An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation

Gullberg, B.; Smail, Ian; Swinbank, A. M.; Dudzevičiūtė, U.; Stach, S. M.; Thomson, A. P.; Almaini, O.; Chen, Chian-Chou; Conselice, Christopher J.; Cooke, Elizabeth A.; Farrah, D.; Ivison, R. J.; Maltby, David T.; Michałowski, M. J.; Simpson, J. M.; Scott, Douglas; Wardlow, J. L.; Weiß, A.

doi:10.1093/mnras/stz2835

Cited by 103 publications

(210 citation statements)

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“…We therefore keep the Sérsic index as a free parameter when fitting the F160W emission but fix the Sérsic index to match an exponential profile (n = 1) for the CO and dust emission. This choice of exponential profile is motivated by the exponential dust-continuum profiles observed for local (e.g., Haas et al 1998;Bianchi 2007;Muñoz-Mateos et al 2009;Bianchi & Xilouris 2011) and high-redshift galaxies (Barro et al 2016;Hodge et al 2016;Tadaki et al 2017a;Calistro Rivera et al 2018;Gullberg et al 2019). Fixing the profile shape for the CO and dust continuum has negligible impact on our conclusions because the half-light radii inferred when forcing n=1 are consistent, within errors, with the values inferred when n is a free parameter.…”

Section: Image-plane Analysismentioning

confidence: 71%

“…The extended dust-continuum emission of ALPS.2 differs not only from what is observed for ALPS.1 and 3, but also from other high-redshift galaxies (Figure 9). In most of these, the dust emission is 2-4 timesmore compact than the stellar emission, e.g., for SMGs the 870 μm half-light radii are typically measured to be 3 kpc, whereas the 1.6 μm emission can extend to 8 kpc (Hodge et al 2015(Hodge et al , 2019Simpson et al 2015;Chen et al 2017;Calistro Rivera et al 2018;Gullberg et al 2019;Lang et al 2019). However, based on observations and radiative transfer models of local galaxies, extended dust disks with sizes comparable to the size of the stellar disk are the norm (Xilouris et al 1999;Bianchi 2007;Muñoz-Mateos et al 2009;Holwerda et al 2012).…”

Section: Dust-continuum Versus Rest-frame Optical Sizesmentioning

confidence: 99%

“…Similarly, for quasar host galaxies at z6 (studied with lower-resolution observations), the dust-continuum sizes also appear z∼2-4 times more compact than those of the CO (Feruglio et al 2018;Wang et al 2019). The dust-continuum and rest-frame optical (but not CO) sizes have also been compared in detail for SMGs (Hodge et al 2016(Hodge et al , 2019Gullberg et al 2019;Lang et al 2019); six massive and compact star-forming galaxies at z∼2.5 (Barro et al 2016); a z∼1.25 starburst (Nelson et al 2019); and massive, Hαselected galaxies at z∼2.2-2.5 (Tadaki et al 2017a). These studies all find that the dust emission is 2-4 timesmore compact than the rest-frame optical emission.…”

Section: Introductionmentioning

confidence: 98%

“…Based on unresolved measurements, the long-wavelength (observedframe 850 μm), dust-continuum emission appears to trace the bulk of the cold, molecular gas in massive, star-forming galaxies as accurately as the traditional tracer, CO(1-0) (Scoville et al 2014;Kaasinen et al 2019). However, resolved observations indicate that the dust-continuum emission stems from a significantly more compact region than the CO emission (e.g., Hodge et al 2015;Simpson et al 2015;Chen et al 2017;Calistro Rivera et al 2018;Gullberg et al 2019), calling into question its application as a molecular gas tracer.…”

Section: Introductionmentioning

confidence: 99%

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A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Kaasinen

Walter

Novak

et al. 2020

ApJ

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We compare the extent of the dust, molecular gas, and stars in three star-forming galaxies, at z=1.4, 1.6, and 2.7, selected from the Hubble Ultra Deep Field based on their bright carbon monoxide (CO) and dust-continuum emission as well as their large rest-frame optical sizes. The galaxies have high stellar masses,  > M M 10 11 * , and reside on, or slightly below, the main sequence of star-forming galaxies at their respective redshifts. We probe the dust and molecular gas using subarcsecond Atacama Large Millimeter/submillimeter Array observations of the 1.3 mm continuum and CO line emission, respectively, and probe the stellar distribution using Hubble Space Telescope observations at 1.6 μm. We find that for all three galaxies the CO emission appears 30% more compact than the stellar emission. For the z=1.4 and 2.7 galaxies, the dust emission is also more compact, by 50%, than the stellar emission, whereas for the z=1.6 galaxy, the dust and stellar emission have similar spatial extents. This similar spatial extent is consistent with observations of local disk galaxies. However, most high-redshift observations show more compact dust emission, likely because of the ubiquity of central starbursts at high redshift and the limited sensitivity of many of these observations. Using the CO emission line, we also investigate the kinematics of the cold interstellar medium in the galaxies, and find that all three have kinematics consistent with a rotation-dominated disk.

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Section: Image-plane Analysismentioning

confidence: 71%

Section: Dust-continuum Versus Rest-frame Optical Sizesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

Kaasinen

Walter

Novak

et al. 2020

ApJ

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“…The blue ellipse illustrates the synthesized beam. 0.3 similar to the scale of dust emission in DSFGs (Simpson et al 2015;Gullberg et al 2019). We produce a second set of images with an outer taper of 0.8 to test if we are missing detections because they are resolved out in the higher resolution imaging and to confirm the reliability of source fluxes from the higher resolution maps.…”

Section: Almacal Data Reductionmentioning

confidence: 99%

ALMACAL VII: first interferometric number counts at 650 μm

Klitsch

Smail

Péroux

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Measurements of the cosmic far-infrared background (CIB) indicate that emission from many extragalactic phenomena, including star formation and black hole accretion, in the Universe can be obscured by dust. Resolving the CIB to study the population of galaxies in which this activity takes place is a major goal of submillimetre astronomy. Here, we present interferometric 650 μm submillimetre number counts. Using the Band 8 data from the ALMACAL survey, we have analysed 81 ALMA calibrator fields together covering a total area of 5.5 arcmin2. The typical central rms in these fields is ∼100 μJy beam−1 with the deepest maps reaching σ = 47 μJy beam−1 at sub-arcsec resolution. Multiwavelength coverage from ALMACAL allows us to exclude contamination from jets associated with the calibrators. However, residual contamination by jets and lensing remain a possibility. Using a signal-to-noise threshold of 4.5σ, we find 21 dusty, star-forming galaxies with 650 μm flux densities of ≥0.7mJy. At the detection limit we resolve ≃100 per cent of the CIB at 650 μm, a significant improvement compared to low-resolution studies at similar wavelength. We have therefore identified all the sources contributing to the EBL at 650 μm and predict that the contribution from objects with flux 0.7 mJy will be small.

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Molecular gas in theHerschel-selected strongly lensed submillimeter galaxies atz ~ 2–4 as probed by multi-JCO lines

Yang

Omont

Beelen

et al. 2017

A&A

141

227

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We present the IRAM-30 m observations of multiple-J CO (J up mostly from 3 up to 8) and [C I]( 3 P 2 → 3 P 1 ) ([C I](2-1) hereafter) line emission in a sample of redshift ∼ 2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [C I](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around J up ∼ 5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density n H 2 ∼ 10 2.5 -10 4.1 cm −3 and the kinetic temperature T k ∼ 20-750 K. The gas thermal pressure P th ranging from ∼ 10 5 K cm −3 to 10 6 K cm −3 is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with n H 2 ∼ 10 2.8 -10 4.6 cm −3 and T k ∼ 20-30 K, which is less correlated with star formation, and a high-excitation one (n H 2 ∼ 10 2.7 -10 4.2 cm −3 , T k ∼ 60-400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the J up ≥ 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2-1) lines follow the tight linear correlation between the luminosities of the [C I](2-1) and the CO(1-0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30) × 10 10 M , derived based on the CO(3-2) fluxes and α CO(1-0) = 0.8M ( K km s −1 pc 2 ) −1 , suggests a typical molecular gas depletion time t dep ∼ 20-100 Myr and a gas to dust mass ratio δ GDR ∼ 30-100 with ∼ 20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L CO /M dust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H 2 O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H 2 O lines are co-spatially located.

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An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation

Cited by 103 publications

References 72 publications

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2

ALMACAL VII: first interferometric number counts at 650 μm

Molecular gas in theHerschel-selected strongly lensed submillimeter galaxies atz ~ 2–4 as probed by multi-JCO lines

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