<i>Euclid</i> preparation
W. GillardAix-Marseille Université, CNRS/IN2P3, CPPMT. MaciaszekCentre National d’Etudes Spatiales – Centre spatial de ToulouseÉric PrietoAix-Marseille Université, CNRS, CNES, LAMF. GruppUniversitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität MünchenA. CostilleAix-Marseille Université, CNRS, CNES, LAMK. JahnkęMax-Planck-Institut für AstronomieJ. D. ClemensAix-Marseille Université, CNRS/IN2P3, CPPMS DusiniINFN-PadovaM. CarleAix-Marseille Université, CNRS, CNES, LAMC SirignanoINFN-PadovaE. MedinaceliINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaS. LigoriINAF-Osservatorio Astrofisico di TorinoE. FranceschiINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaM. TrifoglioINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaWilliam BonAix-Marseille Université, CNRS, CNES, LAMR. BarbierCentre National de la Recherche ScientifiqueS. FerriolCentre National de la Recherche ScientifiqueA SecrounAix-Marseille Université, CNRS/IN2P3, CPPMN. AuricchioINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaPietro BattagliaINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaC. BonoliINAF-Osservatorio Astronomico di PadovaL. CorcioneINAF-Osservatorio Astrofisico di TorinoF HormuthFelix Hormuth EngineeringD. Le MignantAix-Marseille Université, CNRS, CNES, LAMG. MorganteINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaC. PadillaInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and TechnologyR. Toledo-MoreoUniversidad Politécnica de Cartagena, Departamento de Electrónica y Tecnología de ComputadorasL. ValenzianoINFN-BolognaR. BenderUniversitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität MünchenF.J CastanderInstitute of Space Sciences (ICE, CSIC), Campus UABP. B. LiljeInstitute of Theoretical Astrophysics, University of OsloA. BalestraINAF-Osservatorio Astronomico di PadovaClement BarrièreCEA-Saclay, DRF/IRFU, departement d’ingenierie des systemesMichel BerthéCommissariat à l'Énergie Atomique et aux Énergies AlternativesC. BoderndorfMax Planck Institute for Extraterrestrial PhysicsAnne BonnefoiAix-Marseille Université, CNRS, CNES, LAMV. CapobiancoINAF-Osservatorio Astrofisico di TorinoR. CasasInstitut d’Estudis Espacials de Catalunya (IEEC), Edifici RDITH. S. ChoJet Propulsion Laboratory, California Institute of TechnologyFranck DucretAix-Marseille Université, CNRS, CNES, LAMJean-Luc GimenezAix-Marseille Université, CNRS, CNES, LAMW. HolmesJet Propulsion Laboratory, California Institute of TechnologyA. HornstrupCosmic Dawn Center (DAWN)M. JhabvalaNASA Goddard Space Flight CenterE. JulloAix-Marseille Université, CNRS, CNES, LAMR. KohleyESAC/ESA, Camino Bajo del CastilloB. KubikCentre National de la Recherche ScientifiqueR. LaureijsEuropean Space Research and Technology CentreI. LloroSKA Observatory, Jodrell Bank, Lower WithingtonC. MacabiauUniversité Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822Y. MellierInstitut d’Astrophysique de ParisG PolentaSpace Science Data Center, Italian Space AgencyG. D. RaccaLeiden Observatory, Leiden UniversityA RenziINFN-PadovaM. SchirmerMax-Planck-Institut für AstronomieG. SeidelMax-Planck-Institut für AstronomieM. SeiffertJet Propulsion Laboratory, California Institute of TechnologyG. SirriINFN-Sezione di BolognaG. SmadjaCentre National de la Recherche ScientifiqueL StancoINFN-PadovaStefanie WachterCarnegie ObservatoriesH AusselUniversité Paris-SaclayT. AuphanAix-Marseille Université, CNRS/IN2P3, CPPMB. R. GranettINAF-Osservatorio Astronomico di BreraR. CharyUniversity of CaliforniaY. CopinUniversité Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822P. HudelotInstitut d’Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne UniversitéV. Le BrunAix-Marseille Université, CNRS, CNES, LAMF. TorradeflotCentro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT)P. N. AppletonP. CasenoveCentre National d’Etudes Spatiales – Centre spatial de ToulousePierre-Yves ChabaudAix-Marseille Université, CNRS, CNES, LAMM FrailisINAF-Osservatorio Astronomico di TriesteM FumanaINAF-IASF MilanoL. GuzzoINAF-Osservatorio Astronomico di BreraG. MainettiCentre de Calcul de l’IN2P3/CNRSD. MainoINAF-IASF MilanoM. MorescoDipartimento di Fisica e Astronomia “Augusto Righi” – Alma Mater Studiorum Università di BolognaWill J. PercivalDepartment of Physics and Astronomy, University of WaterlooR. ScaramellaINFN-Sezione di RomaM. ScodeggioINAF-IASF MilanoNathaniel R. StickleyCalifornia Institute of TechnologyD. VibertAix-Marseille Université, CNRS, CNES, LAMY. WangInfrared Processing and Analysis CenterJ. ZoubianAix-Marseille Université, CNRS/IN2P3, CPPMN. AghanimInstitut d'Astrophysique SpatialeB. AltieriESAC/ESA, Camino Bajo del CastilloA. AmaraSchool of Mathematics and Physics, University of SurreyS. AndreonINAF-Osservatorio Astronomico di BreraC BaccigalupiINAF-Osservatorio Astronomico di TriesteMarco BaldiDipartimento di Fisica e Astronomia, Università di BolognaS BardelliINAF-Osservatorio di Astrofisica e Scienza dello Spazio di BolognaA BivianoIFPU, Institute for Fundamental Physics of the UniverseA. BonchiUnited Kingdom Space AgencyE. BranchiniINAF-Osservatorio Astronomico di BreraM. BresciaDepartment of Physics “E. Pancini”, University Federico IIJ. BrinchmannFaculdade de Ciências da Universidade do Porto, Rua do Campo de AlegreS. CameraDipartimento di Fisica, Università degli Studi di TorinoG Cañas-HerreraLeiden Observatory, Leiden UniversityC. CarboneINAF-IASF Milano
Ochiq kirishOltin
Litsenziya: cc-by
ABI
Annotatsiya
ESA’s Euclid cosmology mission relies on the very sensitive and accurately calibrated spectroscopy channel of the Near-Infrared Spectrometer and Photometer (NISP). With three operational grisms in two wavelength intervals, NISP provides diffraction-limited slitless spectroscopy over a field of 0.57 deg 2 . A blue grism, BG E , covers the wavelength range 926–1366 nm at a spectral resolution (ℛ) of 440–900 for a 0.″5 diameter source with a dispersion of 1.24 nm px −1 . Two red grisms, RG E , span 1206 to 1892 nm at ℛ = 550–740 and a dispersion of 1.37 nm px −1 . We describe the construction of the grisms as well as the ground testing of the flight model of the NISP instrument, where these properties were established.
Hali tarjima qilinmagan
Mavzular
Identifikatorlar
Iqtiboslar va manbalar
0 ta iqtibos14 ta foydalanilgan manba