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tokens: 2006 ). The observations were carried out over five nights in 2017 March, in clear weather or thin clouds, with seeing 06–10. We used a pixel scale of 025, the 210 grating in H -band and a slit width of 10, yielding a spectral resolution of R ∼ 3000. We adopted a two-point dithering pattern and an exposure time of 5 minutes per frame, for a total on-source time of 21 hr (summed from both spectrographs). To facilitate acquisition, we used a multi-object mask and chose PA = 20° to align the slit to the major axis of the galaxy (Section 2.1 ). The data were reduced using the flame pipeline (Belli et al. 2017 ), which outputs a rectified, sky-subtracted, wavelength-calibrated two-dimensional (2D) spectrum. The corresponding H α PV diagram is shown in Figure 1 (right, color scale). 2.4. One-dimensional Kinematic Profiles To create the one-dimensional (1D) velocity and dispersion profiles in CO, we proceed as described by Genzel et al. ( 2017 ): we first fit a Gaussian profile to the CO line emission in each spaxel of the data cube, smoothed over three spaxels to ensure sufficient signal-to-noise ratio (S/N) in the outer parts of the galaxy. Accounting for the galaxy’s systemic velocity, this results in the 2D velocity map. From this we determine PA kin = 23° as the axis with the steepest velocity gradient. It agrees with PA H , and with the PA of the H α slit observations (Sections 2.1 , 2.3 ). The CO 1D velocity and dispersion profiles are then constructed from 075 diameter apertures (as a compromise between the CO data resolution and the seeing-limited H α data) with the center spaced by 024 along PA kin . To create the 1D profiles in H α , we extract spectra in overlapping bins of two to four spatial pixels and fit a Gaussian profile to the H α line emission. The choice of the number of spatial pixels used for the extraction of individual data points does not substantially affect the extracted values, but allows for increased S/N in the outer disk regions. We trace H α out to 19 kpc (NE, ∼4.4 R e , H ) and 13 kpc (SW, ∼3.1 R e , H ), and CO out to 12 kpc (∼2.8 R e , H ). These physical radii at z ∼ 1.4 are equivalent to probing the rotation curve out to 23–35 kpc for a galaxy of this stellar mass at z ∼ 0 (van der Wel et al. 2014 ). Figure 2 shows the 1D velocity and dispersion profiles in CO and H α along PA kin in observed space. The uncertainties are derived from the Gaussian fits described above where noise has been taken into account. The two tracers agree, indicating that they trace the same mass distribution, most reliably in the outer disk where beam-smearing effects become less important. Figure 2. One-dimensional velocity (left) and velocity dispersion (right) profiles along the kinematic major axis in CO(3–2) (blue circles) and H α (red diamonds). Due to the spatial resolution of the observations, neighboring data points are not independent. The projected distance increases from NE to SW of the kinematic center of the galaxy. The