We exploit the recent determination of the cosmic star formation rate (SFR) density at high redshifts z greater than or similar to 4 to derive astroparticle constraints on three common dark matter (DM) 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 ultraviolet (UV) luminosity functions measured from blank field surveys by the Hubble Space Telescope out to z less than or similar to 10 and down to UV magnitudes M-UV less than or similar to -17. We extrapolate these to fainter yet unexplored magnitude ranges and perform abundance matching with the halo mass functions in a given DM scenario, thus, obtaining a redshift-dependent relationship between the UV magnitude and the halo mass. We then computed the cosmic SFR density by integrating the extrapolated UV luminosity functions down to a faint magnitude limit M-UV(lim), which is determined via the above abundance matching relationship by two free parameters: the minimum threshold halo mass M-H(GF) 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 using a Monte Carlo Markov Chain (MCMC) technique by comparing the cosmic SFR density from our approach to the current observational estimates at z greater than or similar to 4, constraining the WDM particle mass to mX approximate to 1.2(-0.4)(+0.3) ((11.3))((-0.5)) keV, the psi DM particle mass to m(X) approximate to 3.7(-0.4)(+1.8) ((+)(12)(.9.3))((-0.5)) x 10(-22) eV, and the SIDM temperature to T-X approximate to 0.21(-0.06)(+0.)(04) ((+1.8))((-0.07)) keV at 68% (95%) confidence level. Finally, we 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 greater than or similar to 10 from the James Webb Space Telescope (JWST) will be confirmed down to ultra-faint magnitudes.

Astroparticle Constraints from the Cosmic Star Formation Rate Density at High Redshift: Current Status and Forecasts for JWST / Gandolfi, Giovanni; Lapi, Andrea; Ronconi, Tommaso; Danese, Luigi. - In: UNIVERSE. - ISSN 2218-1997. - 8:11(2022), pp. 1-17. [10.3390/universe8110589]

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

Gandolfi, Giovanni;Lapi, Andrea;Ronconi, Tommaso;Danese, Luigi
2022-01-01

Abstract

We exploit the recent determination of the cosmic star formation rate (SFR) density at high redshifts z greater than or similar to 4 to derive astroparticle constraints on three common dark matter (DM) 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 ultraviolet (UV) luminosity functions measured from blank field surveys by the Hubble Space Telescope out to z less than or similar to 10 and down to UV magnitudes M-UV less than or similar to -17. We extrapolate these to fainter yet unexplored magnitude ranges and perform abundance matching with the halo mass functions in a given DM scenario, thus, obtaining a redshift-dependent relationship between the UV magnitude and the halo mass. We then computed the cosmic SFR density by integrating the extrapolated UV luminosity functions down to a faint magnitude limit M-UV(lim), which is determined via the above abundance matching relationship by two free parameters: the minimum threshold halo mass M-H(GF) 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 using a Monte Carlo Markov Chain (MCMC) technique by comparing the cosmic SFR density from our approach to the current observational estimates at z greater than or similar to 4, constraining the WDM particle mass to mX approximate to 1.2(-0.4)(+0.3) ((11.3))((-0.5)) keV, the psi DM particle mass to m(X) approximate to 3.7(-0.4)(+1.8) ((+)(12)(.9.3))((-0.5)) x 10(-22) eV, and the SIDM temperature to T-X approximate to 0.21(-0.06)(+0.)(04) ((+1.8))((-0.07)) keV at 68% (95%) confidence level. Finally, we 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 greater than or similar to 10 from the James Webb Space Telescope (JWST) will be confirmed down to ultra-faint magnitudes.
2022
8
11
1
17
589
10.3390/universe8110589
https://arxiv.org/abs/2211.02840
Gandolfi, Giovanni; Lapi, Andrea; Ronconi, Tommaso; Danese, Luigi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/139872
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