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In recent work, Lelli et al. (2016) argue that the tightness of the baryonicTully-Fisher relation (BTFR) of the SPARC galaxy sample, and the weakness ofthe correlation of its residuals with effective radius, pose challenges to LCDMcosmology. In this Letter we calculate the statistical significance of theseresults in the framework of halo abundance matching, which imposes a canonicalgalaxy-halo connection. Taking full account of sample variance among SPARC-likerealisations of the parent halo population, we find the scatter in thepredicted BTFR to be 3.6 sigma too high, but the correlation of its residualswith galaxy size to be naturally weak. Further, we find abundance matching togenerate BTFR curvature in 3.0 sigma disagreement with the data, and a fractionof galaxies with non-flat rotation curves somewhat larger than observed.

The scatter, residual correlations and curvature of the SPARC baryonic Tully-Fisher relation