“Worst-case” Microlensing in the Identification and Modeling of Lensed Quasars

Although micro-lensing of macro-lensed quasars and supernovae provides unique opportunities for several kinds investigations, it can add unwanted sometimes substantial noise. While flux anomalies may be safely ignored some observations, they severely limit others. "Worst-case" estimates inform the decision whether or not to undertake an extensive examination scenarios. Here, we report "worst-case" uncertainties point sources lensed by singular isothermal potentials, parameterized a convergence equal shear stellar fraction. The results straightforwardly applied non-isothermal potentials utilizing mass sheet degeneracy. We use maps compute fluctuations in image micro-magnifications estimate fraction at which are greatest given convergence. find that worst-case happen $\kappa_\star=\frac{1}{|\mu_{macro}|}$. For macro-minima, both magnification demagnification appear bounded ($1.5>\Delta m>-1.3$, where $\Delta m$ is magnitude relative average macro-magnification). Magnifications macro-saddles as well ($\Delta m > -1.7$). In contrast, demagnifications have unbounded $1/\mu_{macro}\rightarrow0$ $\kappa_\star\rightarrow0$.