Microlensing of an extended source by a power-law mass distribution

Details Microlensing of an extended source by a power-law mass distribution Microlensing of an extended source by a power-law mass distribution

2006-12-19

arxiv.org/abs/astro-ph/0612542v2

Mon.Not.Roy.Astron.Soc.376:263-272,2007

Astronomy and Astrophysics

Astrophysics

11 pages, accepted in MNRAS; low-resolution versions of Figs. 1, 10, and 13; for file with high-resolution figures see http:

Scientific paper

10.1111/j.1365-2966.2007.11426.x

Microlensing promises to be a powerful tool for studying distant galaxies and quasars. As the data and models improve, there are systematic effects that need to be explored. Quasar continuum and broad-line regions may respond differently to microlensing due to their different sizes; to understand this effect, we study microlensing of finite sources by a mass function of stars. We find that microlensing is insensitive to the slope of the mass function but does depend on the mass range. For negative parity images, diluting the stellar population with dark matter increases the magnification dispersion for small sources and decreases it for large sources. This implies that the quasar continuum and broad-line regions may experience very different microlensing in negative-parity lensed images. We confirm earlier conclusions that the surface brightness profile and geometry of the source have little effect on microlensing. Finally, we consider non-circular sources. We show that elliptical sources that are aligned with the direction of shear have larger magnification dispersions than sources with perpendicular alignment, an effect that becomes more prominent as the ellipticity increases. Elongated sources can lead to more rapid variability than circular sources, which raises the prospect of using microlensing to probe source shape.

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