Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds

Crawford, M. K.; Genzel, R.; Townes, C. H.; Watson, D. M.

doi:10.1086/163113

Cited by 232 publications

(241 citation statements)

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“…The line luminosity ratio of the [CII] and CO(1-0) detections for the SPT sources is ∼ 5200 ± 1800, which agrees with the first reported ratio by Crawford et al (1985). The values derived from the SPT sample are consistent with both low-z and high-z comparison samples, but with significantly smaller dispersion.…”

Section: Discussionsupporting

confidence: 86%

“…Crawford et al (1985) assumed [CII] excitation temperatures T ex, [CII] 92 K 10 , and could therefore apply the Rayleigh-Jeans approximation. This assumption was supported by independent estimates of the gas temperature of order ∼ 300 K using other fine-structure lines and assuming optically thin [CII] emission (Ellis & Werner 1984).…”

Section: Determining the Optical Depth Of The [Cii] Linementioning

confidence: 99%

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The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

147

223

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We present [CII] observations of 20 strongly lensed dusty star forming galaxies at 2.1 < z < 5.7 using APEX and Herschel. The sources were selected on their 1.4 mm flux (S 1.4 mm > 20 mJy) from the South Pole Telescope survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. Eleven out of 20 sources observed in [CII] also have low-J CO detections from ATCA. A comparison with midand high-J CO lines from ALMA reveals consistent [CII] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [CII], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [CII] to CO(1-0) luminosity ratios in the SPT sample of 5200 ± 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [CII] and CO emitting gas with a higher [CII] than CO excitation temperature, high CO optical depth τ CO (1-0) 1, and low to moderate [CII] optical depth τ [CII] 1. The geometric structure of photodissociation regions allows for such conditions.

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Section: Discussionsupporting

confidence: 86%

Section: Determining the Optical Depth Of The [Cii] Linementioning

confidence: 99%

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

147

223

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“…Figure 38 schematically illustrates the derived interstellar medium conditions in the central 500 pc (diameter) of the representative starburst galaxy NGC 253. The average conditions in the central regions of these starburst galaxies are far different from 17 Results have been obtained for M82 by Watson et al (1984), Crawford et al (1985), Lugten et al (1986), Wolfire et al (1990), Harris et al (1991), Schilke et al (1993), White et al (1994), Lord et al (1996), and and for NGC 253 and NGC 3256 by Aalto et al (1991a) [CII] 158 m HII region luminosity as a function of the electron density in the HII region (Carral et al, 1994). Thermal pressure equilibrium between the PDR and HII region is assumed, and the HII region is ionization bounded.…”

Section: Starburst Galactic Nucleimentioning

confidence: 96%

“…Hence the ratio of the far-red lines to the radio lines is sensitive to high-density (Ͼ10 5 cm Ϫ3 ) clumps, which become very warm (TϾ1000 K) when illuminated by a strong far-ultraviolet field (G 0 Ͼ10 5 ; Natta et al, 1994). Crawford et al (1985) and Stacey et al (1991) show a linear correlation in the observed integrated intensities of [CII] 158-m and 12 CO Jϭ1 -0 from bright dense galactic PDRs and PDRs in starburst galactic nuclei (see Fig. 32).…”

Section: E CI Recombination Linesmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

723

704

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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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“…PDRs contain ions of low ionisation potential, like C + , giving rise to the strong emission line [C II]λ 158µ. The emission is strongly correlated with H 2 [17] and can be used to estimate the H 2 mass. As an example we can have a look at IC 10 where Madden et al [99] speculate that, as a consequence of the strong UV field and low metallicity, small CO cores are formed, surrounded by extensive [C II] emitting regions containing H 2 .…”

Section: Gas Contentmentioning

confidence: 99%

Star Forming Dwarf Galaxies

Bergvall¹

2011

Astrophysics and Space Science Proceedings

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Star forming dwarf galaxies (SFDGs) have a high gas content and low metallicities, reminiscent of the basic entities in hierarchical galaxy formation scenarios. In the young universe they probably also played a major role in the cosmic reionization. Their abundant presence in the local volume and their youthful character make them ideal objects for detailed studies of the initial stellar mass function (IMF), fundamental star formation processes and its feedback to the interstellar medium. Occasionally we witness SFDGs involved in extreme starbursts, giving rise to strongly elevated production of super star clusters and global superwinds, mechanisms yet to be explored in more detail. SFDGs is the initial state of all dwarf galaxies and the relation to the environment provides us with a key to how different types of dwarf galaxies are emerging. In this review we will put the emphasis on the exotic starburst phase, as it seems less important for present day galaxy evolution but perhaps fundamental in the initial phase of galaxy formation.

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Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds

Cited by 232 publications

References 0 publications

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Photodissociation regions in the interstellar medium of galaxies

Star Forming Dwarf Galaxies

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