We present results from a 2300 arcmin ^ { 2 } survey of the Orion A molecular cloud at 450 and 850 \mu m using the Submillimetre Common-User Bolometer Array ( SCUBA ) on the James Clerk Maxwell Telescope .
The region mapped lies directly south of the OMC1 cloud core and includes OMC4 , OMC5 , HH1/2 , HH34 , and L1641N .
We identify 71 independent clumps in the 850 \mu m map and compute size , flux , and degree of central concentration in each .
Comparison with isothermal , pressure-confined , self-gravitating Bonnor-Ebert spheres implies that the clumps have internal temperatures T _ { d } \sim 22 \pm 5 K and surface pressures { log } ( k ^ { -1 } P { cm } ^ { -3 } { K } ) = 6.0 \pm 0.2 .
The clump masses span the range 0.3 - 22 M _ { \odot } assuming a dust temperature T _ { d } \sim 20 K and a dust emissivity \kappa _ { 850 } = 0.02 cm ^ { 2 } g ^ { -1 } .
The distribution of clump masses is well characterized by a power-law N ( M ) \propto M ^ { - \alpha } with \alpha = 2.0 \pm 0.5 for M > 3.0 M _ { \odot } , indicating a clump mass function steeper than the stellar Initial Mass Function .
Significant incompleteness makes determination of the slope at lower masses difficult .
A comparison of the submillimeter emission map with an H _ { 2 } 2.122 \mu m survey of the same region is performed .
Several new Class 0 sources are revealed and a correlation is found between both the column density and degree of concentration of the submillimeter sources and the likelihood of coincident H _ { 2 } shock emission .