  We interpret the de-reddened UBV data for the field SA 133 to deduce the
stellar density and metallicity distributions function. The logarithmic local
space density for giants, $D^{*}(0)=6.40$, and the agreement of the luminosity
function for dwarfs and sub-giants with the one of Hipparcos confirms the
empirical method used for their separation. The metallicity distribution for
dwarfs gives a narrow peak at [Fe/H]=+0.13 dex, due to apparently bright
limiting magnitude, $V_{o}=16.5$, whereas late-type giants extending up to $z
\sim4.5$ kpc from the galactic plane have a multimodal distribution. The
metallicity distribution for giants gives a steep gradient $d[Fe/H]/dz=-0.75$
dex kpc$^{-1}$ for thin disk and thick disk whereas a smaller value for the
halo, i.e. $d[Fe/H]/dz=-0.45$ dex kpc$^{-1}$.
