  The deflection angle of equatorial light (the light in the equatorial plane)
in Kerr-de Sitter (KdS) spacetime was previously calculated by Sultana
[\href{https://journals.aps.org/prd/abstract/10.1103/PhysRevD.88.042003}{Phys.
Rev. D 88, 042003 (2013)}]. However, we have identified three problems with his
result: (a) Orbit problem, the orbit solution used for computing the deflection
angle is inaccurate as it does not stem from the original equation of motion
(EOM). (b) Position problem, assuming the source and observer are at infinity
is physically unrealistic given the presence of the cosmological horizon. (c)
Static problem, assuming the observer remains at rest in a static slice of
spacetime ignores the expansion of the de Sitter space. In this paper, we
address and correct these issues respectively by (a) deriving the orbit
solution through solving the original EOM directly, (b) employing a widely
accepted definition of the finite-distance deflection, and (c) adopting the
Randers optical space for the spatial projection of null geodesics. Based on
these corrections, we obtain a more precise and applicable result for the
deflection angle of equatorial light in KdS spacetime.
