ALMA reveals a chemically evolved submillimeter galaxy at<i>z</i>= 4.76

Nagao, Tohru; Maiolino, R.; Breuck, C. De; Caselli, P.; Hatsukade, Bunyo; Saigo, Kazuya

doi:10.1051/0004-6361/201219518

Cited by 101 publications

(149 citation statements)

References 46 publications

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“…Other parameters affecting this ratio include density and, to a lesser extent, the radiation field. Figure 4 shows the predictions of Nagao et al (2012) for both a low (navy) and a high (red) density, but only for a single ionization parameter log(U HII ) = −3.5. The [CII]/[NII] ratio of SPT2132-58 corresponds to a metallicity in the 0.5 to 1.5 Z range.…”

Section: Properties Of Ismmentioning

confidence: 99%

An ALMA view of the interstellar medium of thez= 4.77 lensed starburst SPT-S J213242-5802.9

Béthermin

Breuck

Gullberg

et al. 2016

A&A

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We present ALMA detections of the [NII] 205 μm and CO(12−11) emission lines, and the tentative detection of [CI] 3 P 1 − 3 P 0 for the strongly lensed (μ = 5.7 ± 0.5) dusty, star-forming galaxy SPT-S J213242-5802.9 (hereafter SPT2132-58) at z = 4.77. The [NII] and CO(12−11) lines are detected at 11.5 and 8.5σ levels, respectively, by our band 6 observations. The [CI] line is detected at 3.2σ after a reanalysis of existing band 3 data. The [CI] luminosity implies a gas mass of (3.8 ± 1.2) × 10 10 M , and, consequently, a very short depletion timescale of 34 ± 13 Myr and a CO luminosity to gas mass conversion factor α CO of 1.0 ± 0.3 M (K km s −1 pc 2 ) −1 . SPT2132-58 is an extreme starburst with an intrinsic star formation rate of 1100 ± 200 M /yr. We find a [CII]/[NII] ratio of 26 ± 6, which is the highest ratio reported at z > 4. This suggests that SPT2132-58 hosts an evolved interstellar medium (0.5 Z < Z < 1.5 Z ), which may be dominated by photodissociation regions. The CO(2−1) and CO(5−4) transitions have lower CO to far-infrared ratios than local and high-redshift samples, while CO(12−11) is similar to these samples, suggesting the presence of an additional very excited component or an active galactic nucleus.

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Section: Properties Of Ismmentioning

confidence: 99%

An ALMA view of the interstellar medium of thez= 4.77 lensed starburst SPT-S J213242-5802.9

Béthermin

Breuck

Gullberg

et al. 2016

A&A

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“…Recently, the Atacama Large Millimeter/ submillimeter Array (ALMA) has opened a new window, allowing us to exploit fine structure lines at rest-frame farinfrared (FIR) wavelengths to diagnose the ISM properties for these galaxy populations (e.g., Nagao et al 2012;Decarli et al 2014;Inoue et al 2016). The [C II]158 μm (  P P 2 3 2 2 1 2 ) is known to be the dominant coolant of the ISM and one of the brightest lines from star-forming galaxies in the FIR (e.g., Israel et al 1996).…”

Section: Introductionmentioning

confidence: 99%

ALMA Reveals Strong Emission in a Galaxy Embedded in a Giant Lyα Blob at z = 3.1

Umehata

Matsuda

Tamura

et al. 2017

ApJL

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe report the result from observations conducted with the Atacama Large Millimeter/submillimeter Array (ALMA) to detect [C II] 158 μm fine structure line emission from galaxies embedded in one of the most spectacular Lyα blobs (LABs) at z = 3.1, SSA22-LAB1. Of three dusty star-forming galaxies previously discovered by ALMA 860 μm dust continuum survey toward SSA22-LAB1, we detected the [C II] line from one, LAB1-ALMA3 at z = 3.0993±0.0004. No line emission was detected, associated with the other ALMA continuum sources or from three rest-frame UV/optical selected z spec ;3.1 galaxies within the field of view. For LAB1-ALMA3, we find relatively bright [C II] emission compared to the infrared luminosity (L emission could be causally related to the location within the giant LAB, although the relationship between extended Lyα emission and interstellar medium conditions of associated galaxies is yet to be understand.

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“…The gas fractions (fg) of SMGs are, on average, 30 − 50 per cent (Tacconi et al 2008;Riechers et al 2011;Bothwell et al 2013) based on CO observations and assuming a conversion from CO luminosity to MH 2 of αCO = 0.8 − 1.0 M⊙ (K km s −1 pc 2 ) −1 . The typical metallicities (Z) of SMGs are found to be Solar or slightly subSolar, albeit with uncertainties due to possible AGN contamination of emission lines (Swinbank et al 2004;Banerji et al 2011;Nagao et al 2012). The dust-to-metals ratio ηZ out to redshift 6 measured from absolute extinction and metal column densities for a sample of γ-ray burst afterglows and quasar foreground absorption systems is found to be approximately constant (Zafar & Watson 2013).…”

Section: Physical Properties Of Smgsmentioning

confidence: 93%

“…Observational studies show that SMGs typically have stellar masses of ∼ 10 11 M⊙ (e.g. Hainline et al 2011;Magnelli et al 2012), large dust masses (∼ 10 8−9 M⊙; Santini et al 2010;Magdis et al 2012; Simpson et al 2014), high gas fractions ⋆ E-mail:ker7@st-andrews.ac.uk (30 − 50 per cent; Tacconi et al 2008;Bothwell et al 2013) and Solar or sub-Solar metallicities (Swinbank et al 2004;Banerji et al 2011;Nagao et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The dust budget crisis in high-redshift submillimetre galaxies

Rowlands¹,

Gomez²,

Dunne³

et al. 2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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We apply a chemical evolution model to investigate the sources and evolution of dust in a sample of 26 high-redshift (z > 1) submillimetre galaxies (SMGs) from the literature, with complete photometry from ultraviolet to the submillimetre. We show that dust produced only by low-intermediate mass stars falls a factor 240 short of the observed dust masses of SMGs, the well-known 'dust-budget crisis'. Adding an extra source of dust from supernovae can account for the dust mass in 19 per cent of the SMG sample. Even after accounting for dust produced by supernovae the remaining deficit in the dust mass budget provides support for higher supernova yields, substantial grain growth in the interstellar medium or a top-heavy IMF. Including efficient destruction of dust by supernova shocks increases the tension between our model and observed SMG dust masses. The models which best reproduce the physical properties of SMGs have a rapid build-up of dust from both stellar and interstellar sources and minimal dust destruction. Alternatively, invoking a top-heavy IMF or significant changes in the dust grain properties can solve the dust budget crisis only if dust is produced by both low mass stars and supernovae and is not efficiently destroyed by supernova shocks.

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ALMA reveals a chemically evolved submillimeter galaxy atz= 4.76

Cited by 101 publications

References 46 publications

An ALMA view of the interstellar medium of thez= 4.77 lensed starburst SPT-S J213242-5802.9

An ALMA view of the interstellar medium of thez= 4.77 lensed starburst SPT-S J213242-5802.9

ALMA Reveals Strong Emission in a Galaxy Embedded in a Giant Lyα Blob at z = 3.1

The dust budget crisis in high-redshift submillimetre galaxies

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