On the robustness of the microlensing optical depth as a measure of MACHO density

Abstract

(Abridged version): The optical depth is widely used in Galactic microlensing studies as a means to determine the density of MACHOs, since in theory it depends only upon their spatial distribution and is therefore less model-dependent than other microlensing observables. However, since the measured optical depth is restricted to that of events with measurable timescales, inferences of total MACHO density are dependent on the assumed timescale distribution. Using the 2-year LMC results of the MACHO collaboration, we illustrate this point by showing how, for an assumed isothermal halo, the inferred MACHO halo fraction as determined from optical depth estimates depends upon MACHO mass. The analysis highlights the following conclusions: (1) The MACHO density inferred from optical depth measurements depends on the assumed MACHO mass function for a given Galactic distribution function; (2) without extra information on the MACHO mass function, such as can be obtained from the rate-timescale distribution, optical depth measurements can provide a lower limit but not an upper limit on the MACHO density for a given Galactic distribution function; (3) a comparison between the inferred total optical depth of different Galactic models, or of different components in a multi-component Galactic model, requires knowledge of the underlying timescale distribution for each model or component.