  Recent and upcoming stabilized spectrographs are pushing the frontier for
Doppler spectroscopy to detect and characterize low-mass planets.
Specifications for these instruments are so impressive that intrinsic stellar
variability is expected to limit their Doppler precision for most target stars
(Fischer et al. 2016). To realize their full potential, astronomers must
develop new strategies for distinguishing true Doppler shifts from intrinsic
stellar variability. Stellar variability due to star spots, faculae and other
rotationally-linked variability are particularly concerning, as the stellar
rotation period is often included in the range of potential planet orbital
periods. To robustly detect and accurately characterize low-mass planets via
Doppler planet surveys, the exoplanet community must develop statistical models
capable of jointly modeling planetary perturbations and intrinsic stellar
variability. Towards this effort, this note presents simulations of extremely
high resolution, solar-like spectra created with SOAP 2.0 (arXiv:1409.3594)
that includes multiple evolving star spots. We anticipate this data set will
contribute to future studies developing, testing, and comparing statistical
methods for measuring physical radial velocities amid contamination by stellar
variability.
