An ALMA survey of the brightest sub-millimetre sources in the SCUBA-2–COSMOS field

Simpson, J. M.; Smail, Ian; Dudzevičiūtė, U.; Matsuda, Yoshihisa; Hsieh, B. C.; Wang, W. H.; Swinbank, A. M.; Stach, S. M.; An, Fang Xia; Birkin, Jack E.; Ao, Yiping; Bunker, Andrew J.; Chapman, Scott; Chen, Chian-Chou; Coppin, K. E. K.; Ikarashi, Soh; Ivison, R. J.; Mitsuhashi, Ikki; Saito, Tomoki; Umehata, Hideki; Wang, R.; Zhao, Yi

doi:10.1093/mnras/staa1345

Cited by 76 publications

(172 citation statements)

References 107 publications

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“…Our analysis is based on the multi-band photometric catalogue of 707 ALMA-located SMGs in the UKIDSS UDS field, constructed by Dudzevičiūtė et al (2020) from the original ALMA catalogue in Stach et al (2019). We provide a brief summary of the catalogue here and we refer the reader to those papers for the full details.…”

Section: Observations and Analysismentioning

confidence: 99%

“…The 707 SMGs have fluxes of 870 = 0.6-13.6 mJy, after removing the brightest source, which corresponds to a strongly-lensed SMG identifed by Ikarashi et al (2011). Dudzevičiūtė et al (2020) utilised the multi-band imaging of the UDS field gathered by Almaini et al (in prep. ) False colour images ( , and 3.6+4.5 m as the blue, green and red channels respectively) centred on example SMGs from our K-faint sample, with the cross-hair marking the position of the ALMA source in each field.…”

Section: Observations and Analysismentioning

confidence: 99%

“…SPIRE 250-500 m photometry was deblended using the ALMA sources (as well as radio and MIPS priors) following Swinbank et al (2014). Dudzevičiūtė et al (2020) employed the photoenergy balance modelling code (da Cunha et al 2015;Battisti et al 2019) to fit this multiband photometry. Derived parameters include photometric redshifts ( ), far-infared luminosities (8-1000 m, IR ), dust masses ( d ) and -band attenuation ( ), see Dudzevičiūtė et al (2020) for more details of the models and the extensive tests which were applied using both observed and simulated data.…”

Section: Sample Selectionmentioning

confidence: 99%

“…In this work we exploit a large ALMA SMG survey by Stach et al (2019) Almaini et al in prep.). Dudzevičiūtė et al (2020) published an analysis of the multiwavelength properties of these ALMAidentified SMGs. Here we focus on the subset of these SMGs that are faint or undetected in the very deep -band imaging ( AB = 25.3, 5 ) obtained for the UDS region by Almaini et al (in prep.…”

Section: Introductionmentioning

confidence: 99%

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An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies

Smail

Dudzevičiūtė

Stach

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We analyse a robust sample of 30 near-infrared-faint (KAB > 25.3, 5σ) submillimetre galaxies selected from a 0.96 deg2 field, to investigate their properties and the cause of their faintness in optical/near-infrared wavebands. Our analysis exploits precise identifications based on ALMA 870-μm continuum imaging, combined with very deep near-infrared imaging from the UKIDSS-UDS survey. We estimate that submillimetre galaxies with KAB > 25.3 mag represent 15 ± 2 per cent of the total population brighter than S870 = 3.6 mJy, with a potential surface density of ∼ 450 deg−2 above S870 ≥ 1 mJy. As such they pose a source of contamination in surveys for both high-redshift “quiescent” galaxies and very-high-redshift Lyman-break galaxies. We show that these K-faint submillimetre galaxies represent the tail of the broader submillimetre population, with comparable dust and stellar masses to KAB ≤ 25.3 mag submillimetre galaxies, but lying at significantly higher redshifts (z = 3.44 ± 0.06 versus z = 2.36 ± 0.11) and having higher dust attenuation (AV = 5.2 ± 0.3 versus AV = 2.9 ± 0.1). We investigate the origin of the strong dust attenuation and find indications that these K-faint galaxies have smaller dust continuum sizes than the KAB ≤ 25.3 mag galaxies, as measured by ALMA, that suggests their high attenuation is related to their compact sizes. We identify a correlation of dust attenuation with star-formation rate surface density (ΣSFR), with the K-faint submillimetre galaxies representing the higher-ΣSFR and highest-AV galaxies. The concentrated, intense star-formation activity in these systems is likely to be associated with the formation of spheroids in compact galaxies at high redshifts, but as a result of their high obscuration these galaxies are completely missed in UV, optical and even near-infrared surveys.

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Section: Observations and Analysismentioning

confidence: 99%

Section: Observations and Analysismentioning

confidence: 99%

Section: Sample Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies

Smail

Dudzevičiūtė

Stach

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…In this framework, a primary source of confusion stems from the relatively limited amount of information available for sizable samples of high-redshift galaxies, homogeneously selected on and above the main sequence. While a fine sampling of the far-IR spectral energy distribution (SED) has now become more accessible and a fundamental source to derive properties as the dust mass, temperature, and luminosity (e.g., Simpson et al 2014Simpson et al , 2020Scoville et al 2016;Dunlop et al 2017;Brisbin et al 2017;Strandet et al 2017;Franco et al 2018;Zavala et al 2018;Liu et al 2019b;Dudzevičiūtė et al 2020;Hodge & da Cunha 2020, to mention a few recent high-resolution surveys in the (sub)millimeter), direct spectroscopic measurements of the cold gas in distant galaxies remain remarkably time consuming. As a result, systematic investigations of the gas properties focused on either one line transition in large samples of galaxies (e.g., Le Fèvre et al 2020;Freundlich et al 2019;Tacconi et al 2018Tacconi et al , 2020, or several lines in sparser samples, often biased toward the brightest objects as (lensed) SMGs or quasars (e.g., Carilli & Walter 2013;Bothwell et al 2013;Spilker et al 2014;Yang et al 2017;Cañameras et al 2018;Dannerbauer et al 2019).…”

Section: Introductionmentioning

confidence: 99%

CO emission in distant galaxies on and above the main sequence

Valentino

Daddi

Puglisi

et al. 2020

A&A

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We present the detection of multiple carbon monoxide CO line transitions with ALMA in a few tens of infrared-selected galaxies on and above the main sequence at z = 1.1−1.7. We reliably detected the emission of CO (5 − 4), CO (2 − 1), and CO (7 − 6)+[C I](3P2 − 3P1) in 50, 33, and 13 galaxies, respectively, and we complemented this information with available CO (4 − 3) and [C I](3P1 − 3P0) fluxes for part of the sample, and by modeling of the optical-to-millimeter spectral energy distribution. We retrieve a quasi-linear relation between LIR and CO (5 − 4) or CO (7 − 6) for main-sequence galaxies and starbursts, corroborating the hypothesis that these transitions can be used as star formation rate (SFR) tracers. We find the CO excitation to steadily increase as a function of the star formation efficiency, the mean intensity of the radiation field warming the dust (⟨U⟩), the surface density of SFR (ΣSFR), and, less distinctly, with the distance from the main sequence (ΔMS). This adds to the tentative evidence for higher excitation of the CO+[C I] spectral line energy distribution (SLED) of starburst galaxies relative to that for main-sequence objects, where the dust opacities play a minor role in shaping the high-J CO transitions in our sample. However, the distinction between the average SLED of upper main-sequence and starburst galaxies is blurred, driven by a wide variety of intrinsic shapes. Large velocity gradient radiative transfer modeling demonstrates the existence of a highly excited component that elevates the CO SLED of high-redshift main-sequence and starbursting galaxies above the typical values observed in the disk of the Milky Way. This excited component is dense and it encloses ∼50% of the total molecular gas mass in main-sequence objects. We interpret the observed trends involving the CO excitation as to be mainly determined by a combination of large SFRs and compact sizes, as a large ΣSFR is naturally connected with enhanced dense molecular gas fractions and higher dust and gas temperatures, due to increasing ultraviolet radiation fields, cosmic ray rates, as well as dust and gas coupling. We release the full data compilation and the ancillary information to the community.

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In pursuit of giants

Donevski

Lapi

Małek

et al. 2020

A&A

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The dust-to-stellar mass ratio (Mdust/M⋆) is a crucial, albeit poorly constrained, parameter for improving our understanding of the complex physical processes involved in the production of dust, metals, and stars in galaxy evolution. In this work, we explore trends of Mdust/M⋆ with different physical parameters and using observations of 300 massive dusty star-forming galaxies detected with ALMA up to z ≈ 5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that Mdust/M⋆ evolves with redshift, stellar mass, specific star formation rates, and integrated dust size, but that evolution is different for main-sequence galaxies than it is for starburst galaxies. In both galaxy populations, Mdust/M⋆ increases until z ∼ 2, followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between Mdust/M⋆ and M⋆ holds up to z ≈ 5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that the Mdust/M⋆ in starbursts reflects the increase in molecular gas fraction with redshift and attains the highest values for sources with the most compact dusty star formation. State-of-the-art cosmological simulations that include self-consistent dust growth have the capacity to broadly reproduce the evolution of Mdust/M⋆ in main-sequence galaxies, but underestimating it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust-growth timescales relative to observations. The results of phenomenological models based on the main-sequence and starburst dichotomy as well as analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high Mdust/M⋆ is due to rapid dust grain growth in the metal-enriched interstellar medium. This work highlights the multi-fold benefits of using Mdust/M⋆ as a diagnostic tool for: (1) disentangling main-sequence and starburst galaxies up to z ∼ 5; (2) probing the evolutionary phase of massive objects; and (3) refining the treatment of the dust life cycle in simulations.

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An ALMA survey of the brightest sub-millimetre sources in the SCUBA-2–COSMOS field

Cited by 76 publications

References 107 publications

An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies

An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies

CO emission in distant galaxies on and above the main sequence

In pursuit of giants

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