Removal of the Doppler shadow caused by the transiting planet from the start of ingress to the end of egress. Top panel: cross-correlation of the exposures in-transit with a template constructed from a PHOENIX stellar photosphere model. Second panel: same as the top panel, annotated with the predicted RV of the occulted stellar region responsible for the Doppler shadow (dashed line). The expected RV of the planet (dotted line) expected from the system parameters by Lund et al. (2017) and Talens et al. (2018) is also shown. Third panel: model of the Doppler shadow obtained by fitting a Gaussian profile to the shadow feature in each of the in-transit CCFs. Bottom panel: residuals after subtraction.