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


We exploit the recent determination of cosmic star formation rate (SFR) density at redshifts z4 to derive astroparticle constraints on three common dark matter scenarios alternative to standard cold dark matter (CDM): warm dark matter (WDM), fuzzy dark matter (ψDM) and self-interacting dark matter (SIDM). Our analysis relies on the UV luminosity functions measured by the Hubble Space Telescope out to z10 and down to UV magnitudes MUV17. 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 MUVlim, which is determined via the above abundance matching relationship by two free parameters: the minimum threshold halo mass MHGF for galaxy formation, and the astroparticle quantity X characterizing each DM scenario (namely, particle mass for WDM and ψDM, and kinetic temperature at decoupling TX 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 z4, constraining the WDM particle mass to mX1.20.4(0.5)+0.3(11.3) keV, the ψDM particle mass to mX3.70.4(0.5)+1.8(+12.9.3)×1022 eV, and the SIDM temperature to TX0.210.06(0.07)+0.04(+1.8) keV at 68% (95%) 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 z10 from JWST will be confirmed down to ultra-faint magnitudes.


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


The UV luminosity functions at redshifts $z\sim 6$ (red), $7$ (orange), $8$ (green), $9$ (blue), $10$ (magenta), $12$ (cyan) and $17$ (pink). Data points are from \cite{Bouwens21,Oesch18} (filled circles), \cite{Bouwens22} (empty circles), and \cite{Harikane22} (squares). Colored lines illustrate Schechter fits to the blank-field measurements from \cite{Bouwens21}: solid lines refer to the observed luminosity functions, while dotted lines to the intrinsic ones, after correction for dust extinction via the UV continuum slope according to the procedure by \cite{Bouwens14}.