Debate persists as to whether the cosmological constant $Lambda$ can directly modify the power of a gravitational lens. With the aim of reestablishing a consensus on this issue, I conduct a comprehensive analysis of gravitational lensing in the Schwarzschild--de Sitter spacetime, wherein the effects of $Lambda$ should be most apparent. The effective lensing law is found to be in precise agreement with the $Lambda=0$ result: $alpha_mathrm{eff} = 4m/b_mathrm{eff}+15pi m^2/4b_mathrm{eff}^2 +O(m^3/b_mathrm{eff}^3)$, where the effective bending angle $alpha_mathrm{eff}$ and impact parameter $b_mathrm{eff}$ are defined by the angles and angular diameter distances measured by a comoving cosmological observer. [These observers follow the timelike geodesic congruence which (i) respects the continuous symmetries of the spacetime and (ii) approaches local isotropy most rapidly at large distance from the lens.] The effective lensing law can be derived using lensed or unlensed angular diameter distances, although the inherent ambiguity of unlensed distances generates an additional uncertainty $O(m^5/Lambda b_mathrm{eff}^7)$. I conclude that the cosmological constant does not interfere with the standard gravitational lensing formalism.
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