Time series for STEREO-A (left panels) and STEREO-B (right panels) for the 11 October 2013 event. Panel a [g] shows the Alfvénic Mach number (M_A) of the shock on the intersection point with the STA (in red) [STB (in blue)] field line. The solid line represents M_A for the original magnetic field line connecting the surface of the Sun to STA [STB], whereas the dashed lines represent the uncertainties on the M_A. These were calculated using 100 magnetic field lines created by taking random (lon, lat) values in a Gaussian around the original latitude and longitude of the magnetic field line at 20 solar radii (see Sect. 3 for more details). Panel b [h] shows the density compression ratio (XR) and the magnetic compression ratio (MR) of the shock on the intersection point with the STA (in red) [STB (in blue)] field line. As in panel a [g], the solid line represents values for the original magnetic field line connecting the surface of the Sun to STA [STB], whereas the dashed lines represent the uncertainties. Panel c [i] shows the electrons received by STA [STB] SEPT in the 85–125 keV energy band. Panel d [j] shows protons received by STA [STB] HET in the 60–100 MeV energy band. The two vertical magenta dashed lines in panel c, d, i, and j indicate the time of shock connection and the end time of the shock, while the orange and purple dashed lines represent respectively the timings of the hard X-ray and type II radio burst. Panel e [k] shows the electron-to-proton ratio from the two precedent times series for STA [STB]. Panel f [l] shows the anisotropy (in grey) and the background-subtracted anisotropy (in purple) of STA [STB] SEPT electrons of 85–125 keV.