Hostname: page-component-586b7cd67f-t7czq Total loading time: 0 Render date: 2024-12-05T02:16:19.347Z Has data issue: false hasContentIssue false
  • English
  • Français

ALMA detection of the [OIII] 88 μm line in a highly-magnified Lyman break galaxy at z = 6.1

Published online by Cambridge University Press:  10 June 2020

Kaho Sunaga ,
Yoichi Tamura ,
Minju Lee Open the ORCID record for Minju Lee [Opens in a new window] ,
Ken Mawatari ,
Akio K. Inoue Open the ORCID record for Akio K. Inoue [Opens in a new window] ,
Takuya Hashimoto ,
Hiroshi Matsuo  and
Akio Taniguchi
Kaho Sunaga
Affiliation:
Department of Physics, Nagoya University, Japan
Yoichi Tamura
Affiliation:
Department of Physics, Nagoya University, Japan
Minju Lee
Affiliation:
Department of Physics, Nagoya University, Japan National Astronomical Observatory of Japan, Japan
Ken Mawatari
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, Japan
Akio K. Inoue
Affiliation:
Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Japan
Takuya Hashimoto
Affiliation:
Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Japan National Astronomical Observatory of Japan, Japan
Hiroshi Matsuo
Affiliation:
National Astronomical Observatory of Japan, Japan
Akio Taniguchi
Affiliation:
Department of Physics, Nagoya University, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present a 4.7σ detection of the [OIII] 88 μm line in a gravitationally-lensed Lyman break galaxy, RXC J2248-ID3, using the Atacama Large Millimeter/submillimeter Array (ALMA). We did not detect [CII] 158 μm and rest-frame 90 μm dust continuum emission, suggesting that the bulk of the interstellar medium (ISM) is ionized. Our two-component SED model combining the previous Hubble Space Telescope (HST) data and new photometry obtained from Very Large Telescope (VLT), Spitzer and ALMA suggests the presence of young (∼2 Myr) and mature (∼600 Myr) stellar components with the metallicity of Z = 0.2Z⊙. Our findings are in contrast with previous results claiming a very young, metal-poor stellar component.

Keywords

galaxies: high-redshift
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 309 - 311
Copyright
© International Astronomical Union 2020

References

Balestra, I., Vanzella, E., Rosati, P., et al. 2013, A&A, 559, L9Google Scholar
Inoue, A. K., Shimizu, I., Tamura, Y., et al. 2014, ApJ, 780, L18CrossRefGoogle Scholar
Mainali, R., Kollmeier, J. A., Stark, D. P., et al. 2017, ApJ, 836, L1410.3847/2041-8213/836/1/L14CrossRefGoogle Scholar
Mawatari, K., et al. 2018, Proc. IAU Symposium No. 341, in this volumeGoogle Scholar
Monna, A., Seitz, S., Greisel, N., et al. 2014, MNRAS, 438, 1417CrossRefGoogle Scholar