摘要：Context. Stellar signals are the main limitation for precise
radial-velocity (RV) measurements. These signals arise from the photosphere of the stars.
The m s-1 perturbation created by these signals prevents the
detection and mass characterization of small-mass planetary candidates such as
Earth-twins. Several methods have been proposed to mitigate stellar signals in RV
measurements. However, without precisely knowing the stellar and planetary signals in real
observations, it is extremely difficult to test the efficiency of these methods.
Aims. The goal of the RV fitting challenge is to generate simulated RV
data including stellar and planetary signals and to perform a blind test within the
community to test the efficiency of the different methods proposed to recover planetary
signals despite stellar signals.
Methods. In this first paper, we describe the simulation used to model
the measurements of the RV fitting challenge. Each simulated planetary system includes the
signals from instrumental noise, stellar oscillations, granulation, supergranulation,
stellar activity, and observed and simulated planetary systems. In addition to RV
variations, this simulation also models the effects of instrumental noise and stellar
signals on activity observables obtained by HARPS-type high-resolution spectrographs, that
is, the calcium activity index log (\hbox{$R^{\prime}_{HK}$}) and the bisector span and full width at half maximum
of the cross-correlation function.
Results. We publish the 15 systems used for the RV fitting challenge
including the details about the planetary systems that were injected into each of
them.
