The SCUBA HAlf Degree Extragalactic Survey - III. Identification of radio and mid-infrared counterparts to submillimetre galaxies

By R. Ivison, T. Greve, J. Dunlop, J. Peacock, E. Egami, I. Smail, E. Ibar, E. V. Kampen, I. Aretxaga, T. Babbedge and 28 more. 2007

225 citations recorded by the source corpus.

Determining an accurate position for a submillimetre (submm) galaxy (SMG) is the crucial step that enables us to move from the basic properties of an SMG sample – source counts and 2D clustering – to an assessment of their detailed, multiwavelength properties, their contribution to the history of cosmic star formation and their links with present-day galaxy populations. In this paper, we identify robust radio and/or infrared (IR) counterparts, and hence accurate positions, for over two-thirds of the SCUBA HAlf-Degree Extragalactic Survey (SHADES) Source Catalogue, presenting optical, 24-μm and radio images of each SMG. Observed trends in identification rate have given no strong rationale for pruning the sample. Uncertainties in submm position are found to be consistent with theoretical expectations, with no evidence for significant additional sources of error. Employing the submm/radio redshift indicator, via a parametrization appropriate for radio-identified SMGs with spectroscopic redshifts, yields a median redshift of 2.8 for the radio-identified subset of SHADES, somewhat higher than the median spectroscopic redshift. We present a diagnostic colour–colour plot, exploiting Spitzer photometry, in which we identify regions commensurate with SMGs at very high redshift. Finally, we find that significantly more SMGs have multiple robust counterparts than would be expected by chance, indicative of physical associations. These multiple systems are most common amongst the brightest SMGs and are typically separated by 2–6 arcsec, ~15–50/ sin i kpc at z∼ 2, consistent with early bursts seen in merger simulations.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

The n ature of submillimetre galaxies in cosmological hydrodynamic simulations (2009, background): “The major merger hypothesis is supported by the preponderance of close neighbours (e.g. Ivison et al. 2007) and their often disturbed morphologies (Menéndez-Delmestre et al. 2007; Tacconi et al. 2008).”
MOST SUBMILLIMETER GALAXIES ARE MAJOR MERGERS (2010, background): “Ivison et al. (2002, 2007) were able to show that SMGs have an increased likelihood of having close neighbours, suggestive of physical associations.”
A Herschel view of the far-infrared properties of submillimetre galaxies (2012, methodology): “These SCUBA sources were associated in Ivison et al. (2007) with their MAMBO counterparts (Greve et al. 2004).”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “D09 analyze 1.4 GHz radio emission from VLA observations (Ivison et al. 2007; Ibar et al. 2008) of 23185 galaxies from the Ultra-Deep Survey (UDS) portion of the United Kingdom Infrared Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS; Lawrence et al. 2007).”
A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “Excellent positional correspondence is certainly expected since, even for a 3.5-σ source, the predicted 1-σ uncertainty in RA and Dec given a beam-size of 0.7 arcsec (FWHM) is 0.085 arcsec, and the corresponding conservative 3-σ search radius is ' 0.25 arcsec (see Ivison et al. 2007).”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, background): “…per cent of the Great Observatories Origins Deep Survey-North (GOODS-N) 850-μm (Pope et al. 2006), GOODS-N 1.1-mm (Chapin et al. 2009), SHADES 850-μm (Ivison et al. 2007; Clements et al. 2008) and Great Observatories Origins Deep SurveySouth (GOODS-S) 1.1-mm (Yun et al. 2012) sources have multiple…”
Energetic galaxy-wide outflows in high-redshift ultraluminous infrared galaxies hosting AGN activity (2012, background): “However, part of the outflow c uld be obscured by material in the host galaxy, as is likely to be the case in clumpy and dusty systems such as high-redshift ULIRGs (e.g., Ivison et al. 2007; Tacconi et al. 2008; Engel et al. 2010).”
Evidence for a Population of High-Redshift Submillimeter Galaxies from Interferometric Imaging (2007, background): “…of the radio–dim sources above the locus of points from C05 is, as previous authors have speculated (e.g., Carilli & Yun 1999; Chapman et al. 2005; Pope et al. 2006; Ivison et al. 2007), consistent with either colder dust temperatures or a higher average/median redshift than the C05 sample.”
AzTEC millimetre survey of the COSMOS field – I. Data reduction and source catalogue (2008, methodology): “The fraction of AzTEC sources with potential radio counterparts (36 per cent) is consistent with that found in the SCUBA/SHADES survey (Ivison et al. 2007) of 30– 50 per cent, assuming the same limiting flux (45 μJy at 1.4 GHz), but is only marginally consistent (within 2σ , Poisson errors) with…”
The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies (2010, methodology): “…been applied in an attempt to trace the evolution of SMGs, using their optical/near-/mid-IR or FIR/radio SEDs (e.g. Carilli & Yun 1999; Smail et al. 2000; Ivison et al. 2004; Pope et al. 2005, 2006; Aretxaga et al. 2007; Ivison et al. 2007; Clements et al. 2008; Dye et al. 2008; Biggs et al. 2011).”
Cool Gas in High-Redshift Galaxies (2013, methodology): “Submillimeter galaxies were classically selected from the (sub–)millimeter maps obtained at 850 µm by SCUBA at the JCMT and at 1.2mm with MAMBO at the IRAM 30m (e.g. Smail et al. 1997, Hughes et al. 1998, Ivison et al. 2000, 2007, Dannerbauer et al. 2004).”
An ALMA survey of submillimetre galaxies in the Extended Chandra Deep Field South: high-resolution 870 μm source counts (2012, background): “For example, it has been claimed that the brightest (most luminous) SMGs evolve more strongly than fainter systems and hence are preferentially found at the highest redshifts (e.g., Ivison et al. 2002, 2007; Wall et al. 2008; Marsden et al. 2011; Smolčić et al. 2012).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “The advantage of matching submillimeter sources to radio counterparts is that radio sources are much more rare than optically-bright galaxies (Ivison et al., 2007).”
Testing the evolutionary link between submillimetre galaxies and quasars: CO observations of QSOs at z∼ 2 (2008, methodology): “Offsets of the CO emission from the radio position are given in Table 3, assuming that the source is unresolved using equation B2 in Ivison et al. (2007), and are less than 2 σ significant in most cases.”
The Subaru/XMM-Newton Deep Survey (SXDS). IV. Evolution of Lyα Emitters from z = 3.1 to 5.7 in the 1 deg2 Field: Luminosity Functions and AGN (2007, methodology): “The depth of MIPS data is ¼ 48 Jy (see Ivison et al. 2007).”
An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, background): “…redshift (z 2.5) ALMA SMGs tend to be detectable as μJy radio sources due to the strong correlation between the non-thermal radio and far-infrared emission in galaxies (e.g. Yun, Reddy & Condon 2001; Ivison et al. 2002, 2007; Vlahakis, Eales & Dunne 2007; Biggs et al. 2011; Hodge et al. 2013).”
The star formation history of K-selected galaxies (2008, methodology): “Various colour-selected samples have previously been stacked at 1,400 MHz: BzK (Daddi et al. 2005) and EROs (Georgakakis et al. 2006; Simpson et al. 2007; Ivison et al. 2007b).”
The Star Formation History of the Universe as Revealed by Deep Radio Observations (2008, background): “The size of this sample (in terms of area and number of sources) is well positioned between those fields of the similar area but are slightly deeper (by ∼ 40% e.g. the Lockman Hole and the HDFN, Biggs & Ivison 2006) and those of larger area (e.g. AEGIS and COSMOS, Ivison et al. 2007a; Schinnerer et ”
Scuba-2: Iterative map-making with the sub-millimetre user reduction facility (2013, background): “…of high-redshift submillimetre galaxies due to their low surface densities (compared with optical catalogues, for example), and a strong correlation between the radio and submillimetre emission mechanisms (e.g., Smail et al. 2000; Pope et al. 2006; Ivison et al. 2007; Chapin et al. 2009).”
An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, background): “…∼ 15–20′′) means that identifying the SMG counterparts has to date, relied on correlations between their sub-millimetre emission and that in other wavebands where higher spatial resolution is available (usually the radio and / or mid-infrared; e.g. Ivison et al. 2002, 2005, 2007; Pope et al. 2006).”