[ITAL]Infrared Space Observatory[/ITAL] Measurements of [C [CSC]ii[/CSC]] Line Variations in Galaxies

Malhotra, Sangeeta; Hélou, G.; Stacey, G. J.; Hollenbach, D. J.; Lord, S. D.; Beichman, Charles; Dinerstein, H. L.; Hunter, Deidre A.; Lo, K. Y.; Lu, N.; Rubin, R. H.; Silbermann, N. A.; Thronson, H. A.; Werner, M. W.

doi:10.1086/311044

Cited by 194 publications

(227 citation statements)

References 25 publications

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“…However, present-epoch ULIRGs emit roughly ∼ 10% of the expected [CII] flux, given their far infrared luminosities (e.g. Malhotra et al, 1997Malhotra et al, , 2001Luhman et al, 1998Luhman et al, , 2003. A variety of possible explanations have been posited for the apparent deficit.…”

Section: The [Cii]-fir Deficit In Galaxiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: The [Cii]-fir Deficit In Galaxiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…An interesting sidenote to the [CII] observations of the Galaxy are found in Malhotra et al (1997), who present ISO observations of L(CII)/L(far infrared) for a sample of 30 ''normal'' galaxies. They find that in twothirds of the cases the observed ratio is ϳ2 -7ϫ10 Ϫ3 , similar to the Galaxy.…”

Section: Energy Balance Of the Interstellar Gasmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

736

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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“…Given its high frequency (157.74 µm, corresponding to 1900.54 GHz) [CII] studies in the local universe are limited to airborne or satellite missions (e.g. Stacey et al 1991;Malhotra et al 1997;Madden et al 1997). These studies have demonstrated that this single line can indeed carry a good fraction of the total infrared luminosity (L FIR ) of an entire galaxy.…”

Section: Ionized Carbon ([Cii]) To the Rescue!mentioning

confidence: 99%

Detecting the most distant (z>7) objects with ALMA

Walter

Carilli

2007

Astrophys Space Sci

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Detecting and studying objects at the highest redshifts, out to the end of Cosmic Reionization at z > 7, is clearly a key science goal of ALMA. ALMA will in principle be able to detect objects in this redshift range both from high-J (J > 7) CO transitions and emission from ionized carbon, [CII], which is one of the main cooling lines of the ISM. ALMA will even be able to resolve this emission for individual targets, which will be one of the few ways to determine dynamical masses for systems in the Epoch of Reionization. We discuss some of the current problems regarding the detection and characterization of objects at high redshifts and how ALMA will eliminate most (but not all) of them.

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[ITAL]Infrared Space Observatory[/ITAL] Measurements of [C [CSC]ii[/CSC]] Line Variations in Galaxies

Cited by 194 publications

References 25 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Photodissociation regions in the interstellar medium of galaxies

Detecting the most distant (z>7) objects with ALMA

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