The initial mass function contains clues to the processes
 regulating formation of low mass stars and substellar objects
 and also may be important to locating a portion of the dark matter.
 It is very difficult to extend the IMF of field stars into the
 brown dwarf regime because these objects are too cool at the age
 of most nearby stars. However, young brown dwarfs may be detectable
 in nearby, young, open  clusters, of which the Pleiades is the
 prime example. We have developed and tested a very efficient means
 to use V, I, K imaging to identify brown dwarf candidates; we have
 used Praesepe for a test that shows that our technique compares
 closely with recent deep studies based on proper motions.
 We have used these colors to isolate a complete sample of 12 low
 mass brown dwarf candidates in 500 square arcmin of the Pleiades.
 The brown dwarf identification of these sources can be tested
 definitively with longer wavelength measurements with ISO.