论文标题
合唱IV：用Subaru HSC绘制空间不均匀的宇宙回离
CHORUS IV: Mapping the Spatially Inhomogeneous Cosmic Reionization with Subaru HSC
论文作者
论文摘要
空间不均匀性是理解电离过程的重要特征之一。但是，它尚未得到充分量化。 To map this inhomogeneous distribution, we simultaneously detect Ly$α$ emitters (LAEs) and Lyman break galaxies (LBGs) at $z \sim 6.6$ from the Subaru/Hyper Suprime-Cam (HSC) large-area ($\sim1.5\,\mathrm{ deg}^2 = 34000 \，\ mathrm {cmpc}^2 $）深度调查。我们从观察到的LAE与LBG的数字密度比，$ n（\ Mathrm {lae}）/N（\ MathRM {lbg}）$估计中性分数，$ x_ \ mathrm {hi} $，从观察到的数字密度比，$ n（\ mathrm {lae}）/n（\ mathrm {lbg}）$基于数值辐射传递模拟，以选择模型的星系选择了选择的选择。虽然发现在视野内的平均$ x_ \ mathrm {hi} $是$ x_ \ mathrm {hi} <0.4 $，这与以前的研究一致，但在每个$ 140 $ n of $ n（\ mathrm {lbg}）$中的$ n（\ mathrm {lae}）/n（\ mathrm {lae}）/n（pmp）大约三分之一。这可能表明在空间上是不均匀的电源拓扑结构，但它也打开了变化基于星系分布固有的大规模结构的可能性。基于模拟，可能很难将两者与当前调查区分开。我们还发现，高LAE密度区域的Laes填充了高$ \ Mathrm {ew} _0 $，支持观察到的$ n（\ mathrm {lae}）/n（\ mathrm {lbg}）$或多或少地由中性分数驱动，尽管统计意义不是高于统计意义。
The spatial inhomogeneity is one of the important features for understanding the reionization process; however, it has not yet been fully quantified. To map this inhomogeneous distribution, we simultaneously detect Ly$α$ emitters (LAEs) and Lyman break galaxies (LBGs) at $z \sim 6.6$ from the Subaru/Hyper Suprime-Cam (HSC) large-area ($\sim1.5\,\mathrm{ deg}^2 = 34000\,\mathrm{cMpc}^2$) deep survey. We estimate the neutral fraction, $x_\mathrm{HI}$, from the observed number density ratio of LAEs to LBGs, $n(\mathrm{LAE})/n(\mathrm{LBG})$ based on numerical radiative transfer simulation, in which model galaxies are selected to satisfy the observed selection function. While the average $x_\mathrm{HI}$ within the field of view is found to be $x_\mathrm{HI} < 0.4$, which is consistent with previous studies, the variation of $n(\mathrm{LAE})/n(\mathrm{LBG})$ within the field of view for each $140\,\mathrm{pMpc}^2$ is found to be as large as a factor of three. This may suggest a spatially inhomogeneous topology of reionization, but it also leaves open the possibility that the variation is based on the inherent large-scale structure of the galaxy distribution. Based on the simulations, it may be difficult to distinguish between the two from the current survey. We also find that LAEs in the high LAE density region are more populate high $\mathrm{EW}_0$, supporting that the observed $n(\mathrm{LAE})/n(\mathrm{LBG})$ is more or less driven by the neutral fraction, though the statistical significance is not high.
