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tokens: A study (not shown here) of the possible effect of the geometry of the shock did not demonstrate a significant correlation between the observed spectra and the angle θ nB between the normal of the shock and the interplanetary magnetic field. The histogram shown in Figure 3 (d) indicates that the spectral slopes vary within the interval ∼[−2.2, −0.3] with a peak near −1.2. The bulk of the distribution is significantly shallower than the Kolmogorov scaling f −5/3 (red dashed line in Figure 3 (d)) and that reported in the solar wind (e.g., Smith et al. 2006 ). These observations question the ubiquity of the Kolmogorov scaling in the terrestrial magnetosheath, although a small fraction (17%) of the events showed a Kolmogorov spectrum (here defined as the spectral slope −1.5). Figure 3. 2D distribution of the slopes P α ( X GSE , Y GSE ) at MHD scales. The 2D distribution P α ( X GSE , Y GSE ) of the spectral slopes at MHD (a), and the integrated ones along the Y GSE direction (b) and X GSE direction (c). The blue curves represent the average magnetopause and bow shock positions computed using the paraboloidal bow shock model of Filbert Kellogg ( 1979 ) and the magnetopause model of Sibeck et al. ( 1991 ). The number in each bin represents the number of events. (d) The histogram of the measured spectral slopes where the red dashed line indicates the Kolmogorov slope −5/3. On the contrary, the slopes at the sub-ion scales were found not to depend on the location within the magnetosheath as can be seen in Figure 4 (a). This can be explained by the fact that the kinetic scales (≤100 km) are much smaller than the integral (size) scale of the magnetosheath (>10 4 km), meaning that the large-scale boundaries do not influence the small (kinetic) scale turbulence. Furthermore, the histogram of the slopes (Figure 4 (b)) is found to be similar to those reported in the solar wind (Alexandrova et al. 2012 ; Sahraoui et al. 2013 ) and in the magnetosheath (Huang et al. 2014 ; Hadid et al. 2015 ), with a peak near −2.8. This observation suggests that kinetic scale turbulence has a “universal-like” scaling distribution in the sense that it does not depend either on the explored region (magnetosheath or solar wind) or on the nature of the turbulence at MHD scale ( f −1 energy-containing range or f −5/3 inertial range), which is probably due to that kinetic scale turbulence is generated locally so its nature is not affected by large-scale inhomogeneities/fluctuations. Figure 4. 2D distribution of the slopes P α ( X GSE , Y GSE ) at sub-ion scales. The 2D distribution P α ( X GSE , Y GSE ) of the spectral slopes at sub-ion scales (a); the histogram of the spectral slopes (b). The number in each bin represents the number of events. Hadid et al. ( 2015 ) showed that the f −1 range in the magnetosheath of Saturn was populated by random-like fluctuations. It has been speculated that the interaction of the solar wind with the shock destroys the pre-existing correlations