  We provide formulae for the calculation of precise Doppler velocities of
sunlight, in both the case of direct observations of the Sun and in reflection
from the surfaces of solar system objects such as the Moon or asteroids. We
discuss the meaning of a "barycentric correction" of measurements of these
Doppler velocities, which is a different procedure from the analogous
correction for starlight, and provide a formula for reducing such measurements
to the component of the Sun's motion in the direction of the Earth or other
Solar System object. We have implemented this procedure in the public
barycorrpy Python package, and use it to explore the properties of the
barycentric-corrected Doppler velocity of sunlight over 30 years. When measured
directly, we show it is dominated by the non-periodic motion due to Jupiter,
and that the signals of the other planets, including Venus, are not discernible
in Fourier space. We show that "detecting" Venus in the Doppler velocities of
sunlight will require either observing sunlight in reflection from an asteroid,
or modeling the their individual contributions to the motion of the Sun in
counterfactual kinematic or dynamical simulations of the Solar System with and
without them.
