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| UKIDSS Large Area Survey | |
|---|---|
| Name | UKIDSS Large Area Survey |
| Country | United Kingdom |
| Institution | Institute of Astronomy, University of Cambridge; Wide Field Camera team; United Kingdom Infrared Telescope |
| Project | UKIDSS |
| Wavelength | Near-infrared |
| Started | 2005 |
| Area | ~4,000 deg² |
| Bands | Y, J, H, K |
UKIDSS Large Area Survey. The UKIDSS Large Area Survey is a major near-infrared sky survey undertaken as part of UKIDSS with the United Kingdom Infrared Telescope at Mauna Kea, exploiting the Wide Field Camera on the United Kingdom Infrared Telescope to map thousands of square degrees in the Y band, J band, H band, and K band. The program was conceived by teams at the Institute of Astronomy (Cambridge), Imperial College London, and the University of Edinburgh to provide deep, wide-field data complementary to optical surveys such as the Sloan Digital Sky Survey and space missions like Spitzer Space Telescope and WISE.
The Large Area Survey forms one of the five constituent surveys of UKIDSS alongside the Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey, designed to address questions about the low-redshift Universe, Galactic structure, and rare object discovery. Its footprint overlaps legacy projects including SDSS Stripe 82, Pan-STARRS1, and areas imaged by 2MASS, enabling cross-matched catalogs for studies tied to Hubble Space Telescope follow-up and ground-based programs at Subaru Telescope and Very Large Telescope.
The survey used the Wide Field Camera (WFCAM) on the United Kingdom Infrared Telescope with four detectors arranged in a pawprint pattern to tile large areas efficiently, employing the Y band, J band, H band, and K band filters to reach depths between the 2MASS and deeper targeted fields like the Ultra Deep Survey. The design parameters—exposure time, jitter pattern, and microstepping—were optimized against sky background at Mauna Kea and instrumental characteristics from teams at Astronomical Society of the Pacific meetings and instrumentation groups associated with Royal Observatory, Edinburgh. Calibration strategies referenced standards tied to the United Kingdom Infrared Telescope photometric system and cross-calibration with SDSS photometry.
Observations were scheduled in blocks coordinated with observing semesters at UKIRT and processed through pipelines developed at the Cambridge Astronomical Survey Unit and the Wide Field Astronomy Unit at Edinburgh. Raw frames underwent dark subtraction, flat-fielding, sky subtraction, and astrometric calibration against catalogues such as 2MASS and SDSS DR7, with photometric solutions linked to standard stars employed by UKIRT observers. Data reduction incorporated artifact rejection informed by work from groups at Leiden Observatory and software practices described at conferences like the SPIE meetings and used database systems inspired by the VISTA Science Archive.
The survey delivered single-epoch and stacked image products, object catalogs with morphological classifications, and merged catalogs cross-matched with SDSS, 2MASS, and later WISE releases. Data releases were staged through the WFCAM Science Archive and the Wide Field Astronomy Unit with milestone releases in phases parallel to UKIDSS DR1, DR2, and subsequent incremental releases, enabling community access for investigators associated with facilities like Gemini Observatory and the Keck Observatory. Ancillary products included value-added photometric redshift catalogs used in programs tied to COSMOS and calibration datasets for Gaia crosschecks.
Primary goals included discovery of cool brown dwarfs analogous to objects catalogued by Gliese and Henry Draper Catalogue predecessors, identification of high-redshift quasars comparable to those found in SDSS high-redshift quasars, constraints on the low-mass end of the initial mass function in star-forming regions such as Orion and Pleiades, and mapping Galactic structure complementary to 2MASS analyses. Key results included discovery of late-type T and Y dwarf candidates followed up with spectroscopy at Keck Observatory and Gemini Observatory, identification of luminous quasars at redshifts overlapping samples from Sloan Digital Sky Survey and CFHT Legacy Survey, and contributions to studies of galaxy evolution that leveraged comparisons with Spitzer Space Telescope and Herschel Space Observatory datasets.
The project was managed by a consortium including the Institute of Astronomy (Cambridge), University of Leicester, University of Oxford, University of Edinburgh, and Imperial College London with observational support from the United Kingdom Infrared Telescope staff and data handling by the Wide Field Astronomy Unit and the Cambridge Astronomical Survey Unit. Oversight involved international collaborators who coordinated follow-up spectroscopy at facilities such as Keck Observatory, Gemini Observatory, and Subaru Telescope and engaged with survey science teams from SDSS and Pan-STARRS for joint science cases.
The Large Area Survey provided a bridge between all-sky surveys like 2MASS and deep pencil-beam surveys such as the Ultra Deep Survey, supplying targets for space missions including Spitzer Space Telescope and follow-up programs on Hubble Space Telescope and ground-based observatories including VLT and Subaru Telescope. Its catalogs have been widely cited in work on brown dwarf demographics, quasar luminosity functions, and Galactic structure analyses that also draw on Gaia astrometry, ensuring a lasting legacy in near-infrared observational astronomy and contributions to planning for future facilities such as the James Webb Space Telescope and the Vera C. Rubin Observatory.