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Fig. 1


Occurrence probabilities of Jovian radio emissions detected over 26 yr (1990–2015) with the Nançay DecameterArray, displayed as 2D histograms as a function of planetary rotation (CML = Central Meridian Longitude = sub-observer’s longitude) and of the orbital phase of the considered satellite, in 5° × 5° bins (interpolation at 1° resolution was applied to smooth the display). Panel a: occurrence probability of all emissions vs. CML and Io’s orbital phase. The regions of high occurrence within letter-labelled white boxes correspond to Io–Jupiter emissions (usually named Io-A, Io-B …), whereas vertical bands of emission covering restricted CML ranges at all Io phases correspond to non-Io emissions (auroral orinduced by other satellites). Different line styles are used to better distinguish overlapping boxes. Panel b: occurrence probability of non-Io emissions vs. CML and Ganymede’s orbital phase. Ganymede–Jupiter emissions show up within new regions of enhanced occurrence (white boxes), labelled A–D in reference to the non-Io components in which they have been identified (see Fig. 2 for details).

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