  A sample of metal-poor subgiants has been observed with the UVES spectrograph
at the Very Large Telescope and abundances of Li and Be have been determined.
Typical signal-to-noise per spectral bin values for the co-added spectra are of
the order of 500 for the Li I line (670.78 nm) and 100 for the Be II doublet
lines (313.04 nm). The spectral analysis of the observations was carried out
using the Uppsala suite of codes and MARCS (1D-LTE) model atmospheres with
stellar parameters from photometry, parallaxes, isochrones and Fe II lines.
Abundance estimates of the light elements were corrected for departures from
local thermodynamic equilibrium in the line formation. Effective temperatures
and Li abundances seem to be correlated and Be abundances correlate with [O/H].
Standard models predict Li and Be abundances approximately one order of
magnitude lower than main-sequence values which is in general agreement with
the observations. On average, our observed depletions seem to be 0.1 dex
smaller and between 0.2 and 0.4 dex larger (depending on which reference is
taken) than those predicted for Li and Be, respectively. This is not surprising
since the initial Li abundance, as derived from main-sequence stars on the
Spite plateau, may be systematically in error by 0.1 dex or more, and
uncertainties in the spectrum normalisation and continuum drawing may affect
our Be abundances systematically.
