Spectrally resolved C II emission in M 33 (HerM33es)

Braine, J.; Gratier, P.; Krämer, C.; Israel, F.P.; Tak, F. F. S. van der; Mookerjea, B.; Boquien, M.; Tabatabaei, F. S.; Werf, P. van der; Henkel, C.

doi:10.1051/0004-6361/201219360

Cited by 22 publications

(34 citation statements)

References 40 publications

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“…More comparable to the results presented in this paper are the HIFI [C II] maps obtained towards star-forming regions in the dwarf spiral galaxy M 33 by Mookerjea et al (2011) and Braine et al (2012). M 33 has a metallicity somewhat lower than the Milky Way in the solar neighborhood (∼factor 2, Magrini et al 2010), and higher than the SMC.…”

Section: Discussionsupporting

confidence: 87%

Carbon gas in SMC low-metallicity star-forming regions

Requeña-Torres

Israel

Okada

et al. 2016

A&A

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This paper presents [C II], [C I] and CO emission line maps of the star-forming regions N 66, N 25+N 26, and N 88 in the metalpoor Local Group dwarf galaxy SMC. The spatial and velocity structure of the large H II region N 66 reveals an expanding ring of shocked molecular gas centered on the exciting star cluster NGC 346, whereas a more distant dense molecular cloud is being eroded by UV radiation from the same cluster. In the N 25+N 26 and N 88 maps, diffuse [C II] emission at a relatively low surface brightness extends well beyond the compact boundaries of the bright emission associated with the H II regions. In all regions, the distribution of this bright [C II] emission and the less prominent [C I] emission closely follows the outline of the CO complexes, but the intensity of the [C II] and [C I] emission is generally anticorrelated, which can be understood by the action of photodissociation and photoionization processes. Notwithstanding the overall similarity of CO and [C II] maps, the intensity ratio of these lines varies significantly, mostly due to changes in CO brightness. [C II] emission line profiles are up to 50% wider in velocity than corresponding CO profiles. A radiative transfer analysis shows that the [C II] line is the dominant tracer of (CO-dark) molecular hydrogen in the SMC. CO emission traces only a minor fraction of the total amount of gas. The similarity of the spatial distribution and line profile shape, and the dominance of molecular gas associated with [C II] rather than CO emission imply that in the low-metallicity environment of the SMC the small amount of dense molecular gas traced by CO is embedded in the much more extended molecular gas traced only by [C II] emission. The contribution from neutral atomic and ionized hydrogen zones is negligible in the star-forming regions observed.

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Section: Discussionsupporting

confidence: 87%

Carbon gas in SMC low-metallicity star-forming regions

Requeña-Torres

Israel

Okada

et al. 2016

A&A

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“…Detailed observations of the [Cii] kinematics are very difficult, especially in the local Universe, as the line can only be observed with small single-dish space or airborne telescopes. However, the [Cii], CO, and Hi velocity profiles do in general trace each other rather well, although they can differ in some details (Boreiko & Betz 1991;Mookerjea et al 2011;Braine et al 2012). One example of a more detailed study is the Herschel observations of the bright cluster galaxy NGC 4696, where the Hα and [Cii] emission trace each other both morphologically and kinematically (Fig.…”

Section: Stability Of the Diskmentioning

confidence: 96%

ALMA resolves turbulent, rotating [CII] emission in a young starburst galaxy atz= 4.8

Breuck

Williams

Swinbank

et al. 2014

A&A

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We present spatially resolved Atacama Large Millimeter/submillimeter Array (ALMA) [Cii] observations of the z = 4.7555 submillimetre galaxy, ALESS 73.1. Our 0. 5 FWHM map resolves the [Cii] emitting gas which is centred close to the active galactic nucleus (AGN). The gas kinematics are dominated by rotation but with high turbulence, v rot /σ int ∼ 3.1, and a Toomre Q parameter <1 throughout the disk. By fitting three independent thin rotating disk models to our data, we derive a total dynamical mass of 3 ± 2 × 10 10 M . This is close to the molecular gas mass derived from previous CO(2-1) observations, and implies a CO to H 2 conversion factor α CO < 2.3 M (K km s −1 pc 2 ) −1 . The mass budget also constrains the stellar mass to <3.1 × 10 10 M , and entails a gas fraction of f gas 0.4. The diameter of the dust continuum emission is <2 kpc, while the star-formation rate is as high as 1000 M yr −1 . Combined with our stellar mass constraint, this implies an extreme specific star formation rate >80 Gyr −1 , especially since there are no clear indications of recent merger activity. Finally, our high signal-to-noise [Cii] measurement revises the observed [Nii]/[Cii] ratio, which suggests a close to solar metallicity, unless the [Cii] flux contains significant contributions from Hii regions. Our observations suggest that ALESS73.1 is a nascent galaxy undergoing its first major burst of star formation, embedded within an unstable but metal-rich gas disk.

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“…Averaged over all regions we can associate ∼54% with the CO emission in NGC 4214. Braine et al (2012) …”

Section: Comparison With Other Sourcesmentioning

confidence: 99%

Disentangling the ISM phases of the dwarf galaxy NGC 4214 using [C ii] SOFIA/GREAT observations

Fahrion

Cormier

Bigiel

et al. 2017

A&A

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Context. The [C ii] 158 µm fine structure line is one of the dominant cooling lines in the interstellar medium (ISM) and is an important tracer of star formation. Recent velocity-resolved studies with Herschel/HIFI and SOFIA/GREAT showed that the [C ii] line can constrain the properties of the ISM phases in star-forming regions. The [C ii] line as a tracer of star formation is particularly important in low-metallicity environments where CO emission is weak because of the presence of large amounts of CO-dark gas. Aims. The nearby irregular dwarf galaxy NGC 4214 offers an excellent opportunity to study an actively star-forming ISM at low metallicity. We analyzed the spectrally resolved [C ii] line profiles in three distinct regions at different evolutionary stages of NGC 4214 with respect to ancillary H i and CO data in order to study the origin of the [C ii] line. Methods. We used SOFIA/GREAT [C ii] 158 µm observations, H i data from THINGS, and CO(2 → 1) data from HERACLES to decompose the spectrally resolved [C ii] line profiles into components associated with neutral atomic and molecular gas. We use this decomposition to infer gas masses traced by [C ii] under different ISM conditions. Results. Averaged over all regions, we associate about 46% of the [C ii] emission with the H i emission. However, we can assign only ∼9% of the total [C ii] emission to the cold neutral medium (CNM). We found that about 79% of the total molecular hydrogen mass is not traced by CO emission. Conclusions. On average, the fraction of CO-dark gas dominates the molecular gas mass budget. The fraction seems to depend on the evolutionary stage of the regions: it is highest in the region covering a super star cluster in NGC 4214, while it is lower in a more compact, more metal-rich region.

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Spectrally resolved C II emission in M 33 (HerM33es)

Cited by 22 publications

References 40 publications

Carbon gas in SMC low-metallicity star-forming regions

Carbon gas in SMC low-metallicity star-forming regions

ALMA resolves turbulent, rotating [CII] emission in a young starburst galaxy atz= 4.8

Disentangling the ISM phases of the dwarf galaxy NGC 4214 using [C ii] SOFIA/GREAT observations

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