  We use high resolution spectra obtained with FUSE and STIS to obtain
interstellar column densities of H I, D I, O I, S II, Fe II and P II toward the
QSO HE 0226-4110 ( l = 253.4 deg , b = -65.77 deg). We obtain D/H = 21(+8, -6)
ppm. Correcting for a small amount of contamination from D and H in the Local
Bubble, we obtain D/H = 22 (+8, -6) for the warm neutral medium of the lower
Galactic halo. The medium has [O/H] = 0.12(+0.41, -0.20) and [Fe/H] = -1.01
(+0.10, -0.09). This suggests the abundances in the halo toward HE 0226-4110
are not affected by the infall of low metallicity gas and that the gas
originates in the disk and is elevated into the halo by energetic processes
which erode but do not totally destroy the dust grains. We compare our result
to measured values of D/H in other astrophysical sites. The value we measure in
the halo gas is consistent with the hypothesis that for many Galactic disk
lines of sight D is incorporated into dust. The high average value of D/H =
23.1+/-2.4 ppm measured along 5 sight lines through disk gas in the Solar
neighborhood is similar to D/H in the lower Galactic halo. These observations
imply the abundance of deuterium in the Galaxy has only been reduced by a
factor of 1.12+/-0.13 since its formation.
