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 .