  We examine the properties of two galaxy "halos" at z ~ 0.7 in the TON 153
(z_em = 1.01) quasar field. The first absorber-galaxy pair (G1) is a z = 0.672,
L_B = 4.3 L*_B, E/S0 galaxy probed at D = 58 kpc. G1 is associated with a
remarkable five-component Ly-alpha complex having tau_LL < 0.4, W_r(Lya) = 2.8
A, and a velocity spread of v = 1420 km/s. We find no MgII, CIV, NV, nor OVI
absorption in these clouds and infer metallicity upper limits of -3 <
log(Z/Z_sun) < -1, depending upon assumptions of photoionized or collisionally
ionized gas. The second absorber-galaxy pair (G2) is a z = 0.661, L_B = 1.8
L*_B, Sab galaxy probed at D = 103 kpc. G2 is associated with metal--enriched
(log Z/Z_sun ~ -0.4) photoionized gas having N(HI) ~ 18.3 and a velocity spread
of v = 200 km/s. The very different G1 and G2 systems both have gas-galaxy
properties inconsistent with the standard luminosity dependent galaxy "halo"
model commonly invoked for quasar absorption line surveys. We emphasize that
mounting evidence is revealing that extended galactic gaseous envelopes in the
regime of D < 100 kpc do not exhibit a level of homogeneity supporting a
standardized halo model. Selection effects may have played a central role in
the development of a simple model. We discuss the G1 and G2 systems in the
context of Lambda-CDM models of galaxy formation and suggest that the
heterogeneous properties of absorber-galaxy pairs is likely related to the
range of overdensities from which galaxies and gas structures arise.
