Top: SPHERE IFS and IRDIS 5σ detection limits as a function of the angular separation taken from February 7th and 9th, 2017. Bottom: SPHERE IFS and IRDIS 5σ detection limits converted in terms of masses using DUSTY model predictions as a function of the projected physical separation. For IFS, different spectral energy distributions were considered for the injected planets to explore the impact of the flux loss cancellation and different planet properties in the final detection limits. Contrast curves were cut at 0.15 ′′ because of the low transmission of the coronagraph. The location and the predicted mass by the DUSTY models of HIP 65426 b are reported.