Impact of dust correction on the shape of the SFR functions. The unobscured (upper panel) and dust corrected (lower panel) SFR functions are shown for different stellar mass bins (in color) and the whole sample (solid and dotted black lines) in the range 0.6 ≤ z ≤ 1.0. One noticeable feature of the dust correction is the ability to dissociate the SFR functions for each stellar mass bin with a larger correction at high masses and to modify the SFR functions per stellar mass bin from an asymmetric to a nearly Gaussian distribution.