Overview of the fields and plasma parameters used in this study for the time period surrounding a reconnection event identified by S. Eriksson et al. (2024; highlighted in purple). Panel (a) shows the trace magnetic field spectrum and associated fit for the time period associated with the reconnection event (highlighted in panels (b–d)). The right-side panels show the (b) SPANi proton velocity, (c) FIELDS fluxgate magnetometer magnetic field measurements, and (d) ion and electron temperatures measured by the SPANi and SPANe instruments. v_R,T,N and B_R,T,N are the radial, tangential, and normal components of the proton velocity (b) and magnetic field (c), respectively, where R is the direction from the Sun to the spacecraft, T is the cross product of the Sun’s rotation vector with R, and N = R × T (M. A. Hapgood 1992). All data have been filtered to remove time periods where the bulk of the distribution moves out of the SPANi FOV.