Interferometric searches for axion-like dark matter (ALP DM) via the induced photon birefringence in a coherent background have been proposed and analyzed by several authors over the past decade, with tabletop experiments (LIDA, ADBC, DANCE) reporting first results and detailed calculations available for both ground-based (LIGO, GEO600 via DarkGEO) and space-based (LISA, TianQin, Taiji, BBO via Gu'e et al. and Yao et al.) gravitational-wave detectors. We revisit this class of measurements within the framework of Krauss (2019), and provide a detailed treatment of the interplay between the DM coherence length $\lambda_{\rm coh}$, the interferometer arm length $L$, and the detector transfer function, with attention to the distinct suppression regimes $\lambda_{\rm coh} > L$ (cancellation) and $\lambda_{\rm coh} < L$ (random walk). For LIGO the sensitivity is set by the Fabry-P'erot arm cavity response peaking sharply near the cavity free spectral range, reproducing the results of Nagano ; the naive single-pass estimate substantially overstates the reach and cannot be applied directly. For LISA, with the polarization-sensitive modification proposed by Gu'e or Yao , the natural mass range $m_a\sim 4\times {10}^{-19}$–$4\times {10}^{-16}$~eV (LISA science band) is accessible and the projected reach $g_{a\gamma\gamma}\lesssim {\rm few}\times 10^{-13}$~GeV${}^{-1}$ (realistic optical-metrology noise) improves on the CAST bound over most of the band by up to about two orders of magnitude. We discuss directional signatures from the Galactic DM wind, both annual and sidereal, as a discrimination tool for candidate signals. Local DM substructure with anisotropic velocity dispersion can shift and enhance the reach in specific mass windows.