The properties of the interstellar medium within a star-forming galaxy at z= 2.3

Danielson, A. L. R.; Swinbank, A. M.; Smail, Ian; Cox, P.; Edge, A. C.; Weiß, A.; Harris, A. I.; Baker, A. J.; Breuck, C. De; Geach, J. E.; Ivison, R. J.; Krips, M.; Lundgren, Andreas; Longmore, Steven N.; Neri, R.; Flaquer, B. Ocaña

doi:10.1111/j.1365-2966.2010.17549.x

Cited by 125 publications

(164 citation statements)

References 90 publications

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“…No emission is detected in this stack with a 1σ flux limit of 0.06 Jy km s -1 (assuming a linewidth of 400 km s -1 ). This non-detection is consistent with the few detections of dense molecular gas tracers in high-redshift objects that are significantly fainter than the CO emission [45][46][47][48][49][50][51][52][53][54] . Also, no stacked detection was achieved using different combinations of high density tracers (e.g.…”

Section: Stacking Of Fainter Lines In the Frequency Scansupporting

confidence: 86%

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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Section: Stacking Of Fainter Lines In the Frequency Scansupporting

confidence: 86%

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 lensing flux density enhancement has also allowed studies, for the first time at high redshifts, of the spectral line energy distributions (SLEDs) of 13 CO and C 18 O from J = 1 − 0 to J = 7 − 6 transitions of this galaxy Danielson et al (2013). The 13 CO emission from optically thin regions imply a total gas mass for the galaxy of ∼ 1.5 × 10 10 M and a conversion of CO to H 2 mass α CO ∼ 0.9, consistent with bright SMG-like DSFGs for a ULIRG system at z ∼ 2.…”

Section: Smm J2135-0102: the Cosmic Eyelashmentioning

confidence: 99%

“…In combination, Ivison et al (2010d) has suggested that the galaxy contains kpc-scale starburst clumps distributed over a large disk, different from nuclear starbursting local ULIRGS. Further PDR modeling using a combination of 12 CO, [CI], and HCN line intensities are presented in Danielson et al (2011).…”

Section: Smm J2135-0102: the Cosmic Eyelashmentioning

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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“…As the J transition increases, the peak of local emissivity occurs at lower and lower AV, which can then provide information about the state of PDRs in these conditions. Previous work presenting PDR analyses of molecular and atomic emission lines in DSFGs (e.g., Danielson et al 2011;Alaghband-Zadeh et al 2013) have generally used the well-known Kaufman et al (1999) PDR models. There are, however, a number of critical parameters that affect the PDR modelling results, which the Kaufman et al (1999) models do not account for.…”

Section: Pdr Modellingmentioning

confidence: 99%

ALMA observations of atomic carbon inz ∼ 4 dusty star-forming galaxies

Bothwell

Aguirre

Aravena

et al. 2016

Mon. Not. R. Astron. Soc.

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136

180

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We present ALMA [Ci](1−0) (rest frequency 492 GHz) observations for a sample of 13 strongly-lensed dusty star-forming galaxies originally discovered at 1.4mm in a blankfield survey by the South Pole Telescope. We compare these new data with available [Ci] observations from the literature, allowing a study of the ISM properties of ∼ 30 extreme dusty star-forming galaxies spanning a redshift range 2 < z < 5. Using the [Ci] line as a tracer of the molecular ISM, we find a mean molecular gas mass for SPTDSFGs of 6.6 × 10 10 M . This is in tension with gas masses derived via low-J 12 CO and dust masses; bringing the estimates into accordance requires either (a) an elevated CO-to-H 2 conversion factor for our sample of α CO ∼ 2.5 and a gas-to-dust ratio ∼ 200, or (b) an high carbon abundance X CI ∼ 7 × 10 −5 . Using observations of a range of additional atomic and molecular lines (including [Ci], [Cii], and multiple transitions of CO), we use a modern Photodissociation Region code (3d-pdr) to assess the physical conditions (including the density, UV radiation field strength, and gas temperature) within the ISM of the DSFGs in our sample. We find that the ISM within our DSFGs is characterised by dense gas permeated by strong UV fields. We note that previous efforts to characterise PDR regions in DSFGs may have significantly under-estimated the density of the ISM. Combined, our analysis suggests that the ISM of extreme dusty starbursts at high redshift consists of dense, carbon-rich gas not directly comparable to the ISM of starbursts in the local Universe.

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The properties of the interstellar medium within a star-forming galaxy at z= 2.3

Cited by 125 publications

References 90 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

ALMA observations of atomic carbon inz ∼ 4 dusty star-forming galaxies

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