  The compilation of the metallicity values of $\omega$~Centauri stars led to
detection of spatial asymmetry in the metallicity distribution of the bright
giants. It was found that the most and least metal-poor objects are separated
along galactic latitude. Statistical tests show that the chance occurrence of
the phenomenon is very low. The subgiant and the RR~Lyrae samples do not show,
however, similar segregation of the different metallicity objects. The physical
parameters of the variables calculated by using empirical formulae indicate
that the bulk of the RRab stars comprises a very homogeneous group regarding
both their metallicity and mass values. These stars are most probably already
in the evolved stage of their horizontal branch evolution.
