ner_tags: O O O O O O O O O O O O B-CelestialRegion O B-CelestialRegion I-CelestialRegion O O O B-CelestialObject O O B-Wavelength O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Wavelength O B-Wavelength O B-Telescope I-Telescope I-Telescope I-Telescope I-Telescope I-Telescope B-Telescope B-Wavelength B-Wavelength O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation O O O B-CelestialRegion I-CelestialRegion O O B-Citation I-Citation I-Citation I-Citation O B-Citation O O B-Citation I-Citation I-Citation I-Citation O O B-CelestialRegion I-CelestialRegion O O O O O O O O O O O B-Wavelength B-Wavelength B-Telescope B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O B-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation O O B-Survey I-Survey I-Survey I-Survey I-Survey I-Survey B-Survey O B-Person I-Person O B-Survey O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O B-Survey I-Survey I-Survey I-Survey I-Survey I-Survey I-Survey I-Survey I-Survey I-Survey B-Survey O B-Person I-Person O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O B-Wavelength O B-Wavelength O O O O O O B-Software I-Software B-Citation I-Citation I-Citation O O O O O O O O O O O O O O B-ObservationalTechniques I-ObservationalTechniques B-ObservationalTechniques O O O O B-Wavelength I-Wavelength O B-Wavelength I-Wavelength I-Wavelength O O O O O O O O B-ObservationalTechniques I-ObservationalTechniques B-ObservationalTechniques O O O O B-Telescope O O O O O O O O O O O O O O B-Telescope B-Wavelength O B-Telescope B-Wavelength O O O O O O O O O O O O O O O O O O O O O O B-CelestialRegion O B-CelestialRegion I-CelestialRegion O O O O O O O O O O O O O O O B-Survey B-Wavelength O O B-Wavelength O B-Wavelength O B-Wavelength O O O O O O O B-Telescope B-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O O O B-Survey I-Survey I-Survey I-Survey B-Survey O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O B-Wavelength I-Wavelength O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Wavelength B-Wavelength O O O B-CelestialRegion I-CelestialRegion O O O B-Dataset I-Dataset I-Dataset O O B-Survey I-Survey B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O B-CelestialRegion I-CelestialRegion O B-Wavelength O O O O B-Dataset I-Dataset I-Dataset O O B-Survey I-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey I-Survey B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Survey B-Citation I-Citation I-Citation O B-Citation O B-Survey I-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation O B-Survey I-Survey I-Survey B-Survey B-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation O B-Citation O O O B-CelestialRegion I-CelestialRegion O B-CelestialRegion
tokens: ratio 3.5. This process resulted in 726 and 1088 sources in the COSMOS and UDS fields, respectively. The source S2CLSJ021830-053130 with an 850m flux of 50mJy is the lensed candidate discussed by Ikarashi etal. ( 2011 ). 2.2 Radio and mid-infrared The Karl G. Jansky Very Large Array (VLA) 1.4GHz radio data were taken from Schinnerer etal. ( 2007 , 2010 ) for the COSMOS field, and from Ivison etal. ( 2005 , 2007 ) and Arumugam etal. (in preparation) for the UDS field. The catalogues include sources for which 3 detections were obtained. The mid-infrared (mid-IR) Spitzer (Fazio etal. 2004 ; Rieke etal. 2004 ; Werner etal. 2004 ) data are from the Spitzer Extended Deep Survey (SEDS; Ashby etal. 2013 ), the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH, PI: P. Capak), the S-COSMOS project (Sanders etal. 2007 ; Le Floch etal. 2009 ) and the Spitzer Public Legacy Survey of the UKIDSS Ultra Deep Survey (SpUDS; PI: J. Dunlop) 2 described in Caputi etal. ( 2011 ). To obtain the 3.6 and 4.5m photometry, we used the de-confusion code T-PHOT 3 (Merlin etal. 2015 ). This utilizes prior information on the positions and morphologies of objects from a high-resolution image (HRI; in this case the K -band or K s -band images) to construct a model of a given low-resolution image (LRI; in this case the Spitzer imaging) while solving for the fluxes of these objects. The 3 depths of the VLA radio and Spitzer mid-IR imaging in both fields are summarized in Table 1 . Table 1. The 3 depths of the multifrequency data used in the COSMOS and UDS fields. Note. a The two alternative values correspond to the shallower and deeper strips of the UltraVISTA near-IR imaging. 2.3 Optical and near-infrared The optical data in both fields were obtained with Subaru/SuprimeCam (Miyazaki etal. 2002 ), as described in Dye etal. ( 2006 ) and Furusawa etal. ( 2008 ), and from the CanadaFranceHawaii Telescope Legacy Survey (CFHTLS), as described in Bowler etal. ( 2012 ). The deep z -band images are described in Bowler etal. ( 2012 ) and Furusawa etal. ( 2016 ). The near-infrared (near-IR) data in the COSMOS field was obtained from Data Release 2 of the UltraVISTA survey (McCracken etal. 2012 ; Bowler etal. 2014 ), while in the UDS field the near-IR data were provided by Data Release 10 of the UKIRT Infrared Deep Sky Survey (UKIDSS; Lawrence etal. 2007 ; Cirasuolo etal. 2010 ; Fontana etal. 2014 ). In both fields, the optical and near-IR fluxes were measured in 3-arcsec diameter apertures, and the resulting 3 depths of this aperture photometry are summarized in Table 1 . Finally, we used a list of spectroscopic redshifts from 3D- HST (Brammer etal. 2012 ; Skelton etal. 2014 ; Momcheva etal. 2016 ), VIMOS Ultra-Deep Survey (VUDS; Le Fvre etal. 2015 ; Tasca etal. 2017 ), zCOSMOS (Lilly etal. 2007 , 2009 ), MOSFIRE Deep Evolution Field (MOSDEF; Kriek etal. 2015 ), PRIsm MUlti-object Survey (PRIMUS; Coil etal. 2011 ) and from Trump etal. ( 2009 , 2011 ) in the COSMOS field and UDSz