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tokens: dex, log ( g ⋆ ) = 4.25 ± 0.14 (cgs), and V sin i ⋆ = 11.9 ± 0.3 km s −1 . We found no evidence of a double-lined binary or any blends of spectral components. Fig. 2 Transit light curves of EPIC 212036875 b obtained with MuSCAT2 (TCS) in g ′ ( upper left ), r ′ ( upper right ), i ′ ( lower left ), and z ′ ( lower right ) filters. The black solid line is the best-fit model accounting for the de-trending and transit components. The residuals are plotted in the lower portion of each plot. 3.3 Radial velocity follow-up with FIES The RV follow-up was performed with the FIbre-fed Échelle Spectrograph (FIES; Telting et al. 2014 ; Frandsen Lindberg 1999 ) mounted on the 2.56 m Nordic Optical Telescope (NOT) at the Roque de los Muchachos Observatory. We observed nine high-resolution ( R ≈ 67 000) spectra between 9 April and 22 May 2018 as part of our CAT and TAC programmes 57-015, 57-206, and 57-210, and OPTICON programme 2018A-044. To account for the RV offset caused by a major instrument refurbishment that occurred on 30 April 2018, we treated the RV taken between 9 and 26 April, and between 6 and 8 May as two independent data sets. In addition, 14 intermediate-resolution ( R ≈47 000) FIES spectra were also acquired between 12 May 2018 and 26 Feb. 2019, as part of the OPTICON programme 2018B-052 and the Spanish-Nordic programme 58-301. Depending on the sky conditions and scheduling constraints, we set the exposure times to 1800 – 3600 s for both resolutions. To trace the RV drift of the instrument we followed the strategy outlined in Gandolfi et al. (2015) and Buchhave et al. (2010) and bracketed the science exposures with long-exposed (60 – 90 s) ThAr spectra. We used the standard IRAF and IDL routines to reduce the data. The S/N of the extracted spectra ranges between ~35 and 75 per pixel at 5500 Å. Radial velocities were extracted via multi-order cross-correlations with the spectrum of the RV standard star HD 168009, for which we adopted an absolute RV of −64.650 km s −1 ( Udry et al. 1999 ). The FIES RVs are listed in Table A.1 . Figure A.2 shows the generalised Lomb-Scargle periodogram of the offset-corrected Doppler measurements (combined by subtracting the systemic velocities listed in Table 5 ). We found a very significant peak at the orbital frequency of the transiting BD with a false alarm probability FAP ≪ 10 −6 , proving that the Doppler reflex motion of the star induced by the orbiting companion is clearly detected in our data. 3.4 Subaru/IRCS AO imaging In order to obtain high-contrast, high-resolution images of EPIC 212036875, we performed AO imaging with the InfraRed Camera and Spectrograph (IRCS, Kobayashi et al. 2000 ) mounted on the Subaru 8.2 m telescope on 14 June 2018. The target star was used as a natural guide and AO correction was applied to obtain high-contrast K ′ -band images of the target. We used the fine-sampling mode (1 pix ≈ 21 mas), and implemented a five-point dithering to minimise the impacts of bad pixels and