In situ observations at ∼1 au as observed, from left to right, by STEREO-B, STEREO-A and ACE. From top to bottom, (a) electron intensities, (b) magnetic field magnitude, (c)–(d) magnetic field angular direction in the RTN coordinate system, (e) solar wind speed, (f) solar wind proton density, and (g) solar wind proton temperature. The solid vertical lines indicate the passage of interplanetary shocks, and the dashed vertical lines the passage of an ICME by STEREO-A.