  We study the prospects for the current microlensing searches, which have
recently discovered several candidates, to yield useful information about the
flattening of the Galaxy dark matter halo. Models of HI warps and N-body
simulations of galaxy formation suggest that disks commonly form in oblate
halos with a tilt between the disk and halo symmetry axes. The microlensing
optical depth for the Large Magellanic Cloud depends sensitively on the
disk-halo tilt angle in the Milky Way. We conclude that a much larger spread in
values for $\tau(LMC)$ is consistent with rotation curve constraints than
previously thought, and that the ratio $\tau(SMC)/\tau(LMC)$ of the optical
depth to the Small and Large Magellanic clouds is not a clean test of halo
flattening.
