Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas
<i>Context.<i/> Molecular gas is a necessary fuel for star formation. The CO (1−0) transition is often used to deduce the total molecular hydrogen but is challenging to detect in low-metallicity galaxies in spite of the star formation taking place. In contrast, the [C II]<i>λ<i/...
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| Hauptverfasser: | , , , , , , , , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
17 November 2020
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| In: |
Astronomy and astrophysics
Year: 2020, Jahrgang: 643 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202038860 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1051/0004-6361/202038860 Verlag, lizenzpflichtig, Volltext: https://www.aanda.org/articles/aa/abs/2020/11/aa38860-20/aa38860-20.html 
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| Verfasserangaben: | S.C. Madden, D. Cormier, S. Hony, V. Lebouteiller, N. Abel, M. Galametz, I. De Looze, M. Chevance, F.L. Polles, M.-Y. Lee, F. Galliano, A. Lambert-Huyghe, D. Hu, and L. Ramambason |
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| 100 | 1 | |a Madden, Suzanne |e VerfasserIn |0 (DE-588)1224612426 |0 (DE-627)1744147876 |4 aut | |
| 245 | 1 | 0 | |a Tracing the total molecular gas in galaxies |b [CII] and the CO-dark gas |c S.C. Madden, D. Cormier, S. Hony, V. Lebouteiller, N. Abel, M. Galametz, I. De Looze, M. Chevance, F.L. Polles, M.-Y. Lee, F. Galliano, A. Lambert-Huyghe, D. Hu, and L. Ramambason |
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| 520 | |a <i>Context.<i/> Molecular gas is a necessary fuel for star formation. The CO (1−0) transition is often used to deduce the total molecular hydrogen but is challenging to detect in low-metallicity galaxies in spite of the star formation taking place. In contrast, the [C II]<i>λ<i/>158 <i>μ<i/>m is relatively bright, highlighting a potentially important reservoir of H<sub>2<sub/> that is not traced by CO (1−0) but is residing in the C<sup>+<sup/>-emitting regions.<i>Aims.<i/> Here we aim to explore a method to quantify the total H<sub>2<sub/> mass (<i>M<i/><sub>H<sub>2<sub/><sub/>) in galaxies and to decipher what parameters control the CO-dark reservoir.<i>Methods.<i/> We present Cloudy grids of density, radiation field, and metallicity in terms of observed quantities, such as [O I], [C I], CO (1−0), [C II], <i>L<i/><sub>TIR<sub/>, and the total <i>M<i/><sub>H<sub>2<sub/><sub/>. We provide recipes based on these models to derive total <i>M<i/><sub>H<sub>2<sub/><sub/> mass estimates from observations. We apply the models to the <i>Herschel<i/> Dwarf Galaxy Survey, extracting the total <i>M<i/><sub>H<sub>2<sub/><sub/> for each galaxy, and compare this to the H<sub>2<sub/> determined from the observed CO (1−0) line. This allows us to quantify the reservoir of H<sub>2<sub/> that is CO-dark and traced by the [C II]<i>λ<i/>158 <i>μ<i/>m.<i>Results.<i/> We demonstrate that while the H<sub>2<sub/> traced by CO (1−0) can be negligible, the [C II]<i>λ<i/>158 <i>μ<i/>m can trace the total H<sub>2<sub/>. We find 70 to 100% of the total H<sub>2<sub/> mass is not traced by CO (1−0) in the dwarf galaxies, but is well-traced by [C II]<i>λ<i/>158 <i>μ<i/>m. The CO-dark gas mass fraction correlates with the observed <i>L<i/><sub>[C II]<sub/>/<i>L<i/><sub>CO(1−0)<sub/> ratio. A conversion factor for [C II]<i>λ<i/>158 <i>μ<i/>m to total H<sub>2<sub/> and a new CO-to-total-<i>M<i/><sub>H<sub>2<sub/><sub/> conversion factor as a function of metallicity are presented.<i>Conclusions.<i/> While low-metallicity galaxies may have a feeble molecular reservoir as surmised from CO observations, the presence of an important reservoir of molecular gas that is not detected by CO can exist. We suggest a general recipe to quantify the total mass of H<sub>2<sub/> in galaxies, taking into account the CO and [C II] observations. Accounting for this CO-dark H<sub>2<sub/> gas, we find that the star-forming dwarf galaxies now fall on the Schmidt-Kennicutt relation. Their star-forming efficiency is rather normal because the reservoir from which they form stars is now more massive when introducing the [C II] measures of the total H<sub>2<sub/> compared to the small amount of H<sub>2<sub/> in the CO-emitting region. | ||
| 700 | 1 | |a Cormier, Diane |e VerfasserIn |0 (DE-588)1068245999 |0 (DE-627)819837210 |0 (DE-576)427399904 |4 aut | |
| 700 | 1 | |a Hony, Sacha |e VerfasserIn |0 (DE-588)1058892061 |0 (DE-627)797717587 |0 (DE-576)41495789X |4 aut | |
| 700 | 1 | |a Lebouteiller, Vianney |e VerfasserIn |0 (DE-588)1205982906 |0 (DE-627)1691810630 |4 aut | |
| 700 | 1 | |a Abel, N. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Galametz, Maud |e VerfasserIn |0 (DE-588)1208642693 |0 (DE-627)1694952703 |4 aut | |
| 700 | 1 | |a Looze, I. De |e VerfasserIn |4 aut | |
| 700 | 1 | |a Chevance, Mélanie |e VerfasserIn |0 (DE-588)1141805553 |0 (DE-627)1000759342 |0 (DE-576)470814411 |4 aut | |
| 700 | 1 | |a Polles, Fiorella L. |e VerfasserIn |0 (DE-588)1180523857 |0 (DE-627)1067749853 |0 (DE-576)52019473X |4 aut | |
| 700 | 1 | |a Lee, Min-Young |e VerfasserIn |0 (DE-588)1201436079 |0 (DE-627)1685143695 |4 aut | |
| 700 | 1 | |a Galliano, F. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Lambert-Huyghe, A. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Hu, D. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Ramambason, L. |e VerfasserIn |4 aut | |
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