论文标题
高红移时宇宙恒星形成速率密度的限制：JWST的当前状态和预测
Astroparticle Constraints from the Cosmic Star Formation Rate Density at High Redshift: Current Status and Forecasts for JWST
论文作者
论文摘要
我们在红移$ z \ gtrsim 4 $上利用了最近确定宇宙恒星形成率（SFR）密度，以在三种常见的暗物质情景下限制Astroparticle的约束，替代了标准冷暗物质（CDM）：温暖的暗物质（WDM）（WDM），模糊的暗物质（$ dm $ dm）和自我构成物质（SIDM）。我们的分析依赖于Hubble Space望远镜测量的UV光度函数，以$ Z \ Lessim 10 $和下降到UV尺寸$ M _ {\ rm UV} \ LISHSIM -17 $。我们将它们推断为淡淡但未开发的幅度范围，并在给定的DM场景中执行与光环质量函数的丰富度相匹配，从而获得紫外线幅度和光晕质量之间的关系。然后，我们通过将外推的UV光度函数集成到微弱的幅度限制$ m _ {\ rm uv}^{\ rm lim} $来计算宇宙SFR密度，这是通过上述丰度匹配的关系确定的两个免费参数：最小threshold halos $ m $ m _} $ m _} $ _}编队，以及符合每个DM场景的Astroparticle $ x $（即WDM的粒子质量和$ψ$ dm，而动力学温度在SIDM中为$ T_X $）。我们通过将宇宙SFR密度从我们的方法到当前的观察估计值进行比较，在$ z \ gtrsim 4 $中比较宇宙SFR密度，从而将WDM粒子质量限制为$ m_x \ $ m_x \ of 1.2^{+0.3 \，（11.3）_ { - 0.4 0.4 \，（ - 0.4 \ a），（ - 0.5） $ m_x \大约3.7^{+1.8 \，（+12.9.3）} _ { - 0.4 \，（ - 0.5）} \ times 10^{ - 22} $ eV，SIDM温度为$ t_x \ $ t_x \ \ 0.21^{+0.21^{+0.04 \，（+1.8）$ 0.04 \，（+1.8）$ 0.06 _ 0.06 $ 68 \％$（$ 95 \％$）置信度。然后，如果即将通过$ z \ gtrsim 10 $从JWST确认对宇宙SFR密度的精制估计，我们将如何通过对宇宙SFR密度的精制估计来增强此类约束，从而确认其限制。
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 ($ψ$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 $M_{\rm UV}\lesssim -17$. 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 $M_{\rm UV}^{\rm lim}$, which is determined via the above abundance matching relationship by two free parameters: the minimum threshold halo mass $M_{\rm H}^{\rm GF}$ for galaxy formation, and the astroparticle quantity $X$ characterizing each DM scenario (namely, particle mass for WDM and $ψ$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 $m_X\approx 1.2^{+0.3\,(11.3)}_{-0.4\,(-0.5)}$ keV, the $ψ$DM particle mass to $m_X\approx 3.7^{+1.8\,(+12.9.3)}_{-0.4\,(-0.5)}\times 10^{-22}$ eV, and the SIDM temperature to $T_X\approx 0.21^{+0.04\,(+1.8)}_{-0.06\,(-0.07)}$ 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 $z\gtrsim 10$ from JWST will be confirmed down to ultra-faint magnitudes.
