Close-up measurements of energetic ions at shock #1 in a similar format to Fig. 1 for the same time period shown in Fig. 4. Solar-wind density and temperature are not shown. An additional panel shows the pitch-angle distribution for ∼52 keV protons (3rd panel from bottom). In it, intensity is color-coded using the same color scale as for the other panels. At the prevalent IMF magnitude, the proton gyro period is about ten seconds; the shorter-period waves seen in the IMF are therefore not resonant with solar wind or supra-thermal protons.