A 158 μm [C II] LINE SURVEY OF GALAXIES AT<i>z</i>∼ 1-2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE

Stacey, G. J.; Hailey-Dunsheath, S.; Ferkinhoff, Carl; Nikola, Thomas; Parshley, Stephen C.; Benford, Dominic J.; Staguhn, Johannes; Fiolet, N.

doi:10.1088/0004-637x/724/2/957

Cited by 340 publications

(633 citation statements)

References 121 publications

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“…Recent studies indicate that this ratio is a function of environment, with a low value (L [CII] /L FIR ~ 1 x 10 -4 ) for luminous systems dominated by a central black hole (quasars) and a high ratio (up to L [CII] /L FIR ~ 1 x 10 -2 ) for low-metallicity environments. Our relatively high ratio in L [CII] /L FIR is consistent with HDF850.1 being a high redshift star-forming system in a non-quasar environment 17 .…”

supporting

confidence: 85%

“…The resulting [CII]/FIR luminosity ratio of L [CII] /L FIR = 1.7 ± 0.5 x 10 -3 in HDF850.1 is comparable to what is found in normal local star-forming galaxies 17 , but is an order of magnitude higher than what is found in a z=6.42 quasar 10 , the only other high-z system where the [CII] emission could be resolved to date. Recent studies indicate that this ratio is a function of environment, with a low value (L [CII] /L FIR ~ 1 x 10 -4 ) for luminous systems dominated by a central black hole (quasars) and a high ratio (up to L [CII] /L FIR ~ 1 x 10 -2 ) for low-metallicity environments.…”

supporting

confidence: 62%

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The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Walter

Decarli

Carilli

et al. 2012

Nature

282

348

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The Hubble Deep Field (HDF) is a region in the sky that provides one of the deepest multi-wavelength views of the distant universe and has led to the detection of thousands of galaxies seen throughout cosmic time 1 . An early map of the HDF at a wavelength of 850 microns that is sensitive to dust emission powered by star formation revealed the brightest source in the field, dubbed HDF850.1 2 . For more than a decade, this source remained elusive and, despite significant efforts, no counterpart at shorter wavelengths, and thus no redshift, size or mass, could be identified 3-7 . Here we report, using a millimeter wave molecular line scan, an unambiguous redshift determination for HDF850.1 of z=5.183. This places HDF850.1 in a galaxy overdensity at z~5.2 in the HDF, corresponding to a cosmic age of only 1.1 Gyr after the Big Bang. This redshift is significantly higher than earlier estimates 3,4,6,8 and higher than most of the >100 sub-millimeter bright galaxies identified to date. The source has a star formation rate of 850 M sun yr -1 and is spatially resolved on scales of 5 kpc, with an implied dynamical mass of ~1.3x10 11 M sun , a significant fraction of which is present in the form of molecular gas. Despite our accurate redshift and position, a counterpart arising from starlight remains elusive.We have obtained a full frequency scan of the 3 mm band towards the HDF using the IRAM Plateau de Bure Interferometer (PdBI). The observations covered the frequency range from 80-115 GHz in 10 frequency settings at uniform sensitivity and at a resolution (~2.3") that is a good match to galaxy sizes at high redshift. They resulted in the detection of two lines of Carbon Monoxide (CO), the most common tracer for molecular gas at high redshift 9 , at 93.20 GHz and 111.84 GHz at the position of HDF850.1. Identifying these lines with the J=5 and J=6 rotational transitions of CO gives a redshift for HDF850.1 of z=5.183. This redshift was then unambiguously confirmed by the PdBI detection of the 158 μm line of ionized carbon ([CII], redshifted to 307.38 GHz), one of the main cooling lines of the star-forming interstellar medium. Stacking of other molecules covered by our frequency scan that trace higher volume densities did not lead to a detection (see Supplementary Information). Subsequently, the J=2 line of CO has also been detected using the NRAO Jansky Very Large Array (Jansky VLA) at 37.29 GHz. The observed [CII] and CO spectra towards HDF850.1 are shown in Fig. 1.The beamsize of our CO observations (~2.3", 15 kpc at z=5.183) is too large to spatially resolve the molecular gas emission in HDF850.1. However the [CII] and underlying continuum observations (~1.2" x 0.8") show that the source is extended (hitherto, the interstellar medium has been spatially resolved only in extremely rare quasar host galaxies at such high redshift 10 ). A single Gaussian fit yields a deconvolved size of 0.9±0.3", or 5.7±1.9 kpc at the redshift of the source. Fig. 2 shows the maps of total [CII] emission (left) as well as the red-and blue-...

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supporting

confidence: 85%

supporting

confidence: 62%

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Walter

Decarli

Carilli

et al. 2012

Nature

282

348

View full text Add to dashboard Cite

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“…Luminous quasar host galaxies (e.g. 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.…”

Section: Atomic Linesmentioning

confidence: 99%

“…Graciá-Carpio et al, 2011) at high-redshift have all been detected in [CII]. The line is thought to be an important coolant in the ISM, and can make up as much as 1% of the far infrared luminosity of a galaxy (Nikola et al, 1998;Malhotra et al, 2001;Stacey et al, 2010). However, the sites of origin of [CII] emission can be diverse, and thus its power as a diagnostic for the physical conditions in the ISM of early Universe galaxies is still debated.…”

Section: Atomic Linesmentioning

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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Radio Studies of Galaxy Formation: Dense Gas History of the Universe

Carilli

Walter

Riechers

et al. 2011

Reviews in Modern Astronomy

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Deep optical and near-IR surveys have traced the star formation history of the Universe as a function of environment, stellar mass, and galaxy activity (AGN and star formation), back to cosmic reionization and the first galaxies (z ∼ 6 to 8). While progress has been truly impressive, optical and near-IR studies of primeval galaxies are fundamentally limited in two ways: (i) obscuration by dust can be substantial for rest-frame UV emission, and (ii) near-IR studies reveal only the stars and ionized gas, thereby missing the evolution of the cool gas in galaxies, the fuel for star formation. Line and continuum studies at centimeter through submillimeter wavelengths address both these issues, by probing deep into the earliest, most active and dust obscured phases of galaxy formation, and by revealing the molecular and cool atomic gas. We summarize the techniques of radio astronomy to perform these studies, then review the progress on radio studies of galaxy formation. The dominant work over the last decade has focused on massive, luminous starburst galaxies (submm galaxies and AGN host galaxies). The far infrared luminosities are ∼ 10 13 L ⊙ , implying star formation rates, SFR ≥ 10 3 M ⊙ year −1 . Molecular gas reservoirs are found with masses: M(H 2 ) > 10 10 (α/0.8) M ⊙ . The CO excitation in these luminous systems is much higher than in low redshift spiral galaxies. Imaging of the gas distribution and dynamics suggests strongly interacting and merging galaxies, indicating gravitationally induced, short duration (≤ 10 7 year) starbursts. These systems correspond to a major star formation episode in massive ⋆ The Very Large Array of the National Radio Astronomy Observatory, is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc -2 -galaxies in proto-clusters at intermediate to high redshift. Recently, radio observations have probed the more typical star forming galaxy population (SFR ∼ 10 2 M ⊙ year −1 ), during the peak epoch of Universal star formation (z ∼ 1.5 to 2.5). These observations reveal massive gas reservoirs without hyper-starbursts, and show that active star formation occurs over a wide range in galaxy stellar mass. The conditions in this gas are comparable to those found in the Milky Way disk. A key result is that the peak epoch of star formation in the Universe also corresponds to an epoch when the baryon content of star forming galaxies was dominated by molecular gas, not stars. We consider the possibility of tracing out the dense gas history of the Universe, and perform initial, admittedly gross, calculations. We conclude with a description and status report of the Atacama Large Millimeter Array, and the Expanded Very Large Array. These telescopes represent an order of magnitude, or more, improvement over existing observational capabilities from 1 GHz to 1 THz, promising to revolutionize our understanding of galaxy formation.

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A 158 μm [C II] LINE SURVEY OF GALAXIES ATz∼ 1-2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE

Cited by 340 publications

References 121 publications

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Dusty star-forming galaxies at high redshift

Radio Studies of Galaxy Formation: Dense Gas History of the Universe

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