The high latitude radio emissions produced by the Cyclotron Maser Instability (CMI) in Jupiters magnetosphere extend from a few kHz to 40 MHz. Part of the decametric emissions is of auroral origin, and part is driven by the moons Io, Europa and Ganymede. After summarizing the method used to identify Jupiter-satellite radio emissions, which consists in comparing space- and ground-based radio observations to ExPRES simulations of CMI-driven emissions in the time-frequency plane, we present a parametric study of the free parameters required by the ExPRES code (electron distribution function and resonant energy, magnetic field model, lead angle, and altitude of the ionospheric cut-off) in order to assess the accuracy of our simulations in the Io-Jupiter case. We find that Io-DAM arcs are fairly modeled by loss-cone driven CMI with electrons of 1-10 keV energy, using the ISaAC, VIPAL or VIP4 magnetic field model and a simple sinusoidal lead angle model. The altitude of the ionospheric cut-off has a marginal impact on the simulations. We discuss the impact of our results on the identification of Europa-DAM and Ganymede-DAM emissions.
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