  Since the Schwarzschild-de Sitter spacetime is static inside the cosmological
event horizon, if the dark energy state parameter is sufficiently close to
$-1$, apparently one could still expect an effectively static geometry, in the
attraction dominated region inside the maximum turn around radius, $R_{\rm TA,
max}$, of a cosmic structure. We take the first order metric derived recently
assuming a static and ideal dark energy fluid with equation of state
$P(r)=\alpha\rho(r)$ as a source in Ref. [1], which reproduced the expression
for $R_{\rm TA, max}$ found earlier in the cosmological McVittie spacetime.
Here we show that the equality originates from the equivalence of geodesic
motion in these two backgrounds, in the non-relativistic regime. We extend this
metric up to the third order and compute the bending of light using the
Rindler-Ishak method. For $ \alpha\neq -1$, a dark energy dependent term
appears in the bending equation, unlike the case of the cosmological constant,
$\alpha=-1$. Due to this new term in particular, existing data for the light
bending at galactic scales yields, $(1+\alpha)\lesssim {\cal O}(10^{-14})$,
thereby practically ruling out any such static and inhomogeneous dark energy
fluid we started with. Implication of this result pertaining the uniqueness of
the Schwarzschild-de Sitter spacetime in such inhomogeneous dark energy
background is discussed.
