  We report on a new spectroscopic analysis of the very metal deficient star G
64-12 ([Fe/H]=-3.3), aimed at determining, for the first time, its Be content.
The spectra were observed during the Science Verification of UVES, the ESO VLT
Ultraviolet and Visible Echelle Spectrograph. The high resolution (~48,000) and
high S/N (~130 per pixel) achieved at the wavelengths of the BeII resonance
doublet allowed an accurate determination of its abundance: log N(Be/H) =
-13.10 +/- 0.15 dex. The Be abundance is significantly higher than expected
from previous measurements of Be in stars of similar metallicity (3D and NLTE
corrections acting to make a slightly higher value than an LTE analysis). When
compared to iron, the high [Be/Fe] ratio thus found may suggest a flattening in
the beryllium evolutionary trend at the lowest metallicity end or the presence
of dispersion at early epochs of galactic evolution.
