Best-fit white-light (5.06–10.55 μm) light curves of HD 3167 b’s secondary eclipse from our SPARTA (blue), Eureka! (red), and exoTEDRF (green) reductions. Top: binned raw white-light fluxes. The best-fit full SPARTA model (with integration-level x decorrelation), Eureka!, and exoTEDRF models are shown alongside the quadratic ramp component as dashed lines. Middle: binned fluxes after dividing by the best-fit systematics model for each reduction. Retrieved eclipse depths and uncertainties are shown on the right. Bottom: binned residuals of the best-fit full models. For all plots, Eureka! and exoTEDRF data are offset by 0.001 and 0.002 days for visual clarity.