论文标题
从干涉强度映射中提取HI天体物理学
Extracting HI Astrophysics from Interferometric Intensity Mapping
论文作者
论文摘要
我们提出了一种新的中性氢（HI）的晕晕模型，该模型在红移$ z \ sim0.1 $和$ z \ sim1.0 $上校准了Galaxy形成模拟，我们采用了我们对HI天体物理学上的干涉HI强度映射的约束功率进行研究。我们证明，对小型HI功率谱的约束可以打破HI密度$ω_ {\ rm HI} $与HI偏见$ b _ {\ rm hi} $之间的变性。对于$ z \ sim0.1 $，我们预测，$ω_ {\ rm hi} $的准确度量最高为6％，高度级别的高偏见$ b _ {\ rm hi}^0 $最高可用于使用平方千里（ska）pathfinder pathfinder pathfinder and ulasherian skaap and ustral skaap and ustral skaap and ustraian patheranian skaap and ustrian skaap and skaap）我们还提出了对HARO模型框架中HI Shot噪声的新描述，其中考虑了HI质量的星系及其宿主光晕质量之间的关系。此外，鉴于高质量阈值以上HI星系的数量密度，未来的调查也将能够仅使用HI SHOT噪声来限制HI质量函数。使用标准的Schechter函数，这将导致在10％级别的限制。该技术将有可能提供一种与现有方法无关的测量HI质量功能的新方法。我们预测，SKA将能够进一步提高低降距限制，并在较高的红移下对HI天体物理学的开创性测量。
We present a new halo model of neutral hydrogen (HI) calibrated to galaxy formation simulations at redshifts $z\sim0.1$ and $z\sim1.0$ that we employ to investigate the constraining power of interferometric HI intensity mapping on HI astrophysics. We demonstrate that constraints on the small-scale HI power spectrum can break the degeneracy between the HI density $Ω_{\rm HI}$ and the HI bias $b_{\rm HI}$. For $z\sim0.1$, we forecast that an accurate measurement of $Ω_{\rm HI}$ up to 6% level precision and the large-scale HI bias $b_{\rm HI}^0$ up to 1% level precision can be achieved using Square Kilometre Array (SKA) pathfinder data from MeerKAT and Australian SKA Pathfinder (ASKAP). We also propose a new description of the HI shot noise in the halo model framework in which a scatter of the relation between the HI mass of galaxies and their host halo mass is taken into account. Furthermore, given the number density of HI galaxies above a certain HI mass threshold, future surveys will also be able to constrain the HI mass function using only the HI shot noise. This will lead to constraints at the 10% level using the standard Schechter function. This technique will potentially provide a new way of measuring the HI Mass Function, independent from existing methods. We predict that the SKA will be able to further improve the low-redshift constraints by a factor of 3, as well as pioneering measurements of HI astrophysics at higher redshifts.
