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We present deep wide-field photometry of three recently discovered faintMilky Way satellites: Leo V, Pisces II, and Canes Venatici II. Our main goalsare to study the structure and star formation history of these dwarfs; we alsosearch for signs of tidal disturbance. The three satellites have similarhalf-light radii ($\sim 60-90$ pc) but a wide range of ellipticities. Both LeoV and CVn II show hints of stream-like overdensities at large radii. Ananalysis of the satellite color-magnitude diagrams shows that all three objectsare old ($>$ 10 Gyr) and metal-poor ([Fe/H] $\sim -2$), though neither themodels nor the data have sufficient precision to assess when the satellitesformed with respect to cosmic reionization. The lack of an observed youngerstellar population ($\la 10$ Gyr) possibly sets them apart from the othersatellites at Galactocentric distances $\ga 150$ kpc. We present a newcompilation of structural data for all Milky Way satellite galaxies and use itto compare the properties of classical dwarfs to the ultra-faints. Theellipticity distribution of the two groups is consistent at the$\sim$2-$\sigma$ level. However, the faintest satellites tend to be morealigned toward the Galactic center, and those satellites with the highestellipticity ($\ga 0.4$) have orientations ($\Delta \theta_{GC}$) in the range$20^{\circ} \lesssim \Delta \theta_{GC} \lesssim 40^{\circ}$. This latterobservation is in rough agreement with predictions from simulations of dwarfgalaxies that have lost a significant fraction of their dark matter halos andare being tidally stripped.

Tidal Signatures in the Faintest Milky Way Satellites: The Detailed Properties of Leo V, Pisces II and Canes Venatici II