GAS AND DUST IN A SUBMILLIMETER GALAXY AT<i>z</i>= 4.24 FROM THE<i>HERSCHEL</i>ATLAS

Cox, P.; Krips, M.; Neri, R.; Omont, A.; Güsten, R.; Menten, K. M.; Wyrowski, F.; Weiß, A.; Beelen, A.; Gurwell, M. A.; Dannerbauer, H.; Ivison, R. J.; Negrello, M.; Aretxaga, I.; Hughes, D. H.; Auld, Robbie Richard; Baes, M.; Blundell, R.; Buttiglione, S.; Cava, A.; Cooray, Asantha; Dariush, Aliakbar; Dunne, L.; Dye, S.; Eales, Stephen Anthony; Frayer, D. T.; Fritz, J.; Gavazzi, R.; Hopwood, R.; Ibar, E.; Jarvis, M. J.; Maddox, S.; Michałowski, M. J.; Pascale, Enzo; Pohlen, M.; Rigby, E. E.; Smith, D. J. B.; Swinbank, A. M.; Temi, P.; Valtchanov, I.; Werf, P. van der; Zotti, G. de

doi:10.1088/0004-637x/740/2/63

Cited by 168 publications

(190 citation statements)

References 72 publications

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“…Maiolino et al, 2005;Iono et al, 2006;Maiolino et al, 2009;Walter et al, 2009;Wagg et al, 2010;Stacey et al, 2010;Gallerani et al, 2012;Carniani et al, 2013), SMGs (e.g. Ivison et al, 2010d;Stacey et al, 2010;Cox et al, 2011;De Breuck et al, 2011;Swinbank et al, 2012;Wagg et al, 2012;George et al, 2013;Huynh et al, 2013) and normal star-forming galaxies (e.g. Graciá-Carpio et al, 2011) at high-redshift have all been detected in [CII].…”

Section: Atomic Linesmentioning

confidence: 99%

“…The data at moderate redshifts is from Farrah et al (2013) and Rigopoulou et al (2014). The high-z data is subdivided into quasars and SMGs, and comes from Cox et al (2011) Willott et al (2013) A number of studies have used extremely high resolution [CII] observations to constrain the size of the emitting region of high-z quasar host galaxies. Walter et al (2009) derived a source size of ∼ 1.5 kpc, and suggested that the galaxy was undergoing an Eddington-limited starburst event.…”

Section: [Cii] Morphologies and Dynamicsmentioning

confidence: 99%

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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: Atomic Linesmentioning

confidence: 99%

Section: [Cii] Morphologies and Dynamicsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…Seventeen have been added to the number of z > 4 [CII] detections in the past decade (Maiolino et al 2005(Maiolino et al , 2009Iono et al 2006;Wagg et al 2010;Ivison et al 2010;De Breuck et al 2011;Cox et al 2011;Swinbank et al 2012;Venemans et al 2012;Walter et al 2012;Riechers et al 2013;Wang et al 2013;Rawle et al 2014;De Breuck et al 2014;Neri et al 2014). Many of these objects have been selected based on the presence of a luminous active galactic nuclei (AGN; e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Maiolino et al 2005;Stacey et al 2010;Wang et al 2013), while others have been selected as starburst galaxies (e.g. Ivison et al 2010;Hailey-Dunsheath et al 2010;Stacey et al 2010;Cox et al 2011;Swinbank et al 2012;Walter et al 2012;Riechers et al 2013;Brisbin et al 2015). This leads to a heterogeneous sample of high-z [CII] detections, containing a mixture of AGN and starburst-dominated systems.…”

Section: Introductionmentioning

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

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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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“…Source-count models seem to need a redshift cutoff at ∼ 4 to explain 850 and 1100 µm counts (see section 12). The Herschel-Hermes survey detects plenty of z > 3 galaxies (eg Rowan-Robinson et al 2010) and Herschel-ATLAS has detected a z = 4.2 starburst galaxy (Cox et al 2011). But it still seems surprising that we have not detected more z > 4 submillimetre galaxies.…”

Section: Submillimetre Galaxiesmentioning

confidence: 75%

Panchromatic radiation from galaxies as a probe of galaxy formation and evolution

Rowan-Robinson

2011

Proc. IAU

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Abstract. I review work on modelling the infrared and submillimetre SEDs of galaxies. The underlying physical assumptions are discussed and spherically symmetric, axisymmetric, and 3-dimensional radiative transfer codes are reviewed. Models for galaxies with Spitzer IRS data and for galaxies in the Herschel-Hermes survey are discussed. Searches for high redshift infrared and submillimetre galaxies, the star formation history, the evolution of dust extinction, and constraints from source-counts, are briefly discussed.Keywords. infrared galaxies, radiative transfer, star formation Early work on radiative transfer models for infrared sourcesDuring the 1960s and early 1970s very simplistic models began to be developed for infrared sources associated with circumstellar dust shells, HII regions and star-forming regions. These models assumed that the dust grain density n(r) and temperature T(r) have a power-law dependence on radius r and that the dust is optically thin. Scattering was neglected and so the emission was simply calculated as a sum of n(r)Q ν B ν (T (r)), integrated over r.The first complete solution of the spherically symmetric radiative transfer problem for an optically thick dust cloud was by Leung (1975). He used detailed grain properties and carried out a full solution of the moment equations, including anisotropic scattering. The grain temperature was solved for by assuming radiative balance. Yorke & Krugel (1977) modelled the dynamical evolution of an HII region, including the interaction between gas and dust. Radiative transfer was approximated by diffusion. These two papers marked a tremendous step forward in the quality of models for infrared sources. To take advantage of numerical techniques which had been used in modelling stellar atmospheres, Leung essentially assumed that the radiation field is isotropic through most of the cloud (the Eddington approximation).Rowan-Robinson (1980) carried out a numerical solution of the full radiative transfer equation. The intensity, I ν (θ, r), was calculated throughout the cloud using a grid of values in ν, r, θ. This showed that the Eddington approximation is a poor assumption throughout a dust cloud and revealed the phenomenon of sideways beaming of the radiation field at the inner edge of cloud. Viewed from a distance a dust cloud surrounding a star should show a ring of bright emission in the mid infrared, coming from the inner edge of the dust cloud. A second interesting phenomenon revealed by a full solution of the radiative transfer equation is that of back radiation onto the star. The dust cloud radiates at the star and so the net spectrum of emission emerging from the star is no longer a blackbody, but has absorption bands at the wavelengths of dust emission features (Rowan-Robinson 1982). Rowan-Robinson & Harris (1982 applied this code to all the bright circumstellar dust shells in the AFGL survey. 446at https://www.cambridge.org/core/terms. https://doi

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GAS AND DUST IN A SUBMILLIMETER GALAXY ATz= 4.24 FROM THEHERSCHELATLAS

Abstract: We report ground-based follow-up observations of the exceptional source,

Cited by 168 publications

References 72 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

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

Panchromatic radiation from galaxies as a probe of galaxy formation and evolution

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