Journal
ASTRONOMY & ASTROPHYSICS
Volume 542, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201219518
Keywords
galaxies: high-redshift; galaxies: individual: LESS J033229.4-275619; submillimeter: galaxies; submillimeter: ISM
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Funding
- JSPS [23654068]
- STFC [ST/F002092/1, ST/I001557/1, ST/J003018/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002092/1, ST/J003018/1, ST/I001557/1] Funding Source: researchfish
- Grants-in-Aid for Scientific Research [23654068, 23540268] Funding Source: KAKEN
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The chemical properties of high-z galaxies provide important information for constraining galaxy evolutionary scenarios. However, widely used metallicity diagnostics based on rest-frame optical emission lines are unusable for heavily dust-enshrouded galaxies (such as submillimeter galaxies; SMGs), especially at z > 3. Here we focus on the flux ratio of the far-infrared fine-structure emission lines [N (II)] 205 mu m and [C (II)] 158 mu m to assess the metallicity of high-z SMGs. Through ALMA cycle 0 observations, we have detected the [N (II)] 205 mu m emission in a strongly [C (II)]-emitting SMG, LESS J033229.4-275619 at z = 4.76. The velocity-integrated [N (II)]/[C (II)] flux ratio is 0.043 +/- 0.008. This is the first measurement of the [N (II)]/[C (II)] flux ratio in high-z galaxies, and the inferred flux ratio is similar to the ratio observed in the nearby universe (similar to 0.02-0.07). The velocity-integrated flux ratio and photoionization models suggest that the metallicity in this SMG is consistent with solar, implying that the chemical evolution has progressed very rapidly in this system at z = 4.76. We also obtain a tight upper limit on the CO(12-11) transition, which translates into CO(12-11)/CO(2-1) < 3.8 (3s). This suggests that the molecular gas clouds in LESS J033229.4-275619 are not significantly affected by the radiation field emitted by the AGN in this system.
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