Time delay measurements for the 3 brightest quasar images of DES J0408−5354 using the data shown in Fig. 3. The time delay measurements are carried out in 3 different ways. Results using the WFI data with the spline fitting method are shown in blue and those in purple show the regression difference method. Results for the combined WFI+Euler data set using the spline fitting method are shown in green. For comparison we also show, in black, the spline fitting result when using only the high-cadence WFI data and no model for the microlensing extrinsic variations. A negative Δt(AB) means that the signal from image A reaches the observer’s plane before B.