The thesan project: predictions for multitracer line intensity mapping in the epoch of reionization
The thesan project: predictions for multitracer line intensity mapping in the epoch of reionization
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Thesan 项目：再电离时代多示踪剂谱线强度图的预测
DOI：
10.1093/mnras/stac1557
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发表时间：
2022
影响因子：
4.8
通讯作者：
Hernquist, Lars
中科院分区：
文献类型：
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作者：
Kannan, Rahul;Smith, Aaron;Garaldi, Enrico;Shen, Xuejian;Vogelsberger, Mark;Pakmor, Rüdiger;Springel, Volker;Hernquist, Lars
线强度映射（LIM）作为研究高红移宇宙中星系形成和宇宙学的一种强有力的技术正在迅速崛起。我们使用大体积、高分辨率的反电离模拟，给出了来自星系星际介质（ISM）和宇宙中中性氢气21厘米发射的选择谱线的LIM估计。结合Hiiregions的亚分辨率光电离模型和Monte Carlo辐射传输计算，估计了高红移星系（z > 5.5）的尘埃衰减光谱能量分布（SEDs）。我们表明，衍生的光度特性，如紫外线（UV）光度函数和紫外线连续斜率与观测推断值相匹配，证明了SED模型的准确性。我们对最亮发射线的光度-恒星形成率关系（L-SFR）进行了拟合，发现推导出的标度关系与广泛使用的低区之间存在重要差异，因为再电离时代星系的ISM通常比低红移星系的ISM富含较少的金属。我们利用这些关系构建了星云发射线的线强度图，并与21厘米发射线交叉相关。有趣的是，相关转换符号（k跃迁）的波数在很大程度上取决于再电离模型，在较小程度上取决于目标发射线，这与跃迁探测电离区域典型尺寸的图像一致。导出的尺度关系和强度图代表了预测和解释当前和即将进行的LIM实验结果的及时的最先进的框架。
Line intensity mapping (LIM) is rapidly emerging as a powerful technique to study galaxy formation and cosmology in the high-redshift Universe. We present LIM estimates of select spectral lines originating from the interstellar medium (ISM) of galaxies and 21 cm emission from neutral hydrogen gas in the Universe using the large volume, high resolutionthesanreionization simulations. A combination of subresolution photoionization modelling for Hiiregions and Monte Carlo radiative transfer calculations is employed to estimate the dust-attenuated spectral energy distributions (SEDs) of high-redshift galaxies (z≳ 5.5). We show that the derived photometric properties such as the ultraviolet (UV) luminosity function and the UV continuum slopes match observationally inferred values, demonstrating the accuracy of the SED modelling. We provide fits to the luminosity–star formation rate relation (L–SFR) for the brightest emission lines and find that important differences exist between the derived scaling relations and the widely used low-zones because the ISM of reionization era galaxies is generally less metal enriched than in their low-redshift counterparts. We use these relations to construct line intensity maps of nebular emission lines and cross-correlate with the 21 cm emission. Interestingly, the wavenumber at which the correlation switches sign (ktransition) depends heavily on the reionization model and to a lesser extent on the targeted emission line, which is consistent with the picture thatktransitionprobes the typical sizes of ionized regions. The derived scaling relations and intensity maps represent a timely state-of-the-art framework for forecasting and interpreting results from current and upcoming LIM experiments.