VELC raster scan spectroscopic observations on 2024 August 4 (00:30–01:05 UT) in the 5303 Å channel showing the emission-line intensity, FWHM, and Doppler velocity. The orange circle (in dotted lines) and red circle indicate the solar limb and VELC occulter, respectively. Solar north is straight up, and east is to the left. Exposure time is 4 s, and gain is 1×. Five frames were binned on board in each raster step. Coronal emission can be observed until the edge of the FoV on the solar east. There is good correspondence between the structures seen in the intensity, FWHM, and Doppler maps. No coronal structures could be seen above the north and south limbs in VELC (J. Singh et al. 2025), due to the generally very weak 5303 Å emission there (M. Waldmeier 1957; R. Fisher & S. Musman 1975; M. Mierla et al. 2005).