CHORUS. I. Cosmic HydrOgen Reionization Unveiled with Subaru: Overview

Author:

Inoue Akio K123ORCID,Yamanaka Satoshi23ORCID,Ouchi Masami456,Iwata Ikuru47ORCID,Shimasaku Kazuhiro89,Taniguchi Yoshiaki1011,Nagao Tohru11,Kashikawa Nobunari8,Ono Yoshiaki5,Mawatari Ken35,Shibuya Takatoshi12,Hayashi Masao4ORCID,Ikeda Hiroyuki13,Zhang Haibin514,Liang Yongming478,Lee Chien-Hsiu15ORCID,Hilmi Miftahul58,Kikuta Satoshi16,Kusakabe Haruka17,Furusawa Hisanori47ORCID,Hayashino Tomoki18,Kajisawa Masaru11,Matsuda Yuichi47,Nakajima Kimihiko4,Momose Rieko8,Harikane Yuichi419,Saito Tomoki20,Kodama Tadayuki21,Kikuchihara Shotaro58ORCID,Iye Masanori4,Goto Tomotsugu22

Affiliation:

1. Department of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

2. Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan

3. Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, 3-1-1 Nakagaito, Daito, Osaka 574-8530, Japan

4. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan

5. Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Japan

6. Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), WPI, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan

7. Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

8. Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

9. Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

10. The Open University of Japan, 2-11 Wakaba, Mihama-ku, Chiba, Chiba 261-8586, Japan

11. Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan

12. Kitami Institute of Technology, 165 Koen-cho, Kitami, Hokkaido 090-8507, Japan

13. National Institute of Technology, Wakayama College, 77 Noshima, Nada-cho, Gobo, Wakayama 644-0023, Japan

14. Department of Astronomy, Tsinghua University, No. 1 Qinghuayuan, Beijing 100084, China

15. NSF’s National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ 85719, USA

16. Center for Computational Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8577, Japan

17. Observatoire de Genève, Université de Genève, 51 chemin de Pégase, 1290 Versoix, Switzerland

18. Research Center for Neutrino Science, Tohoku University, Aramaki, Aoba-ku, Sendai 980-8578, Japan

19. Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

20. Nishi-Harima Astronomical Observatory, Centre for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo, Sayo-gun, Hyogo 679-5313, Japan

21. Astronomical Institute, Tohoku University, 6-3 Aramaki, Aoba-ku, Sendai 980-8578, Japan

22. Institute of Astronomy, National Tsing Hua University, 101 Section 2 Kuang Fu Road, Hsinchu 300, Taiwan, ROC

Abstract

Abstract To determine the dominant sources for cosmic reionization, the evolution history of the global ionizing fraction, and the topology of the ionized regions, we have conducted a deep imaging survey using four narrow-band (NB) and one intermediate-band (IB) filters on the Subaru/Hyper Suprime-Cam (HSC), called Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS). The central wavelengths and full-widths-at-half-maximum of the CHORUS filters are, respectively, 386.2 nm and 5.5 nm for NB387, 526.0 nm and 7.9 nm for NB527, 717.1 nm and 11.1 nm for NB718, 946.2 nm and 33.0 nm for IB945, and 971.2 nm and 11.2 nm for NB973. This combination, including NB921 (921.5 nm and 13.5 nm) from the Subaru Strategic Program with HSC (HSC SSP), is carefully designed, as if they were playing a chorus, to observe multiple spectral features simultaneously, such as Lyman continuum, Lyα, C iv, and He ii for $z$ = 2–7. The observing field is the same as that of the deepest footprint of the HSC SSP in the COSMOS field and its effective area is about 1.6 deg2. We present an overview of the CHORUS project, which includes descriptions of the filter design philosophy, observations and data reduction, multiband photometric catalogs, assessments of the imaging quality, measurements of the number counts, and example use cases for the data. All the imaging data, photometric catalogs, masked pixel images, data of limiting magnitudes and point spread functions, results of completeness simulations, and source number counts are publicly available through the HSC SSP database.

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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