Overview plot in the 5-min vicinity of the shock on 2021 November 3. Panels (a)–(c), (e), and (g)–(h) show the same as Fig. 1, but on a shorter timescale. Panels (d) and (f) show the spectrogram of dynamic energy spectra measured by the northward (d) and sunward (f) telescopes in the spacecraft frame. The color scale represents the intensities of the differential flux multiplied by the energy squared. The dashed black line in panel (d) indicates the velocity dispersion feature, and the dashed black line in panel (f) indicates the inverse-velocity dispersion feature. (i): PA coverage of the four EPT telescopes. (j): X-component of the IMF B_x (black) and X-component of the solar wind velocity V_x (blue) in the spacecraft frame. (k): Angle between the IMF and the shock normal, local θ_Bn, and the angle between the IMF and the radial direction, θ_Br. These two angles are equal to each other because the shock normal almost aligns with the radial direction. The apparent magnetic kinks or switchbacks are plotted in red, and the horizontal dotted line indicates the average angle in the ambient solar wind plasma. The vertical solid brown line marks the shock arrival. The vertical dashed lines bound an upstream and a downstream interval with labels at the top, which are analyzed in Fig. 5.