We present 2 ^ { \prime \prime } to 7 ^ { \prime \prime } resolution 3 mm continuum and CO ( J=1 - 0 ) line emission and near infrared K _ { s } , H _ { 2 } , and [ FeII ] images toward the massive star forming region W75 N. The CO emission uncovers a complex morphology of multiple , overlapping outflows .
A total flow mass of > 255 M _ { \odot } extends 3 pc from end-to-end and is being driven by at least four late to early-B protostars .
More than 10 % of the molecular cloud has been accelerated to high velocities by the molecular flows ( > 5.2 km s ^ { -1 } relative to v _ { LSR } ) and the mechanical energy in the outflowing gas is roughly half the gravitational binding energy of the cloud .
The W75 N cluster members represent a range of evolutionary stages , from stars with no apparent circumstellar material to deeply embedded protostars that are actively powering massive outflows .
Nine cores of millimeter-wavelength emission highlight the locations of embedded protostars in W75 N. The total mass of gas & dust associated with the millimeter cores ranges from 340 M _ { \odot } to 11 M _ { \odot } .
The infrared reflection nebula and shocked H _ { 2 } emission have multiple peaks and extensions which , again , suggests the presence of several outflows .
Diffuse H _ { 2 } emission extends about 0.6 parsecs beyond the outer boundaries of the CO emission while the [ FeII ] emission is only detected close to the protostars .
The infrared line emission morphology suggests that only slow , non-dissociative J-type shocks exist throughout the pc-scale outflows .
Fast , dissociative shocks , common in jet-driven low-mass outflows , are absent in W75 N. Thus , the energetics of the outflows from the late to early B protostars in W75 N differ from their low-mass counterparts – they do not appear to be simply scaled-up versions of low-mass outflows .