A complete CO survey of the Large Magellanic Cloud

Cohen, R. S.; Dame, T. M.; Garay, Guido; Montani, J.; Rubio, M.; Thaddeus, P.

doi:10.1086/185243

Cited by 239 publications

(208 citation statements)

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“…A full PDR model analysis will be presented in a follow-up paper (Okada et al in prep.). N159 is located south of 30 Dor as a part of the molecular ridge (Cohen et al 1988;Mizuno et al 2001). Three CO cores are identified (N159 W, E, and S; Johansson et al 1998).…”

Section: Introductionmentioning

confidence: 99%

Velocity resolved [C ii], [C i], and CO observations of the N159 star-forming region in the Large Magellanic Cloud: a complex velocity structure and variation of the column densities

Okada

Requeña-Torres

Güsten

et al. 2015

A&A

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Context. The [C ii] 158 µm fine structure line is one of the dominant cooling lines in star-forming active regions. Together with models of photon-dominated regions, the data is used to constrain the physical properties of the emitting regions, such as the density and the radiation field strength. According to the modeling, the [C ii] 158 µm line integrated intensity compared to the CO emission is expected to be stronger in lower metallicity environments owing to lower dust shielding of the UV radiation, a trend that is also shown by spectral-unresolved observations. In the commonly assumed clumpy UV-penetrated cloud scenario, the models predict a [C ii] line profile similar to that of CO. However, recent spectral-resolved observations by Herschel/HIFI and SOFIA/GREAT (as well as the observations presented here) show that the velocity resolved line profile of the [C ii] emission is often very different from that of CO lines, indicating a more complex origin of the line emission including the dynamics of the source region. Aims. The Large Magellanic Cloud (LMC) provides an excellent opportunity to study in great detail the physics of the interstellar medium (ISM) in a low-metallicity environment by spatially resolving individual star-forming regions. The aim of our study is to investigate the physical properties of the star-forming ISM in the LMC by separating the origin of the emission lines spatially and spectrally. In this paper, we focus on the spectral characteristics and the origin of the emission lines, and the phases of carbon-bearing species in the N159 star-forming region in the LMC. Methods. We mapped a 4 ′ ×(3 ′ -4 ′ ) region in N159 in [C ii] 158 µm and [N ii] 205 µm with the GREAT instrument on board SOFIA. We also observed CO(3-2), (4-3), (6-5), 13 CO(3-2), and [C i] 3 P 1 -3 P 0 and 3 P 2 -3 P 1 with APEX. All spectra are velocity resolved. Results. The emission of all transitions observed shows a large variation in the line profiles across the map and in particular between the different species. At most positions the [C ii] emission line profile is substantially wider than that of CO and [C i]. We estimated the fraction of the [C ii] integrated line emission that cannot be fitted by the CO line profile to be 20% around the CO cores, and up to 50% at the area between the cores, indicating a gas component that has a much larger velocity dispersion than the ones probed by the CO and [C i] emission. We derived the relative contribution from C + , C, and CO to the column density in each velocity bin. The result clearly shows that the contribution from C + dominates the velocity range far from the the velocities traced by the dense molecular gas. Spatially, the region located between the CO cores of N159 W and E has a higher fraction of C + over the whole velocity range. We estimate the contribution of the ionized gas to the [C ii] emission using the ratio to the [N ii] emission, and find that the ionized gas contributes ≤ 19% to the [C ii] emission at its peak position, and ≤ 15% over the whol...

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Section: Introductionmentioning

confidence: 99%

Velocity resolved [C ii], [C i], and CO observations of the N159 star-forming region in the Large Magellanic Cloud: a complex velocity structure and variation of the column densities

Okada

Requeña-Torres

Güsten

et al. 2015

A&A

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“…37 in their of Cohen et al (1988). The diameter of CO-37 is given as 234 pc, the CO mass as 6.3 × 10 6 M , and the virial mass as 13.2 × 10 6 M .…”

Section: Introductionmentioning

confidence: 99%

First spectroscopically confirmed discovery of an extragalactic T Tauri star

Wichmann

Schmitt

Krautter³

2001

A&A

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Abstract.We report the first spectroscopic discovery of an extragalactic bona-fide T Tauri star. The object, LTS J054427-692659, is a low-mass, late-type star located within the LMC dark cloud Hodge II 139. It shows Hα emission with an equivalent width of 78Å, in line with galactic T Tauri stars, but in excess of any main-sequence dwarf star. The only known plausible interpretation of LTS J054427-692659 is a LMC T Tauri star.

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“…Figure 2 shows the [C ii]/ 12 CO J = 1−0 line intensity ratio observed in galaxies as a function of oxygen abundance, 12 + log[O/H], derived from optical-UV emission line observations of H ii regions in the galaxies. The [C ii] and CO data are, respectively, from Nakagawa et al (1998) and Dame et al (1987) for the Galaxy; Mochizuki et al (1994) and Cohen et al (1988) for the Large Magellanic Cloud (LMC); Madden et al (1997) and Becker (1990) for IC 10. The CO intensity scale of Dame et al (1987) was corrected as described in Bronfman et al (1988).…”

Section: Resultsmentioning

confidence: 99%

Search for the [CII] 158 micron emission toward the blue compact dwarf galaxy I Zw 36

Mochizuki

Onaka

2001

A&A

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) and is at least one order of magnitude lower than those in irregular galaxies (I [C ii] /ICO 2 10 4 ) with low metallicities, in spite of the lower metallicity in I Zw 36 (12 + log[O/H] = 7.9) than in the irregulars. The observed difference in the line ratio between I Zw 36 and the irregulars can be accounted for by a higher gas density (10 3 cm −3 < ∼ nH < ∼ 10 4 cm −3 ) in I Zw 36, because the higher CO-formation rate at the higher density enables CO molecules to survive even against the photodissociation enhanced by the low dust abundance. The expected higher gas density in I Zw 36 may be related to change in large-scale gravitational potential with galactic evolution, if blue compact dwarfs and irregulars have evolutionary links.

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A complete CO survey of the Large Magellanic Cloud

Cited by 239 publications

References 0 publications

Velocity resolved [C ii], [C i], and CO observations of the N159 star-forming region in the Large Magellanic Cloud: a complex velocity structure and variation of the column densities

Velocity resolved [C ii], [C i], and CO observations of the N159 star-forming region in the Large Magellanic Cloud: a complex velocity structure and variation of the column densities

First spectroscopically confirmed discovery of an extragalactic T Tauri star

Search for the [CII] 158 micron emission toward the blue compact dwarf galaxy I Zw 36

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