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tokens: work is different from traditional KAW theory of , but is close to the theoretical prediction of from Boldyrev Perez ( 2012 ) and Boldyrev Loureiro ( 2019 ) and the simulation from Cerri et al. ( 2019 ). It also corresponds to α = 1.13 in the framework of the model by Landi et al. ( 2019 ). Hence a modified CB premise may be needed to understand the kinetic turbulence in magnetosheath. We note that, for most of the events, the weak and scale-independent anisotropy in the perpendicular plane appears to agree with recent PIC simulation of KAW turbulence (D. Grošelj 2020, private communication) but is inconsistent with results of Boldyrev Loureiro ( 2019 ), which predicts a much stronger anisotropy and a steeper scaling of or L ⊥ ∝ , depending on different current sheet configurations for the tearing instability. Capturing the active signatures of current sheet disruption/reconnection (i.e., Mallet et al. 2017 , Loureiro Boldyrev 2017 ) from in situ observation is a challenging task, but will contribute to understanding its effects on the anisotropy. The spectral anisotropy of kinetic plasma turbulence is believed to be associated with dispersion and intermittency effects (Zhao et al. 2016 ; Landi et al. 2019 ). For example, the anisotropic scalings are different below and above ion cyclotron frequency and also differs for sheet and tube-like turbulence (Zhao et al. 2016 ). To illustrate the possible connection between intermittency and spectral anisotropy, we specifically compare the results from two events. Figure 5 shows the excess Kurtosis and anisotropy relation for the total magnetic field. The excess Kurtosis is defined as , where S 4 ( l ) is the fourth-order structure function. In both panels of Figure 5 , the solid lines represent the results from event 1, which is recorded on 2017 October 4 and is used as our example of spectral anisotropy in Section 3 , while the dashed–dotted lines represent the results from event 2, which is recorded on 2017 December 24. As plotted in three directions l ⊥ , L ⊥ , l ∥ , the value of K ( l ) is around zero at large scales, meaning the roughly Gaussian distribution of the fluctuations. Toward small scales, K ( l ) displays an increase tendency before it drops down. Such non-Gaussian statistics ( K ( l ) > 0) confirms the presence of intermittency in the magnetosheath, while the scale-dependent profile of Kurtosis is similar with solar wind observations (He et al. 2019 ). For the kinetic-scale parallel–perpendicular anisotropy, we find that it can be considerably affected by the intermittency. As shown in Figure 5 , the stronger the intermittency (see the larger Kurtosis of the solid lines in the left panel), the stronger the anisotropy level (see the larger vertical distances between the solid blue curve and the gray line in the right panel). This phenomenon is consistent with previously observations at large scales, which emphasize the key role of intermittency in generating the spectral anisotropy