论文标题
Uchuu- $ν^2 $ GC星系和AGN：JWST，Euclid和LSST的高红移AGN的宇宙差异预测
Uchuu-$ν^2$GC galaxies and AGN: Cosmic variance forecasts of high-redshift AGN for JWST, Euclid, and LSST
论文作者
论文摘要
高红移（$ z \ gtrsim 6 $）在高红移（$ z \ gtrsim 6 $）上的光度函数的测量值有望遭受现场到场方差的影响，包括宇宙和泊松方差。未来的调查，例如欧几里得望远镜和詹姆斯·韦伯太空望远镜（JWST）的调查，也将受到现场差异的影响。 We use the Uchuu simulation, a state-of-the-art cosmological $N$-body simulation with 2.1 trillion particles in a volume of $25.7~\mathrm{Gpc}^3$, combined with a semi-analytic galaxy and AGN formation model, to generate the Uchuu-$ν^2$GC catalog, publicly available, that allows us to investigate the field-to-field variance of the AGN的光度函数。使用此Uchuu- $ν^2 $ GC模型，我们将宇宙方差量化为调查区域，AGN光度和红移的函数。通常，宇宙方差随着调查区域的增加和降低红移而降低。我们发现，在$ z \ sim6-7 $时，宇宙差异取决于AGN的光度。这是因为AGN居住的典型的暗物质光环质量并不显着取决于光度。由于AGN的稀有性，泊松方差主要是总场到场方差，尤其是对于明亮的AGN。我们还研究了与星系形成物理学相关的参数对场方差的影响。我们讨论了来自最近观察结果对AGN光度函数的微弱末端的估计中存在的不确定性，并扩展了这一点，以预测预期的AGN数量及其对即将进行的Euclid，JWST和空间和时间的遗产调查（LSST）的差异。
Measurements of the luminosity function of active galactic nuclei (AGN) at high redshift ($z\gtrsim 6$) are expected to suffer from field-to-field variance, including cosmic and Poisson variances. Future surveys, such as those from the Euclid telescope and James Webb Space Telescope (JWST), will also be affected by field variance. We use the Uchuu simulation, a state-of-the-art cosmological $N$-body simulation with 2.1 trillion particles in a volume of $25.7~\mathrm{Gpc}^3$, combined with a semi-analytic galaxy and AGN formation model, to generate the Uchuu-$ν^2$GC catalog, publicly available, that allows us to investigate the field-to-field variance of the luminosity function of AGN. With this Uchuu-$ν^2$GC model, we quantify the cosmic variance as a function of survey area, AGN luminosity, and redshift. In general, cosmic variance decreases with increasing survey area and decreasing redshift. We find that at $z\sim6-7$, the cosmic variance depends weakly on AGN luminosity. This is because the typical mass of dark matter haloes in which AGN reside does not significantly depend on luminosity. Due to the rarity of AGN, Poisson variance dominates the total field-to-field variance, especially for bright AGN. We also examine the effect of parameters related to galaxy formation physics on the field variance. We discuss uncertainties present in the estimation of the faint-end of the AGN luminosity function from recent observations, and extend this to make predictions for the expected number of AGN and their variance for upcoming observations with Euclid, JWST, and the Legacy Survey of Space and Time (LSST).
