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The structure and kinematics of ionized gas in the star-forming region in theBCD galaxy VIIZw403 (UGC6456) are analyzed using observations with the SCORPIOfocal reducer on the 6-m Special Astrophysical Observatory telescope in threemodes: direct imaging (in the H-alpha, [OIII], and [SII] lines), long-slitspectroscopy, and spectroscopy with a scanning Fabry-Perot interferometer. Inaddition to the previously known bright HII regions and the faint giant ringthat surrounds the entire star-forming region, many new faint diffuse and arcstructures have been detected. Fine structure of the giant ring has beenrevealed. We do not confirm the previously detected expansion of the brightshells around young stellar associations with a velocity of 50-70 km/s. We haveestimated their expansion velocities to be no higher than 15-20 km/s; thecorresponding kinematic age, no younger than 3-4 Myr, agrees well with the ageof the compact OB associations related to them. We associate the faint extendedfilamentary and diffuse regions of ionized gas identified in nearly the entirecentral 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] andH-alpha line wings (up to 300 km/s from the line center) have been detected inthe brightest HII region. Such velocities have been observed in the galaxy forthe first time. The previously published H-alpha luminosity measurements forthe galaxy are refined.Comment: to appear in Astronomy Letters, 13 pages, 6 postscript figures, 1 in  colou

Structure and kinematics of the interstellar medium in the star-forming region in the BCD galaxy VII Zw 403 (UGC 6456)