  In this paper we present the analysis of Hubble Space Telescope (HST)
observations of the globular cluster Omega Centauri. Our analysis combines data
obtained in this work with previously published HST data from an earlier
article of this series and encompasses a broad portion of the cluster's radial
extension. Our findings reveal a significant radial variation in the fraction
of stars within the two most populous stellar populations showing that one of
the main second-population groups (referred to as bMS) is more centrally
concentrated than the first-population group (referred to as rMS).
Additionally, we explore the spatial variations of the other less populous
stellar populations (referred to as MSa and MSd) and find a qualitatively
similar, but weaker, radial decrease in the fraction of stars in these
populations at larger distances from the cluster centre. Only one of the
populations identified (MSe) does not show any significant radial variation.
