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Appendix A: Kinematic alignments versus apparent ellipticity

All the kinematic parameters presented in this study are determined on the plane of the sky. Therefore, it is expected that any intrinsic kinematic property would be affected by the inclination of the galaxy with respect to the plane of the sky. In this appendix we show the same kinematic misalignments presented in Sect. 4 with respect to the apparent ellipticity as proxy of the apparent inclination of the galaxies.

	Fig. A.1 Distribution of the ellipticity as proxy of the inclination for the galaxies used in this study. Dashed lines represent the unbarred galaxies, dotted-lines correspond to the weakly barred galaxies and solid lines shows the distribution of strong barred galaxies.
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In Fig. A.1 we plot the distribution of the non-interacting galaxies with respect to the ellipticity. We have a fair coverage of galaxies at different inclinations, in particular for the low-inclined ones (ϵ < 0.5). To have consistent results, we also try to have the same fraction of barred vs. unbarred galaxies in different ellipticity bins.

In Fig. A.2 we plot the morpho-kinematic misalignments explained in Sect. 4.1 against the ellipticity for both components, as well as the internal kinematic misalignment in each component (Fig. A.3) and the comparison of the kinematic PA between the stars and the gas (Fig. A.4). We find large morpho-kinematic misalignments in galaxies with low ellipticities (ϵ< 0.3, see Fig. A.2).

For the kinematic parameters independent of the morphology (i.e., Figs. A.3 and A.4), we find rather similar values in different ellipticity bins. In each panel of these figures, we plot an estimation of the projections effects as function of the ellipticity assuming a face-on misalignment of 60° (see Fig. A.2) in

any of the (morpho-)kinematic indicators. This value was chosen to approximately match the misalignments found at large ellipticities. Within uncertainties, all the galaxies display internal kinematic misalignments that are smaller than the ones expected for their inclinations. In other words, for these misalignments, we do not find large scatters at low ellipticities, as expected for a quantity heavily affected by projection effects.

Fig. A.2 Difference between the morphological PA (PAmorph) and the kinematic PA (PAkin) against the ellipticity of the outermost isophote of the galaxy for the stars (top panel) and the ionised gas (bottom panel). Both kinematic sides of the velocity maps were compared with PAmorph. In each panel, the green filled circles represent the unbarred galaxies, blue diamonds are weakly barred galaxies, and violet squares correspond to barred galaxies. For early-type galaxies we use empty circles. Labels indicate the 3σ outliers. Dashed lines represent the projection effect of a morpho-kinematic misalignment of 60° measured in the plane of the galaxy. In each panel, the grey area represents the 2σ dispersion of the sample.

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Fig. A.3 Internal kinematic misalignment between the receding PA (PAkin,rec) and approaching (PAkin,app) kinematic position angle against the ellipticity. In each panel the green filled circles represent the unbarred galaxies, blue diamonds correspond to weakly barred galaxies, and violet squares represent the barred galaxies. Empty circles represent the early type galaxies. Labels indicate the 3σ outlier. Dashed lines represent the projection effect of a morpho-kinematic misalignment of 60° measured in the plane of the galaxy. In each panel, the grey area represents the 2σ dispersion of the sample.

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Fig. A.4 Stellar and ionised gas difference respects the ellipticity. The green filled circles represent the unbarred galaxies, blue diamonds correspond to weakly barred galaxies, and violet squares represent the barred galaxies. Empty circles represent the early-type galaxies. Dashed lines represent the projection effect of a morpho-kinematic misalignment of 60° measured in the plane of the galaxy. In each panel, the grey area represents the 2σ dispersion of the sample.

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Appendix B: Tables

Appendix C: Stellar and Ionised velocity fields

In this appendix we present the velocity field of the 80 non-interacting galaxies. Each row present one galaxy similar to the one in Fig. 1, from left to right: SDSS r-band image of the galaxy. The white solid line represents the photometric PA measured at the same galactocentric distance as the kinematic PA (PA_morph, see Sect. 3). The dashed line represents the photometric PA measured at the outermost isophote of the image (PA, see Sect. 4.3). The next two panels show the stellar and ionised gas velocity maps, respectively. Green points highlight the locations where the maximum velocity is located at a given radius, determined from the position–velocity diagram.

Black lines for each kinematic side represent the average kinematic PA (PA_kin), while white thin lines along the zero-velocity curve show the average minor kinematic PA. The next panel shows the distance from the galactic centre versus the maximum for the stellar (blue) and ionised gas (red) components. The curve along 0 km s^-1 represents the velocities along the zero-velocity curve. Uncertainty in velocity are determined from Monte Carlo simulations. The last panel shows the dependence of the different PA with respect to the radius. PA_morph, , and are represented by open circles, filled blue diamonds, and filled red squares, respectively. For barred galaxies, we highlight the length of the bar and its orientation with dashed lines.

	Fig. C.1 Stellar and ionised gas velocity fields for the sample of galaxies used in this study.
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© ESO, 2014