Notes. Shown are the inclination i of the galaxy disc relative to the plane of the sky in Col. (2), the total stellar mass M_⋆ in Col. (3), the position angle of the galaxy disc PA_gal in Col. (4) (all from S⁴G; Sheth et al. 2010; Muñoz-Mateos et al. 2013, 2015), the mean redshift-independent distance d from the NASA Extragalactic Database (NED, http://ned.ipac.caltech.edu/) in Col. (5), the spatial scale of the observations in Col. (6), and the kinematic radius of the nuclear disc in Col. (7) (Gadotti et al. 2020). Column (8) states the source of the structural components described in the following columns: HE refers to the results from Herrera-Endoqui et al. (2015) while LC designates the multi-component decompositions of de Lorenzo-Cáceres et al. (2019). We refer the reader to Sect. 3.1 for a comparison of the results of both methods. Columns (9)–(12) provide the position angle of the inner bar PA_ib, its full semi-major axis a_full from photometric decompositions, the inner bar semi-major axis from visual inspections a_vis, and the inner bar axial ratio b/a. We note that no kinematic radius could be determined for NGC 1291, due to the face-on orientation of the galaxy. NGC 1433 is not included in the photometric decompositions of de Lorenzo-Cáceres et al. (2019).