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tokens: UT ( middle ), and 10:44:00 UT ( right ), denoted by dashed black lines in panel a . The radio contours are overlaid on AIA 211 Å running-difference images and LASCO C2 running-difference images that show the progression of the CME. Panel c : flux density spectra at NRH (red dots) and RSTN (orange triangles) frequencies at the same times as in panel b . The NRH flux densities were estimated over the northern source denoted Type IV in panel b . Flux density spectra were computed using the flux densities of the second component of the Type IV burst source at three times: 10:47, 10:55 and 11:03 UT, in Fig. 7 c. There is a clear power-law decrease at all times in Fig. 7 c, and this trend remains consistent from 10:47 UT until ∼11:05 UT (Fig. 6 ). After 11:05 UT, at 408–445 MHz, the Type IV radio source emission becomes faint and is comparable in brightness to active region and quiet-Sun emissions, as it drops below 10 sfu. At 10:47 UT, we estimate a negative spectral index of −1.6 that also includes contributions from a second source to the north in Fig. 7 b. After 10:49 UT (Fig. 4 c), the power-law decrease becomes clearer because only the Type IV source is present, and we estimate spectral indices of −3.3 at 10:49 UT and −2.3 at 11:03 UT. The second component of the Type IV burst shows an outward movement through time at all frequencies. The centroid locations of the second component of the Type IV burst are shown in Fig. 8 at 298 MHz. The centroids have been split into two periods: a stationary period at 10:44:20–10:49:20 (Fig. 8 a) and a moving period at 10:49:20–11:10:00 UT (Fig. 8 b). The centroids are superimposed on an AIA 171 Å running-difference image in Fig. 8 a and on a 174 Å running-difference image from the Sun Watcher using the Active Pixel System detector and Image Processing (SWAP; Berghmans et al. 2006 ) on board PROBA2 in Fig. 7 b. The SWAP image is used to show a larger field of view, and it has been limb-enhanced to show faint coronal loops beyond the solar limb. Fig. 8. Moving Type IV centroids at 298 MHz split into two phases: a stationary phase ( panel a ) and a moving phase ( panel b ). The centroids are overlaid on AIA 171 Å ( panel a ) and SWAP 174 Å ( panel b ) running-difference images that show the expansion of coronal loops in the negative x -direction behind the CME. The movement of the radio sources in panel b is coincident with the outward growth of the cusp-shaped loop system. The Type IV burst appears stationary for ∼5 min, but at this time, other sources are present. It is possible that various radio sources are superimposed, and we cannot accurately determine a centroid location. The moving period is characterised by the radio source moving away from the solar disc, and it starts after 10:49 UT, when the spectral index also shows a clear power-law decrease that remains consistent over time (Fig. 7 ). In both panels, the centroids are coincident with a cusp-shaped loop system that rises to increasing