Atomic Carbon and CO Isotope Emission in the Vicinity of DR 15

Oka, Tomoharu; Yamamoto, Satoshi; Iwata, Mitsuhiro; Maezawa, Hiroyuki; Ikeda, Masafumi; Ito, Tetsuya; Kamegai, Kazuhisa; Sakai, Takeshi; Sekímoto, Yutaro; Tatematsu, Ken’ichi; Arikawa, Yuji; Aso, Yukio; Noguchi, Takashi; Shi, Shuaiyi; Miyazawa, Keisuke; Saito, Shuji; Ozeki, Hiroyuki; Fujiwara, Hideo; Ohishi, Masatoshi; Inatani, Junji

doi:10.1086/321536

Cited by 45 publications

(38 citation statements)

References 28 publications

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“…For v = −0.83 to +0.9 km s −1 , the bulk of the DR15 cloud appears as a ring of emission that connects to the DR12 cloud and L889. Close to the nominal position of DR15, two infrared dark clouds (IRDCs, Egan et al 1998;Oka et al 2001) can be identified. They both have the same velocity range of ∼-1.5 to ∼2.5 km s −1 .…”

Section: Channel Maps Of 13 Co 2 → 1 Emissionmentioning

confidence: 99%

A new view of the Cygnus X region

Schneider

Bontemps

Simon

et al. 2006

A&A

216

356

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Context. The Cygnus X region is one of the richest star formation sites in the Galaxy. There is a long-standing discussion about whether the region is a chance superposition of several complexes along the line of sight or a single coherent complex at a distance of 1.5 to 2 kpc. Aims. Combining a 13 CO 2 → 1 survey taken with the KOSMA 3 m telescope with mid-IR images from MSX provides a way to improve our understanding of the spatial structure of the complex. The physical properties of the molecular gas can be derived in more detail as it was done in former studies. Methods. Cygnus X has been mapped in 13 CO J = 2 → 1 (10.8 deg 2 ) at an angular resolution of 130 , as well as for smaller areas in 12 CO and 13 CO J = 3 → 2 (90 ), using the KOSMA 3 m submm-telescope. Results. We identified 91 clumps in 13 CO 2 → 1 that have a typical excitation temperature of 10−30 K, an average density of 1.3 × 10 3 cm −3 , radii of 1−8 pc, and masses of a few hundred to several ten thousand M . The main cloud complexes, the northern part (M 2.8 × 10 5 M ) including DR21 and W75N and the southern region (M 4.5 × 10 5 M ) with IC 1318 b/c and AFGL2591, show differences in their physical properties. The 13 CO emission is closely associated with mid-IR emission seen with MSX. We find evidence that Cygnus OB2 and Cygnus OB9 are affecting the molecular material in Cygnus X. Conclusions. Since essentially all molecular cloud complexes in Cygnus X form groups that are connected by molecular emission (visible in channel and position-velocity maps) and partly show evidence of interaction with UV radiation, we conclude that most of the objects seen in this region are located at the same distance, i.e., that of the OB2 cluster at ∼1.7 kpc, which is also consistent with the distances of other OB associations (OB9, OB1) in Cygnus X.

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Section: Channel Maps Of 13 Co 2 → 1 Emissionmentioning

confidence: 99%

A new view of the Cygnus X region

Schneider

Bontemps

Simon

et al. 2006

A&A

216

356

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“…The optical depth of the [C I] emission and the column density of C were derived using the equations reported by Oka et al (2001) and Tsukagoshi et al (2015). Here, the beam filling factor f d was derived from the ratio of the solid angle of the disk to that of the telescope beam (Ω A ): Table 2).…”

Section: Optical Depth Of the [C I] Emission And Column Density Of Cmentioning

confidence: 99%

“…Assuming the local thermodynamic equilibrium, we derived the column density of atomic carbon, N(C), as (Oka et al 2001)…”

Section: Optical Depth Of the [C I] Emission And Column Density Of Cmentioning

confidence: 99%

“…Our result is an order of magnitude lower than previous estimates made from [C II] observations for β Pictoris: 7.1×10 −3 M ⊕ (Cataldi et al 2014) and 2×10 −3 M ⊕ (Kral et al 2016). Under the local thermodynamic equilibrium and optically thin condition, the CO column density was calculated as (e.g., Oka et al 2001)…”

Section: Optical Depth Of the [C I] Emission And Column Density Of Cmentioning

confidence: 99%

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Detection of Submillimeter-wave [C i] Emission in Gaseous Debris Disks of 49 Ceti and β Pictoris

Higuchi

Sato

Tsukagoshi

et al. 2017

ApJL

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We have detected [C I]3 P 1 -3 P 0 emissions in the gaseous debris disks of 49 Ceti and β Pictoris with the 10 m telescope of the Atacama Submillimeter Telescope Experiment, which is the first detection of such emissions. The line profiles of [C I] are found to resemble those of CO(J=3-2) observed with the same telescope and the Atacama Large Millimeter/submillimeter Array. This result suggests that atomic carbon (C) coexists with CO in the debris disks, and is likely formed by the photodissociation of CO. Assuming an optically thin [C I] emission with the excitation temperature ranging from 30 to 100 K, the column density of C is evaluated to be (2.2±0.2)×10 17 and (2.5±0.7)×10 16 cm −2 for 49 Ceti and β Pictoris, respectively. The C/CO column density ratio is thus derived to be 54±19 and 69±42 for 49 Ceti and β Pictoris, respectively. These ratios are higher than those of molecular clouds and diffuse clouds by an order of magnitude. The unusually high ratios of C to CO are likely attributed to a lack of H 2 molecules needed to reproduce CO molecules efficiently from C. This result implies a small number of H 2 molecules in the gas disk; i.e., there is an appreciable contribution of secondary gas from dust grains.

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“…Especially the large spatial extension of neutral carbon and the high abundance deep inside molecular clouds appears to be in contradiction with standard PDR models. This is also addressed by the [C ] vs. CO studies of Plume et al (1994) in S 140, Oka et al (2001) in DR15, Kamegai et al (2003) in ρ Ophiuchi, and Oka et al (2004) in NGC 1333. In a study of the translucent cloud MCLD 123.5 + 24.9, Bensch et al (2003) find lower than expected [C ] intensities and [C ] to CO ratios.…”

Section: Introductionmentioning

confidence: 96%

Emission of CO, C I, and C II in W3 Main

Krämer

Jakob

Mookerjea

et al. 2004

A&A

158

200

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Abstract. We used the KOSMA 3m telescope to map the core 7 × 5 of the Galactic massive star forming region W3 Main in the two fine structure lines of atomic carbon and four mid-J transitions of CO and et al. 1991), this data set allows us to study the physical structure of the molecular cloud interface regions where the occurence of carbon is believed to change from C + to C 0 , and to CO. The molecular gas in W3 Main is warmed by the far ultraviolet (FUV) field created by more than a dozen OB stars. Detailed modelling shows that most of the observed line intensity ratios and absolute intensities are consistent with a clumpy photon dominated region (PDR) of a few hundred unresolved clumps per 0.84 pc beam, filling between 3 and 9% of the volume, with a typical clump radius of 0.025 pc (2.2 ), and typical mass of 0.44 M . The high-excitation lines of CO stem from a 100−200 K layer, as do the [C ] lines. The bulk of the gas mass is however at lower temperatures.

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Atomic Carbon and CO Isotope Emission in the Vicinity of DR 15

Cited by 45 publications

References 28 publications

A new view of the Cygnus X region

A new view of the Cygnus X region

Detection of Submillimeter-wave [C i] Emission in Gaseous Debris Disks of 49 Ceti and β Pictoris

Emission of CO, C I, and C II in W3 Main

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