Example correlation maps (left panels) and phase-folded correlations (right panels) obtained from cross-correlating the thousands of water lines across each spectrum of our WASP-69b observations with models at Doppler shifts of −100 km s−1 to +100 km s−1. The color represents the correlation strength. The top panels show the analysis process for our data, and the bottom panels show the same process repeated on the data with a water model injected (see Figure 11). The signal from water is visible in the bottom left panel as a diagonal line across the in-transit portion of the map, corresponding to roughly −0.01 to + 0.01 orbital phase. Likewise, the signal is visible at the Keplerian velocity of the exoplanet in the bottom-right panel, at the expected Vsys and Kp of the planet: 0 km s−1 and ∼127 km s−1 respectively. The cross indicates this position in both panels. The fact that no similar signal is visible in the original analysis of our data indicates that water is not present in the atmosphere of WASP-69b at the strength of the injected model.