deletions | additions       diff --git a/Microlensing.tex b/Microlensing.tex  index 38c89f1..0e58f9d 100644  --- a/Microlensing.tex  +++ b/Microlensing.tex 
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For each lens in the OM10 catalog we assign an $f_{\star}$ at each image position as follows. The OM10 catalog provides the velocity dispersion for a given lens which we use to estimate the i=band luminosity and effective radius of the galaxy by drawing from the Fundamental Plane [REF]. Assuming a standard \citet{deVaucoleurs1948} profile for the brightness distribution centered on the lens, an isothermal ellipsoid for the total mass distribution, and a mass-to-light ratio of {\bf GGD: what???}, $f_{\star}$ is the ratio of stellar mass density to total mass density at each image position.  Given $\kappa$ and $\gamma$ from the OM10 catalog and estimating $f_{\star}$ as above, we generate magnification maps like the one shown in {\bf (GGD: again, a figure would be nice} which represent the magnification of a point source as a function of position in the source plane. To use this make map  to generate temporal microlensing fluctuations we first smooth it by a Gaussian source profile with a size of {\bf (GGD: Kai, what are you using???)} and then trace a linear path along a random direction in the map. This path is converted from source plane position to time units via $v_{\rm rel}$ [REF]. The effect of having a finite source is to smooth out and reduce the amplitude of the microlensing fluctuations.