论文标题
部分可观测时空混沌系统的无模型预测
Phenomenological power spectrum models for H$α$ emission line galaxies from the Nancy Grace Roman Space Telescope
论文作者
论文摘要
高纬度光谱调查（HLSS）是NASA的Nancy Grace Roman Space望远镜的参考基线光谱调查，在$ 2000 $^2 $ footprint上，$^$^2 $ footprint在$ z = 1-2 $ = 1-2 $上，$ \ sim 10 $ \ sim 10 $ \ sim 10 $ \ sim 10 $ \ sim 10 $ \ sim。在这项工作中，我们使用现实的罗马星系模拟目录来探索测得的功率谱的最佳现象学建模。我们考虑两种用于建模红移空间扭曲的方法（kaiser挤压，另一种在$β$上的窗口函数，这些方法选择了$β$，选择了相干的径向辐射式成对速度，$ $ m_a $和$ m_b $），两种模型的bary骨和固定级别（smears smears of smears smeartios of Baryons of smeartios）的模型（ where these smearing scales are kept as a free parameters, P$_{dw}(k|k_*)$ and P$_{dw}(k|Σ_\perp,Σ_\parallel)$, respectively), and two analytical emulations of nonlinear growth (one employing the halo model and another formulated from simulated galaxy clustering of a semi-analytical model, $ f_ {hm} $和$ f_ {sam} $）。 We find that the best model combination employing $F_{HM}$ is $P_{dw}(k|k_*)*F_{HM}*M_B$, while the best combination employing $F_{SAM}$ is $P_{dw}(k|k_*)*F_{SAM}*M_B$, which leads to unbiased measurements of cosmological 参数。我们将它们与大规模结构扰动理论模型$ p_ {eft}（k |θ）$的有效领域理论进行了比较，并发现我们的简单现象学模型在整个RedShift范围内与$ k_ {max} = 0.25 $和$ 0.3 $ $ h $/mpc相当。我们期望我们开发的工具可用于探测黑暗能量和使用罗马人以准确而健壮的方式测试重力。
The High Latitude Spectroscopic Survey (HLSS) is the reference baseline spectroscopic survey for NASA's Nancy Grace Roman space telescope, measuring redshifts of $\sim 10$M H$α$ emission line galaxies over a $2000$ deg$^2$ footprint at $z=1-2$. In this work, we use a realistic Roman galaxy mock catalogue to explore optimal phenomenological modeling of the measured power spectrum. We consider two methods for modeling the redshift-space distortions (Kaiser squashing and another with a window function on $β$ that selects out the coherent radial infall pairwise velocities, $M_A$ and $M_B$, respectively), two models for the nonlinear impact of baryons that smears the BAO signal (a fixed ratio between the smearing scales in the perpendicular and parallel dimensions and another where these smearing scales are kept as a free parameters, P$_{dw}(k|k_*)$ and P$_{dw}(k|Σ_\perp,Σ_\parallel)$, respectively), and two analytical emulations of nonlinear growth (one employing the halo model and another formulated from simulated galaxy clustering of a semi-analytical model, $F_{HM}$ and $F_{SAM}$, respectively). We find that the best model combination employing $F_{HM}$ is $P_{dw}(k|k_*)*F_{HM}*M_B$, while the best combination employing $F_{SAM}$ is $P_{dw}(k|k_*)*F_{SAM}*M_B$, which leads to unbiased measurements of cosmological parameters. We compare these to the Effective Field Theory of Large-Scale Structure perturbation theory model $P_{EFT}(k|Θ)$, and find that our simple phenomenological models are comparable across the entire redshift range for $k_{max}=0.25$ and $0.3$ $h$/Mpc. We expect the tools that we have developed to be useful in probing dark energy and testing gravity using Roman in an accurate and robust manner.
