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Large Binocular Telescope
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==Instruments== [[File:LBT Raid.jpg|thumb|Computer systems for LBT]] [[File:LBT Linux.jpg|thumb|Computer workstation for LBT]] Some current or planned LBT telescope instruments:<ref name="BBC"/> * LBC β optical and near ultraviolet wide field prime focus cameras. One is optimized for the blue part of the optical spectrum and one for the red. (Both cameras operational) * PEPSI β A high resolution and very high-resolution optical spectrograph and imaging polarimeter at the combined focus. (In development) * MODS β two optical multi object and longslit spectrographs plus imagers. Capable of running in a single mirror or binocular mode. (MODS1 operational β MODS2 in integration on the mountain) * LUCI β two [[Multi-Object Spectrometer|multi-object]] and [[Long-slit spectroscopy|longslit]] infrared spectrographs plus imagers, one for each side (associated with one of the 8m mirrors) of the telescope. The imager has 2 cameras and can observe in both seeing-limited and diffraction-limited (with adaptive optics) modes. End of commissioning and hand over to the LBTO was in 2018.{{citation needed|date=November 2018}} * LINC/Nirvana β wide-field interferometric imaging with adaptive optics at the combined focus (in commissioning). * LBTI/LMIRCAM β 2.9 to 5.2 micron [[Fizeau]] imaging and medium resolution grism spectroscopy at the combined focus. * LBTI/NOMIC β N band nulling imager for the study of protoplanetary and debris disks at the combined focus. (In commissioning phase β first stabilization of the fringes in December 2013) * FLAO β first light adaptive optics to correct atmospheric distortion * [[ARGOS (optics system)|ARGOS]] β multiple laser guide star unit capable of supporting ground layer or multi conjugate adaptive optics. End of commissioning and handover to LBTO was in 2018.<ref>{{Cite web|url=http://www.lbto.org/LBT%20Website%20General%20Public/Advanced%20Rayleigh%20guided%20Ground%20layer%20adaptive%20Optics%20System.htm |title=Advanced Rayleigh guided Ground layer adaptive Optics System |access-date=24 June 2015 |url-status=dead |archive-url=https://web.archive.org/web/20131102160628/http://www.lbto.org/LBT%20Website%20General%20Public/Advanced%20Rayleigh%20guided%20Ground%20layer%20adaptive%20Optics%20System.htm |archive-date= 2 November 2013 }}</ref> ===LUCI=== LUCI (originally LUCIFER: '''L'''arge Binocular Telescope Near-infrared Spectroscopic '''U'''tility with '''C'''amera and '''I'''ntegral '''F'''ield Unit for '''E'''xtragalactic '''R'''esearch) is the near-infrared instrument for the LBT.<ref name=planck>{{cite web |url=http://www.mpe.mpg.de/ir/lucifer/ |title=LUCI β A Near-Infrared Camera & Spectrograph for the LBT |publisher=Max Planck Institute for Extraterrestrial Physics |access-date=5 July 2016}}</ref><ref>{{cite web |first=Rebecca |last=Boyle |title = LUCIFER instrument helps astronomers to see through darkness observable remote MOST objects |date=23 April 2010 |url=http://www.popsci.com/science/article/2010-04/devil-named-telescope-helps-astronomers-see-through-darkness|access-date=29 September 2015}}</ref> <ref>{{cite web |url=http://www.astronomy.com/news/2010/04/lucifer-allows-astronomers-to-watch-stars-being-born |title=LUCIFER allows astronomers to watch stars being born |publisher=Astronomy Magazine β Kalmbach Publishing |access-date=5 July 2016 |date=23 April 2010 |author=University of Arizona}}</ref> The name of the instrument was changed to LUCI in 2012. LUCI operates in the 0.9β2.5 ΞΌm spectral range using a 2048 x 2048 element Hawaii-2RG detector array from Teledyne and provides imaging and spectroscopic capabilities in seeing- and diffraction-limited modes. In its focal plane area, long-slit and multi-slit masks can be installed for single-object and multi-object spectroscopy. A fixed collimator produces an image of the entrance aperture in which either a mirror (for imaging) or a grating can be positioned. Three camera optics with numerical apertures of 1.8, 3.75 and 30 provide image scales of 0.25, 0.12, and 0.015 arcsec/detector element for wide field, seeing-limited and diffraction-limited observations. LUCI is operated at cryogenic temperatures, and is therefore enclosed in a [[cryostat]] of 1.6 m diameter and 1.6 m height, and cooled to about β200 Β°C by two closed-cycle coolers.<ref name=planck/>
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