Big Three Dragons: Molecular Gas in a Bright Lyman-break Galaxy at z = 7.15
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- Hashimoto_2023_ApJ_952_48
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We report Atacama Large Millimeter/submillimeter Array Band 3 observations of CO(6−5), CO(7−6), and [C i](2−1) in B14-65666 (“Big Three Dragons”), one of the brightest Lyman-break galaxies at z > 7 in the rest-frame ultraviolet continuum, far-infrared continuum, and emission lines of [O iii] 88 μm and [C ii] 158 μm. CO(6−5), CO(7−6), and [C i](2−1), whose 3σ upper limits on the luminosities are approximately 40 times fainter than the [C ii] luminosity, are all not detected. The L [C II]/L CO(6-5) and L [C II]/L CO(7-6) ratios are higher than the typical ratios obtained in dusty star-forming galaxies or quasar host galaxies at similar redshifts, and they may suggest a lower gas density in the photodissociated region in B14-65666. By using the (1) [C ii] luminosity, (2) dust mass-to-gas mass ratio, and (3) a dynamical mass estimate, we find that the molecular gas mass (M mol) is (0.05-11) × 1010 M ⊙. This value is consistent with the upper limit inferred from the nondetection of mid-J CO and [C i](2−1). Despite the large uncertainty in M mol, we estimate a molecular gas-to-stellar mass ratio (μ gas) of 0.65-140 and a gas depletion time (τ dep) of 2.5-550 Myr; these values are broadly consistent with those of other high-redshift galaxies. B14-65666 could be an ancestor of a passive galaxy at z ≳ 4 if no gas is fueled from outside the galaxy.
| Originalsprog | Engelsk |
|---|---|
| Artikelnummer | 48 |
| Tidsskrift | Astrophysical Journal |
| Vol/bind | 952 |
| Udgave nummer | 1 |
| Antal sider | 10 |
| ISSN | 0004-637X |
| DOI | |
| Status | Udgivet - 18 jul. 2023 |
Bibliografisk note
Funding Information:
We thank the anonymous referee for providing valuable comments that greatly improved this paper. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan (HJH02007) and by JSPS KAKENHI grant Nos. 20K22358 and 22H01258. A.K.I., Y.S., and Y.F. are supported by NAOJ ALMA Scientific Research grant No. 2020-16B. A.K.I. acknowledges support from JSPS KAKENHI grant No. 23H00131. Y.T. acknowledges support from JSPS KAKENHI grant No. 22H04939. K.K. acknowledges support from the Knut and Alice Wallenberg Foundation. We thank Yoshito Shimajiri for support in analyzing ALMA data. We appreciate Hajime Fukushima, Shigeki Inoue, Satoshi Kikuta, Masami Ouchi, Hidenobu Yajima, and Atsuhi Yasuda for discussion. We would like to thank Editage (www.editage.com) for English language editing. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01673. 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 HST data used in this work are obtained through the data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.
Funding Information:
We thank the anonymous referee for providing valuable comments that greatly improved this paper. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan (HJH02007) and by JSPS KAKENHI grant Nos. 20K22358 and 22H01258. A.K.I., Y.S., and Y.F. are supported by NAOJ ALMA Scientific Research grant No. 2020-16B. A.K.I. acknowledges support from JSPS KAKENHI grant No. 23H00131. Y.T. acknowledges support from JSPS KAKENHI grant No. 22H04939. K.K. acknowledges support from the Knut and Alice Wallenberg Foundation. We thank Yoshito Shimajiri for support in analyzing ALMA data. We appreciate Hajime Fukushima, Shigeki Inoue, Satoshi Kikuta, Masami Ouchi, Hidenobu Yajima, and Atsuhi Yasuda for discussion. We would like to thank Editage ( www.editage.com ) for English language editing. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2018.1.01673. 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 HST data used in this work are obtained through the data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
ID: 361380932