UDS Data Summary

The UDS is a deep infrared imaging survey, centred on the Subaru-XMM Deep Field (J0218-05). A survey area of 0.8 sq. degrees is achieved by tiling 4 observations with the UKIRT Wide-Field Camera. The UDS is the deepest J,H,K imaging survey to date over such a large area.

The DR11 release reaches median depths of J=25.6, H=25.1, K=25.3 (5σ, AB). This will be the final release of JHK data over the full UDS field. The infrared images and catalogues are available from the UDS DR11 information page, and the WFCAM Science Archive. Details of the key earlier releases are available at the tabs above for reference.

A preliminary 12-band photometric catalogue with photometric redshifts and stellar masses can be found here. An updated set of photometric redshifts is currently in preparation. Further details of the available multi-wavelength imaging and spectroscopy can be found below.

Multi Wavelength Imaging

The legacy value of the UDS survey is significantly enhanced by the rich array of multiwavelength data in this field. The key datasets are outlined below. Click on the facility for more information.


Facility Waveband Area (sq deg) Depth*
Chandra 0.5-10 keV 0.3 5x10-16 erg cm-2 s-1
XMM-Newton 0.5-10 keV 1.3 1x10-15 erg cm-2 s-1
CFHT Megaprime U-band 1.0 U=26.75
Subaru Suprimecam B, V, R, i', z' 1.3 B=27.6, V=27.2, R=27.0, i′=27.0, z′=26.0
VISTA Y 4.5 Y=24.6
HST WFC3 J, H 0.05 J,H ~ 27 (point source)
UKIRT WFCAM J, H, K 0.8 J=25.6, H=25.1, K=25.3
SPITZER IRAC/MIPS 3.6-24μm 0.8 [3.6, 4.5 μm]~ 24 AB (SpUDS), ~25.5 AB (SEDS)
Herschel SPIRE 100-500μm 0.7 ~11 mJy (100-500μm)
SCUBA2, AzTEC, ALMA 850μm/1.1mm 0.96 0.9 mJy/beam (1σ)
VLA 1.4 GHz 0.8 7 μJy/beam (1σ)

* Depths quoted are 5σ AB (2 arcsec) depths for optical/NIR wavelengths unless otherwise stated. Click for further information.

Spectroscopy

There have been several large specroscopic programmes observing the UDS field:

  • The UDSz ESO Large Programme obtained optical spectra for over 3000 K-band selected galaxies to a limit of K=23 (AB), using the VIMOS (R~200) and FORS2 (R~660) spectrographs.
  • The ESO VANDELS survey contains spectra for over ~700 galaxies in the UDS. Medium-resolution spectra (R~600) were obtained over the central 0.2 sq degrees (centred on the CANDELS HST region).
  • The northern half of the UDS field was observed within the VIPERS Large Programme, surveying galaxies to I<22.5 (AB), predominantly at z<1. Approximately 1000 secure redshifts were obtained within the UDS.
  • Several thousand low resolution grism spectra and redshifts are availble from the 3D-HST project.
In addition to the major projects above, many other groups have taken spectra in the UDS/SXDF region, including programmes led by Masayuki Akiyama (Subaru FOCAS and AAT 2dF), Chris Simpson (VLT VIMOS), Scott Croom (AAOmega) and Ian Smail (AAOmega). A number of published redshifts can also be found in Yamada et al. 2005, Simpson et al. 2006, Geach et al. 2007, van Breukelen et al. 2007, Ouchi et al. 2008, Smail et al. 2008 , Ono et al. 2010. A compilation of over 4000 of these additional redshifts can be found here, combining data from the projects led by Akiyama, Simpson, Croom, Geach, Smail and van Breukelen. Most of these are unpublished, and the reliability cannot be guaranteed. A description of the catalogue columns can be found here. Please note that this catalogue contains a high fraction of AGN. Many can be identified by cross-correlation with the X-ray and radio catalogues, or from listed spectroscopic features (where available).

Filter response curves

Citing UKIDSS when using UDS data

When you use UDS data please credit the efforts of those who built the camera and implemented the surveys. Wording similar to the following would be appreciated: 'The UKIDSS project is defined in Lawrence et al (2007). Further details on the UDS can be found in Almaini et al. (in prep). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Casali et al, 2007). The photometric system is described in Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in Irwin et al (in prep) and Hambly et al (2008)."

HST icon The central 0.3 sq degree of the UDS field were observed with the Chandra X-ray Observatory, with a total exposure time of 1.25Ms exposure. The limiting depth is approximately 5x10-16erg cm-2 s-1 (0.5-10 keV). Further details can be found in Kocevski et al. (2017).

2XMM icon X-ray data was obtained as part of the Subaru-XMM Deep Survey (SXDS). This is available from the XMM-Newton Survey Science Centre. There are 7 contiguous fields with a total exposure of 400ks. The catalogue of X-ray sources is available from the paper of Ueda et al. (2008). This is also provided here for convenience.

CFHT logo U-band data was obtained using CFHT Megaprime (PIs: Almaini & Foucaud), reaching a depth of U~26.75 (5σ). The U-band image resampled to the UDS K-band image frame are available here courtesy of David Maltby.


Subaru icon Deep Subaru imaging data is publicly available from the Subaru archive or from the SXDS DR1 release page. Details are provided in Furusawa et al. (2008). The 3-σ (AB) depths are B=28.4, V=27.8, R=27.7, i'= 27.7, z'= 26.7. Mosaics resampled to the UDS K-band image frame are available here courtesy of David Maltby.

spitzer icon The UDS region was included in the VISTA VIDEO survey (PI: Jarvis), which will add Y-band imaging to a depth of YAB~24.6 in addition to expanding the J,H,K coverage over 4.5 sq degrees to ~24AB.


HST icon The central 0.05 sq degrees of the UDS field was observed with HST WFC3 as part of the 900-orbit CANDELS HST Multi-cycle Treasury Program (PI: Faber). Point-source depths of ~27 (AB) were achieved in the F125W and F160W filters. Partially overlapping ACS imaging was also obtained in F606W and F814W.

spitzer icon The SpUDS Spitzer Legacy Survey (PI: Dunlop) observed the field using IRAC and MIPS, achieving depths of ~24AB (5σ) at 3.6 and 4.5μm, and ~300 μJy (15σ) at 24μm. Deeper IRAC data was obtained in the central 0.17 sq degree region as part of the SEDS project, reaching ~26AB at 3.6 and 4.5μm. The UDS field was also imaged using IRAC to ~25AB as part of the SPLASH survey.

spitzer icon The UDS was observed by the Herschel Space Observatory within the HerMES programme (PI: Oliver) using both PACS and SPIRE to a typical depth of ~11mJy (100-500μm). Data can be obtained from the NASA/IPAC archive.


JCMT Submillimetre data is available from the SCUBA2 Cosmology Legacy Survey. Source catalogues are published in Geach et al. (2017), and can be downloaded here. The submillimetre sources were subsequently observed with ALMA, as published in Stach et al. (2019). Maps and catalogues from the AzTEC 1.1mm survey are published in Austermann et al. (2010).

VLA icon VLA radio data has been obtained at 1.4 GHz using a combination of A, B and C configurations (PIs: Simpson & Ivison). The final combined VLA map is in preparation (contact Rob Ivison for details), reaching ~7 μJy per beam (rms) in the centre of the field. The 100μJy catalogue from the B/C-array data can be obtained from Simpson et al. (2006) .