We derived astroparticle constraints in different dark matter scenarios that are alternatives to cold dark matter (CDM): thermal relic warm dark matter, WDM; fuzzy dark matter, $\psi$DM; self-interacting dark matter, SIDM; sterile neutrino dark matter, $\nu$DM. Our framework is based on updated determinations of the high-redshift UV luminosity functions for primordial galaxies to redshift $z\sim 10$, on redshift-dependent halo mass functions in the above DM scenarios from numerical simulations, and on robust constraints on the reionization history of the Universe from recent astrophysical and cosmological datasets. First, we built an empirical model of cosmic reionization characterized by two parameters, namely the escape fraction $f_{\mathrm{esc}}$ of ionizing photons from primordial galaxies, and the limiting UV magnitude $M_{\mathrm{UV}}^{\lim }$ down to which the extrapolated UV luminosity functions steeply increased. Second, we performed standard abundance matching of the UV luminosity function and the halo mass function, obtaining a relationship between UV luminosity and the halo mass, whose shape depends on an astroparticle quantity X specific to each DM scenario (e.g., WDM particle mass); we exploited such a relationship to introduce (in the analysis) a constraint from primordial galaxy formation, in terms of the threshold halo mass above which primordial galaxies can efficiently form stars. Third, we performed Bayesian inference on the three parameters $f_{\mathrm{esc}}$, $M_{\mathrm{UV}}^{\lim }$, and X via a standard MCMC technique, and compared the outcomes of different DM scenarios on the reionization history. We also investigated the robustness of our findings against educated variations of still uncertain astrophysical quantities. Finally, we highlight the relevance of our astroparticle estimates in predicting the behavior of the high-redshift UV luminosity function at faint, yet unexplored magnitudes, which may be tested with the advent of the James Webb Space Telescope.

中文翻译：

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来自宇宙再电离和原始星系形成的天体粒子约束

我们推导出了不同暗物质场景中的天体粒子约束，这些场景可以替代冷暗物质（CDM）：热遗迹暖暗物质，WDM；模糊的暗物质，$\psi$DM; 自相互作用暗物质，SIDM；无菌中微子暗物质，$\nu$DM。我们的框架基于对原始星系红移的高红移紫外光度函数的更新确定$z～10$，来自数值模拟的上述 DM 场景中与红移相关的晕质量函数，以及来自近期天体物理学和宇宙学数据集的对宇宙再电离历史的稳健约束。首先，我们建立了一个以两个参数为特征的宇宙再电离经验模型，即逃逸分数$F_{\mathrm{Esc键}}$来自原始星系的电离光子，以及极限紫外线强度${米}_{\mathrm{紫外线}}^{林}$外推的紫外光度函数急剧增加。其次，我们对紫外光度函数和光晕质量函数进行了标准丰度匹配，得到了紫外光度和光晕质量之间的关系，其形状取决于每个 DM 场景特定的天体粒子数量X（例如，WDM 粒子质量）；我们利用这种关系引入（在分析中）原始星系形成的约束，根据阈值晕质量，原始星系可以有效地形成恒星。第三，我们对三个参数进行了贝叶斯推理$F_{\mathrm{Esc键}}$,${米}_{\mathrm{紫外线}}^{林}$, 和X通过标准 MCMC 技术, 并比较了不同 DM 场景对再电离历史的结果。我们还调查了我们的研究结果对仍然不确定的天体物理量的有根据的变化的稳健性。最后，我们强调了我们的天体粒子估计与预测高红移紫外光度函数在微弱但尚未探索的幅度下的行为的相关性，这可能会随着詹姆斯韦伯太空望远镜的出现而得到检验。