  We present \textit{Chandra} observations of the radio-quiet Broad Absorption
Line (BAL) QSO PG 1254+047. We find that it is a weak X-ray source, with a
total of $44\pm 7$ photons measured in 36 ksec across the observed energy range
$0.7 - 6.0$ keV. Its X-ray weakness is consistent with the known correlation
between $\alpha_{ox}$ and the strength of the UV absorption lines. The spectral
energy distribution suggests that PG 1254+047 is intrinsically X-ray weak, in
addition to being heavily X-ray absorbed. The X-ray absorption column density
is $N_{H} > 10^{23}$ cm$^{-2}$ for neutral gas, while the intrinsic
(unabsorbed) emission spectrum has $\alpha_{ox} > 2$. The data are fit best by
including an ionized (rather than neutral) absorber, with column density $N_{H}
\gtrsim 2\times 10^{23}$ cm$^{-2}$. The degree of ionization is consistent with
the UV BALs, as is the total column density if the strongest UV lines are
saturated. If the X-ray absorber forms in a wind that is radiatively
accelerated to the BAL velocities, then the wind must be launched from a radius
of about $10^{16}$ cm with a mass loss rate of $\sim 1$ M$_\odot$ yr$^{-1}$.
