The folder   Jup-enc   contains the data from the Zarka et al., JGR, 2004 paper.
Il includes an   aaareadme.txt   that describes its content.

The flux density (Jup_2000_1.sav) and ephemeris (jupeph.sav) data were gathered, with new thresholding and gaps labeling, using the program   make_jupiter_cassini_sav.pro   to produce the new save-set   Jupiter_Cassini.sav   where flux density data is in the array   x(174720, 206).
The data was recorded in 3 RPWS modes: Monopole (79% of the time), Dipole (5%), and Mixed (5%). Gaps represent 11% of the time.

Then the program   integ_jup.pro   performed the detrending in 2 different ways. The original flux density data were renamed   x_raw(174720, 206)   and the detrended data produced are   x1(174720, 206)   and   x2(174720, 206).
As decribed in the paper Zarka et al., JGR, 2020,
x1   results from (i) subtraction from spectra in each of the above 3 modes of a background recomputed separately for each mode, followed by (ii) interpolation of isolated spikes < -4σ or > 10σ on surrounding values at the same frequency. 
As an alternative detrending,
x2   results from  (i) equalization of re-computed backgrounds to the one in Monopole mode (i.e. no background subtraction but only subtraction from each spectrum in Dipole or Mixed mode of the difference between the corresponding background and the one in Monopole mode), followed by (ii) interpolation of isolated spikes < -4σ or > 10σ on surrounding values at the same frequency, then (iii) subtraction of a polynomial (parabolic) fit of the residual long term variation at each frequency, (iv) equalization of intensity histograms at each frequency relative to each other, and (v) a second pass of spikes elimination (ii).
Results are similar, except that x2 preserving better very low values down to -20 dB of the Galactic background (that are rather set to 0 dB in x1).
Gaps are set to -1.

Circular polarization was then computed from Cassini data (kronos database in Meudon) using the program   high_res_plot.pro   called for each day of Jupiter_Cassini_2.sav by   batch_high_res_plot.pro   using the frequency ramp   framp.sav   from   Jupiter_Cassini_2.sav
Results were gathered in a single array   xpol(174720, 206).
The content of Jupiter_Cassini.sav (with x renamed x_raw) plus x1, x2 (detrended flux densities) and xpol (circular polarization)  were saved in Jupiter_Cassini_3.sav

The catalog of radio components contours is in   emissions.sav
The save sets   emissions.sav   and   Jupiter_Cassini_3.sav   can be used together by the program   plot_all_3.pro   to produce the summary plots in   allplots_3.pdf