Determining the Physical Lens Parameters of the Binary Gravitational Microlensing Event MOA-2009-BLG-016

TL;DR

This paper analyzes the microlensing event MOA-2009-BLG-016 to determine the physical parameters of the binary lens system, including mass and distance, by modeling the light curve and addressing degeneracies in the solutions.

Contribution

The study provides a detailed analysis of the binary lens parameters and identifies multiple degenerate solutions, advancing understanding of microlensing event modeling and binary lens characterization.

Findings

Detected a brown-dwarf companion with ~0.04 solar masses.

Identified three classes of degenerate solutions for the binary parameters.

Measured the Einstein radius and parallax to determine lens mass and distance.

Abstract

We report the result of the analysis of the light curve of the microlensing event MOA-2009-BLG-016. The light curve is characterized by a short-duration anomaly near the peak and an overall asymmetry. We find that the peak anomaly is due to a binary companion to the primary lens and the asymmetry of the light curve is explained by the parallax effect caused by the acceleration of the observer over the course of the event due to the orbital motion of the Earth around the Sun. In addition, we detect evidence for the effect of the finite size of the source near the peak of the event, which allows us to measure the angular Einstein radius of the lens system. The Einstein radius combined with the microlens parallax allows us to determine the total mass of the lens and the distance to the lens. We identify three distinct classes of degenerate solutions for the binary lens parameters, where two are manifestations of the previously identified degeneracies of close/wide binaries and positive/negative impact parameters, while the third class is caused by the symmetric cycloid shape of the caustic. We find that, for the best-fit solution, the estimated mass of the lower-mass component of the binary is (0.04 +- 0.01) M_sun, implying a brown-dwarf companion. However, there exists a solution that is worse only by \Delta\chi^2 ~ 3 for which the mass of the secondary is above the hydrogen-burning limit. Unfortunately, resolving these two degenerate solutions will be difficult as the relative lens-source proper motions for both are similar and small (~ 1 mas/yr) and thus the lens will remain blended with the source for the next several decades.