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# 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

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 ${m}_{X}\approx {1.2}_{-0.4\phantom{\rule{0.167em}{0ex}}\left(-0.5\right)}^{+0.3\phantom{\rule{0.167em}{0ex}}\left(11.3\right)}$ keV, the $\psi$DM particle mass to ${m}_{X}\approx {3.7}_{-0.4\phantom{\rule{0.167em}{0ex}}\left(-0.5\right)}^{+1.8\phantom{\rule{0.167em}{0ex}}\left(+12.9.3\right)}×{10}^{-22}$ eV, and the SIDM temperature to ${T}_{X}\approx {0.21}_{-0.06\phantom{\rule{0.167em}{0ex}}\left(-0.07\right)}^{+0.04\phantom{\rule{0.167em}{0ex}}\left(+1.8\right)}$ 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

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