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We derive astroparticle constraints in different dark matter scenariosalternative to cold dark matter (CDM): thermal relic warm dark matter, WDM;fuzzy dark matter, $\psi$DM; self-interacting dark matter, SIDM; sterileneutrino dark matter, $\nu$DM. Our framework is based on updated determinationsof the high-redshift UV luminosity functions for primordial galaxies out toredshift $z\sim 10$, on redshift-dependent halo mass functions in the above DMscenarios from numerical simulations, and on robust constraints on thereionization history of the Universe from recent astrophysical and cosmologicaldatasets. First, we build up an empirical model of cosmic reionizationcharacterized by two parameters, namely the escape fraction $f_{\rm esc}$ ofionizing photons from primordial galaxies, and the limiting UV magnitude$M_{\rm UV}^{\rm lim}$ down to which the extrapolated UV luminosity functionsare steeply increasing. Second, we perform standard abundance matching of theUV luminosity function and the halo mass function, obtaining a relationshipbetween UV luminosity and halo mass whose shape depends on an astroparticlequantity $X$ specific of each DM scenario (e.g., WDM particle mass); we exploitsuch a relation to introduce in the analysis a constraint from primordialgalaxy formation, in terms of the threshold halo mass above which primordialgalaxies can efficiently form stars. Third, we implement a sequential updatingBayesian MCMC technique to perform joint inference on the three parameters$f_{\rm esc}$, $M_{\rm UV}^{\rm lim}$, $X$, and to compare the outcomes ofdifferent DM scenarios on the reionization history. Finally, we highlight therelevance of our astroparticle estimates in predicting the behavior of thehigh-redshift UV luminosity function at faint, yet unexplored magnitudes, thatmay be tested with the advent of the James Webb Space Telescope.

Astroparticle Constraints from Cosmic Reionization and Primordial Galaxy Formation