## 2 Data and Methods
\begin{table}
\begin{tabular}{c c c c c c c} \hline
**Location** & **Station ID** & **Owner** & **Latitude** & **Longitude** & **AACGM Lat** & **AACGM Lon** \\ \hline Concordia & DMC0 & INGV & 75.10\({}^{\circ}\) S & 123.35\({}^{\circ}\) E & 88.98\({}^{\circ}\) S & 57.64\({}^{\circ}\) E \\ SANAE & SNA0 & INGV & 71.67\({}^{\circ}\) S & 2.84\({}^{\circ}\) W & 61.83\({}^{\circ}\) S & 44.91\({}^{\circ}\) E \\ \hline \end{tabular}
\end{table} 
Table 1: Locations, identifiers, geographic and Altitude Adjusted Corrected GeoMagnetic coordinates (AACGM Lat and AACGM Lon) of the ISMRs used in this study. ISMR = Ionospheric Scintillation Monitoring Receiver. Satellite Program (DMSP) satellites F16-F19 to investigate the link between high-latitude particle precipitation and the occurrence of irregularities. SSUSI, indeed, consists of sensors intended to provide global auroral observations at five wavelengths in the ultraviolet range (115-180 nm), with high spatial resolution (7-9 km at nadir) by scanning across the track of the DMSP trajectory every 15 s [44; 45]. In this study to represent the aurora we used the emission from N2 Lyman-Birge-Hopfield long filter (LBHL) band (165-180 nm), according to [PERSON] and [PERSON] [46]. In addition, we leveraged on the ionospheric electrostatic potential provided by the Super Dual Auroral Radar Network (SuperDARN, [47]) in the form of convection maps to better characterize the dynamics of high latitudes. Although such maps provide only an average picture of the high-latitude ionosphere dynamics, they can be useful to link the local and global evolution of polar cap dynamics to the conditions of the Earth's magnetosphere and the interplanetary medium (especially in those regions where the number of the observed echoes is not negligible). Moreover, in situ measurements of plasma density collected in the topside ionosphere by Langmuir probes on board the Swarm constellation [48] were analyzed to investigate the electron density distribution during the geomagnetic storm. Specifically, we studied the occurrence of polar cap patches (PCPs) identified by using the Swarm IPDxIRP Level 2 product, which is capable of detecting the occurrence of PCPs by means of electron density measurements taken at magnetic latitudes higher than 77\({}^{\circ}\) with a time sampling of 2 Hz. The PCPs correspond to plasma density variations that are at least twice the background density [49]. Values of the PCP flag different from zero indicates the presence of patches along Swarm orbit. Furthermore, to correlate the electron density variability with the storm's drivers, we computed and analyzed the electron density root mean square (_rms_) for each time series corresponding to a polar crossing above \(170^{\circ}\) | of magnetic latitude, for two of the three satellites of the constellation (specifically for Swarm A and Swarm B). Since during the geomagnetic storm here analyzed, Swarm A was flying at an altitude of around 445 km and Swarm B of around 510 km, this data allow us to estimate the average variability of the electron density through the polar cap at different altitudes and times of the day. Data collected by the fluxgate magnetometers co-located with the selected GNSS receivers were used to support the description of the ionospheric area entering the field of view of the receiver. OMNI solar wind and IMF data with a 1-min resolution [50] were used to relate the interplanetary medium conditions to the ionospheric scenario where irregularities causing scintillations appear and evolve. Finally, to investigate the high-latitude ionosphere response in terms of geomagnetic indices, we used \(AE\) (Auoral Electrojet), \(AU\) (Auoral Upper) and \(AL\) (Auoral Lower) indices at a 1-min resolution [51]. Tables 2 and 3 summarize the measurements chosen for the investigation, specifying the sampling time, the instrument type and the location at which such measurements were acquired.