Statistical Correlation between the Distribution of Lyα Emitters and Intergalactic Medium H i at z ∼ 2.2 Mapped by the Subaru/Hyper Suprime-Cam,The Astrophysical Journal

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Statistical Correlation between the Distribution of Lyα Emitters and Intergalactic Medium H i at z ∼ 2.2 Mapped by the Subaru/Hyper Suprime-Cam
The Astrophysical Journal ( IF 4.8 ) Pub Date : 2021-01-19 , DOI: 10.3847/1538-4357/abcd93
Yongming Liang _{1,

2,

3} , Nobunari Kashikawa _{2,

3,

4} , Zheng Cai ₅ , Xiaohui Fan ₆ , J. Xavier Prochaska ₇ , Kazuhiro Shimasaku _{3,

4} , Masayuki Tanaka _{1,

2} , Hisakazu Uchiyama ₂ , Kei Ito _{1,

2,

3} , Rhythm Shimakawa ₂ , Kentaro Nagamine _{8,

9,

10} , Ikkoh Shimizu _{2,

11} , Masafusa Onoue ₁₂ , Jun Toshikawa _{13,

14}

Affiliation

Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), Mitaka, Tokyo 181-8588, Japan
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Research Center for the Early Universe, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Department of Astronomy, Tsinghua University, Beijing 100084, People’s Republic of China
Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA
UCO/Lick Observatory, University of California, 1156 High Street, Santa Cruz, CA 95064, USA
Department of Earth and Space Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, Japan
Kavli IPMU (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Parkway, Las Vegas, NV 89154-4002, USA
Shikoku Gakuin University, 3-2-1 Bunkyocho, Zentsuji, Kagawa, 765-8505, Japan
Max-Planck-Institut fr Astronomie, Knigstuhl 17, D-69117 Heidelberg, Germany
Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa, Chiba 277-8582, Japan
Department of Physics, University of Bath, Claverton Down, Bath, BA2 7AY, UK

The correlation between neutral Hydrogen (HI) in the intergalactic medium (IGM) and galaxies now attracts great interests. We select four fields which include several coherently strong Ly$\alpha$ absorption systems at $z\sim2.2$ detected by using background quasars from the whole SDSS/(e)BOSS database. Deep narrow-band and $g$-band imaging are performed using the Hyper Suprime-Cam on the Subaru Telescope. We select out 2,642 Ly$\alpha$ emitter (LAE) candidates at $z=2.177\pm0.023$ down to the Ly$\alpha$ luminosity of $L_{\text{Ly}\alpha}\approx 2 \times 10^{42} {\rm erg~s}^{-1}$ to construct the galaxy overdensity maps, covering an effective area of 5.39 deg$^2$. Combining the sample with the Ly$\alpha$ absorption estimated from 64 (e)BOSS quasar spectra, we find a moderate to strong correlation between the LAE overdensity $\delta_{\rm LAE}$ and the effective optical depth $\tau_{\rm LoS}$ in line-of-sights, with $P$-value$=0.09\%$ ($<0.01\%$) when the field that contains a significant quasar overdensity is in(ex)cluded. The cross-correlation analysis also clearly suggests that up to $4\pm1$ pMpc, LAEs tend to cluster in the regions rich in HI gas, indicated by the high $\tau_{\rm LoS}$, and avoid the low $\tau_{\rm LoS}$ region where the HI gas is deficient. By averaging the $\tau_{\rm LoS}$ as a function of the projected distance ($d$) to LAEs, we find a $30\%$ excess signal at $2\sigma$ level at $d<200$ pkpc, indicating the dense HI in circumgalactic medium, and a tentative excess at $400

中文翻译：

斯巴鲁/超级超级相机映射的 Lyα 发射体分布与 z ∼ 2.2 处的星系间介质 H i 之间的统计相关性

星系际介质 (IGM) 中的中性氢 (HI) 与星系之间的相关性现在引起了极大的兴趣。我们选择了四个场，其中包括通过使用来自整个 SDSS/(e)BOSS 数据库的背景类星体在 $z\sim2.2$ 处检测到的几个连贯的强 Ly$\alpha$ 吸收系统。使用斯巴鲁望远镜上的 Hyper Suprime-Cam 进行深窄带和 $g$ 波段成像。我们在 $z=2.177\pm0.023$ 上选择了 2,642 个 Ly$\alpha$ 发射器（LAE）候选者，直到 $L_{\text{Ly}\alpha}\approx 2 \times 的 Ly$\alpha$ 光度10^{42} {\rm erg~s}^{-1}$ 构建星系超密度图，覆盖有效面积为 5.39 deg$^2$。将样品与从 64 (e)BOSS 类星体光谱估计的 Ly$\alpha$ 吸收相结合，我们发现 LAE 过密度 $\delta_{\rm LAE}$ 与视线中的有效光学深度 $\tau_{\rm LoS}$ 之间存在中等至强相关性，其中 $P$-value$=0.09 \%$ ($<0.01\%$) 当包含显着类星体超密度的场被排除在外时。互相关分析也清楚地表明，高达 $4\pm1$ pMpc，LAEs 倾向于聚集在富含 HI 气体的区域，由高 $\tau_{\rm LoS}$ 表示，并避免低 $\tau_ {\rm LoS}$ HI 气体不足的区域。通过将 $\tau_{\rm LoS}$ 作为到 LAE 的投影距离 ($d$) 的函数求平均值，我们在 $d<200$ pkpc 处发现 $2\sigma$ 水平的 $30\%$ 过量信号，表明环星系介质中的密集 HI，以及 400 美元的暂定过剩 01\%$) 当包含显着类星体超密度的场被排除在外时。互相关分析也清楚地表明，高达 $4\pm1$ pMpc，LAEs 倾向于聚集在富含 HI 气体的区域，由高 $\tau_{\rm LoS}$ 表示，并避免低 $\tau_ {\rm LoS}$ HI 气体不足的区域。通过将 $\tau_{\rm LoS}$ 作为到 LAE 的投影距离 ($d$) 的函数求平均值，我们在 $d<200$ pkpc 处发现 $2\sigma$ 水平的 $30\%$ 过量信号，表明环星系介质中的密集 HI，以及 400 美元的暂定过剩 01\%$) 当包含显着类星体超密度的场被排除在外时。互相关分析也清楚地表明，高达 $4\pm1$ pMpc，LAEs 倾向于聚集在富含 HI 气体的区域，由高 $\tau_{\rm LoS}$ 表示，并避免低 $\tau_ {\rm LoS}$ HI 气体不足的区域。通过将 $\tau_{\rm LoS}$ 作为到 LAE 的投影距离 ($d$) 的函数求平均值，我们在 $d<200$ pkpc 处发现 $2\sigma$ 水平的 $30\%$ 过量信号，表明环星系介质中的密集 HI，以及 400 美元的暂定过剩并避免 HI 气体不足的低 $\tau_{\rm LoS}$ 区域。通过将 $\tau_{\rm LoS}$ 作为到 LAE 的投影距离 ($d$) 的函数求平均值，我们在 $d<200$ pkpc 处发现 $2\sigma$ 水平的 $30\%$ 过量信号，表明环星系介质中的密集 HI，以及 400 美元的暂定过剩并避免 HI 气体不足的低 $\tau_{\rm LoS}$ 区域。通过将 $\tau_{\rm LoS}$ 作为到 LAE 的投影距离 ($d$) 的函数求平均值，我们在 $d<200$ pkpc 处发现 $2\sigma$ 水平的 $30\%$ 过量信号，表明环星系介质中的密集 HI，以及 400 美元的暂定过剩

更新日期：2021-01-19

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