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The DESI Experiment Part II: Instrument Design

DESI CollaborationKorea Astronomy and Space Science InstituteAmir AghamousaUniversity of California [Berkeley]Aguilar, JessicaBoston University [Boston]Steve AhlenUniversity of EdinburghShadab AlamAllen, Lori E.Instituto de Astrofisica de CanariasCarlos Allende PrietoFermi National Accelerator LaboratoryJames AnnisLawrence Berkeley National Laboratory [Berkeley]S. BaileyLaboratoire de Physique Nucléaire et de Hautes ÉnergiesChristophe BallandInstitut de Física d’Altes Energies [Barcelone]O. BallesterYale University [New Haven]C. BaltayOhio State University [Columbus]L. BeauforeLawrence Berkeley National Laboratory [Berkeley]C. BebekThe University of Notre Dame [Sydney]Timothy C. BeersDepartment of Astronomy, University of MichiganEric F. BellInstitut de Ciencies del CosmosJosé Luis BernalRobert BesunerUniversity of PortsmouthFlorian BeutlerChris BlakeEcole Polytechnique Fédérale de LausanneHannes BleulerLaboratoire d'Astrophysique de MarseilleMichael BlomqvistRobert BlumNational Optical Astronomy ObservatoryA. BoltonCerro Tololo Inter-American ObservatoryCésar BriceñoDavid J. BrooksThe University of UtahJoel R. BrownsteinFermi National Accelerator LaboratoryE. Buckley‐GeerYale University [New Haven]A. BurdenInstitut de Recherches sur les lois Fondamentales de l'UniversE. BurtinAPC - CosmologieNicolás G. BuscaLawrence Berkeley National Laboratory [Berkeley]R. N. CahnYan-Chuan CaiInstitut de Física d’Altes Energies [Barcelone]L. Cardiel-SasR. G. CarlbergInstitut de Recherches sur les lois Fondamentales de l'UniversPierre-Henri CartonInstitut de Ciencies de l'Espai [Barcelona]R. CasasInstitut de Ciencies de l'Espai [Barcelona]F. J. CastanderCarreterra Mexico-TolucaJorge L. Cervantes–CotaLawrence Berkeley National Laboratory [Berkeley]T. ClaybaughMadeline CloseDepartment of Astronomy, The Ohio State UniversityCarl T. CokerShaun ColeJohan ComparatAndrew P. CooperCentre de Physique des Particules de MarseilleM.-C. CousinouInstitut de Ciencies de l'Espai [Barcelona]Martín CrocceLaboratoire d'Astrophysique de MarseilleJean-Gabriel CubyDaniel P. CunninghamT. M. DavisKyle S. DawsonUniversidad Nacional Autónoma de México = National Autonomous University of MexicoAxel de la MacorraJuan de VicenteEcole Polytechnique Fédérale de LausanneTimothée DelubacDepartment of Astronomy, The Ohio State UniversityMark DerwentArjun DeyGovinda DhunganaZhejie DingP. DoelYutong T. DuanCentre de Physique des Particules de MarseilleAnne EaletJerry EdelsteinUniversity of WyomingSarah EftekharzadehHarvard-Smithsonian Center for AstrophysicsDaniel J. EisensteinOhio State University [Columbus]Ann ElliottCentre de Physique des Particules de MarseilleS. EscoffierMatthew EvattLawrence Berkeley National Laboratory [Berkeley]Parker FagreliusArizona State University [Tempe]Xiaohui FanKevin FanningArya FarahiJay FarihiGinevra FavoleFeng YuEnrique FernandezUniversity of WyomingJoseph FindlayHarvard-Smithsonian Center for AstrophysicsDouglas P. FinkbeinerMichael J. FitzpatrickB. FlaugherSamuel FlenderLawrence Berkeley National Laboratory [Berkeley]Andreu Font-RiberaJ. E. Forero-RomeroInstitute for Astronomy [Honolulu]Pablo FosalbaCarlos S. FrenkMichele FumagalliBoris GaensickeGiuseppe GalloJ. García-BellidoInstitut de Ciencies de l'Espai [Barcelona]E. GaztañagaN. P. Gentile FusilloTerry GerardIrena GershkovichTommaso GiannantonioEcole Polytechnique Fédérale de LausanneDenis GilletGuillermo Gonzalez-De-RiveraCentre de Physique des Particules de MarseilleVioleta González-PérezShelby GottHarvard-Smithsonian Center for AstrophysicsOr GraurG. GutiérrezLaboratoire de Physique Nucléaire et de Hautes ÉnergiesJulien Guy

2016en

ABI

Annotatsiya

DESI (Dark Energy Spectropic Instrument) is a Stage IV ground-based dark energy experiment that will study baryon acoustic oscillations and the growth of structure through redshift-space distortions with a wide-area galaxy and quasar redshift survey. The DESI instrument is a robotically-actuated, fiber-fed spectrograph capable of taking up to 5,000 simultaneous spectra over a wavelength range from 360 nm to 980 nm. The fibers feed ten three-arm spectrographs with resolution $R= λ/Δλ$ between 2000 and 5500, depending on wavelength. The DESI instrument will be used to conduct a five-year survey designed to cover 14,000 deg$^2$. This powerful instrument will be installed at prime focus on the 4-m Mayall telescope in Kitt Peak, Arizona, along with a new optical corrector, which will provide a three-degree diameter field of view. The DESI collaboration will also deliver a spectroscopic pipeline and data management system to reduce and archive all data for eventual public use.

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Identifikatorlar

DOI: 10.48550/arxiv.1611.00037

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