Detections of [C ii] 158 μm and [O iii] 88 μm in a Local Lyman Continuum Emitter, Mrk 54, and Its Implications to High-redshift ALMA Studies

Ryota Ura; Takuya Hashimoto; Akio K. Inoue; Dario Fadda; Matthew Hayes; Johannes Puschnig; Erik Zackrisson; Yoichi Tamura; Hiroshi Matsuo; Ken Mawatari; Yoshinobu Fudamoto; Masato Hagimoto; Nario Kuno; Yuma Sugahara; Satoshi Yamanaka; Tom J. L. C. Bakx; Yurina Nakazato; Mitsutaka Usui; Hidenobu Yajima; Naoki Yoshida

doi:10.3847/1538-4357/acc530

The Astrophysical Journal (Jan 2023)

Detections of [C ii] 158 μm and [O iii] 88 μm in a Local Lyman Continuum Emitter, Mrk 54, and Its Implications to High-redshift ALMA Studies

Ryota Ura,
Takuya Hashimoto,
Akio K. Inoue,
Dario Fadda,
Matthew Hayes,
Johannes Puschnig,
Erik Zackrisson,
Yoichi Tamura,
Hiroshi Matsuo,
Ken Mawatari,
Yoshinobu Fudamoto,
Masato Hagimoto,
Nario Kuno,
Yuma Sugahara,
Satoshi Yamanaka,
Tom J. L. C. Bakx,
Yurina Nakazato,
Mitsutaka Usui,
Hidenobu Yajima,
Naoki Yoshida

Affiliations

Ryota Ura: Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan ; [email protected]
Takuya Hashimoto: ORCiD; Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan ; [email protected]; Tomonaga Center for the History of the Universe (TCHoU), Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan
Akio K. Inoue: ORCiD; Department of Physics, School of Advanced Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan; Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan
Dario Fadda: ORCiD; SOFIA Science Center, Universities Space Research Association , MS 232-11, Moffett Field, CA 94035, USA
Matthew Hayes: ORCiD; The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden
Johannes Puschnig: ORCiD; The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden; Argelander-Institut für Astronomie , Auf dem Hügel 71, D-53121, Bonn, Germany
Erik Zackrisson: ORCiD; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University , Box 516, SE-751 20 Uppsala, Sweden
Yoichi Tamura: ORCiD; Department of Physics, Graduate School of Science, Nagoya University , Nagoya 464-8602, Japan
Hiroshi Matsuo: ORCiD; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Graduate University for Advanced Studies (SOKENDAI) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Ken Mawatari: ORCiD; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Yoshinobu Fudamoto: ORCiD; Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Masato Hagimoto: ORCiD; Department of Physics, Graduate School of Science, Nagoya University , Nagoya 464-8602, Japan
Nario Kuno: ORCiD; Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan ; [email protected]; Tomonaga Center for the History of the Universe (TCHoU), Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan
Yuma Sugahara: ORCiD; Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Satoshi Yamanaka: ORCiD; General Education Department, National Institute of Technology , Toba College, 1-1, Ikegami-cho, Toba, Mie 517-8501, Japan
Tom J. L. C. Bakx: ORCiD; Department of Physics, Graduate School of Science, Nagoya University , Nagoya 464-8602, Japan; National Astronomical Observatory of Japan , 2-21-1, Osawa, Mitaka, Tokyo, Japan
Yurina Nakazato: ORCiD; Department of Physics, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan
Mitsutaka Usui: Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan ; [email protected]
Hidenobu Yajima: ORCiD; Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba , Tsukuba, Ibaraki 305-8571, Japan ; [email protected]; Center for Computational Sciences, University of Tsukuba , Ten-nodai, 1-1-1 Tsukuba, Ibaraki 305-8577, Japan
Naoki Yoshida: ORCiD; Department of Physics, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan; Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan

DOI: https://doi.org/10.3847/1538-4357/acc530
Journal volume & issue: Vol. 948, no. 1
p. 3

Abstract

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We present integral field, far-infrared (FIR) spectroscopy of Mrk 54, a local Lyman continuum emitter, obtained with FIFI-LS on the Stratospheric Observatory for Infrared Astronomy. This is only the second time, after Haro 11, that [C ii ] 158 μ m and [O iii ] 88 μ m spectroscopy of the known LCEs have been obtained. We find that Mrk 54 has a strong [C ii ] emission that accounts for ∼1% of the total FIR luminosity, whereas it has only moderate [O iii ] emission, resulting in the low [O iii ]/[C ii ] luminosity ratio of 0.22 ± 0.06. In order to investigate whether [O iii ]/[C ii ] is a useful tracer of f _esc (LyC escape fraction), we examine the correlations of [O iii ]/[C ii ] and (i) the optical line ratio of O _32 ≡ [O iii ] 5007 Å/[O ii ] 3727 Å, (ii) specific star formation rate, (iii) [O iii ] 88 μ m/[O i ] 63 μ m ratio, (iv) gas-phase metallicity, and (v) dust temperature based on a combined sample of Mrk 54 and the literature data from the Herschel Dwarf Galaxy Survey and the LITTLE THINGS Survey. We find that galaxies with high [O iii ]/[C ii ] luminosity ratios could be the result of high ionization (traced by O _32 ), bursty star formation, high ionized-to-neutral gas volume filling factors (traced by [O iii ] 88 μ m/[O i ] 63 μ m), and low gas-phase metallicities, which is in agreement with theoretical predictions. We present an empirical relation between the [O iii ]/[C ii ] ratio and f _esc based on the combination of the [O iii ]/[C ii ] and O _32 correlation, and the known relation between O _32 and f _esc . The relation implies that high-redshift galaxies with high [O iii ]/[C ii ] ratios revealed by the Atacama Large Millimeter/submillimeter Array may have f _esc ≳ 0.1, significantly contributing to the cosmic reionization.

Published in The Astrophysical Journal

ISSN: 1538-4357 (Online)
Publisher: IOP Publishing
Country of publisher: United Kingdom
LCC subjects: Science: Astronomy: Astrophysics
Website: https://iopscience.iop.org/journal/0004-637X

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