  We present the calibration of the [$\alpha/$Fe] element in terms of
ultra-violet excess for 465 dwarf stars with spectral type F0-K2. We used a
single calibration, fitted to a third degree polynomial with a square of the
correlation coefficient 0.74 and standard deviation 0.05 mag, for all stars due
to their small colour range, $0.1<(g-r)_0\leq 0.6$ mag, and high frequency in
the blueward of the spectrum which minimize the guillotine effect. Our
calibration provides [$\alpha/$Fe] elements in the range $(-0.05, 0.35]$ dex.
We applied the procedure to a high-latitude field, $85^\circ \leq b \leq
90^\circ$ with size 78 deg$^2$ and we could estimate the [$\alpha/$Fe] elements
of 23,414 dwarf stars which occupy a Galactic region up to a vertical distance
of $z=9$ kpc. We could detect a small positive gradient, $d[\alpha/{\rm
Fe}]/dz=+0.032 \pm0.002$ dex kpc$^{-1}$, for the range $0<z<5$ kpc, while the
distribution of the [$\alpha/$Fe] element is flat for further $z$ distances.
