tokens: or the ansae (symmetric enhancements at the ends of the stellar bar) observed in the inner bar. Fig. 1 shows a 3.6 m S 4 G image of NGC 1291 where these stellar structures are visible. Figure 1. S 4 G 3.6 m images of NGC 1291. The left-hand panel shows the main outer structures described in Section 2 , i.e. the outer ring, outer disc, lens, and outer bar. The blue square represents the MUSE 1 arcmin × 1 arcmin field of view. The right-hand panels show a zoom-in (upper panel) and contour (lower panel) images highlighting the central photometric structures, i.e. inner disc, inner bar, and central bulge. They correspond to the actual field of view observed with MUSE, which is slightly offset with respect to the centre of the galaxy. North is up and East is left. 3 TIMER OBSERVATIONS OF NGC 1291 The TIMER project is a survey employing the MUSE integral-field spectrograph to study the central 1 arcmin × 1 arcmin of a sample of 24 nearby ( d 40Mpc) barred galaxies with nuclear rings and other central structures such as nuclear spiral arms, inner bars, and inner discs (see Paper I ). One of the project’s main goals is to study the star formation histories of such structures to infer the cosmic epoch of the formation of the bar and the dynamical settling of the main disc of the host galaxy. The methodology was demonstrated with a pilot study of NGC 4371 (Gadotti et al. 2015 ). The corresponding observations of NGC 1291 were performed during ESO Period 97 (2016 April to September) with a typical seeing on the combined data cube of 1.1 arcsec (spaxel size = 0.2 arcsec), mean spectral resolution of 2.65 Å (full width at half-maximum), and spectral coverage from 4750 Å to 9350 Å. NGC 1291, being one of the closest galaxies in the TIMER sample, the MUSE 1 arcmin × 1 arcmin field of view (FoV) corresponds to a (almost) square region of ≈2.5 kpc on a side (i.e. 1 arcsec corresponds to 42 pc). The MUSE pipeline (version 1.6) was used to reduce the data set (Weilbacher et al. 2012 ), correcting for bias and applying flat-fielding and illumination corrections, as well as wavelength calibration. The exposures were flux-calibrated through the observation of a spectrophotometric standard star, which was also used to remove telluric features. Dedicated empty-sky exposures and a PCA methodology were employed to remove signatures from the sky background. Finally, the exposures were also finely registered astrometrically, so that the point spread function of the combined cube is similar to that in individual exposures. More details can be found in Gadotti et al. ( 2018 ). 3.1 Stellar kinematics The fully reduced data cube was spatially binned using the Voronoi scheme of Cappellari Copin ( 2003 ) to achieve a signal-to-noise ratio of approximately 40 per pixel on each spatial bin. We used the penalized pixel fitting ( ppxf ) code developed by Cappellari Emsellem ( 2004 ) to extract the stellar kinematics from the binned spectra, masking emission lines and using the
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