Euclid: IV. The NISP Calibration Unit
Hormuth, F.; Jahnke, K.; Schirmer, M.; Lee C., G.-Y.; Scott, T.; Barbier, R.; Ferriol, S.; Gillard, W.; Grupp, F.; Holmes, R.; Holmes, W.; Kubik, B.; Macias-Perez, J.; Laurent, M.; Marpaud, J.; Marton, M.; Medinaceli, E.; Morgante, G.; Toledo-Moreo, R.; Trifoglio, M.; Rix, Hans-Walter; Secroun, A.; Seiffert, M.; Stassi, P.; Wachter, S.; Gutierrez C., M.; Vescovi, C.; Amara, A.; Andreon, S.; Auricchio, N.; Baccigalupi, C.; Baldi, M.; Balestra, A.; Bardelli, S.; Battaglia, P.; Bender, R.; Bodendorf, C.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Capobianco, V.; Carbone, C.; Cardone V., F.; Carretero, J.; Casas, R.; Casas, S.; Castellano, M.; Castignani, G.; Cavuoti, S.; Cimatti, A.; Colodro-Conde, C.; Congedo, G.; Conselice C., J.; Conversi, L.; Copin, Y.; Corcione, L.; Courbin, F.; Courtois H., M.; Da Silva, A.; Degaudenzi, H.; De Lucia, G.; Dinis, J.; Douspis, M.; Dubath, F.; Ducret, F.; Dupac, X.; Dusini, S.; Fabricius, M.; Farina, M.; Farrens, S.; Faustini, F.; Fotopoulou, S.; Fourmanoit, N.; Frailis, M.; Franceschi, E.; Franzetti, P.; Fumana, M.; Galeotta, S.; Garilli, B.; George, K.; Gillis, B.; Giocoli, C.; Grazian, A.; Guzzo, L.; Haugan S. V., H.; Hoekstra, H.; Hook, I.; Hornstrup, A.; Hudelot, P.; Jhabvala, M.; Keihänen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kohley, R.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Le Mignant, D.; Ligori, S.; Lilje P., B.; Lindholm, V.; Lloro, I.; Mainetti, G.; Maiorano, E.; Mansutti, O.; Marcin, S.; Marggraf, O.; Markovic, K.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Maurogordato, S.; McCracken H., J.; Mei, S.; Melchior, M.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mohr J., J.; Moresco, M.; Morris P., W.; Moscardini, L.; Munari, E.; Nakajima, R.; Neissner, C.; Nichol R., C.; Niemi, S.-M.; Nightingale J., W.; Padilla, C.; Paech, K.; Paltani, S.; Pasian, F.; Pedersen, K.; Percival W., J.; Pettorino, V.; Pires, S.; Polenta, G.; Poncet, M.; Popa L., A.; Raison, F.; Rebolo, R.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rossetti, E.; Rusholme, B.; Saglia, R.; Sakr, Z.; Sánchez A., G.; Sapone, D.; Sartoris, B.; Sauvage, M.; Schewtschenko J., A.; Schneider, P.; Schrabback, T.; Sefusatti, E.; Seidel, G.; Serrano, S.; Sirignano, C.; Sirri, G.; Smadja, G.; Stanco, L.; Steinwagner, J.; Tallada-Crespí, P.; Tavagnacco, D.; Taylor A., N.; Teplitz H., I.; Tereno, I.; Torradeflot, F.; Tutusaus, I.; Valenziano, L.; Vassallo, T.; Veropalumbo, A.; Wang, Y.; Weller, J.; Zacchei, A.; Zamorani, G.; Zerbi F., M.; Zucca, E.; Biviano, A.; Bolzonella, M.; Boucaud, A.; Bozzo, E.; Burigana, C.; Calabrese, M.; Di Ferdinando, D.; Escartin Vigo J., A.; Farinelli, R.; Gracia-Carpio, J.; Kazandjian M., V.; Mauri, N.; Scottez, V.; Tenti, M.; Viel, M.; Wiesmann, M.; Akrami, Y.; Allevato, V.; Anselmi, S.; Aubourg, E.; Ballardini, M.; Bethermin, M.; Blanchard, A.; Blot, L.; Borgani, S.; Borlaff A., S.; Borsato, E.; Bruton, S.; Cabanac, R.; Calabro, A.; Canas-Herrera, G.; Cappi, A.; Carvalho C., S.; Casenove, P.; Castro, T.; Chambers K., C.; Charles, Y.; Contarini, S.; Cooray A., R.; Cucciati, O.; Davini, S.; De Caro, B.; de la Torre, S.; Desprez, G.; Díaz-Sánchez, A.; Diaz J., J.; Di Domizio, S.; Dole, H.; Escoffier, S.; Ferrari A., G.; Ferreira P., G.; Ferrero, I.; Finelli, F.; Fontana, A.; Fornari, F.; Gabarra, L.; Ganga, K.; García-Bellido, J.; Gaztanaga, E.; Giacomini, F.; Gozaliasl, G.; Hall, A.; Hartley W., G.; Hildebrandt, H.; Hjorth, J.; Huertas-Company, M.; Ilbert, O.; Jacobson, J.; Jimenez Muñoz, A.; Joudaki, S.; Kajava J. J., E.; Kansal, V.; Karagiannis, D.; Kirkpatrick C., C.; Laudisio, F.; Legrand, L.; Libet, G.; Loureiro, A.; Maggio, G.; Magliocchetti, M.; Mancini, C.; Mannucci, F.; Maoli, R.; Martins C. J. A., P.; Matthew, S.; Maurin, L.; Metcalf R., B.; Miluzio, M.; Moretti, C.; Nadathur, S.; Walton Nicholas, A.; Patrizii, L.; Pezzotta, A.; Pöntinen, M.; Popa, V.; Porciani, C.; Potter, D.; Risso, I.; Rocci, P.-F.; Rollins R., P.; Sahlén, M.; Scarlata, C.; Schneider, A.; Schultheis, M.; Sereno, M.; Shulevski, A.; Silvestri, A.; Simon, P.; Spurio Mancini, A.; Stadel, J.; Tao, C.; Testera, G.; Teyssier, R.; Toft, S.; Tosi, S.; Troja, A.; Tucci, M.; Valieri, C.; Valiviita, J.; Vergani, D.; Verza, G.; Zalesky, L.; Archidiacono, M.; Atrio-Barandela, F.; Bouvard, T.; Caro, F.; Dimauro, P.; Fang, Y.; Ferguson A. M., N.; Finoguenov, A.; Gasparetto, T.; Le Brun A. M., C.; Le Graet, J.; Liaudat T., I.; Montoro, A.; Murray, C.; Oguri, M.; Pagano, L.; Paoletti, D.; Sarpa, E.; Tanidis, K.; Vernizzi, F.; Viitanen, A.; Kovačić, I.; Lesgourgues, J.; Martín-Fleitas, J.; Mora, A.; Euclid Collaboration
Euclid: IV. The NISP Calibration Unit
EDP Sciences
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2025082785848
https://urn.fi/URN:NBN:fi-fe2025082785848
Tiivistelmä
The near-infrared calibration unit (NI-CU) on board Euclid’s Near-Infrared Spectrometer and Photometer (NISP) is the first astronomical calibration lamp based on light-emitting diodes (LEDs) to be operated in space. Euclid is a mission in ESA’s Cosmic Vision 2015–2025 framework to explore the dark universe and provide a next-level characterisation of the nature of gravitation, dark matter, and dark energy. Calibrating photometric and spectrometric measurements of galaxies to better than 1.5% accuracy in a survey homogeneously mapping ∼14 000 deg2 of extragalactic sky requires a very detailed characterisation of near-infrared (NIR) detector properties as well as constant monitoring of them in flight. To cover two of the main contributions – relative pixel-to-pixel sensitivity and non-linearity characteristics – and to support other calibration activities, NI-CU was designed to provide spatially approximately homogeneous (<12% variations) and temporally stable illumination (0.1–0.2% over 1200 s) over the NISP detector plane with minimal power consumption and energy dissipation. NI-CU covers the spectral range ∼[900,1900] nm – at cryo-operating temperature – at five fixed independent wavelengths to capture wavelength-dependent behaviour of the detectors, with fluence over a dynamic range of ≳100 from ∼15 ph s−1 pixel−1 to >1500 ph s−1 pixel−1. For this functionality, NI-CU is based on LEDs. We describe the rationale behind the decision and design process, the challenges in sourcing the right LEDs, and the qualification process and lessons learned. We also provide a description of the completed NI-CU, its capabilities, and performance as well as its limits. NI-CU has been integrated into NISP and the Euclid satellite, and since Euclid’s launch in July 2023, it has started supporting survey operations.
Kokoelmat
- Rinnakkaistallenteet [27094]