We compared the star formation rate in different dark matter (DM) models with UV luminosity data from JWST up to z≃25 and legacy data from HST. We find that a transition from a Salpeter population to top-heavy Pop III stars is likely at z≃10, and that beyond z=10-15 the feedback from supernovae and active galactic nuclei is progressively reduced, so that at z≃25 the production of stars is almost free from any feedback. We compared fuzzy and warm DM models that suppress small-scale structures with the CDM paradigm, and find that the fuzzy DM mass > 5. 6 ̊m eV and the warm DM mass > 1. 5 ̊m keV at a 95% CL. The fits of the star formation rate parametrisation do not depend strongly on the DM properties within the allowed range. We find no preference over CDM for enhanced matter perturbations associated with axion mini-clusters or primordial black holes. The scale of the enhancement of the power spectrum should be > 25 ̊m Mpc at the 95% CL, excluding axion mini-clusters produced for mₐ < 6. 6 ̊m eV or heavy primordial black holes that constitute a fraction f_ ̊m PBH ̊m PBH (m_ ̊m PBH of DM. KCL-PH-TH/2025-12, CERN-TH-2025-085, AION-REPORT/2025-03
Urrutia et al. (2025) studied this question.