A survey of the Large Magellanic Cloud in the (C II) 158 micron line

Mochizuki, Kenji; Nakagawa, Takao; Doi, Yasuo; Yui, Yukari Y.; Okuda, H.; Shibai, Hiroshi; Yui, M.; Nishimura, Tetsuo; Low, F. J.

doi:10.1086/187432

Cited by 58 publications

(69 citation statements)

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“…Both the intensity (1.0 ± 0.3 × 10 −4 erg cm −2 s −1 sr −1 ) measured by Boreiko & Betz (1991) towards N11 B(CO) and their upper limit for N11 B(H 2 ) are in rather good agreement with our map results. Mochizuki et al (1994) measured a beam-averaged intensity 0.6 × 10 −4 erg cm −2 s −1 sr −1 in a 12.4 beam, roughly corresponding to the area mapped and shown in Fig. 1.…”

Section: Results and Analysismentioning

confidence: 85%

“…Because of its low ionisation potential of 11.3 eV, neutral carbon is the most abundant heavy element that can be ionised by the relatively unobstructed far-ultraviolet (FUV) radiation. Mochizuki et al (1994) have surveyed the whole LMC in the [C II] line at a relatively low resolution of 12.4 (corresponding to a linear resolution of 194 pc) with the balloon-borne facility BICE. Their survey reveals a number of bright, discrete [C II] sources in addition to extended emission.…”

Section: Introductionmentioning

confidence: 99%

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C⁺emission from the Magellanic Clouds

Israel

Maloney

2011

A&A

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Context. We study the λ 158 μm [C II] fine-structure line emission from star-forming regions as a function of metallicity. Aims. We have measured and mapped the [C II] emission from the very bright HII region complexes N 11 in the LMC and N 66 in the SMC; as well as the SMC H II regions N 25, N 27, N 83/N 84, and N 88 with the FIFI instrument on the Kuiper Airborne Observatory. Methods. In both LMC and SMC, the ratio of [C II] line to CO line and to the far-infrared continuum emission is much higher than seen almost anywhere else, including Milky Way star-forming regions, and whole galaxies. Results. In the low metallicity, low dust-abundance environment of the LMC and the SMC UV mean free path lengths are much greater than those in the higher-metallicity Milky Way. The increased photoelectric heating efficiencies cause significantly greater relative [C II] line emission strengths. At the same time, similar decreases in PAH abundances have the opposite effect by diminishing photoelectric heating rates. Consequently, in low-metallicity environments relative [C II] strengths are high but exhibit little further dependence on actual metallicity. Relative [C II] strengths are slightly higher in the LMC than in the SMC which has both lower dust and lower PAH abundances.

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Section: Results and Analysismentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

C⁺emission from the Magellanic Clouds

Israel

Maloney

2011

A&A

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“…A number of observations have been made of the Magellanic Clouds in CO, [CII] 158 m, and other PDR lines (e.g., Boreiko and Betz, 1991;Rubio et al, 1993aRubio et al, , 1993bMochizuki et al, 1994;Poglitsch et al, 1995;Israel et al, 1996;Stark et al, 1997). One of the major conclusions of this work is that the low metallicity in the Magellanic Clouds leads to a greater penetration of the far ultraviolet and a greater CO dissociation in molecular clumps.…”

Section: ϩ Halos Around Molecular Cores In the Magellanic Clouds Anmentioning

confidence: 79%

“…One of the major conclusions of this work is that the low metallicity in the Magellanic Clouds leads to a greater penetration of the far ultraviolet and a greater CO dissociation in molecular clumps. The result is that the ratio of [CII]/CO is on average 20 times the typical value in the Galactic plane (Mochizuki et al 1994), although there is considerable variation from point to point (Israel et al, 1996). Pak et al (1998) present [CII], H 2 , and CO observations of the Magellanic Clouds and model the giant molecular clouds in these galaxies as having larger column densities than Milky Way giant molecular clouds, with relatively small CO cores and extended [CII] halos.…”

Section: ϩ Halos Around Molecular Cores In the Magellanic Clouds Anmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

756

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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“…Nevertheless, Stacey et al (1991) found that even starburst galaxies, which have intense interstellar UV fields, cannot have [C ii]/ 12 CO J = 1-0 line intensity ratios higher than 5 10 3 (ratios when the mainbeam temperature scale is adopted for the CO intensity instead of the T * R scale). Line ratios exceeding this limit ([C ii]/CO > 10 4 ) have been observed on a galactic scale only toward irregular galaxies (Mochizuki et al 1994;Lord et al 1995;Madden et al 1997) and a few spirals in the Virgo cluster (Smith & Madden 1997).…”

Section: Introductionmentioning

confidence: 96%

Search for the [CII] 158 micron emission toward the blue compact dwarf galaxy I Zw 36

Mochizuki

Onaka

2001

A&A

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) and is at least one order of magnitude lower than those in irregular galaxies (I [C ii] /ICO 2 10 4 ) with low metallicities, in spite of the lower metallicity in I Zw 36 (12 + log[O/H] = 7.9) than in the irregulars. The observed difference in the line ratio between I Zw 36 and the irregulars can be accounted for by a higher gas density (10 3 cm −3 < ∼ nH < ∼ 10 4 cm −3 ) in I Zw 36, because the higher CO-formation rate at the higher density enables CO molecules to survive even against the photodissociation enhanced by the low dust abundance. The expected higher gas density in I Zw 36 may be related to change in large-scale gravitational potential with galactic evolution, if blue compact dwarfs and irregulars have evolutionary links.

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A survey of the Large Magellanic Cloud in the (C II) 158 micron line

Cited by 58 publications

References 0 publications

C⁺emission from the Magellanic Clouds

C⁺emission from the Magellanic Clouds

Photodissociation regions in the interstellar medium of galaxies

Search for the [CII] 158 micron emission toward the blue compact dwarf galaxy I Zw 36

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A survey of the Large Magellanic Cloud in the (C II) 158 micron line

Cited by 58 publications

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C+emission from the Magellanic Clouds

C+emission from the Magellanic Clouds

Photodissociation regions in the interstellar medium of galaxies

Search for the [CII] 158 micron emission toward the blue compact dwarf galaxy I Zw 36

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C⁺emission from the Magellanic Clouds

C⁺emission from the Magellanic Clouds