50-70 km/s. We have
estimated their expansion velocities to be no higher than 15-20 km/s; the
corresponding kinematic age, no younger than 3-4 Myr, agrees well with the age
of the compact OB associations related to them. We associate the faint extended
filamentary and diffuse regions of ionized gas identified in nearly the entire
central region of the galaxy and the giant HII ring with the older (10 Myr)
stellar population of the most recent starburst. Weak high-velocity [OIII] and
H-alpha line wings (up to 300 km/s from the line center) have been detected in
the brightest HII region. Such velocities have been observed in the galaxy for
the first time. The previously published H-alpha luminosity measurements for
the galaxy are refined.
