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| UKIDSS Deep Extragalactic Survey | |
|---|---|
| Name | UKIDSS Deep Extragalactic Survey |
| Abbreviation | DXS |
| Survey | UKIDSS |
| Telescope | United Kingdom Infrared Telescope |
| Instrument | Wide Field Camera |
| Start | 2005 |
| Wavelength | Near-infrared |
| Area | ~35 deg² |
| Bands | J, H, K |
| Data release | Multiple |
UKIDSS Deep Extragalactic Survey is a near-infrared deep sky programme conducted as part of the United Kingdom Infrared Telescope's United Kingdom Infrared Deep Sky Survey, aiming to map extragalactic fields to faint magnitudes. The project linked observing efforts at the United Kingdom Infrared Telescope, coordinated survey planning at the Wide Field Camera (WFCAM), and produced catalogues used by researchers at institutions such as the University of Cambridge, the Institute of Astronomy, Cambridge, the University of Edinburgh, and the European Southern Observatory.
The survey was conceived within the framework of the United Kingdom Infrared Deep Sky Survey and executed using facilities at the Mauna Kea Observatories, leveraging instrumentation development involving teams from the United Kingdom Astronomy Technology Centre, the Royal Greenwich Observatory heritage, and collaborators at the Max Planck Society. The DXS targeted extragalactic fields overlapping legacy fields from the Sloan Digital Sky Survey, the Two Micron All Sky Survey, and the Spitzer Space Telescope programmes to enable cross-mission science, engaging researchers affiliated with the Royal Observatory, Edinburgh, the University of Oxford, the Imperial College London, and partners at the National Astronomical Observatory of Japan. The survey footprint, depth, and band selection were driven by scientific priorities established in workshops attended by scientists from the California Institute of Technology, the University of California, Berkeley, the Harvard–Smithsonian Center for Astrophysics, and the Max-Planck-Institut für Astronomie.
DXS design centered on deep imaging in the J and K bands using the Wide Field Camera (WFCAM) mounted on the United Kingdom Infrared Telescope. Instrument teams included engineers and scientists with links to the Science and Technology Facilities Council, the European Space Agency, and the National Aeronautics and Space Administration. The survey strategy adopted a tiling scheme informed by precedents set by surveys such as the VISTA Hemisphere Survey, the COSMOS survey, and the UKIDSS Large Area Survey, coordinating calibration with photometric standards tied to the Two Micron All Sky Survey and astrometry referenced to the Sloan Digital Sky Survey. Detector characteristics and readout modes were tested against requirements from groups at the University of Hawaii, the California Institute of Technology, and the Jet Propulsion Laboratory.
Observing blocks were scheduled at Mauna Kea Observatories to exploit seasonal conditions and minimize thermal background, with nightly operations managed by staff connected to the United Kingdom Infrared Telescope and visiting teams from the University of Durham, the University of Leicester, and the University of St Andrews. Data acquisition employed microstepping and interleaved dither patterns similar to those used in the UltraVISTA and UKIDSS Ultra Deep Survey projects, enabling background subtraction strategies developed in collaboration with scientists from the Max Planck Institute for Extraterrestrial Physics and the Institut d'Astrophysique de Paris. Pipeline processing and calibration used algorithms tested against reductions from the Sloan Digital Sky Survey and the 2MASS team, with data products generated by software groups affiliated with the Cambridge Astronomical Survey Unit, the Wide Field Astronomy Unit, and the Centre for Astrophysics Research.
Primary goals included measuring the evolution of the galaxy luminosity function, constraining the mass assembly of galaxies, and identifying high-redshift quasars and galaxy clusters, building on theoretical frameworks from groups at the Institute of Astronomy, Cambridge, the Max Planck Institute for Astrophysics, and the Kavli Institute for Cosmology. Key results encompassed robust measurements of the near-infrared luminosity function that informed models published by researchers at the University of Durham, the University of Oxford, and the European Southern Observatory; detections of massive galaxies at z~1–3 that were followed up with spectroscopy at the Keck Observatory, the Gemini Observatory, and the Very Large Telescope; and the identification of candidate high-redshift quasars later observed with the Subaru Telescope and the Hubble Space Telescope. Synergies were demonstrated with surveys such as the Sloan Digital Sky Survey, the Spitzer Space Telescope programmes, and the Herschel Space Observatory, enabling multiwavelength studies pursued by teams at the Harvard–Smithsonian Center for Astrophysics, the Max Planck Institute for Astronomy, and the Crafoord Prize-linked research groups.
DXS released calibrated catalogues, image stacks, and quality-assurance metrics through data releases coordinated by the Wide Field Astronomy Unit and archived in systems used by the Cambridge Astronomical Survey Unit, the VizieR collections accessed by researchers at the Centre de Données astronomiques de Strasbourg, and national data centers such as the Space Telescope Science Institute. Catalogues included photometry, astrometry, and flags matched to external catalogues from the Sloan Digital Sky Survey, the 2MASS project, and the Spitzer Space Telescope legacy products, facilitating cross-matching by investigators at the University of California, Santa Cruz, the University of Toronto, and the Max Planck Institute for Extraterrestrial Physics. Access policies mirrored those of contemporaneous surveys like the UKIDSS Large Area Survey and the UKIDSS Ultra Deep Survey, enabling use by research groups at the University of Edinburgh, the University of Manchester, and the Open University.
The legacy of the programme persists through its incorporation into multiwavelength studies combining data from the Sloan Digital Sky Survey, the Spitzer Space Telescope, the Herschel Space Observatory, and the Atacama Large Millimeter/submillimeter Array, providing target lists exploited by follow-up spectroscopy at the Keck Observatory, the Gemini Observatory, and the Very Large Telescope. The survey informed design choices for subsequent projects such as the VISTA Deep Extragalactic Observations and influenced survey strategy discussions at forums attended by delegations from the European Southern Observatory, the National Research Council (Canada), and the Max Planck Society. Ongoing archival science continues within groups at the University of Cambridge, the Imperial College London, and the University of Oxford, ensuring that the dataset contributes to studies of galaxy evolution, large-scale structure, and high-redshift active galactic nuclei pursued by international consortia including teams at the Harvard–Smithsonian Center for Astrophysics and the Kavli Institute for Cosmology.
Category:Astronomical surveys