ALMA resolves turbulent, rotating [CII] emission in a young starburst galaxy at<i>z</i>= 4.8

Breuck, C. De; Williams, R. J.; Swinbank, A. M.; Caselli, P.; Coppin, K. E. K.; Davis, Timothy A.; Maiolino, R.; Nagao, Tohru; Smail, Ian; Walter, Fabian; Weiß, A.; Zwaan, M. A.

doi:10.1051/0004-6361/201323331

Cited by 121 publications

(141 citation statements)

References 117 publications

(198 reference statements)

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“…The peaks of the 345 GHz continuum for the four sources are detected at 7.4-8.3σ, with an optimized aperture size determined by using a curve of growth we recover between 44±3 and 81±12% of the integrated flux density measured from the low-resolution ALMA Cycle 0/1 observations (Swinbank et al 2012;De Breuck et al 2014;Simpson et al 2015a). This suggests that our maps are missing a fraction of the emission from the most extended low surface brightness dust on scales 200 kpc.…”

Section: Discussionmentioning

confidence: 74%

“…The ALMA Cycle 0 continuum observations of these SMGs were reported in Hodge et al (2013) (see Table 1) and revealed serendipitous detections of [C II] in ALESS 61.1 and ALESS 65.1, establishing the redshifts as z=4.4189 and z=4.4445, respectively (Swinbank et al 2012). The redshift of ALESS 73.1 was already known (z=4.756) and is also detected in [C II] emission from ALMA Cycle 0 observation De Breuck et al 2014).…”

Section: Samplementioning

confidence: 73%

“…To maximize the recovered flux, we applied an outer uvtaper of 350 kλ, resulting in our lowest-resolution maps of ∼1.3 kpc (see bottom row of Figure 1), which recover 80%-100% of the continuum flux detected in the ALMA Cycle 0/1 observations (Swinbank et al 2012;De Breuck et al 2014;Simpson et al 2015a, see Table 2). It is only for ALESS 73.1 that there is an indication that we are still resolving out some flux in these low-resolution maps, where we recover 80±5% of the flux detected in ALMA Cycle 0/1.…”

Section: Discussionmentioning

confidence: 99%

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The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

Gullberg

Swinbank

Smail

et al. 2018

ApJ

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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-pro t 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 present deep, high-resolution (0 03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C II] λ157.7 μm emission in four z∼4.4-4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 μm (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology-as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0 03) and depth of these observations (s~-27 47 345 GHz μJy beam −1 ). The four SMGs are bright [C II] emitters. We extract [C II] spectra from the high-resolution data, and recover ∼20%-100% of the [C II] flux and ∼40%-80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0 2 resolution, our maps recover ∼80%-100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C II] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 μm dust continuum by a factor of 1.6±0.4. By considering the [ ] L C II /L FIR ratio as a function of the star formation rate surface density (S SFR ), we revisit the [C II] deficit and suggest that the decline in the [ ] L C II /L FIR ratio as a function of S SFR is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.

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Section: Discussionmentioning

confidence: 74%

Section: Samplementioning

confidence: 73%

Section: Discussionmentioning

confidence: 99%

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The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

Gullberg

Swinbank

Smail

et al. 2018

ApJ

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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%

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

151

230

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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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“…However, evidence has been mixed regarding the frequency of mergers within the SMG population (e.g., Riechers et al 2008aRiechers et al , 2008bTacconi et al 2008;Davé et al 2010;Hayward et al 2011Hayward et al , 2013Swinbank et al 2011;Hodge et al 2012Hodge et al , 2013Hodge et al , 2015Aguirre et al 2013;Riechers et al 2013Riechers et al , 2014De Breuck et al 2014;Narayanan et al 2015;Sharon et al 2015). Independent of merger state, theoretical studies have found it necessary to invoke AGN-powered feedback to end the starbursts of massive galaxies (e.g., Somerville et al 2008).…”

Section: Introductionmentioning

confidence: 99%

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

Sharon

Riechers

Hodge

et al. 2016

ApJ

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133

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We present CO(1-0) observations obtained at the Karl G. Jansky Very Large Array for 14z 2 galaxies with existing CO(3-2) measurements, including 11 galaxies thatcontain active galactic nuclei (AGNs) and three submillimeter galaxies (SMGs). We combine this sample with an additional 15z 2 galaxies from the literature that have both CO(1-0) and CO(3-2) measurements in order to evaluate differences in CO excitation between SMGs and AGN host galaxies, tomeasure the effects of CO excitation on the derived molecular gas properties of these populations, and to look for correlations between the molecular gas excitation and other physical parameters. With our expanded sample of CO(3-2)/CO(1-0) line ratio measurements, we do not find a statistically significant difference in the mean line ratio between SMGs and AGN host galaxies as can be found in the literature; we instead find =  r 1.03 0. for both populations combined). We also do not measure a statistically significant difference between the distributions of the line ratios for these populations at the p=0.05 level, although this result is less robust. We find no excitation dependence on the index or offset of the integrated Schmidt-Kennicutt relation for the two CO lines, and weobtain indices consistent with N=1 for the various subpopulations. However, including low-z "normal" galaxies increases our best-fit Schmidt-Kennicutt index toÑ 1.2. While we do not reproduce correlations between the CO line width and luminosity, we do reproduce correlations between CO excitation and star-formation efficiency.

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ALMA resolves turbulent, rotating [CII] emission in a young starburst galaxy atz= 4.8

Cited by 121 publications

References 117 publications

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift

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

A Total Molecular Gas Mass Census in Z ∼ 2–3 Star-Forming Galaxies: Low-J Co Excitation Probes of Galaxies’ Evolutionary States

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