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 ( \lesssim 10 Gyr ) possibly sets them apart from the other satellites at Galactocentric distances \gtrsim 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 ( \gtrsim 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 .