Low-coronal and coronal observations of the possible solar/CME counterparts associated with the ICME periods under study. (a) STEREO-A/EUVI full disk image of the solar disk in the 304 Å band on June 2, 2020, 03:56 UT. A filament on the northwest limb, later observed to disappear, is visible inside the white square. A zoom of the squared area is provided in the bottom left corner of the panel. (b) STEREO-A/COR1 white-light image of the corona on June 3, 2020, 03:24 UT. A slow CME propagating at ∼275° latitude (likely associated with the ICME1 signatures observed by Solar Orbiter) is visible inside the white square. A zoom of the squared area is provided in the bottom left corner of the panel. (c) SDO/AIA full disk image of the solar disk in the 171 Å band on June 3, 2020, 08:48 UT. Eruptive plasma close to west limb at ∼40° north is visible inside the white square. A zoom of the squared area is provided in the bottom left corner of the panel. The SDO/HMI colorized magnetogram on May 25, 2020, 12:00 UT, showing the bipolar magnetic region likely associated with the filament eruption, is displayed in the bottom right corner of the panel. (d) SOHO/LASCO-C2 white-light image of the corona on June 4, 2020, 02:24 UT. A CME is clearly visible as a bright feature propagating at ∼240° latitude inside the white square: This can correspond to ICME2, encountered by Solar Orbiter. A zoom of the squared area is provided in the bottom left corner of the panel. An animated version of each panel, generated using JHelioviewer (Müller et al. 2017), is available online. The animations run from June 2, 2020, 00:00 UT to June 6, 2020, 23:59 UT.