Outside the Lyman-break box: detecting Lyman continuum emitters at 3.5 < z < 5.1 with CLAUDS
Creators
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1.
Swinburne University of Technology
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2.
Centre of Excellence for All-Sky Astrophysics
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3.
Saint Mary's University
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National Research Council Canada
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Infrared Processing and Analysis Center
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University College London
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Waseda University
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Space Telescope Science Institute
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9.
Johns Hopkins University
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Laboratoire d'Astrophysique de Marseille
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University of Geneva
Abstract
Identifying non-contaminated sample of high-redshift galaxies with escaping Lyman continuum (LyC) flux is important for understanding the sources and evolution of cosmic reionization. We present CLAUDS (CFHT Large Area u-band deep survey) u-band photometry of the COSMOS field to probe LyC radiation from spectroscopically confirmed galaxies at z ≥ 3.5 and outside the standard Lyman-break galaxy colour-selection expectations. Complementary to the CLAUDS data, we use Subaru multifilter photometry, Hubble Space Telescope (HST) multifilter imaging, and the spectroscopic surveys D10K, VUDS, and 3D-HST. We present a sample of Lyman continuum galaxy (LCG) candidates in the redshift range 3.5 ≲ z ≲ 5.1. Here, we introduce 5 LCG candidates, where two are flagged quality 1 and three quality 2. The estimated f^(abs)_(esc) for quality 1 candidates are in the range ∼5−73 per cent and ∼30−93 per cent. These estimates are based on our derived parameters from individual galaxies as inputs to a range of BPASS models as well as mean intergalactic medium (IGM) and maximal intergalactic and circumgalactic media (IGM+CGM) transmission. We conclude that our search for LCGs is most likely biased to lines of sight with low H I densities or free from Lyman limit systems. Our two best LCG candidates have EW (Lyα) ≤ 50 Å and we find no correlation or anticorrelation between EW (Lyα), f^(abs)_(esc), and Robs, the ratio of ionizing to non-ionizing observed flux in the measured passbands. Stacking candidates without solid LyC detections (S/N < 3) results in an estimated f^(abs)_(esc) from galaxies not greater than 1 per cent.
Additional Information
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) Accepted 2020 March 29. Received 2020 February 17; in original form 2019 December 9. We would like to thank Ikuru Iwata for constructive comments and suggestions that helped to improve this manuscript. We would like to thank anonymous referee for very useful comments which gave us a possibility to address several issues that were initially overlooked. AKI is supported by JSPS KAKENHI grant number 17H01114. This research was conducted by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. Support for program number HST-GO-15100 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. JC acknowledges the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), CE170100004. The HSC collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. This paper makes use of software developed for the Large Synoptic Survey Telescope (LSST). We thank the LSST Project for making their code available as free software at http://dm.lsst.org The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant number NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant number AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. Based [in part] on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center at NAOJ. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France. The HST data matched to the VUDS-DR1 are described in Grogin et al. (2011) and Koekemoer et al. (2011) for CANDELS and include data from the ERS (Windhorst et al. 2011). This work is based on observations taken by the 3D-HST Treasury Program (HST-GO-12177 and HST-GO-12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.Attached Files
Published - staa920.pdf
Accepted Version - 2004.00158.pdf
Files
2004.00158.pdf
Additional details
Identifiers
- Eprint ID
- 104055
- Resolver ID
- CaltechAUTHORS:20200625-112850623
Related works
- Describes
- https://arxiv.org/abs/2004.00158 (URL)
Funding
- Japan Society for the Promotion of Science (JSPS)
- 17H01114
- Australian Research Council
- CE170100013
- NASA
- HST-GO-15100
- NASA
- NAS5-26555
- Australian Research Council
- CE170100004
- University of Tokyo
- Ministry of Education, Culture, Sports, Science and Technology (MEXT)
- Japan Science and Technology Agency
- Toray Science Foundation
- National Astronomical Observatory of Japan
- Kavli Institute for the Physics and Mathematics of the Universe
- High Energy Accelerator Research Organization (KEK)
- Princeton University
- Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)
- NASA
- NNX08AR22G
- NSF
- AST-1238877
- University of Maryland
- Eotvos Lorand University (ELTE)
- Los Alamos National Laboratory
- NASA
- HST-GO-12177
- NASA
- HST-GO-12328
Dates
- Created
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2020-06-25Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)