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Fig. 1
Example of quadruply-imaged lensed quasar where the lensed images are in “cusp configuration” (J1131−1231, from Claeskens et al. 2006). In such a system, the flux of image A (saddle-point of the arrival time surface) is expected to be equal to the sum of the fluxes of B and C (minima of the arrival time surface).
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