A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Euclid: III. The NISP Instrument
Tekijät: Jahnke, K.; Gillard, W.; Schirmer, M.; Ealet, A.; Maciaszek, T.; Prieto, E.; Barbier, R.; Bonoli, C.; Corcione, L.; Dusini, S.; Grupp, F.; Hormuth, F.; Ligori, S.; Martin, L.; Morgante, G.; Padilla, C.; Toledo-Moreo, R.; Trifoglio, M.; Valenziano, L.; Bender, R.; Castander, F. J.; Garilli, B.; Lilje, P. B.; Rix, H. -W.; Andersen, M. I.; Auricchio, N.; Balestra, A.; Barriere, J. -C.; Battaglia, P.; Berthe, M.; Bodendorf, C.; Boenke, T.; Bon, W.; Bonnefoi, A.; Caillat, A.; Capobianco, V; Carle, M.; Casas, R.; Cho, H.; Costille, A.; Ducret, F.; Ferriol, S.; Franceschi, E.; Gimenez, J. -L; Holmes, W.; Hornstrup, A.; Jhabvala, M.; Kohley, R.; Kubik, B.; Laureijs, R.; Le Mignant, D.; Lloro, I.; Medinaceli, E.; Mellier, Y.; Polenta, G.; Racca, G. D.; Renzi, A.; Salvignol, J. -C; Secroun, A.; Seidel, G.; Seiffert, M.; Sirignano, C.; Sirri, G.; Strada, P.; Smadja, G.; Stanco, L.; Wachter, S.; Anselmi, S.; Borsato, E.; Caillat, L.; Cogato, F.; Colodro-Conde, C.; Crouzet, P. -E.; Conforti, V.; D'Alessandro, M.; Copin, Y.; Cuillandre, J. -C; Davies, J. E.; Davini, S.; Derosa, A.; Diaz, J. J.; Di Domizio, S.; Di Ferdinando, D.; Farinelli, R.; Ferrari, A. G.; Fornari, F.; Gabarra, L.; Garcia, R.; Gutierrez, C. M.; Giacomini, F.; Lagier, P.; Gianotti, F.; Krause, O.; Madrid, F.; Laudisio, F.; Macias-Perez, J.; Naletto, G.; Niclas, M.; Marpaud, J.; Mauri, N.; da Silva, R.; Passalacqua, F.; Paterson, K.; Patrizii, L.; Risso, I; Solheim, B. G. B.; Scodeggio, M.; Stassi, P.; Steinwagner, J.; Tenti, M.; Testera, G.; Travaglini, R.; Tosi, S.; Troja, A.; Tubio, O.; Valieri, C.; Vescovi, C.; Ventura, S.; Aghanim, N.; Altieri, B.; Amara, A.; Amiaux, J.; Andreon, S.; Appleton, P. N.; Aussel, H.; Baccigalupi, C.; Baldi, M.; Bardelli, S.; Basset, A.; Bonchi, A.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Camera, S.; Carbone, C.; Cardone, V. F.; Carretero, J.; Casas, S.; Castellano, M.; Castignani, G.; Cavuoti, S.; Chabaud, P. -Y.; Cimatti, A.; Congedo, G.; Conselice, C. J.; Conversi, L.; Courbin, F.; Courtois, H. M.; Crocce, M.; Cropper, M.; Cuby, J. -G.; Da Silva, A.; Degaudenzi, H.; De Lucia, G.; Di Giorgio, A. M.; Dinis, J.; Douspis, M.; Dubath, F.; Duncan, C. A. J.; Dupac, X.; Fabricius, M.; Farina, M.; Farrens, S.; Faustini, F.; Fosalba, P.; Fotopoulou, S.; Fourmanoit, N.; Frailis, M.; Franzetti, P.; Galeotta, S.; George, K.; Gillis, B.; Giocoli, C.; Gomez-Alvarez, P.; Granett, B. R.; Grazian, A.; Guzzo, L.; Hailey, M.; Haugan, S. V. H.; Hoar, J.; Hoekstra, H.; Hook, I; Hudelot, P.; Ilic, S.; Joachimi, B.; Keihaenen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kitching, T.; Kummel, M.; Kunz, M.; Kurki-Suonio, H.; Lahav, O.; Liebing, P.; Lindholm, V.; Lorenzo Alvarez, J.; Mainetti, G.; Maino, D.; Maiorano, E.; Mansutti, O.; Marcin, S.; Marggraf, O.; Markovic, K.; Martignac, J.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Masters, D. C.; Maurogordato, S.; Mccracken, H. J.; Mei, S.; Melchior, M.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mohr, J. J.; Moresco, M.; Morris, P. W.; Moscardini, L.; Nakajima, R.; Neissner, C.; Nichol, R. C.; Niemi, S. -M; Nutma, T.; Paech, K.; Paltani, S.; Pasian, F.; Peacock, J. A.; Pedersen, K.; Percival, W. J.; Pettorino, V.; Pires, S.; Poncet, M.; Popa, L. A.; Pozzetti, L.; Raison, F.; Rebolo, R.; Refregier, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rosset, C.; Rossetti, E.; Rottgering, H. J. A.; Rusholme, B.; Saglia, R.; Sakr, Z.; Sanchez, A. G.; Sapone, D.; Sauvage, M.; Scaramella, R.; Schewtschenko, J. A.; Schneider, P.; Schrabback, T.; Sefusatti, E.; Serrano, S.; Tallada-Crespi, P.; Tavagnacco, D.; Taylor, A. N.; Teplitz, H., I; Tereno, I.; Torradeflot, F.; Tutusaus, I; Vassallo, T.; Verdoes Kleijn, G.; Veropalumbo, A.; Vibert, D.; Wang, Y.; Weller, J.; Zacchei, A.; Zamorani, G.; Zerbi, F. M.; Zoubian, J.; Zucca, E.; Biviano, A.; Bolzonella, M.; Boucaud, A.; Bozzo, E.; Burigana, C.; Calabrese, M.; Casenove, P.; Escartin Vigo, J. A.; Fabbian, G.; Finelli, F.; Gracia-Carpio, J.; Liu, C.; Pezzotta, A.; Poentinen, M.; Porciani, C.; Scottez, V.; Viel, M.; Wiesmann, M.; Akrami, Y.; Allevato, V; Aubourg, E.; Ballardini, M.; Bertacca, D.; Bethermin, M.; Blanchard, A.; Blot, L.; Borgani, S.; Borlaff, A. S.; Bruton, S.; Cabanac, R.; Calabro, A.; Calderone, G.; Canas-Herrera, G.; Cappi, A.; Carvalho, C. S.; Castro, T.; Chambers, K. C.; Charles, Y.; Chary, R.; Colbert, J.; Contarini, S.; Contini, T.; Cooray, A. R.; Costanzi, M.; Cucciati, O.; De Caro, B.; de la Torre, S.; Desprez, G.; Diaz-Sanchez, A.; Dole, H.; Escoffier, S.; Ferreira, P. G.; Ferrero, I; Finoguenov, A.; Fontana, A.; Ganga, K.; Garcia-Bellido, J.; Gautard, V.; Gaztanaga, E.; Gozaliasl, G.; Gregorio, A.; Hall, A.; Hartley, W. G.; Hemmati, S.; Hildebrandt, H.; Hjorth, J.; Hosseini, S.; Huertas-Company, M.; Ilbert, O.; Jacobson, J.; Jimenez Munoz, A.; Joudaki, S.; Kajava, J. J. E.; Kansal, V; Karagiannis, D.; Kirkpatrick, C. C.; Lacasa, F.; Le Brun, V.; Le Graet, J.; Legrand, L.; Libet, G.; Liu, S. J.; Loureiro, A.; Magliocchetti, M.; Mancini, C.; Mannucci, F.; Maoli, R.; Martins, C. J. A. P.; Matthew, S.; Maurin, L.; Mcpartland, C. J. R.; Metcalf, R. B.; Migliaccio, M.; Miluzio, M.; Monaco, P.; Moretti, C.; Nadathur, S.; Nicastro, L.; Walton, Nicholas A.; Odier, J.; Oguri, M.; Popa, V.; Potter, D.; Pourtsidou, A.; Rocci, P. -F; Rollins, R. P.; Sahlen, M.; Scarlata, C.; Schaye, J.; Schneider, A.; Schultheis, M.; Sereno, M.; Shankar, F.; Shulevski, A.; Sikkema, G.; Silvestri, A.; Simon, P.; Spurio Mancini, A.; Stadel, J.; Stanford, S. A.; Tanidis, K.; Tao, C.; Tessore, N.; Teyssier, R.; Toft, S.; Tucci, M.; Valiviita, J.; Vergani, D.; Vernizzi, F.; Verza, G.; Vielzeuf, P.; Weaver, J. R.; Zalesky, L.; Zinchenko, I. A.; Archidiacono, M.; Atrio-Barandela, F.; Bennett, C. L.; Bouvard, T.; Caro, F.; Conseil, S.; Dimauro, P.; Duc, P. -A.; Fang, Y.; Ferguson, A. M. N.; Gasparetto, T.; Kovacic, I; Kruk, S.; Le Brun, A. M. C.; Liaudat, T. I.; Montoro, A.; Mora, A.; Murray, C.; Pagano, L.; Paoletti, D.; Radovich, M.; Sarpa, E.; Tommasi, E.; Viitanen, A.; Lesgourgues, J.; Levi, M. E.; Martin-Fleitas, J.; Oppizzi, F.; Euclid Collaboration
Kustantaja: EDP SCIENCES S A
Kustannuspaikka: LES ULIS CEDEX A
Julkaisuvuosi: 2025
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Artikkelin numero: A3
Vuosikerta: 697
Sivujen määrä: 31
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202450786
Verkko-osoite: https://doi.org/10.1051/0004-6361/202450786
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/492351097
The Near-Infrared Spectrometer and Photometer (NISP) on board the Euclid satellite provides multiband photometry and R greater than or similar to 450 slitless grism spectroscopy in the 950-2020 nm wavelength range. In this reference article, we illuminate the background of NISP's functional and calibration requirements, describe the instrument's integral components, and provide all its key properties. We also sketch the processes needed to understand how NISP operates and is calibrated as well as its technical potentials and limitations. Links to articles providing more details and the technical background are included. The NISP's 16 HAWAII-2RG (H2RG) detectors with a plate scale of 0 ''.3 pixel(-1) deliver a field of view of 0.57 deg(2). In photometric mode, NISP reaches a limiting magnitude of similar to 24.5 AB mag in three photometric exposures of about 100 s in exposure time for point sources and with a S/N of five. For spectroscopy, NISP's pointsource sensitivity is a signal-to-noise ratio = 3.5 detection of an emission line with flux similar to 2 x 10(-16) erg s(-1) cm(-2) integrated over two resolution elements of 13.4 angstrom in 3 x 560 s grism exposures at 1.6 mu m (redshifted H alpha). Our calibration includes on-ground and in-flight characterisation and monitoring of the pixel-based detector baseline, dark current, non-linearity, and sensitivity to guarantee a relative photometric accuracy better than 1.5% and a relative spectrophotometry better than 0.7%. The wavelength calibration must be accurate to 5 angstrom or better. The NISP is the state-of-the-art instrument in the near-infrared for all science beyond small areas available from HST and JWST - and it represents an enormous advance from any existing instrumentation due to its combination of field size and high throughput of telescope and instrument. During Euclid's six-year survey covering 14 000 deg(2) of extragalactic sky, NISP will be the backbone in determining distances of more than a billion galaxies. Its near-infrared data will become a rich reference imaging and spectroscopy data set for the coming decades.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
Julkaisussa olevat rahoitustiedot:
The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum für Luft- und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid web site (http://www.euclid-ec.org).
