C + Emission from the Magellanic Clouds. I. The Bright H II Region Complexes N159 and N160

Israel, F. P.; Maloney, P. R.; Geis, N.; Herrmann, F.; Madden, S. C.; Poglitsch, A.; Stacey, G. J.

doi:10.1086/177458

Cited by 102 publications

(186 citation statements)

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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%

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Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

737

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

confidence: 79%

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.

737

712

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“…Characterizing unambiguously the ISM conditions thus requires the use of additional FIR cooling lines (such as [N ] or [O ]). In dwarf galaxies, the FIR lines were only detected by the KAO and ISO LWS in bright or Local Group dwarf galaxies (e.g., Poglitsch et al 1995;Israel et al 1996;Madden et al 1997;Hunter et al 2001). These studies found that the FIR lines are exceptionally bright compared to the dust emission.…”

Section: Introductionmentioning

confidence: 98%

“…This H 2 gas not traced by CO is known as the CO-dark gas (e.g., Wolfire et al 2010). Interpreting the FIR observations in terms of excitation led to the first evidence of such a reservoir of dark gas, not seen by CO but by C + (Poglitsch et al 1995;Israel et al 1996;Madden et al 1997). This demonstrates the potential of the FIR lines as calibrators of the dark gas at low metallicity and star formation tracers (De Looze et al 2014a) that could be used for high-redshift studies.…”

Section: Introductionmentioning

confidence: 99%

TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

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Context. The far-infrared (FIR) lines are important tracers of the cooling and physical conditions of the interstellar medium (ISM) and are rapidly becoming workhorse diagnostics for galaxies throughout the universe. There are clear indications of a different behavior of these lines at low metallicity that needs to be explored. Aims. Our goal is to explain the main differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies, and how this translates in ISM properties. ] 57 µm fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-L TIR ratios with L TIR , L TIR /L B , metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. Results. We find that the FIR lines together account for up to 3 percent of L TIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of Harboring compact phases of a low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that of metal-rich galaxies. Methods

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“…Previous observational studies of [C ii] emission from external galaxies include the statistical studies by Crawford et al (1985), Stacey et al (1991), and Malhotra et al (2001). More recently, the [C ii] emission from a few individual galaxies e.g., LMC (Israel et al 1996), M 51 (Nikola et al 2001;Kramer et al 2005), NGC 6946 (Madden et al 1993;Contursi et al 2002), M 83 (Kramer et al 2005), NGC 1313 (Contursi et al 2002), M 31 (Rodriguez-Fernandez et al 2006), and NGC1097 (Contursi et al 2002;Beirão et al 2010) has been observed. These papers explore the origin of the [C ii] emission.…”

Section: Introductionmentioning

confidence: 99%

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

Mookerjea

Krämer

Buchbender

et al. 2011

A&A

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ContextResults. The [C ii] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [C ii] observed with PACS and CO over the mapped region. There is even less spatial correlation between [C ii] and the atomic gas traced by H i. Detailed comparison of the observed intensities towards the H ii region with models of photo-ionization and photon-dominated regions, confirms that a significant fraction, 20-30%, of the observed [C ii] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio of [C ii] to the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the H ii region.

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C + Emission from the Magellanic Clouds. I. The Bright H II Region Complexes N159 and N160

Cited by 102 publications

References 0 publications

Photodissociation regions in the interstellar medium of galaxies

Photodissociation regions in the interstellar medium of galaxies

TheHerschelDwarf Galaxy Survey

TheHerschelM 33 extended survey (HerM33es): PACS spectroscopy of the star-forming region BCLMP 302

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