SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization
We present luminosity functions (LFs) and angular correlation functions (ACFs) derived from 18,960 Ly α emitters (LAEs) at z = 2.2−7.3 over a wide survey area of ≲24 deg ^2 that are identified in the narrowband data of the HSC-SSP and CHORUS surveys. Confirming the large sample with 241 spectroscop...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4365/adb1c0 |
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| author | Hiroya Umeda Masami Ouchi Satoshi Kikuta Yuichi Harikane Yoshiaki Ono Takatoshi Shibuya Akio K. Inoue Kazuhiro Shimasaku Yongming Liang Akinori Matsumoto Shun Saito Haruka Kusakabe Yuta Kageura Minami Nakane |
| author_facet | Hiroya Umeda Masami Ouchi Satoshi Kikuta Yuichi Harikane Yoshiaki Ono Takatoshi Shibuya Akio K. Inoue Kazuhiro Shimasaku Yongming Liang Akinori Matsumoto Shun Saito Haruka Kusakabe Yuta Kageura Minami Nakane |
| author_sort | Hiroya Umeda |
| collection | DOAJ |
| description | We present luminosity functions (LFs) and angular correlation functions (ACFs) derived from 18,960 Ly α emitters (LAEs) at z = 2.2−7.3 over a wide survey area of ≲24 deg ^2 that are identified in the narrowband data of the HSC-SSP and CHORUS surveys. Confirming the large sample with 241 spectroscopically identified LAEs, we determine Ly α LFs and ACFs in the brighter luminosity range down to 0.5 L _⋆ , and confirm that our measurements are consistent with previous studies but offer significantly reduced statistical uncertainties. The improved precision of our ACFs allows us to clearly detect one-halo terms at some redshifts, and provides large-scale bias measurements that indicate host halo masses of ∼10 ^11 M _⊙ over z ≃ 2−7. By comparing our Ly α LF (ACF) measurements with reionization models, we estimate the neutral hydrogen fractions in the intergalactic medium to be x _H _i < 0.05 (= ${0.06}_{-0.03}^{+0.12}$ ) at z = 5.7 and x _H _i = $0.1{5}_{-0.08}^{+0.10}$ ( ${0.21}_{-0.14}^{+0.19}$ ), $0.1{8}_{-0.12}^{+0.14}$ , and $0.7{5}_{-0.13}^{+0.09}$ at z = 6.6, 7.0, and 7.3, respectively. Our findings suggest that the neutral hydrogen fraction remains relatively low, x _H _i ≲ 0.2, at z = 5−7, but increases sharply at z > 7, reaching x _H _i ∼ 0.9 by z ≃ 8−9, as indicated by recent JWST studies. The combination of our results from LAE observations with recent JWST observations suggests that the major epoch of reionization occurred at z ∼ 7−8, likely driven by the emergence of massive sources emitting significant ionizing photons. |
| format | Article |
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| spelling | doaj-art-32a32dd67bd849da84ff898a978258782025-08-20T02:06:40ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127723710.3847/1538-4365/adb1c0SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of ReionizationHiroya Umeda0https://orcid.org/0009-0008-0167-5129Masami Ouchi1https://orcid.org/0000-0002-1049-6658Satoshi Kikuta2https://orcid.org/0000-0003-3214-9128Yuichi Harikane3https://orcid.org/0000-0002-6047-430XYoshiaki Ono4https://orcid.org/0000-0001-9011-7605Takatoshi Shibuya5Akio K. Inoue6https://orcid.org/0000-0002-7779-8677Kazuhiro Shimasaku7https://orcid.org/0000-0002-2597-2231Yongming Liang8https://orcid.org/0000-0002-2725-302XAkinori Matsumoto9Shun Saito10https://orcid.org/0000-0002-6186-5476Haruka Kusakabe11https://orcid.org/0000-0002-3801-434XYuta Kageura12Minami Nakane13https://orcid.org/0009-0000-1999-5472Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies) , Osawa 2-21-1, Mitaka, Tokyo, 181-8588, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo , Kashiwa, Chiba 277-8583, JapanDepartment of Astronomy, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; Department of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UKInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jpKitami Institute of Technology , 165 Koen-cho, Kitami, Hokkaido 090-8507, JapanWaseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan; Department of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, JapanDepartment of Astronomy, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan; Research Center for the Early Universe, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanKavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo , Kashiwa, Chiba 277-8583, Japan; Institute for Multi-messenger Astrophysics and Cosmology, Department of Physics, Missouri University of Science and Technology , 1315 North Pine Street, Rolla, MO 65409, USANational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; ume@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanWe present luminosity functions (LFs) and angular correlation functions (ACFs) derived from 18,960 Ly α emitters (LAEs) at z = 2.2−7.3 over a wide survey area of ≲24 deg ^2 that are identified in the narrowband data of the HSC-SSP and CHORUS surveys. Confirming the large sample with 241 spectroscopically identified LAEs, we determine Ly α LFs and ACFs in the brighter luminosity range down to 0.5 L _⋆ , and confirm that our measurements are consistent with previous studies but offer significantly reduced statistical uncertainties. The improved precision of our ACFs allows us to clearly detect one-halo terms at some redshifts, and provides large-scale bias measurements that indicate host halo masses of ∼10 ^11 M _⊙ over z ≃ 2−7. By comparing our Ly α LF (ACF) measurements with reionization models, we estimate the neutral hydrogen fractions in the intergalactic medium to be x _H _i < 0.05 (= ${0.06}_{-0.03}^{+0.12}$ ) at z = 5.7 and x _H _i = $0.1{5}_{-0.08}^{+0.10}$ ( ${0.21}_{-0.14}^{+0.19}$ ), $0.1{8}_{-0.12}^{+0.14}$ , and $0.7{5}_{-0.13}^{+0.09}$ at z = 6.6, 7.0, and 7.3, respectively. Our findings suggest that the neutral hydrogen fraction remains relatively low, x _H _i ≲ 0.2, at z = 5−7, but increases sharply at z > 7, reaching x _H _i ∼ 0.9 by z ≃ 8−9, as indicated by recent JWST studies. The combination of our results from LAE observations with recent JWST observations suggests that the major epoch of reionization occurred at z ∼ 7−8, likely driven by the emergence of massive sources emitting significant ionizing photons.https://doi.org/10.3847/1538-4365/adb1c0ReionizationGalaxy formationLuminosity functionLyman-alpha galaxies |
| spellingShingle | Hiroya Umeda Masami Ouchi Satoshi Kikuta Yuichi Harikane Yoshiaki Ono Takatoshi Shibuya Akio K. Inoue Kazuhiro Shimasaku Yongming Liang Akinori Matsumoto Shun Saito Haruka Kusakabe Yuta Kageura Minami Nakane SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization The Astrophysical Journal Supplement Series Reionization Galaxy formation Luminosity function Lyman-alpha galaxies |
| title | SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization |
| title_full | SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization |
| title_fullStr | SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization |
| title_full_unstemmed | SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization |
| title_short | SILVERRUSH. XIV. Lyα Luminosity Functions and Angular Correlation Functions from 20,000 Lyα Emitters at z ∼ 2.2–7.3 from up to 24 deg2 HSC-SSP and CHORUS Surveys: Linking the Postreionization Epoch to the Heart of Reionization |
| title_sort | silverrush xiv lyα luminosity functions and angular correlation functions from 20 000 lyα emitters at z ∼ 2 2 7 3 from up to 24 deg2 hsc ssp and chorus surveys linking the postreionization epoch to the heart of reionization |
| topic | Reionization Galaxy formation Luminosity function Lyman-alpha galaxies |
| url | https://doi.org/10.3847/1538-4365/adb1c0 |
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