Left: image reconstruction of Achernar obtained by applying the MIRA software to the H band VLTI/PIONIER observations. Middle: convolution of this reconstructed MIRA image convolved by a Gaussian beam of FWHM = 1.6 mas (=0.61λ/B_max) corresponding to the diffraction limit of the PIONIER observations. Right: Reconstructed MIRA image minus the best-fit CHARRON image (Fig. 11 convolved by the Gaussian diffraction limit beam to mach the resolution of reconstructed image). The difference between the images is very small, <1.5% in modulus, relative to the total MIRA image flux), indicating that essentially only the photosphere of Achernar contributes to the PIONIER data, without any additional circumstellar component. The dotted ellipse approximately represents the border of the apparent photosphere of Achernar given by the best-fit CHARRON RVZ model.