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\subsection{Multiple Imaging by a Foreground Galaxy}  \label{sec:time_delay_dist}  For a given lens system, the time delays between images can be as short as $\sim$days $\sim$a day  for close pairs of images to as long as $\sim$100s of days for images on opposite side sides  of the lensing galaxy. The magnitude of these time delays (as well as the other observables) depends on the redshifts of thesource $z_{\rm src}$ and the  lens galaxy $z_{\rm lens}$, $z_l$ and more mildly on the source redshift $z_s$ {\bf [EL:true?]},  and therefore it is important to understand the expected distribution of those parameters in the LSST data. \citet[][hereafter OM10]{OM10} generated a mock catalog of LSST lensed AGN based on plausible models for the source quasars and lens galaxies, and simple assumptions for the detectability of lensed quasars (including published 10$\sigma$ limiting magnitude estimates, and the assumption that lenses will be detected if the third (second) brightest image for a given quad (double) is above this limit). This catalog provides a distribution of time delays that will be present in the LSST data which we can use to guideor  generation of mock light curves. Figure \ref{fig:tdel_hist} shows the $\log_{10} \Delta t$ distributions for the OM10 double and quad sample. The distributions are roughly log-normal with means $\sim$10s of days and tails extending below 1 day for the quads, and above 100 days for the doubles. Lenses in both of these tails will have time delays that are difficult to measure, because cadence isn't high enough or because the observing  seasons are not long enough. We expect some fraction of time delay measurements to fail catastrophically in this way, but we also expect the catastrophe rate to vary with measurement algorithm.