The X-ray detected fraction in local (z < 0.25) dwarfs as a function of the stellar mass of the host galaxy. Our model for the multiwavelength active fraction is calibrated against these data, for several X-ray luminosity ranges, and corrected to take into account that some active BHs might not be detectable in the X-ray domain. The upturn of the X-ray detected fraction (and active fraction, see Figure 3) at low stellar mass is due to the breaking of some of the assumptions in our model, including the flat prior in the distribution of BH masses. Data are obtained from Mezcua et al. (2018a) and Birchall et al. (2020).