Submillimeter and far-infrared line observations of M17 SW - A clumpy molecular cloud penetrated by ultraviolet radiation

Stutzki, J.; Stacey, G. J.; Genzel, R.; Harris, A. I.; Jaffe, D. T.; Lugten, J. B.

doi:10.1086/166663

Cited by 191 publications

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“…The [C II] 158 μm line emission is widespread in this region and peaks at the northern bar and the southern bar (Fig. 14d), in a good agreement with previous observations (Stutzki et al 1988;Matsuhara et al 1989). Fig.…”

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confidence: 91%

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Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Okada

Kawada

Murakami

et al. 2010

A&A

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Aims. We investigate the structure of the interstellar medium (ISM) and identify the location of possible embedded excitation sources from far-infrared (FIR) line and mid-infrared continuum emission maps. Methods. We carried out imaging spectroscopic observations of four giant Galactic star-forming regions with the Fourier transform spectrometer (FTS) onboard AKARI. We obtained [O III] 88 μm and [C II] 158 μm line intensity maps of all the regions: G3.270-0.101, G333.6-0.2, NGC 3603, and M 17. Results. For G3.270-0.101, we obtained high-spatial-resolution [O III] 88 μm line-emission maps and a FIR continuum map for the first time, which imply that [O III] 88 μm emission identifies the excitation sources more clearly than the radio continuum emission. In G333.6-0.2, we found a local [O III] 88 μm emission peak, which is indicative of an excitation source. This is supported by the 18 μm continuum emission, which is considered to trace the hot dust distribution. For all regions, the [C II] 158 μm emission is distributed widely as suggested by previous observations of star-forming regions. Conclusions. We conclude that [O III] 88 μm emission traces the excitation sources more accurately than the radio continuum emission, especially where there is a high density and/or column density gradient. The FIR spectroscopy provides a promising means of understanding the nature of star-forming regions.

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confidence: 91%

“…14e,f). This indicates that the northern bar has a much lower column density than the southern bar (Elmegreen & Lada 1976;Stutzki et al 1988;Ando et al 2002;Wilson et al 2003) …”

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confidence: 99%

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Okada

Kawada

Murakami

et al. 2010

A&A

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“…The [CII] and [CI] lines in contrast originate from the lower-density interclump gas in the M17SW core. Figure 28 shows a schematic diagram of the derived morphology of M17SW from the PDR models and observations of Meixner et al Besides the M17SW photodissociation region, the [CII] and [CI] emission is extended over a size scale of Ӎ10 pc (Keene et al, 1985;Stutzki et al, 1988;Matsuhara et al, 1989). This emission may well be associated with clumps illuminated at large distances by far-ultraviolet radiation penetrating FIG.…”

Section: The Molecular Transition Observed In Edge-on Pdrsmentioning

confidence: 98%

“…12 This emission scale size is much larger than that expected for a homogeneous region at the density indicated by the line ratios. Figure 23 shows the observations of NGC 1977 compared with models of a ho-12 These include Stutzki et al, 1988;Matsuhara et al, 1989;Howe et al, 1991;White and Padman, 1991;Stacey et al, 1993;Jaffe et al, 1994;Plume et al, 1994 (Justtanont et al, 1997). f Temperatures derived from observations.…”

Section: Fig 22 the Luminosity In The [Cii] Andmentioning

confidence: 99%

“…Level populations and IR emission spectra have been calculated for a variety of model clouds. 14 Pure rotational spectra of H 2 have been calculated by Burton,13 See, for example, Gü sten and Fiebig, 1988;Massi et al, 1988;Stutzki et al, 1988;Stutzki and Gü sten, 1990;Tauber and Goldsmith, 1990;Chrysostomou et al, 1992Chrysostomou et al, , 1993Minchin et al, 1993;Hobson et al, 1994;Tauber et al, 1994 14 See Black and Dalgarno, 1976;Black and van Dishoeck, 1987; (Howe et al, 1991). The uniform-density model (nϭ3ϫ10 4 cm Ϫ3 ) has a far-ultraviolet attenuation length of 0.01 pc, while the clumped gas model corresponds to a far-ultraviolet attenuation scale length of 0.4 pc.…”

Section: B the H 2 Spectrummentioning

confidence: 99%

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Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

742

712

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The interstellar medium of galaxies is the reservoir out of which stars are born and into which stars inject newly created elements as they age. The physical properties of the interstellar medium are governed in part by the radiation emitted by these stars. Far-ultraviolet (6 eVϽh Ͻ13.6 eV) photons from massive stars dominate the heating and influence the chemistry of the neutral atomic gas and much of the molecular gas in galaxies. Predominantly neutral regions of the interstellar medium in which the heating and chemistry are regulated by far ultraviolet photons are termed PhotoDissociation Regions (PDRs). These regions are the origin of most of the non-stellar infrared (IR) and the millimeter and submillimeter CO emission from galaxies. The importance of PDRs has become increasingly apparent with advances in IR and submillimeter astronomy. The IR emission from PDRs includes fine structure lines of C, C ϩ , and O; rovibrational lines of H 2 ; rotational lines of CO; broad mid-IR features of polycyclic aromatic hydrocarbons; and a luminous underlying IR continuum from interstellar dust. The transition of H to H 2 and C ϩ to CO occurs within PDRs. Comparison of observations with theoretical models of PDRs enables one to determine the density and temperature structure, the elemental abundances, the level of ionization, and the radiation field. PDR models have been applied to interstellar clouds near massive stars, planetary nebulae, red giant outflows, photoevaporating planetary disks around newly formed stars, diffuse clouds, the neutral intercloud medium, and molecular clouds in the interstellar radiation field-in summary, much of the interstellar medium in galaxies. Theoretical PDR models explain the observed correlations of the [CII] 158 m with the CO Jϭ1 -0 emission, the CO Jϭ1 -0 luminosity with the interstellar molecular mass, and the [CII] 158 m plus [OI] 63 m luminosity with the IR continuum luminosity. On a more global scale, PDR models predict the existence of two stable neutral phases of the interstellar medium, elucidate the formation and destruction of star-forming molecular clouds, and suggest radiation-induced feedback mechanisms that may regulate star formation rates and the column density of gas through giant molecular clouds. [S0034-6861(99)01001-6] CONTENTS

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On the clumpy structure of molecular clouds

et al. 1993

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lko-dimensional hydrodynamic calculations for a self-gravitating, magnetic and compressible medium are carried out. The results based on numerical simulations show that the joint effect of the nonlinearity of the hydrodynamic equations and self-gravity is the mechanism for generating the observed complex structure of molecular clouds (eg. clumps and filaments). IR addition, parameters such as the evolution time of molecular clouds, the density contrast, fractal dimension, and the velocity probability distribution are derived. Their possible relation to the observed properties of molecular clouds are discussed.

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Submillimeter and far-infrared line observations of M17 SW - A clumpy molecular cloud penetrated by ultraviolet radiation

Cited by 191 publications

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Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Photodissociation regions in the interstellar medium of galaxies

On the clumpy structure of molecular clouds

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