We present deep , wide-field imaging of the M51 system using CWRU ’ s Burrell Schmidt telescope at KPNO to study the faint tidal features that constrain its interaction history . Our images trace M51 ’ s tidal morphology down to a limiting surface brightness of \mu _ { B,lim } \sim 30 mag arcsec ^ { -2 } , and provide accurate colors ( \sigma _ { \bv } < 0.1 ) down to \mu _ { B } \sim 28 . We identify two new tidal streams in the system ( the South and Northeast Plumes ) with surface brightnesses of \mu _ { B } = 29 and luminosities of \sim 10 ^ { 6 } L _ { \astrosun,B } . While the Northeast Plume may be a faint outer extension of the tidal “ crown ” north of NGC 5195 ( M51b ) , the South Plume has no analogue in any existing M51 simulation and may represent a distinct tidal stream or disrupted dwarf galaxy . We also trace the extremely diffuse Northwest Plume out to a total extent of 20′ ( 43 kpc ) from NGC 5194 ( M51a ) , and show it to be physically distinct from the overlapping bright tidal streams from M51b . The Northwest Plume ’ s morphology and red color ( \bv = 0.8 ) instead argue that it originated from tidal stripping of M51a ’ s extreme outer disk . Finally , we confirm the strong segregation of gas and stars in the Southeast Tail , and do not detect any diffuse stellar component in the H i portion of the tail . Extant simulations of M51 have difficulty matching both the wealth of tidal structure in the system and the lack of stars in the H i tail , motivating new modeling campaigns to study the dynamical evolution of this classic interacting system .