arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2201.10169astro-ph.COastro-ph.GA
收藏

在$z=2$上使用$α$森林层析成像来约束波动Gunn-Peterson近似

Constraining the Fluctuating Gunn-Peterson Approximation Using Lyman-$α$ Forest Tomography at $z=2$

Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz

备注：
Accepted for publication by ApJ. 27 pages, 18 figures, 2 tables
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

波动Gunn-Peterson近似（FGPA）是一种常用的方法，用于从$N$ -体模拟的物质密度场生成模拟Lyman-$α$（Ly $α$）森林在宇宙正午（$z\gtrsim 2$）的吸收串，而无需运行昂贵的流体动力学模拟。受最近的发展，在三维IGM层析观测以及物质密度场重建技术应用于星系红移样品在$z\sim 2$，我们研究的可能性，直接检查之间的关系的Ly $α$传输和底层的物质密度场的观测测试FGPA。具体来说，我们分析了EAGLE，Illustris，IllustrisTNG和Nyx宇宙学流体动力学模拟，这是用不同的代码和子网格模型运行。虽然FGPA是一个很好的描述IGM在较低的密度区域，在较高的密度的透射密度分布的斜率显着影响的反馈过程，导致FGPA打破在该制度。即使没有额外的反馈，我们发现显着的偏差所产生的非线性结构增长的流体动力学效应。然后，我们继续使用现实的模拟数据进行比较，假设最近的CLAMATO调查的视线采样和光谱特性，并发现这将是具有挑战性的FGPA和流体动力学模型与当前的数据集之间的辨别。然而，未来超大型望远镜的改进视线采样或斯巴鲁PFS等多路分光调查的大量数据应该允许对FGPA进行严格的测试，并有可能检测星系反馈对IGM的影响。

英文摘要：

The fluctuating Gunn-Peterson approximation (FGPA) is a commonly-used method to generate mock Lyman-$α$ (Ly$α$) forest absorption skewers at Cosmic Noon ($z\gtrsim 2$) from the matter-density field of $N$-body simulations without running expensive hydrodynamical simulations. Motivated by recent developments in 3D IGM tomography observations as well as matter density field reconstruction techniques applied to galaxy redshift samples at $z\sim 2$, we examine the possibility of observationally testing FGPA by directly examining the relationship between the Ly$α$ transmission and the underlying matter density field. Specifically, we analyze the EAGLE, Illustris, IllustrisTNG and Nyx cosmological hydrodynamic simulations, that were run with different codes and sub-grid models. While the FGPA is an excellent description of the IGM in lower-density regions, the slope of the transmission-density distribution at higher densities is significantly affected by feedback processes causing the FGPA to break down in that regime. Even without added feedback, we find significant deviations caused by hydrodynamical effects arising from non-linear structure growth. We then proceed to make comparisons using realistic mock data assuming the sightline sampling and spectral properties of the recent CLAMATO survey, and find that it would be challenging to discern between the FGPA and hydrodynamical models with current data sets. However, the improved sightline sampling from future extremely large telescopes or large volumes from multiplexed spectroscopic surveys such as Subaru PFS should allow for stringent tests of the FGPA, and make it possible to detect the effect of galaxy feedback on the IGM.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑