This article was accepted into the corpus but its outbound wikilinks were never NER-processed — typical at the deepest BFS hop or when the run's entity cap was reached. No expansion funnel to show.
| WEAVE | |
|---|---|
| Name | WEAVE |
| Caption | Wide-field multi-object spectrograph at the William Herschel Telescope |
| Location | La Palma |
| Altitude | 2395 m |
| Wavelength | Optical, near-infrared |
| Type | Multi-object spectrograph |
| Telescope | William Herschel Telescope |
| First light | 2019 (commissioning) |
| Operator | Isaac Newton Group of Telescopes |
| Collaborators | Leiden Observatory, Institute of Astronomy, Cambridge, University of Oxford, Rutherford Appleton Laboratory |
WEAVE WEAVE is a wide-field, multi-object spectroscopic facility deployed at the William Herschel Telescope on La Palma. It is designed to provide high-multiplex, moderate- to high-resolution spectroscopy to support large survey programs across stellar, Galactic, and extragalactic astronomy. The instrument integrates fibre positioning, dual-arm spectrographs, and data reduction systems to produce calibrated spectra for studies linked to missions and facilities such as Gaia, Euclid, SDSS, and LSST.
WEAVE is optimized for surveys requiring simultaneous spectroscopy of hundreds to thousands of targets within a single pointing, enabling follow-up of catalogues from Gaia, Pan-STARRS, UKIDSS, 2MASS, and radio surveys like LOFAR. Its operational model couples queue scheduling and survey-driven observing strategies used by facilities including VLT, Keck Observatory, Subaru Telescope, and AAT. The instrument supports community-led and consortium surveys analogous to programs at SDSS and DESI.
The instrument employs a robotic fibre positioner concept similar in function to systems used by 2dF and DESI, with a focal-plane architecture matched to the prime focus of the host telescope. Light from the telescope is fed via fibres into a pair of spectrographs, a blue arm and a red arm, following design principles from instruments such as AAOmega, Fibre Multi-Object Spectrograph, and HERMES. The spectrographs use volume-phase holographic gratings and dichroics comparable to those in X-shooter and UVES to deliver continuous coverage and selectable resolution modes inspired by Sloan Digital Sky Survey spectrographs.
WEAVE's focal plane supports several hundred deployable fibres plus dedicated integral-field units, combining multi-object spectroscopy with small integral-field capability in the style of MUSE and SAMI. Resolution modes span moderate (R~5000) to high (R~20,000) spectral resolving power, enabling chemical abundance work similar to programs undertaken with APOGEE, GALAH, and RAVE. Wavelength coverage extends from the blue optical to the red optical/near-infrared, overlapping bands used by Gaia's spectrophotometry and complementing spectroscopic windows exploited by HST and JWST in follow-up roles.
WEAVE supports Galactic archaeology, stellar astrophysics, extragalactic redshift surveys, and time-domain follow-up. For Galactic studies it targets samples derived from Gaia and Kepler/K2 to dissect Milky Way structure in the tradition of SEGUE and RAVE. Extragalactic programs include redshift surveys to probe large-scale structure akin to BOSS and eBOSS, and galaxy evolution studies that complement imaging from HST, Euclid, and LSST. Time-domain science leverages alerts from Zwicky Transient Facility and ATLAS for spectroscopic classification comparable to the follow-up strategies employed by Pan-STARRS transient programs.
The data reduction pipeline delivers wavelength-calibrated, sky-subtracted, flux-calibrated one-dimensional spectra and higher-level catalogs of redshifts, radial velocities, and elemental abundances, following workflows similar to pipelines developed for SDSS, Gaia-ESO Survey, and GALAH. Quality assurance and science archives are organized to interoperate with virtual observatory standards used by ESO, CADC, and STScI. Public data releases are planned on cadences resembling the release strategies of SDSS and Gaia to maximize community access and legacy value.
Operations are coordinated by the Isaac Newton Group of Telescopes with scientific leadership from European institutes including Leiden Observatory, University of Oxford, Cambridge University, and Rutherford Appleton Laboratory. The consortium model mirrors collaborative frameworks seen in projects such as SDSS, DESI, and LSST. Observing campaigns combine queued service observing and classical runs to serve survey efficiency while accommodating community proposals, integrating scheduling approaches used at WHT, VISTA, and AAT.
Conception and funding drew on expertise from instrument teams involved in AFOSC, AAOmega, and HERMES, with design reviews and prototype testing at partner institutes such as RAL and Leiden Observatory. Development milestones included laboratory integration of the spectrographs, fibre-positioner validation, and on-telescope commissioning phases paralleling timelines experienced by DESI and MUSE. The project progressed through staged commissioning in the late 2010s and early 2020s, aligning its survey plans with data influxes from missions like Gaia and observatories such as Pan-STARRS.
Category:Spectrographs Category:William Herschel Telescope instruments