DETECTION OF THE 158 μm [C II] TRANSITION AT
                    <i>z</i>
                    = 1.3: EVIDENCE FOR A GALAXY-WIDE STARBURST

Hailey-Dunsheath, S.; Nikola, Thomas; Stacey, G. J.; Oberst, Thomas E.; Parshley, Stephen C.; Benford, Dominic J.; Staguhn, Johannes; Tucker, C.

doi:10.1088/2041-8205/714/1/l162

Cited by 114 publications

(153 citation statements)

References 38 publications

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“…Hailey-Dunsheath et al, 2010;Wagg et al, 2010;De Breuck et al, 2011;Ferkinhoff et al, 2011;Swinbank et al, 2012;Coppin et al, 2012). These studies have found that at typical ULIRG luminosities, where local galaxies exhibit a clear [CII]/FIR deficit, some high-z SMGs appear to show a [CII] excess.…”

Section: The [Cii]-fir Deficit In Galaxiesmentioning

confidence: 92%

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: 92%

Dusty star-forming galaxies at high redshift

2014

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“…The physical parameters for the ISM in low-and high-z galaxies predicted by basic PDR models can be compared with observed data in a diagnostic diagram (Figure 12) first presented by Wolfire et al (1989) and updated by e.g. Stacey et al (1991aStacey et al ( , 2010 and Hailey-Dunsheath et al (2010). The diagram has the advantage of plotting ratios where the lensing magnification factors for high-z sources, beam-filling factors for low-z sources and filling factors for the PDRs (which are unknown, but assumed the same for [CII] and CO(1-0)) are divided out.…”

Section: Implications Of the Photodissociation Region Structurementioning

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

147

224

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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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“…The [C ] 157 µm line has been studied in a variety of objects, such as Galactic PDRs (e.g., Bennett et al 1994;Pineda et al 2013), normal spiral galaxies (Stacey et al 1991;Malhotra et al 1997;Negishi et al 2001;Brauher et al 2008), lowmetallicity galaxies (Poglitsch et al 1995;Madden et al 1997;Hunter et al 2001;Israel & Maloney 2011;Cigan et al 2015), ultra-luminous IR galaxies (ULIRG, Luhman et al 1998;Farrah et al 2013), and high-redshift galaxies (Maiolino et al 2009;Stacey et al 2010;Hailey-Dunsheath et al 2010;Swinbank et al 2012;De Breuck et al 2014). From those studies (see Genzel & Cesarsky 2000, for a review), the [C ] line emerges as the brightest cooling line of the ISM in star-forming galaxies and as a good tracer of the star formation activity, accounting for ∼0.1-1% of the FIR luminosity (e.g., Stacey et al 2010;Pierini et al 2003;Boselli et al 2002;De Looze et al 2011, 2014aSargsyan et al 2014).…”

Section: Introductionmentioning

confidence: 99%

TheHerschelDwarf Galaxy Survey

Cormier

Madden

Lebouteiller

et al. 2015

A&A

234

399

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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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DETECTION OF THE 158 μm [C II] TRANSITION AT z = 1.3: EVIDENCE FOR A GALAXY-WIDE STARBURST

Cited by 114 publications

References 38 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

TheHerschelDwarf Galaxy Survey

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