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In the context of this paper, microlenses present as oblate clusters of darkmatter structures called massive astrophysical compact halo object(MACHO) inthe galactic halo are considered. The NFW density profile [1] is derived fromthe observational data and works best in the halo region of the exterior partof the galaxy. Hence this profile is used to plot the potential, deflectionangle, and critical and caustic curves for the aforementioned microlenses usingnumerical methods. Moreover, this model is compared with an older densityprofile model [2], and the differences in their caustic and critical curves arepointed out. This leads to the conclusion that the NFW model produces causticand critical curves that occupy a smaller region than portrayed by the causticand critical curves produced by the older density profile model. However, thedifferences are not that significant to these structures act as microlenses asthey are so small and beyond the scope of modern telescopes, and thus only thelight curves can be detected from these structures.

Microlensing of halo objects in the exterior part of the Galaxy