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tokens: g ′) and Δμ( r ′ − i ′), with the maximum at only ρ = 0.30 and p = 0.08. The only exception is for the PAS profiles from the r ′ − i ′ breaks sub-sample, where there is a correlation of ρ = 0.49 and p = 0.02. This correlation is due to the same points as the correlation of h 0 with Δ h 0 ( r ′ − i ′0) in the PAS. 4.4.4 Correlations with absolute magnitude, maximum rotation and specific angular momentum Martín-Navarro et al. ( 2012 ) found that the truncation radius of a galaxy is strongly correlated with the maximum rotational velocity v rot of a galaxy, having a correlation of ρ truncation = 0.81. The breaks in their sample were correlated at only ρ break = 0.50. In contrast, Pohlen Trujillo ( 2006 ) report no correlation with rotation. They do report a weak correlation of the brightness at the feature with the absolute magnitude M B,abs . We explore possible correlations of the feature radii R f , surface brightness at the feature μ and differences in brightness between bands at the feature μΔ with absolute magnitude M abs and maximum rotation v rot in Table 7 . We find only one weak correlation in the difference between the g ′ and r ′ surface brightness at the feature radius, as measured with the EP method, with the rotation velocity v rot . The correlation strength is ρ = 0.36 and p = 0.03. Martín-Navarro et al. ( 2012 ) also perform a correlation test of the break and truncation radii with the specific angular momentum j , calculated using the empirical expression by Navarro Steinmetz ( 2000 ), 4 As this is a rescaling of v rot , the correlation remains the same. They find that the feature radius only correlates well beyond r b = 8 kpc. For a smaller disc with v rot 100 kms −1 , r break and v rot are essentially unlinked. When examining the full radii range, we also do not find a statistically significant correlation. The same holds when limiting ourselves to all features beyond r > 8. 4.4.5 Effect of inclination In Section 4.4.2 , we found that the PAS profiles typically tend to have sharper breaks than the ellipse-fit profiles and EP. As the PAS projects data as if it was edge-on, it is also interesting to compare the effect of inclinations in this. To this end, we have tested the correlation of a / b (major axis over minor axis) with scalelengths h 0 and h f , h 0 / h f and R f / h f , in Table 7 . The results are also visualized in Fig. 12 . Figure 12. Correlation of various parameters with inclination (expressed as a / b ). Top row shows with scalelength h 0 (left) and h f (right). Bottom row has the h 0 / h f (right) and R f / h f (left) correlations. The statistical correlation tests are plotted in each panel. Boxes represent the PAS points, while circles represent the EP points. Open markers represent truncations, while filled markers represent boxes. We find no significant correlation between a / b and inner scalelength h 0 . There may be a negative trend visible in the truncation-only sample, as both the EP and PAS profiles