Speaker
Description
The future space-based gravitational-wave observatory LISA will detect massive black hole binaries (MBHBs) with signal-to-noise ratios (SNRs) reaching thousands. Such precision demands accurate modeling of the detector response. Current formulations neglect spacecraft motion during light travel time, omitting velocity-dependent terms of order $v/c \sim 10^{-4}$. We derive these corrections and quantify their impact relative to the state-of-the-art simulator lisagwresponse. The corrections yield residual SNRs up to $\sim 2$ for the loudest events, and fractional differences up to $0.04%$ in other regimes. While small, these effects are comparable to waveform modeling uncertainties and leave distinctive imprints on sky localization, making them relevant for parameter estimation and mock data generation.
