Tidal Signatures in the Faintest Milky Way Satellites: The Detailed
  Properties of Leo V, Pisces II and Canes Venatici II
  We present deep wide-field photometry of three recently discovered faint
Milky Way satellites: Leo V, Pisces II, and Canes Venatici II. Our main goals
are to study the structure and star formation history of these dwarfs; we also
search for signs of tidal disturbance. The three satellites have similar
half-light radii ($\sim 60-90$ pc) but a wide range of ellipticities. Both Leo
V and CVn II show hints of stream-like overdensities at large radii. An
analysis of the satellite color-magnitude diagrams shows that all three objects
are old ($>$ 10 Gyr) and metal-poor ([Fe/H] $\sim -2$), though neither the
models nor the data have sufficient precision to assess when the satellites
formed with respect to cosmic reionization. The lack of an observed younger
stellar population ($\la 10$ Gyr) possibly sets them apart from the other
satellites at Galactocentric distances $\ga 150$ kpc. We present a new
compilation of structural data for all Milky Way satellite galaxies and use it
to compare the properties of classical dwarfs to the ultra-faints. The
ellipticity distribution of the two groups is consistent at the
$\sim$2-$\sigma$ level. However, the faintest satellites tend to be more
aligned toward the Galactic center, and those satellites with the highest
ellipticity ($\ga 0.4$) have orientations ($\Delta \theta_{GC}$) in the range
$20^{\circ} \lesssim \Delta \theta_{GC} \lesssim 40^{\circ}$. This latter
observation is in rough agreement with predictions from simulations of dwarf
galaxies that have lost a significant fraction of their dark matter halos and
are being tidally stripped.
