探测宇宙正午时期的多相际大尺度结构和多相IGM——来自欧几里得、CSST、JPCam和JUST联合调查的见解
Probing Large-scale Structure and the Multi-Phase IGM at the Cosmic Noon -- Insights from a Joint Survey with Euclid, CSST, JPCam, and JUST
AI总结：
通过联合调查，利用多波段观测技术探测宇宙正午时期的多相际大尺度结构和IGM，提高photo-z准确性并研究星系际环境。
摘要：
我们提出了一个潜在的欧几里得/CSST/JPCam/JUST联合调查的科学和技术依据，旨在探测欧几里得北深场（EDF-N）约20平方度范围内宇宙正午时期的多相际大尺度结构和多相IGM。该调查围绕三个相连的目标展开：（1）通过广波段和窄波段光度学的结合提高光度学红移（photo-z）的准确性，从而能够可靠地识别大尺度结构；（2）利用专门的窄波段成像探测扩展的CGM发射；（3）通过背景星系的吸收线光谱学测绘前景IGM。这些组成部分建立了一个综合的观测框架，以研究银河生态系统——在宇宙正午时期将星系与其际环境联系起来。我们显示，J-PAS-like窄波段系统在JPCam中使用显著提高了仅通过欧几里得/CSST广波段数据获得的photo-z准确性，尤其是对于z~1.0-1.4的恒星形成星系。这使能够直接通过photo-z测量识别星系团和（原型）星团。堆叠的JPCam窄波段成像也应该能够探测到扩展的[O II]发射CGM晕。我们然后构建了模拟的3D气体分布模型和现实的星系目录，并进一步构建了模拟的CSST和JUST背景星系光谱，添加了Lyalpha和Mg II吸收。从CSSTLyalpha森林重建的3DH I场可靠地恢复了大尺度结构；然而，我们的模拟表明，通过光谱堆叠或通过两点相关函数方法检测扩散IGM的Mg II吸收是不可能的。我们得出结论，限制扩散IGM的金属度将需要未来设施如39米E-ELT的更深入和更高分辨率的光谱学。
英文摘要：
We present scientific and technical justifications of a potential coordinated Euclid/CSST/JPCam/JUST survey of the Euclid Deep Field North (EDF-N), aimed at probing the multi-phase circumgalactic and intergalactic medium (CGM/IGM) at the cosmic noon over ~20 deg$^2$. The survey is structured around three connected goals: (1) improving photometric redshift (photo-z) accuracy through the combination of broad- and narrow-band photometry, enabling reliable identification of large-scale structures; (2) probing extended CGM emission with dedicated narrow-band imaging; and (3) mapping foreground IGM via absorption-line spectroscopy of background galaxies. Together, these components establish an integrated observational framework to investigate galactic ecosystems -- linking galaxies to their circumgalactic and intergalactic environments -- at cosmic noon. We show that the J-PAS-like narrow-band system used in JPCam substantially improves photo-z accuracies from only the Euclid/CSST broad-band data, especially for star-forming galaxies at z~1.0-1.4. This enables the identification of galaxy groups and (proto-)clusters directly from photo-z measurements. Stacked JPCam narrow-band imaging should also detect extended [O II]-emitting CGM halos. We then construct mock 3D gas distribution model and realistic galaxy catalog, and further construct mock CSST and JUST background galaxy spectra adding Lyalpha and Mg II absorptions. The reconstructed 3D H I field from CSST Lyalpha forest reliably recovers large-scale structures; however, our simulations indicate that detecting diffuse IGM Mg II absorption with JUST is infeasible, either through spectral stacking or via the two-point correlation function method. We conclude that constraining the metallicity of the diffuse IGM will require significantly deeper and higher-resolution spectroscopy expected from future facilities such as the 39 m E-ELT.
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