tokens: in Section 5 . To facilitate discussion, we define as a reference value. In order for MI to be disfavoured by less than 3σ, must be lowered by with fixed degrees of freedom. Hence, it would likely require a combination of (1) a different definition of r bar , (2) different values for the mass-to-light ratios, possibly including radial dependence, (3) removal of statistical outliers, and (4) other effects. Regarding point (1): There is an unaccounted bias in that the bins are defined by r bar , a point that is affected by uncertainty. The impact of this bias can be roughly estimated by moving r bar one point towards smaller (larger) radii. Doing so yields a reduction in χ 2 relative to , however with the accompanying degrees of freedom . The reduction in degrees of freedom (galaxies) are due to the criterion of at least two points at small radii. Considering the reduced chi square changes from to after the shift to smaller radii, it can be concluded that although the shift in r bar greatly affects the χ 2 it only slightly reduces the statistical disfavouring of MI. Regarding point (2): The dependence on the mass-to-light ratios may significantly affect g bar and consequently both the expected value of MI and the specification of r bar . The fixed mass-to-light ratios used here ( and ) are not optimal for all galaxies. This is clear from the rotation curve plots in Appendix C , where for some galaxies v bar > v obs for limited radial range (e.g. as is the case for CAMB and NGC 4217). To roughly gauge the effect of radically different mass-to-light ratios, we take (corresponding to galaxies dominated by DM at all radii, Lelli et al. 2017 ), yielding an increase in the χ 2 relative to (the result become slightly more significant). This is, however, just an example and one can imagine changing individual mass-to-light ratios and uncertainties potentially having a great impact on the result. Regarding point (3): Fig. 5 shows the distribution of residuals. Of the galaxies with | R i | > 4 UGC11455, NGC 4217, NGC 3109, ESO563-G021, and D631-7 have quality flag 1 whereas CAMB have quality flag 2 (listed in the SPARC data base). This indicates that the disfavouring of MI is not rooted in bad data (Fig. B1 in Appendix B shows residuals after discarding all galaxies with quality flag larger than 1). That being said, as mentioned in point (2), the fixed mass-to-light ratios used are too large in case of NGC 4217 and CAMB and possibly also affect the innermost radii of UGC11455 and ESO563-G021. It can also be argued that the high residual value in case of ESO563-G021 is at least partially rooted in a peculiar selection of points (e.g. see Fig. C1 in Appendix C ). Hence, although data are of good quality, for several of the significant outliers, there are valid arguments that could at least partially explain the high residuals. To be conservative and test the dependence on the outliers, we proceed to discard all galaxies with | R i | > 4. Doing so yield a
ner_tags: O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O B-CelestialObject O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula B-CelestialObject B-CelestialObject I-CelestialObject B-CelestialObject I-CelestialObject B-CelestialObject O B-CelestialObject O O O O O B-CelestialObject O O O O O O O B-Database I-Database I-Database O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O B-CelestialObject O O O O O O O O B-CelestialObject O B-CelestialObject O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O