利用低温大孔径强度映射实验进行河外星系科学
Extragalactic Science with the Experiment for Cryogenic Large-aperture Intensity Mapping
AI总结：
本文预测了球载低温望远镜EXCLAIM对河外星系[CII]和CO谱线发射的交叉相关探测灵敏度，表明其能有效区分文献中的多种强度模型，并将联合约束转化为对星系晕光度-质量关系及恒星形成率密度的限制。
摘要：
低温大孔径强度映射实验（EXCLAIM）是一个球载低温望远镜，它将对银河系和宇宙网发出的弥漫辐射光谱进行巡天观测，以探究整个宇宙时间尺度上的恒星形成、星际介质和星系演化。EXCLAIM的主要河外星系科学巡天在频率范围ν=420-540 GHz内，使用R=512光谱仪沿天赤道测绘了305平方度的区域，目标是观测红移2.5<z<3.5范围内的[CII]谱线发射以及z<1范围内的几条CO谱线。与星系红移星表的交叉相关可以将目标红移处大尺度结构的谱线发射分离出来。在本文中，我们预测了两点和条件一点交叉相关的灵敏度。我们预测，在广泛的[CII]强度模型范围内，EXCLAIM将能够在不同红移处探测到[CII]-类星体（QSO）交叉功率谱和条件体素强度分布（CVID），从而能够区分文献中的这些模型。这些功率谱预测包含了谱线互混和连续谱前景污染的影响。然后，我们将来自交叉功率谱和CVID的[CII]联合约束转化为对[CII]晕光度-质量关系L_[CII](M)模型参数以及来自[CII]发射的恒星形成率密度（SFRD）的约束。我们还开发了CO的灵敏度估计，展示了区分不同模型的能力。
英文摘要：
The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a balloon-borne cryogenic telescope that will survey the spectrum of diffuse emission from both the Milky Way and the cosmic web to probe star formation, the interstellar medium, and galaxy evolution across cosmic time. EXCLAIM's primary extragalactic science survey maps 305 deg$^2$ along the celestial equator with an R=512 spectrometer over the frequency range ν=420-540 GHz, targeting emission of the [CII] line over redshifts 2.5<z<3.5 and several CO lines for z<1. Cross-correlation with galaxy redshift catalogs isolates line emission from the large-scale structure at target redshifts. In this paper, we forecast the sensitivity for both the two-point and conditional one-point cross-correlation. We predict that EXCLAIM will detect both the [CII]-QSO cross-power spectrum and the conditional voxel intensity distribution (CVID) at various redshifts under a broad range of [CII] intensity models, allowing it to differentiate among these models in the literature. These forecasts for the power spectra include the effects of line interlopers and continuum foreground contamination. We then convert the joint [CII] constraints from both the cross-power spectrum and the CVID into constraints on the [CII] halo luminosity-mass relation $L_\mathrm{[CII]}(M)$ model parameters and the star formation rate density (SFRD) from [CII] emission. We also develop sensitivity estimates for CO, showing the ability to differentiate between models.
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