AST/RO Observations of Atomic Carbon near the Galactic Center

Ojha, R.; Stark, A. A.; Hsieh, Henry H.; Lane, Alan M.; Chamberlin, Richard; Bania, T. M.; Bolatto, Alberto D.; Jackson, James M.; Wright, Gregory A.

doi:10.1086/318693

Cited by 62 publications

(54 citation statements)

References 19 publications

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“…Recent studies in the Milky Way and nearby galaxies have shown that CO and C I have very similar distributions supporting the interpretation that their emission arises from the same gas volume (Fixsen et al 1999;Ojha et al 2001;Ikeda et al 2002). The results from the carbon line and the CO(3−2) line by the PdBI also support that the molecular gas detected in CO is cospatial with the gas detected in the carbon line, as mentioned in Sect.…”

Section: Excitation Temperature From C Isupporting

confidence: 75%

The CO line SED and atomic carbon in IRAS F10214+4724

Weiß

Downes

et al. 2008

A&A

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Using the IRAM 30 m telescope and the Plateau de Bure interferometer we have detected the C I( 3 P 2 → 3 P 1 ) and the CO 3−2, 4−3, 6−5, 7−6 transitions as well as the dust continuum at 3 and 1.2 mm towards the distant luminous infrared galaxy IRAS F10214+4724 at z = 2.286. The C I( 3 P 2 → 3 P 1 ) line is detected for the first time towards this source and IRAS F10214+4724 now belongs to a sample of only 3 extragalactic sources at any redshift where both of the carbon fine structure lines have been detected. The source is spatially resolved by our C I( 3 P 2 → 3 P 1 ) observation and we detect a velocity gradient along the east-west direction. The CI line ratio allows us to derive a carbon excitation temperature of 42 +12 −9 K. The carbon excitation in conjunction with the CO ladder and the dust continuum constrain the gas density to n(H 2 ) = 10 3.6−4.0 cm −3 and the kinetic temperature to T kin = 45−80 K, similar to the excitation conditions found in nearby starburst galaxies. The rest-frame 360 μm dust continuum morphology is more compact than the line emitting region, which supports previous findings that the far infrared luminosity arises from regions closer to the active galactic nucleus at the center of this system.

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Section: Excitation Temperature From C Isupporting

confidence: 75%

The CO line SED and atomic carbon in IRAS F10214+4724

Weiß

Downes

et al. 2008

A&A

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“…Observations of the forbidden fine-structure lines of neutral atomic carbon in the Milky Way and nearby galaxies (Ojha et al 2001, Gerin & Phillips 2000, and references therein) have revealed a close association with CO emission. Because the critical density for excitation of both the [Ci]( 3 P 1 → 3 P 0 ) transition at 492.160 GHz and the ( 3 P 2 → 3 P 1 ) transition at 809.342 GHz is roughly that of CO(1-0), these observations suggest that the CO and [Ci] emission originates in the same volume.…”

Section: Atomic Carbonmentioning

confidence: 96%

Molecular Gas at High Redshift

Solomon

Bout

2005

Annu. Rev. Astron. Astrophys.

850

1,013

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The Early Universe Molecular Emission Line Galaxies (EMGs) are a population of galaxies with only 36 examples that hold great promise for the study of galaxy formation and evolution at high redshift. The classification, luminosity of molecular line emission, molecular mass, far-infrared (FIR) luminosity, star formation efficiency, morphology, and dynamical mass of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year −1 and the molecular mass from 4 × 10 9 to 1 × 10 11 M⊙. At the lower end, these star formation rates, gas masses, and diameters are similar to those of local ultraluminous infrared galaxies, and represent starbursts in centrally concentrated disks, sometimes, but not always, associated with active galactic nuclei.

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“…Early simple plane-parallel modeling of these regions, predicting [C I] just in narrow gas slabs between CO and [C II], generated an initial skepticism on the real usefulness of [C I] transitions as molecular gas tracers, recently overcome by a growing body of theoretical and observational work. Modern PDR models including non-equilibrium chemistry (Stoerzer et al 1997), turbulent mixing (Xie et al 1995;Glover et al 2015), clumpy geometries (Stutzki et al 1998), and the effect of cosmic rays Bisbas et al 2015Bisbas et al , 2017 can better explain the detection of [C I] fully concomitant with CO (1 − 0) and 13 CO over a wide range of conditions, with a surprisingly constant ratio N ([C I])/N (CO) ∼ 0.1 − 0.2 and tightly correlated intensities (e.g., Keene et al 1996;Ojha et al 2001;Ikeda et al 2002).…”

Section: Introductionmentioning

confidence: 99%

A Survey of Atomic Carbon [C i] in High-redshift Main-sequence Galaxies

Valentino

Magdis

Daddi

et al. 2018

ApJ

126

168

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We present the first results of an ALMA survey of the lower fine structure line of atomic carbon [C I]( 3 P 1 − 3 P 0 ) in far infrared-selected galaxies on the main sequence at z ∼ 1.2 in the COSMOS field. We compare our sample with a comprehensive compilation of data available in literature for local and high-redshift starbursting systems and quasars. We show that the [C I]( 3 P 1 → 3 P 0 ) luminosity correlates on global scales with the infrared luminosity L IR similarly to low-J CO transitions. We report a systematic variation of L [C I] 3 P1 − 3 P0 /L IR as a function of the galaxy type, with the ratio being larger for main-sequence galaxies than for starbursts and sub-millimeter galaxies at fixed L IR . The L [C I] 3 P1 − 3 P0 /L CO(2−1) and M [C I] /M dust mass ratios are similar for main-sequence galaxies and for local and high-redshift starbursts within a 0.2 dex intrinsic scatter, suggesting that [C I] is a good tracer of molecular gas mass as CO and dust. We derive a fraction of f [C I] = M [C I] /M C ∼ 3 − 13% of the total carbon mass in the atomic neutral phase. Moreover, we estimate the neutral atomic carbon abundance, the fundamental ingredient to calibrate [C I] as a gas tracer, by comparing L [C I] 3 P1 − 3 P0 and available gas masses from CO lines and dust emission. We find lower [C I] abundances in mainsequence galaxies than in starbursting systems and sub-millimeter galaxies, as a consequence of the canonical α CO and gas-to-dust conversion factors. This argues against the application to different galaxy populations of a universal standard [C I] abundance derived from highly biased samples.

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AST/RO Observations of Atomic Carbon near the Galactic Center

Cited by 62 publications

References 19 publications

The CO line SED and atomic carbon in IRAS F10214+4724

The CO line SED and atomic carbon in IRAS F10214+4724

Molecular Gas at High Redshift

A Survey of Atomic Carbon [C i] in High-redshift Main-sequence Galaxies

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