  In this second of a two-paper sequence, we present Monte Carlo population
simulation results of brown dwarf companion data collected during the Cornell
High-order Adaptive Optics Survey for brown dwarf companions (CHAOS). Making
reasonable assumptions of orbital parameters (random inclination, random
eccentricity and random longitude of pericentre) and age distributions, and
using published mass functions, we find that the brown dwarf companion fraction
around main sequence stars is 0.0%-9.3% for the 25-100 AU semi-major axis
region. We find a corresponding L-dwarf companion fraction of 0.0%-3.3%. We
compare our population analysis methods and results with techniques and results
presented by several other groups. In this comparison we discover that
systematic errors (most notably resulting from orbital projection effects)
occur in the majority of previously published brown dwarf companion population
estimates, leading authors to claim results not supported by the observational
data.
