Scattered-light is a relevant noise source in current ground-based gravitational-wave detectors and a critical design concern for next-generation observatories. Beamtube scattered-light estimates usually combine optical propagation simulations with analytical couplings that do not fully propagate the frequency-dependent optomechanical response of the interferometer to the strain readout. In this work, we use improved analytical transfer factors to convert scattered-light field perturbations in the Fabry-Pérot arm cavities into equivalent strain noise, consistently including radiation-pressure coupling, signal-extraction dynamics, microscopic detunings, and the homodyne readout angle. The formalism keeps the full amplitude and phase quadrature content of the scattered field, including the cross terms that arise in both diffraction and backscattering noise. For diffraction, we also identify the regime in which the linearized coupling to baffle motion is valid, avoiding unnecessary phase wrapping. Using representative LIGO, Cosmic Explorer, and Einstein Telescope–Low Frequency configurations, we show that legacy estimates are recovered in phase-dominated regimes but can differ when radiation-pressure coupling, quadrature correlations, or detuned signal extraction become important. In particular, the revised Einstein Telescope–Low Frequency estimate changes substantially with respect to previous beamtube noise budgets due to the detuned signal-extraction cavity. These results provide a more complete framework for scattered-light noise estimations for present and future gravitational-wave detectors.

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• Gravitational waves
• Gravitational wave detectors