tokens: to be aligned with its projected morphological major axis. The coincidence in PAs from the kinematics and morphology is thus generally a criterion in determining the nature of a galaxy. In practice, complications arise for a variety of physical reasons (e.g., presence of nonaxisymmetric structures, nearby companions with overlapping outer isophotes, spatially nonuniform extinction), compounded by surface brightness sensitivity and spatial resolution limitations for high-redshift galaxies. We examined the agreement between the derived kinematic position angle PA kin (Section 4.3 ) and the morphological position angle PA morph , quantified via the “kinematic misalignment” . We exclude GMASS-2540 here because it is not fully covered by the SINFONI AO data and because of its low H α surface brightness emission hampering a reliable PA kin determination. Following the same motivation as in Section 6.1 , we adopted as PA morph the PA from the H -band morphologies, when available, and from the H α maps otherwise. As noted in Section 5.4 , the PA H α and PA H are similar within 1.5 σ , and we verified that our conclusions would not be affected by instead adopting PA H α for all objects. For our sample, the mean and median ΔPA are 23 and 13 , respectively. For 73% of the galaxies, the alignment is better than 30 . Figure 8 shows the PA offsets as a function of the adopted axis ratio q and effective radius R e . Not unexpectedly, and as seen in other high-redshift samples (e.g., Wisnioski et al. 2015 ; Harrison et al. 2017 ), our galaxies broadly follow a trend of increasing ΔPA for more face-on and smaller sources. Of the 10 objects with ΔPA > 30°, eight are compact sources with distortions/extensions in their outer isophotes, asymmetric light distributions in their inner brighter regions, or little or irregular velocity structure (Q1623-BX502, Q1623-BX513, GMASS-2303, SA12-6339, ZC400528, ZC401925, ZC404221, and ZC411737). The other two sources are large, massive, and fairly face-on disks for which the misalignment can be attributed to morphological features (a noncircular ring with a clump on one side for Deep3a-6004 and clumps in a tail-like structure for ZC400569N; see Section 7.2 for more details). Figure 8. Kinematic misalignment ΔPA as a function of morphological axis ratio q for the SINS/zC-SINF AO sample. The symbols are color-coded and sized according to the effective radius R e of the galaxies. The five compact objects with ill-defined axis ratios and to which we assigned q = 0.64, corresponding to the for randomly oriented disks (Section 6.1 ), are plotted as squares connected with red dotted lines to their nominal best-fit q , shown as circles with a red arrow pointing toward the adopted value. Most of the well-resolved objects show very good agreement between their kinematic and morphological PAs, especially for the more edge-on systems. A larger proportion of the compact sources have ΔPA > 30°, reflecting ill-defined PAs due to
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