Atomic Carbon in M82: Physical Conditions Derived from Simultaneous Observations of the [C [CSC]i[/CSC]] Fine-Structure Submillimeter-Wave Transitions

Stützki, J.; Graf, U. U.; Haas, S.; Honingh, C. E.; Hottgenroth, D.; Jacobs, K.; Schieder, R.; Simon, R.; Staguhn, Johannes; Winnewisser, G.; Martin, Robert N.; Peters, William L.; McMullin, J. P.

doi:10.1086/310514

Cited by 91 publications

(88 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…four times higher than estimated by Stutzki et al (1997), although not ruled out by their results -see also Schilke et al (1993).…”

Section: However the I([ci])/i(mentioning

confidence: 66%

“…Beyond the Local Group, i.e. at distances larger than 1 Mpc, [CI] has been mapped in bright galaxies such as IC 342 (Büttgenbach et al 1992), M 82 (Schilke et al 1993;White et al 1994;Stutzki et al 1997) and NGC 253 (Israel et al 1995;Harrison et al 1995), as well as M 83 (Petitpas & Wilson 1998;Israel & Baas 2001) and NGC 6946 (Israel & Baas 2001). A survey of 13 galaxies, including limited Gerin & Phillips (2000).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Neutral atomic carbon in centers of galaxies

Israel

Baas

2002

A&A

View full text Add to dashboard Cite

Abstract. We present measurements of the emission from the centers of fifteen spiral galaxies in the 3 P1-3 P0 [CI] fine-structure transition at 492 GHz. Observed galaxy centers range from quiescent to starburst to active. The intensities of neutral carbon, the J = 2-1 transition of 13 CO and the J = 4-3 transition of 12 CO are compared in matched beams. Most galaxy centers emit more strongly in [CI] than in 13 CO, completely unlike the situation pertaining to Galactic molecular cloud regions.[CI] intensities are lower than, but nevertheless comparable to J = 4-3 12 CO intensities, again rather different from Galactic sources. The ratio of [CI] to 13 CO increases with the central [CI] luminosity of a galaxy; it is lowest for quiescent and mild starburst centers, and highest for strong starburst centers and active nuclei. Comparison with radiative transfer model calculations shows that most observed galaxy centers have neutral carbon abundances close to, or exceeding, carbon monoxide abundances, rather independent from the assumed model gas parameters. The same models suggest that the emission from neutral carbon and carbon monoxide, if assumed to originate in the same volumes, arises from a warm and dense gas rather than a hot and tenuous, or a cold and very dense gas. The observed [CI] intensities together with literature [CII] line and far-infrared continuum data likewise suggest that a significant fraction of the emission originates in medium-density gas (n = 10 3 -10 4 cm −3 ), subjected to radiation fields of various strengths.

show abstract

“…four times higher than estimated by Stutzki et al (1997), although not ruled out by their results -see also Schilke et al (1993).…”

Section: However the I([ci])/i(mentioning

confidence: 66%

Section: Introductionmentioning

confidence: 99%

Neutral atomic carbon in centers of galaxies

Israel

Baas

2002

A&A

View full text Add to dashboard Cite

show abstract

“…Firstly, most of the galactic data were obtained toward prominent sites of massive star formation, where the UV radiation field is also exceptionally intense. Secondly, judging from Ci, in the Cloverleaf the excitation of the molecular gas is intermediate between conditions found for the starburst galaxy M 82 (T ex,CI ∼ 50 K) and the central region of the Milky Way (T ex,CI ∼ 22 K) (Stutzki et al 1997;Weiß et al 2003). Thirdly, polycyclic aromatic hydrocarbon (PAH) features are as strong as expected with respect to the far infrared luminosity when compared with more nearby ultraluminous star-forming galaxies, favoring "normal" conditions and a predominantly starburst nature of the Cloverleaf's huge FIR emission (Lutz et al 2007).…”

Section: Chemical Fractionation and Isotope Selective Photodissociationmentioning

confidence: 83%

Weak¹³CO in the Cloverleaf quasar: evidence for a young, early generation starburst

Henkel¹,

Downes

Weiß³

et al. 2010

A&A

View full text Add to dashboard Cite

Observations of 12 CO at high redshift indicate rapid metal enrichment in the nuclear regions of at least some galaxies in the early universe. However, the enrichment may be limited to nuclei that are synthesized by short-lived massive stars, excluding classical "secondary" nuclei like 13 C. Testing this idea, we used the IRAM Interferometer to tentatively detect the 13 CO J = 3 → 2 line at a level of 0.3 Jy km s −1 toward the Cloverleaf quasar at z = 2.5. This is the first observational evidence for 13 C at high redshift. The 12 CO/ 13 CO J = 3 → 2 luminosity ratio is with 40 +25 −8 much higher than ratios observed in molecular clouds of the Milky Way and in the ultraluminous galaxy Arp 220, but may be similar to that observed toward NGC 6240. Large Velocity Gradient models simulating seven 12 CO transitions and the 13 CO line yield 12 CO/ 13 CO abundance ratios in excess of 100. It is possible that the measured ratio is affected by a strong submillimeter radiation field, which reduces the contrast between the 13 CO line and the background. It is more likely, however, that the ratio is caused by a real deficiency of 13 CO. This is already apparent in local ultraluminous galaxies and may be even more severe in the Cloverleaf because of its young age ( < ∼ 2.5 Gyr). A potential conflict with optical data, indicating high abundances also for secondary nuclei in quasars of high redshift, may be settled if the bulk of the CO emission is originating sufficiently far from the active galactic nucleus of the Cloverleaf.

show abstract

“…Stutzki et al 1997). The [C ii] to bolometric infrared flux is also useful for constraining the FUV field (Wolfire et al 1989;Kaufman et al 1999), but is only useful towards LOSs with a single velocity component.…”

Section: Comparison With Pdr Model Calculationsmentioning

confidence: 99%

A sample of [C II] clouds tracing dense clouds in weak FUV fields observed byHerschel

Pineda¹,

Velusamy²,

Langer³

et al. 2010

A&A

View full text Add to dashboard Cite

The [C ii] fine-structure line at 158 μm is an excellent tracer of the warm diffuse gas in the ISM and the interfaces between molecular clouds and their surrounding atomic and ionized envelopes. Here we present the initial results from Galactic observations of terahertz C + (GOT C+), a Herschel key project devoted to studying the [C ii] emission in the Galactic plane using the HIFI instrument. We used the [C ii] emission, together with observations of CO, as a probe to understand the effects of newly formed stars on their interstellar environment and characterize the physical and chemical state of the star-forming gas. We collected data along 16 lines-ofsight passing near star-forming regions in the inner Galaxy near longitudes 330• and 20• . We identified fifty-eight 3.5 and 10 5.5 cm −3 and weak FUV strength (χ 0 = 1−10). We find two regions where our analysis suggest high densities >10 5 cm −3 and strong FUV fields (χ 0 = 10 4 −10 6 ), likely associated with massive star formation. We suggest that [C ii] emission in conjunction with CO isotopes is a good tool for differentiating regions of massive star formation (high densities/strong FUV fields) and regions that are distant from massive stars (lower densities/weaker FUV fields) along the line-of-sight.

show abstract

Atomic Carbon in M82: Physical Conditions Derived from Simultaneous Observations of the [C [CSC]i[/CSC]] Fine-Structure Submillimeter-Wave Transitions

Cited by 91 publications

References 23 publications

Neutral atomic carbon in centers of galaxies

Neutral atomic carbon in centers of galaxies

Weak¹³CO in the Cloverleaf quasar: evidence for a young, early generation starburst

A sample of [C II] clouds tracing dense clouds in weak FUV fields observed byHerschel

Contact Info

Product

Resources

About

Atomic Carbon in M82: Physical Conditions Derived from Simultaneous Observations of the [C [CSC]i[/CSC]] Fine-Structure Submillimeter-Wave Transitions

Cited by 91 publications

References 23 publications

Neutral atomic carbon in centers of galaxies

Neutral atomic carbon in centers of galaxies

Weak13CO in the Cloverleaf quasar: evidence for a young, early generation starburst

A sample of [C II] clouds tracing dense clouds in weak FUV fields observed byHerschel

Contact Info

Product

Resources

About

Weak¹³CO in the Cloverleaf quasar: evidence for a young, early generation starburst