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tokens: is produced by the planet. We then Fourier transform the masked data back into phase versus velocity and display that in Fig. 6 . This shows an apparent retrograde trace, which we attribute to the shadow of a planet. This is again similar to what is seen in WASP-33 (Johnson et al. 2015 ). Figure 6. The spectral profiles through transit after removing the stellar pulsations via Fourier filtering. The planet trace is then readily seen moving in a retrograde direction. The left-hand panel shows the simultaneous TRAPPIST photometry of the transit. The planet's Doppler shadow seems to disappear towards the end of the transit (see Fig. 6 ). It is likely that it has been reduced during the filtering process, as a result of imperfect separation of the planetary and stellar-pulsation signals. This might have some effect on fitting the alignment angle λ, which depends on the slope of the Doppler shadow, but should have less effect on the other fitted quantities. In order to parametrize the planet's orbit, we then fitted the CCFs through transit, in a manner similar to the methods in Brown et al. ( 2017 ). Since we had subtracted the ‘minimum CCF’ above, we first add that back in to the filtered CCFs in order to reintroduce the stellar line profile, which is a key feature for constraining the value of v sin i ⋆ . The parameters that define the shape of the CCF line profile are the projected spin–orbit misalignment angle λ, the stellar line-profile full width at half-maximum (FWHM), the FWHM of the line perturbation due to the planet v FWHM , the stellar γ-velocity and v sin i ⋆ . These parameters were fitted using an MCMC fitting algorithm which assumes a Gaussian shape for the line perturbation caused by the planet. Both v sin i ⋆ and v FWHM have two data constraints, one from the shape of the line-broadening profile, and one from the slope of the trajectory of the bump across the line profile (given knowledge of λ). The value of v sin i ⋆ obtained in the spectral analysis was used as a prior in the fit. Initial values for the stellar line FWHM and the γ-velocity were obtained by fitting a Gaussian profile to the CCFs. The λ angle and v FWHM were given no prior. Details of the fitting algorithm are given in Collier Cameron et al. ( 2010a ), and the resulting system parameters are listed in Table 3 . Lastly, in Fig. 7 we show the pulsations without the planet trace, obtained by filtering to leave only the prograde quadrants, and then transforming back into velocity space. Figure 7. The spectral profiles through transit after removing the planet shadow via Fourier filtering. The stellar pulsations are seen moving in a prograde direction. 6 EVOLUTIONARY STATUS We then used MINES weeper , a newly developed Bayesian approach to determining stellar parameters using the MIST stellar evolution models (Choi et al. 2016 ). Examples of the use of MINES weeper in determining stellar parameters are shown in Rodriguez et al. ( 2017a , b ). We model the available B