To obtain cm/s precision, stellar surface magneto-convection must be
disentangled from observed radial velocities (RVs). In order to understand and
remove the convective signature, we create Sun-as-a-star model observations
based on a 3D magnetohydrodynamic solar simulation. From these Sun-as-a-star
model observations, we find several line characteristics are correlated with
the induced RV shifts. The aim of this campaign is to feed directly into future
high precision RV studies, such as the search for habitable, rocky worlds, with
forthcoming spectrographs such as ESPRESSO.Comment: 6 pages, 3 figures; presented at the 18th Cambridge Workshop on Cool
Stars, Stellar Systems, and the Sun (CoolStars18); to appear in the
proceedings of Lowell Observatory (9-13 June 2014), edited by G. van Belle &
H. Harris. Updated with correct y-axis units on righthand plot in figure
