Extended Data Fig. 8: Multi-wavelength view of the coronal structure with Hinode/SOT, IRIS and SDO/AIA.

a, From top left to bottom right we show in order of increasing temperature formation, the common FOV of the coordinated observation at the same time shown in Fig. 1. Chromospheric temperatures are represented by the SOT Ca ii H and IRIS 2,796 Å channels (\({\mathrm{log}}\,T\approx 4-4.2\)). Lower transition region temperatures are represented by IRIS 1,400 Å and AIA 304 Å (\({\mathrm{log}}\,T\approx 4.8-5\)). Upper transition region temperatures are represented by AIA 131 Å and 171 Å (\({\mathrm{log}}\,T\approx 5.7-5.9\)). Coronal temperatures are best observed by AIA 193 Å and 211 Å (\({\mathrm{log}}\,T\approx 6.2-6.3\)). A radial filter has been applied to the SOT, IRIS 2,796 Å and IRIS 1,400 Å images to decrease the disk intensity and to make the off-limb features more visible.b, Same as in a but at the last IRIS observation time (SOT has stopped observing at this time). Note the appearance of the coronal loop following the occurrence of nanojets. See Supplementary Video 7.