Rights statement: This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version Ian Smail, U Dudzevičiūtė, S M Stach, O Almaini, J E Birkin, S C Chapman, Chian-Chou Chen, J E Geach, B Gullberg, J A Hodge, S Ikarashi, R J Ivison, D Scott, Chris Simpson, A M Swinbank, A P Thomson, F Walter, J L Wardlow, P van der Werf, An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies, Monthly Notices of the Royal Astronomical Society, Volume 502, Issue 3, April 2021, Pages 3426–3435, https://doi.org/10.1093/mnras/stab283 is available online at: https://academic.oup.com/mnras/article-abstract/502/3/3426/6127308
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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
}
TY - JOUR
T1 - An ALMA survey of the S2CLS UDS field
T2 - optically invisible submillimetre galaxies
AU - Smail, Ian
AU - Dudzevičiūtė, U.
AU - Stach, S. M.
AU - Almaini, O.
AU - Birkin, J. E.
AU - Chapman, S. C.
AU - Chen, Chian-Chou
AU - Geach, J. E.
AU - Gullberg, B.
AU - Hodge, J. A.
AU - Ikarashi, S.
AU - Ivison, R. J.
AU - Scott, D.
AU - Simpson, Chris
AU - Swinbank, A. M.
AU - Thomson, A. P.
AU - Walter, F.
AU - Wardlow, J. L.
AU - van der Werf, P.
N1 - This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version Ian Smail, U Dudzevičiūtė, S M Stach, O Almaini, J E Birkin, S C Chapman, Chian-Chou Chen, J E Geach, B Gullberg, J A Hodge, S Ikarashi, R J Ivison, D Scott, Chris Simpson, A M Swinbank, A P Thomson, F Walter, J L Wardlow, P van der Werf, An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies, Monthly Notices of the Royal Astronomical Society, Volume 502, Issue 3, April 2021, Pages 3426–3435, https://doi.org/10.1093/mnras/stab283 is available online at: https://academic.oup.com/mnras/article-abstract/502/3/3426/6127308
PY - 2021/4/1
Y1 - 2021/4/1
N2 - We analyse a robust sample of 30 near-infrared-faint (KAB> 25.3, 5σ) submillimetre galaxies (SMGs) selected from a 0.96deg2 field to investigate their properties and the cause oftheir faintness in optical/near-infrared wavebands. Our analysisexploits precise identifications based on Atacama Large Millimeter Array(ALMA) 870-μm continuum imaging, combined with very deepnear-infrared imaging from the UKIDSS Ultra Deep Survey. We estimatethat SMGs with KAB > 25.3 mag represent 15 ± 2 percent of the total population brighter than S870 = 3.6 mJy,with a potential surface density of ∼450 deg-2 aboveS870 ≥ 1 mJy. As such, they pose a source of contaminationin surveys for both high-redshift 'quiescent' galaxies and very highredshift Lyman-break galaxies. We show that these K-faint SMGs representthe tail of the broader submillimetre population, with comparable dustand stellar masses to KAB ≤ 25.3 mag SMGs, but lying atsignificantly 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 investigatethe origin of the strong dust attenuation and find indications thatthese K-faint galaxies have smaller dust continuum sizes than theKAB ≤ 25.3 mag galaxies, as measured by ALMA, whichsuggests their high attenuation is related to their compact sizes. Weidentify a correlation of dust attenuation with star formation ratesurface density (ΣSFR), with the K-faint SMGsrepresenting the higher ΣSFR and highest AVgalaxies. The concentrated, intense star formation activity in thesesystems is likely to be associated with the formation of spheroids incompact galaxies at high redshifts, but as a result of their highobscuration these galaxies are completely missed in ultraviolet,optical, and even near-infrared surveys.
AB - We analyse a robust sample of 30 near-infrared-faint (KAB> 25.3, 5σ) submillimetre galaxies (SMGs) selected from a 0.96deg2 field to investigate their properties and the cause oftheir faintness in optical/near-infrared wavebands. Our analysisexploits precise identifications based on Atacama Large Millimeter Array(ALMA) 870-μm continuum imaging, combined with very deepnear-infrared imaging from the UKIDSS Ultra Deep Survey. We estimatethat SMGs with KAB > 25.3 mag represent 15 ± 2 percent of the total population brighter than S870 = 3.6 mJy,with a potential surface density of ∼450 deg-2 aboveS870 ≥ 1 mJy. As such, they pose a source of contaminationin surveys for both high-redshift 'quiescent' galaxies and very highredshift Lyman-break galaxies. We show that these K-faint SMGs representthe tail of the broader submillimetre population, with comparable dustand stellar masses to KAB ≤ 25.3 mag SMGs, but lying atsignificantly 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 investigatethe origin of the strong dust attenuation and find indications thatthese K-faint galaxies have smaller dust continuum sizes than theKAB ≤ 25.3 mag galaxies, as measured by ALMA, whichsuggests their high attenuation is related to their compact sizes. Weidentify a correlation of dust attenuation with star formation ratesurface density (ΣSFR), with the K-faint SMGsrepresenting the higher ΣSFR and highest AVgalaxies. The concentrated, intense star formation activity in thesesystems is likely to be associated with the formation of spheroids incompact galaxies at high redshifts, but as a result of their highobscuration these galaxies are completely missed in ultraviolet,optical, and even near-infrared surveys.
KW - galaxies: evolution
KW - galaxies: formation
KW - cosmology: observations
KW - submillimetre: galaxies
U2 - 10.1093/mnras/stab283
DO - 10.1093/mnras/stab283
M3 - Journal article
VL - 502
SP - 3426
EP - 3435
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -