The Euclid mission objective is to understand why the expansion of the Universe is accelerating through by mapping the geometry of the dark Universe by investigating the distance-redshift relationship and tracing the evolution of cosmic structures. The Euclid project is part of ESA's Cosmic Vision program with its launch planned for 2020 (ref [1]). The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments and is operating in the near-IR spectral region (900- 2000nm) as a photometer and spectrometer. The instrument is composed of: - a cold (135K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly (corrector and camera lens), a filter wheel mechanism, a grism wheel mechanism, a calibration unit and a thermal control system - a detection subsystem based on a mosaic of 16 HAWAII2RG cooled to 95K with their front-end readout electronic cooled to 140K, integrated on a mechanical focal plane structure made with molybdenum and aluminum. The detection subsystem is mounted on the optomechanical subsystem structure - a warm electronic subsystem (280K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data This presentation describes the architecture of the instrument at the end of the phase C (Detailed Design Review), the expected performance, the technological key challenges and preliminary test results obtained for different NISP subsystem breadboards and for the NISP Structural and Thermal model (STM).

Euclid Near Infrared Spectrometer and Photometer instrument concept and first test results obtained for different breadboards models at the end of phase C

PATRIZII, LAURA;CHIARUSI, TOMMASO;FORNARI, FEDERICO;MARGIOTTA, ANNARITA;MAURI, NICOLETTA;PASQUALINI, LAURA;SIRRI, GABRIELE;SPURIO, MAURIZIO;TENTI, MATTEO;TRAVAGLINI, RICCARDO;
2016

Abstract

The Euclid mission objective is to understand why the expansion of the Universe is accelerating through by mapping the geometry of the dark Universe by investigating the distance-redshift relationship and tracing the evolution of cosmic structures. The Euclid project is part of ESA's Cosmic Vision program with its launch planned for 2020 (ref [1]). The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments and is operating in the near-IR spectral region (900- 2000nm) as a photometer and spectrometer. The instrument is composed of: - a cold (135K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly (corrector and camera lens), a filter wheel mechanism, a grism wheel mechanism, a calibration unit and a thermal control system - a detection subsystem based on a mosaic of 16 HAWAII2RG cooled to 95K with their front-end readout electronic cooled to 140K, integrated on a mechanical focal plane structure made with molybdenum and aluminum. The detection subsystem is mounted on the optomechanical subsystem structure - a warm electronic subsystem (280K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data This presentation describes the architecture of the instrument at the end of the phase C (Detailed Design Review), the expected performance, the technological key challenges and preliminary test results obtained for different NISP subsystem breadboards and for the NISP Structural and Thermal model (STM).
Proceedings of SPIE - The International Society for Optical Engineering
99040T
99040T
Maciaszek, Thierry; Ealet, Anne; Jahnke, Knud; Prieto, Eric; Barbier, Rémi; Mellier, Yannick; Beaumont, Florent; Bon, William; Bonefoi, Anne; Carle, Michael; Caillat, Amandine; Costille, Anne; Dormoy, Doriane; Ducret, Franck; Fabron, Christophe; Febvre, Aurélien; Foulon, Benjamin; Garcia, Jose; Gimenez, Jean-Luc; Grassi, Emmanuel; Laurent, Philippe; Mignant, David Le; Martin, Laurent; Rossin, Christelle; Pamplona, Tony; Sanchez, Patrice; Vives, Sebastien; Clémens, Jean Claude; Gillard, William; Niclas, Mathieu; Secroun, Aurélia; Serra, Benoit; Kubik, Bogna; Ferriol, Sylvain; Amiaux, Jérome; Barrière, Jean Christophe; Berthe, Michel; Rosset, Cyrille; Macias-Perez, Juan Francisco; Auricchio, Natalia; De Rosa, Adriano; Franceschi, Enrico; Guizzo, Gian Paolo; Morgante, Gianluca; Sortino, Francesca; Trifoglio, Massimo; Valenziano, Luca; Patrizii, Laura; Chiarusi, T.; Fornari, F.; Giacomini, F.; Margiotta, A.; Mauri, N.; Pasqualini, L.; Sirri, G.; Spurio, M.; Tenti, M.; Travaglini, R.; Dusini, Stefano; Dal Corso, F.; Laudisio, F.; Sirignano, C.; Stanco, L.; Ventura, S.; Borsato, Enrico; Bonoli, Carlotta; Bortoletto, Favio; Balestra, Andrea; D'Alessandro, Maurizio; Celi, Eduardo Medina; Farinelli, Ruben; Corcione, Leonardo; Ligori, Sebastiano; Grupp, Frank; Wimmer, Carolin; Hormuth, Felix; Seidel, Gregor; Wachter, Stefanie; Padilla, Cristobal; Lamensans, Mikel; Casas, Ricard; Lloro, Ivan; Toledo-Moreo, Rafael; Gomez, Jaime; Colodro-Conde, Carlos; Lizán, David; Diaz, Jose Javier; Lilje, Per B.; Toulouse-Aastrup, Corinne; Andersen, Michael I.; Sørensen, Anton N.; Jakobsen, Peter; Hornstrup, Allan; Jessen, Niels-Christian; Thizy, Cédric; Holmes, Warren; Israelsson, Ulf; Seiffert, Michael; Waczynski, Augustyn; Laureijs, René J.; Racca, Giuseppe; Salvignol, Jean-Christophe; Boenke, Tobias; Strada, Paolo
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11585/582395
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