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Stellar signals are the main limitation for precise radial-velocity (RV)measurements. These signals arise from the photosphere of the stars. The m/sperturbation created by these signals prevents the detection and masscharacterization of small-mass planetary candidates such as Earth-twins.Several methods have been proposed to mitigate stellar signals in RVmeasurements. However, without precisely knowing the stellar and planetarysignals in real observations, it is extremely difficult to test the efficiencyof these methods.  The goal of the RV fitting challenge is to generate simulated RV dataincluding stellar and planetary signals and to perform a blind test within thecommunity to test the efficiency of the different methods proposed to recoverplanetary signals despite stellar signals.  In this first paper, we describe the simulation used to model themeasurements of the RV fitting challenge. Each simulated planetary systemincludes the signals from instrumental noise, stellar oscillations,granulation, supergranulation, stellar activity, and observed and simulatedplanetary systems. In addition to RV variations, this simulation also modelsthe effects of instrumental noise and stellar signals on activity observablesobtained by HARPS-type high-resolution spectrographs, that is, the calciumactivity index log(R'hk) and the bisector span and full width at half maximumof the cross-correlation function.  We publish the 15 systems used for the RV fitting challenge including thedetails about the planetary systems that were injected into each of them (dataavailable at CDS and here: https://rv-challenge.wikispaces.com.

Radial Velocity Fitting Challenge. I. Simulating the data set including realistic stellar radial-velocity signals