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Published December 1, 2023 | Version Published
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J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467

Creators

  • 1. ROR icon University of Tokyo
  • 2. ROR icon National Astronomical Observatory of Japan
  • 3. ROR icon The Graduate University for Advanced Studies, SOKENDAI
  • 4. ROR icon Nagoya University
  • 5. ROR icon California Institute of Technology

Abstract

Dusty star-forming galaxies (DSFGs) are among the most massive and active star-forming galaxies during the cosmic noon. Theoretical studies have proposed various formation mechanisms of DSFGs, including major merger-driven starbursts and secular star-forming disks. Here, we report J0107a, a bright (∼8 mJy at observed-frame 888 μm) DSFG at z = 2.467 that appears to be a gas-rich massive disk and might be an extreme case of the secular disk scenario. J0107a has a stellar mass M⋆ ∼ 5 × 1011M⊙, molecular gas mass Mmol ≳ 1011M⊙, and a star formation rate of ∼500M⊙ yr−1. J0107a does not have a gas-rich companion. The rest-frame 1.28 μm JWST NIRCam image of J0107a shows a grand-design spiral with a prominent stellar bar extending ∼15 kpc. The Atacama Large Millimeter/submillimeter Array Band 7 continuum map reveals that the dust emission originates from both the central starburst and the stellar bar. 3D disk modeling of the CO(4–3) emission line indicates a dynamically cold disk with rotation-to-dispersion ratio V_(max)/ σ ∼ 8. The results suggest a bright DSFG may have a nonmerger origin, and its vigorous star formation may be triggered by the bar and/or rapid gas inflow.

Copyright and License

© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

 

Acknowledgement

We are grateful to the anonymous reviewer for the helpful and constructive comments that improved the quality of this manuscript. S.M. is supported by Japan Society for the Promotion of Science (JSPS) KAKENHI with grant No. 23KJ0450. Y.T. is supported by JSPS KAKENHI (No. 22H04939). This paper makes use of the following ALMA data: ADS/JAO.ALMA #2013.1.00469.S, #2013.1.01057.S, #2015.1.00973.S, #2015.1.00902.S, and #2013.1.00740.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The Flatiron Institute is supported by the Simons Foundation.

Software References

numpy (Harris et al. 2020), scipy (Virtanen et al. 2020), matplotlib (Hunter 2007), astropy (Astropy Collaboration et al. 2018), photutils (Bradley et al. 2022), dynesty (Speagle 2020)

Data Availability

The JWST data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi:10.17909/g4k8-3922.

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Huang_2023_ApJL_958_L26.pdf

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Additional details

Identifiers

ISSN
2041-8213

Related works

Is supplemented by
Dataset: 10.17909/g4k8-3922 (DOI)

Funding

Japan Society for the Promotion of Science
23KJ0450
Simons Foundation