We exploit the recent determination of cosmic star formation rate (SFR)
density at redshifts $z\gtrsim 4$ to derive astroparticle constraints on three
common dark matter scenarios alternative to standard cold dark matter (CDM):
warm dark matter (WDM), fuzzy dark matter ($\psi $ DM) and self-interacting dark
matter (SIDM). Our analysis relies on the UV luminosity functions measured by
the Hubble Space Telescope out to $z\lesssim 10$ and down to UV magnitudes
${M}_{\mathrm{U}\mathrm{V}}\lesssim -17$ . We extrapolate these to fainter yet unexplored
magnitude ranges, and perform abundance matching with the halo mass functions
in a given DM scenario, so obtaining a relationship between the UV magnitude
and the halo mass. We then compute the cosmic SFR density by integrating the
extrapolated UV luminosity functions down to a faint magnitude limit ${M}_{\mathrm{U}\mathrm{V}}^{\mathrm{l}\mathrm{i}\mathrm{m}}$ , which is determined via the above abundance matching
relationship by two free parameters: the minimum threshold halo mass ${M}_{\mathrm{H}}^{\mathrm{G}\mathrm{F}}$ for galaxy formation, and the astroparticle quantity $X$
characterizing each DM scenario (namely, particle mass for WDM and $\psi $ DM,
and kinetic temperature at decoupling ${T}_{X}$ for SIDM). We perform Bayesian
inference on such parameters via a MCMC technique by comparing the cosmic SFR
density from our approach to the current observational estimates at $z\gtrsim 4$ , constraining the WDM particle mass to ${m}_{X}\approx {1.2}_{-0.4{\textstyle \phantom{\rule{0.167em}{0ex}}}(-0.5)}^{+0.3{\textstyle \phantom{\rule{0.167em}{0ex}}}(11.3)}$ keV, the $\psi $ DM particle mass to
${m}_{X}\approx {3.7}_{-0.4{\textstyle \phantom{\rule{0.167em}{0ex}}}(-0.5)}^{+1.8{\textstyle \phantom{\rule{0.167em}{0ex}}}(+12.9.3)}\times {10}^{-22}$ eV, and the
SIDM temperature to ${T}_{X}\approx {0.21}_{-0.06{\textstyle \phantom{\rule{0.167em}{0ex}}}(-0.07)}^{+0.04{\textstyle \phantom{\rule{0.167em}{0ex}}}(+1.8)}$ keV at
$68\mathrm{\%}$ ($95\mathrm{\%}$ ) confidence level. We then forecast how such constraints will be
strengthened by upcoming refined estimates of the cosmic SFR density, if the
early data on the UV luminosity function at $z\gtrsim 10$ from JWST will be
confirmed down to ultra-faint magnitudes.

PREPRINT

# Astroparticle Constraints from the Cosmic Star Formation Rate Density at High Redshift: Current Status and Forecasts for JWST

Giovanni Gandolfi, Andrea Lapi, Tommaso Ronconi, Luigi Danese

Submitted on 5 November 2022

## Abstract

## Preprint

Comment: 18 pages, accepted in MDPI Universe. arXiv admin note: text overlap with arXiv:2205.09474

Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Astrophysics of Galaxies