Map of the residual CCF flux during the transit of KELT-9 b. The observations of two nights are binned by 2 in phase. The 1st and 4th contacts are traced with the horizontal dashed white lines; the 0 km s⁻¹ and ± v sin i_* are traced with vertical dashed white lines. Top panel: local stellar spectrum tracing the spin-orbit misalignment through the Rossiter-McLaughlin effect. The solid black line shows our best fit. The exoplanet transmission CCF, that has a slanted shape following the orbital velocity (dashed black line), traces the metal detections by Hoeijmakers et al. (2018, 2019). Bottom panel: residual CCF flux after the removal of the local stellar and of the planetary atmosphere spectra. The residuals are dominated by the stellar pulsations, whose strengths are 10 × lower than the local stellar signal (see the color scale). The pulsations are due to pressure-mode in a δ Scuti-type star.