  The Large Synoptic Survey Telescope (LSST) surveys have initially been
optimized to omit the inner part of the Milky Way disk/bar from deep and
cadence observations. However it is now clear that the LSST will be powerful
for Galactic astronomy and may play a crucial role in continuing to extend the
Gaia astrometric catalog until a future satellite, either optical or IR,
carries on. LSST will provide metallicities and kinematics for the bulge, and
will map halo structures to as distant as 450 kpc, nearly half the distance to
the Andromeda galaxy. Thanks to the unprecedented calibration effort for its
photometric system, and surprisingly good astrometry (transverse velocity
measurements of 0.2 mas/yr at r=21; 1 mas/yr at r=24). LSST will provide
photometric abundances and distance constraints for a billion or more Milky Way
stars to distances of 450 kpc, and kinematics from proper motions to $\sim100$
kpc. Single observation depths reach $\sim 24$ in the $ugrizy$ bands, while
depths at end of mission reach $\sim 27$. Although halo structures such as
streams and dwarf galaxies are initially identified by the RR Lyrae and giants,
their structure will be fleshed out by the 100$\times$ more abundant dwarfs
that will be detected to 100 kpc (single observation) and $\sim 300$ kpc by end
of mission. More complete mapping of stream structures may constrain the mass
distribution of dark matter and perhaps confirm the interaction of dark matter
halos and streams. I also describe the Blanco DECam Bulge Survey, a 200 deg$^2$
LSST pathfinder survey of the bulge in $ugrizy$ using the Dark Energy Camera on
the Blanco 4m telescope. The purpose of this article is to encourage active
workers on the Milky Way and Local Volume to participate in the LSST project,
in particular to urge that the Galactic Plane receive the same cadence and
depth coverage as the rest of the extragalactic sky.
