Testing Covarying Coupling Constants (CCC) against the full SPARC rotation-curve sample: a like-for-like comparison with MOND and NFW

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2026
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Abstract
Abstract The Covarying Coupling Constants (CCC) framework, developed to account for high-redshift JWST observations, contains a mechanism – a covarying-constant virtual mass field keyed to local density – that modifies galactic dynamics without particle dark matter. We test it against the full Spitzer Photometry and Accurate Rotation Curves (SPARC) sample of 175 disc galaxies, extending an earlier study of a few objects. Working in an inverse formulation, in which each model predicts the baryonic rotation curve from the observed one, we compare CCC against Modified Newtonian Dynamics (MOND) and one- and two-parameter Navarro–Frenk–White (NFW) haloes on identical footing, using the reduced $\chi ^2_\nu$. We show that the published sharp density turn-off is unphysical and replace it with a smooth transition – the density-space analogue of the MOND interpolating function, with no new parameter. One-parameter smooth-CCC then performs comparably to galaxy-by-galaxy fitted MOND (lower $\chi ^2_\nu$ in 56 per cent of galaxies, mean $\chi ^2_\nu$ of 2.58 versus 2.65; the difference is not significant), while two-parameter NFW shows a substantially broader fit-quality distribution and a larger tail of poor or boundary-limited fits (mean $\chi ^2_\nu \approx 7$). The CCC turn-off density is not universal (scatter 0.82 dex) and correlates with galaxy size, as expected for a spherical reconstruction of flattened discs. Recast as an acceleration, however, $a_t = V_{\mathrm{flat}}^2/R_t$ has scatter 0.33 dex (91-galaxy resolved subset), matching the MOND scale a0 (0.34 dex), of comparable magnitude (∼2 × 10−10 m s−2), with its size correlation removed. Though not designed for galactic dynamics, CCC describes rotation curves as well as galaxy-by-galaxy fitted MOND.
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Authors Rajendra P. Gupta, Nikolaos Samaras
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Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1777
URL
https://doi.org/10.1093/mnras/stag1777
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