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| VLT/FLAMES | |
|---|---|
| Name | FLAMES |
| Caption | Fibre Large Array Multi Element Spectrograph at ESO's Paranal Observatory |
| Type | Multi-object spectrograph |
| Telescope | Unit Telescope 2 (Kueyen) |
| Location | Paranal Observatory, Atacama Desert, Chile |
| Institution | European Southern Observatory |
| First light | 2003 |
| Wavelength | 370–950 nm |
| Spectral resolution | 5,600–46,000 |
VLT/FLAMES VLT/FLAMES is a multi-object, intermediate- to high-resolution spectrograph installed on Unit Telescope 2 (Kueyen), part of the Very Large Telescope at Paranal Observatory in the Atacama Desert. The facility instrument was developed by a consortium led by the European Southern Observatory with partners including institutes from France, Italy, Germany, and United Kingdom, and it supports surveys across stellar, Galactic, and extragalactic fields. It has enabled large programs coordinated with facilities such as Hubble Space Telescope, Spitzer Space Telescope, and ground-based observatories like Subaru Telescope and Keck Observatory.
FLAMES provides multi-object spectroscopy using deployable fibre systems feeding the high-resolution spectrograph UVES and the medium-resolution spectrograph GIRAFFE. The instrument’s design choices were informed by predecessors and contemporaries including 2dF, DEIMOS, GMOS, MOSFIRE, and AAOmega. FLAMES has been central to large surveys such as the Gaia-ESO Survey, the FLAMES Tarantula Survey, and programs that complement missions like Gaia, CoRoT, and Kepler.
The instrument comprises the fibre positioner system called OzPoz mounted at the Nasmyth focus and the spectrographs UVES and GIRAFFE. OzPoz deploys 132 science fibres and 15 calibration fibres across a 25-arcminute field comparable to systems like VIMOS and FORS2. GIRAFFE offers multi-order echelle capabilities with spectral setups analogous to configurations used by HARPS and HIRES, while UVES provides cross-dispersed echelle coverage matching standards of McDonald Observatory instruments. Optical components trace heritage to manufacturers and institutes such as Observatoire de Paris, INAF, and Max Planck Institute for Astronomy.
FLAMES operates in simultaneous modes: a GIRAFFE-only multi-object mode, a UVES+GIRAFFE combined mode, and specific integral-field configurations comparable to SINFONI and MUSE in concept. Spectral resolution ranges from about 5,600 in low-resolution settings to ~46,000 with UVES, enabling radial velocity precision competitive with surveys like RAVE and APOGEE. Typical throughput and signal-to-noise performance depend on seeing at Paranal Observatory, airmass, and sky brightness akin to conditions quantified at La Silla Observatory and Cerro Tololo Inter-American Observatory.
FLAMES has driven major results in stellar astrophysics, Galactic archaeology, and extragalactic kinematics. Key programs include the Gaia-ESO Survey mapping chemical abundances in open clusters, the FLAMES Tarantula Survey probing massive stars in the Large Magellanic Cloud, and studies of globular clusters such as NGC 6397 and Omega Centauri. FLAMES data underpinned discoveries related to stellar rotation and multiplicity in projects involving ESO Large Programmes, constraints on stellar evolution used in models developed by groups at Geneva Observatory and Padova Astronomical Observatory, and dynamical mass measurements of dwarf galaxies like Sculptor and Fornax that inform work by teams associated with Max Planck Institute for Astronomy and Institute of Astrophysics of the Canary Islands.
Data reduction pipelines for GIRAFFE and UVES were developed drawing on software practices from ESO pipelines, with calibration strategies referencing methods used for SDSS and LAMOST. The reduction chain includes bias subtraction, flat-fielding, wavelength calibration with thorium-argon lamps similar to techniques at Keck Observatory, and sky subtraction tailored for fibre-fed systems like 2dF. Archive products are ingested into the ESO Science Archive Facility and have been cross-matched with catalogs from Gaia, 2MASS, WISE, Pan-STARRS, and Sloan Digital Sky Survey for legacy science.
FLAMES was proposed in the late 1990s as a next-generation instrument to complement the array of VLT instruments such as UVES, ISAAC, and FORS1/FORS2. The consortium included teams from Observatoire de Lyon, University of Bologna, Leiden Observatory, and Observatoire de Paris, coordinated through ESO. Commissioning campaigns occurred at Paranal Observatory with first-light operations in 2003, followed by integration into the VLT instrument program alongside upgrades to UT2 systems and observatory infrastructure.
FLAMES remains a product of multinational collaboration among European institutes and continues to be used in coordinated efforts with missions like Gaia and facilities such as ALMA, VISTA, and Chandra X-ray Observatory. Upgrades and maintenance have involved teams from INAF, CNRS, Max Planck Society, and observatory engineering groups at ESO, with software enhancements to pipelines and observing tools compliant with standards set by the International Virtual Observatory Alliance.
Category:European Southern Observatory instruments