ADF22-WEB: Detection of a molecular gas reservoir in a massive quiescent galaxy located in a $z\approx3$ proto-cluster core
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| Formato: | Preprint |
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2025
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| _version_ | 1866916606345478144 |
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| author | Umehata, Hideki Kubo, Mariko Nakanishi, Kouichiro |
| author_facet | Umehata, Hideki Kubo, Mariko Nakanishi, Kouichiro |
| contents | We present a study of the molecular gas reservoirs and dust contents in three quiescent galaxies (QGs) located in the core of the $z=3.09$ SSA22 proto-cluster. Using the Atacama Large Millimeter/submillimeter Array (ALMA), we detect CO(3--2) emission in one galaxy, ADF22-QG1, marking the first direct detection of molecular gas in a quiescent galaxy from the early universe. The detected galaxy, ADF22-QG1, has a molecular gas mass of log$M_{\rm H_2}$/M$_\odot = 10.26 \pm 0.07$ assuming a CO-to-H$2$ conversion factor $α_{\rm CO} = 4.4$ (log$M_{\rm H_2}$/M$_\odot = 9.52 \pm 0.07$ for $α_{\rm CO} = 0.8$), corresponding to a gas mass fraction of $f_{\rm gas} \approx 14\%$ (2.5\%). The gas-to-dust ratio $δ_{\rm gdr}\gtrsim170$ ($δ_{\rm gdr}\gtrsim30$) for $α_{\rm CO} = 4.4$ ($α_{\rm CO} =0.8$) is also derived for the first time for a QG at the epoch. For the other two galaxies, ADF22-QG2 and ADF22-QG3, non detections of CO(3--2) emission provide upper limits, $f_{\rm gas} \approx 17\%$ (3.1\%) and $f_{\rm gas} \approx 13\%$ (2.4\%), respectively. The inferred gas-consumption history of ADF22-QG1, based on its star-formation history, suggests that (i) dusty star-forming galaxies (DSFGs) at $z = 4$--$6$ are plausible progenitors, and (ii) the cessation of gas accretion from cosmic web filaments plays an important role in their evolution to quenched systems. Furthermore, the presence of a detectable molecular gas reservoir in ADF22-QG1 indicates that additional mechanisms, such as morphological quenching, may be required to fully explain its quiescent nature. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2502_06538 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | ADF22-WEB: Detection of a molecular gas reservoir in a massive quiescent galaxy located in a $z\approx3$ proto-cluster core Umehata, Hideki Kubo, Mariko Nakanishi, Kouichiro Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics We present a study of the molecular gas reservoirs and dust contents in three quiescent galaxies (QGs) located in the core of the $z=3.09$ SSA22 proto-cluster. Using the Atacama Large Millimeter/submillimeter Array (ALMA), we detect CO(3--2) emission in one galaxy, ADF22-QG1, marking the first direct detection of molecular gas in a quiescent galaxy from the early universe. The detected galaxy, ADF22-QG1, has a molecular gas mass of log$M_{\rm H_2}$/M$_\odot = 10.26 \pm 0.07$ assuming a CO-to-H$2$ conversion factor $α_{\rm CO} = 4.4$ (log$M_{\rm H_2}$/M$_\odot = 9.52 \pm 0.07$ for $α_{\rm CO} = 0.8$), corresponding to a gas mass fraction of $f_{\rm gas} \approx 14\%$ (2.5\%). The gas-to-dust ratio $δ_{\rm gdr}\gtrsim170$ ($δ_{\rm gdr}\gtrsim30$) for $α_{\rm CO} = 4.4$ ($α_{\rm CO} =0.8$) is also derived for the first time for a QG at the epoch. For the other two galaxies, ADF22-QG2 and ADF22-QG3, non detections of CO(3--2) emission provide upper limits, $f_{\rm gas} \approx 17\%$ (3.1\%) and $f_{\rm gas} \approx 13\%$ (2.4\%), respectively. The inferred gas-consumption history of ADF22-QG1, based on its star-formation history, suggests that (i) dusty star-forming galaxies (DSFGs) at $z = 4$--$6$ are plausible progenitors, and (ii) the cessation of gas accretion from cosmic web filaments plays an important role in their evolution to quenched systems. Furthermore, the presence of a detectable molecular gas reservoir in ADF22-QG1 indicates that additional mechanisms, such as morphological quenching, may be required to fully explain its quiescent nature. |
| title | ADF22-WEB: Detection of a molecular gas reservoir in a massive quiescent galaxy located in a $z\approx3$ proto-cluster core |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2502.06538 |