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Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas.
- Source :
- Astronomy & Astrophysics / Astronomie et Astrophysique; Nov2020, Vol. 643, p1-21, 21p
- Publication Year :
- 2020
-
Abstract
- Context. 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]λ158 μm is relatively bright, highlighting a potentially important reservoir of H<subscript>2</subscript> that is not traced by CO (1−0) but is residing in the C<superscript>+</superscript>-emitting regions. Aims. Here we aim to explore a method to quantify the total H<subscript>2</subscript> mass (M<subscript>H<subscript>2</subscript></subscript>) in galaxies and to decipher what parameters control the CO-dark reservoir. Methods. 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], L<subscript>TIR</subscript>, and the total M<subscript>H<subscript>2</subscript></subscript>. We provide recipes based on these models to derive total M<subscript>H<subscript>2</subscript></subscript> mass estimates from observations. We apply the models to the Herschel Dwarf Galaxy Survey, extracting the total M<subscript>H<subscript>2</subscript></subscript> for each galaxy, and compare this to the H<subscript>2</subscript> determined from the observed CO (1−0) line. This allows us to quantify the reservoir of H<subscript>2</subscript> that is CO-dark and traced by the [C II]λ158 μm. Results. We demonstrate that while the H<subscript>2</subscript> traced by CO (1−0) can be negligible, the [C II]λ158 μm can trace the total H<subscript>2</subscript>. We find 70 to 100% of the total H<subscript>2</subscript> mass is not traced by CO (1−0) in the dwarf galaxies, but is well-traced by [C II]λ158 μm. The CO-dark gas mass fraction correlates with the observed L<subscript>[C II]</subscript>/L<subscript>CO(1−0)</subscript> ratio. A conversion factor for [C II]λ158 μm to total H<subscript>2</subscript> and a new CO-to-total-M<subscript>H<subscript>2</subscript></subscript> conversion factor as a function of metallicity are presented. Conclusions. 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<subscript>2</subscript> in galaxies, taking into account the CO and [C II] observations. Accounting for this CO-dark H<subscript>2</subscript> 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<subscript>2</subscript> compared to the small amount of H<subscript>2</subscript> in the CO-emitting region. [ABSTRACT FROM AUTHOR]
- Subjects :
- DWARF galaxies
GALAXIES
GAS reservoirs
STAR formation
STARBURSTS
GASES
Subjects
Details
- Language :
- English
- ISSN :
- 00046361
- Volume :
- 643
- Database :
- Complementary Index
- Journal :
- Astronomy & Astrophysics / Astronomie et Astrophysique
- Publication Type :
- Academic Journal
- Accession number :
- 148681376
- Full Text :
- https://doi.org/10.1051/0004-6361/202038860