Euclid Quick Data Release (Q1)

作者：G. Polenta, M. Frailis, Anahita Alavi, P. N. Appleton, Petra Awad, A Bonchi, R. J. Bouwens, L. Bramante, D. Busonero, G. Calderone, F Cogato, Simon Conseil, M. Correnti, R da Silva, I. Das, F Faustini, Y. Fu, T Gasparetto, W. Gillard, A Grazian, Shoubaneh Hemmati, J. Jacobson, K. Jahnkę, B. Kubik, X. Liu, C. Macabiau, E. Medinaceli, P. Morris, K. Paterson, M. Radovich, M. Schirmer, A. Shulevski, H.I Teplitz, B. Venemans, N. Aghanim, B. Altieri, A. Amara, S. Andreon, N. Auricchio, H. Aussel, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, Alberto Basset, P Battaglia, A. N. Belikov, R. Bender, A. Biviano, E Branchini, M. Brescia, J. Brinchmann, A. Caillat, S Camera, G Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, F. J. Castander, M. Castellano, G. Castignani, S. Cavuoti, K. C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, C.J. Conselice, L. Conversi, Y. Copin, L. Corcione, A. Costille, F. Courbin, H. M. Courtois, A. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, H. Dole, F. Dubath, C. A. J. Duncan, X. Dupac, S Dusini, A. Ealet, S. Escoffier, Maximilian Fabricius, M. Farina, R. Farinelli, S. Ferriol, F. Finelli⋆, S. Fotopoulou, N. Fourmanoit, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, P. Gómez-Álvarez, J. Gracia-Carpio, B. R. Granett, F Grupp, S. V. H. Haugan, J. Hoar, H Hoekstra, W. Holmes, I. Hook, F. Hormuth, A. Hornstrup, P. Hudelot, M. Jhabvala, E. Keihänen, S. Kermiche, A. Kiessling, K Kuijken, M Kümmel, M. Kunz, H. Kurki‐Suonio, Q. Le Boulc'h, A.M.C Le Brun, D. Le Mignant, P. Liebing, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G Mainetti, D. Maino, E. Maiorano, O. Mansutti, S. Marcin, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R. Massey, S. Maurogordato, H. J. McCracken, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A Mora, M. Moresco, L. Moscardini, R. Nakajima, C. Neissner, R. C. Nichol, S.-M Niemi, J.W Nightingale, C Padilla, S. Paltani, F. Pasian, K. Pedersen, Will J. Percival, V. Pettorino, S. Pires, M. Poncet, L. A. Popa, L. Pozzetti, Giuseppe D. Racca, F. Raison, R. Rébolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, B. Rusholme, R. P. Saglia, Z. Sakr, A.G. Sánchez, D. Sapone, B. Sartoris, J.A Schewtschenko, P. Schneider, M. Scodeggio, A. Secroun, E. Sefusatti, G. Seidel, M. D. Seiffert, S. Serrano, Pardis Simon, C. Sirignano, G. Sirri, A. Spurio Mancini, L Stanco, J. Steinwagner, P. Tallada-Crespí, D. Tavagnacco, A.N. Taylor, I. Tereno, N Tessore, Sune Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. A. Valentijn, L Valenziano, J. Väliviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Yun Wang, J. Weller, A. Zacchei, G Zamorani, F. M. Zerbi, I.A Zinchenko, E. Zucca, V. Allevato, M. Ballardini, M. Bolzonella, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, A. Cappi, P Casenove, D. Di Ferdinando, J.A. Escartin Vigo, G. Fabbian, L. Gabarra, J Martín-Fleitas, S Matthew, N. Mauri, Achille Nucita, A Pezzotta, M. Pöntinen, C. Porciani, I Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, I.T Andika, S Anselmi, M. Archidiacono, F. Atrio‐Barandela, Christophe Benoıst, P. Bergamini, Daniele Bertacca, M. Béthermin, G. Rodighiero, Alain Blanchard, L Blot, S Borgani, Alejandro S. Borlaff, M.L Brown, S Bruton, Antonello Calabrò, B. Camacho Quevedo, F Caro, C.S. Carvalho, T. Castro, Yann Philippe Charles, R. Chary, A.R. Cooray, O Cucciati, S. Davini, F. De Paolis, G. Desprez, A. Díaz‐Sánchez, J.J Diaz, S. Di Domizio, J. M. Diego, P.-A Duc, A Enia, Yuhong Fang, A. M. N. Ferguson, A.G Ferrari, P.G Ferreira, A. Finoguenov, A. Fontana, A. Franco, K. Ganga, J. García-Bellido, V Gautard, E. Gaztañaga, F. Giacomini, F. Gianotti, Anthony H. Gonzalez, G. Gozaliasl, A. Gregorio, A. Gruppuso, M Guidi, C. M. Gutiérrez, A Hall, W.G. Hartley, C. Hernández–Monteagudo, H Hildebrandt, J. Hjorth, J. J. E. Kajava, Y. W. Kang, V. Kansal, D. Karagiannis, K Kiiveri, C. C. Kirkpatrick, Sandor Kruk, V. Le Brun, J Le Graet, L. Legrand, Maria Lembo, F Lepori, G Leroy, G.F Lesci, Julien Lesgourgues, L. Leuzzi, T.I Liaudat, S.J Liu, A. Loureiro, J. F. Macías–Pérez, G. Maggio, M. Magliocchetti, F. Mannucci, R. Maoli, C. J. A. P. Martins, L. Maurin, Conor McPartland, M Miluzio, P Monaco, A Montoro, Chiara Moretti, G Morgante, S. Nadathur, Krishna Naidoo, P. Natoli, A. Navarro-Alsina, S Nesseris, L. Nicastro, F Passalacqua, L. Patrizii, A. Pisani, D. Potter, S Quai, P.-F Rocci, G. Rodighiero, S Sacquegna, M Sahlén, D. B. Sanders, E Sarpa, C. Scarlata, Aurel Schneider, D Sciotti, E. Sellentin, Francesco Shankar, L. C. Smith, G. Testera, C. Tao, G. Testera, Romain Teyssier, S. Tosi, A. Troja, M. Tucci, C Valieri, A. Venhola, D. Vergani, G Verza, P Vielzeuf, N. A. Walton, John R. Weaver, M. Bella, D. Scott · 发表于：Astronomy and Astrophysics · 年份：2025 · DOI：10.1051/0004-6361/202554657 · 被引用次数：14 · 研究领域：Astronomy and Astrophysical Research、History and Developments in Astronomy、Solar and Space Plasma Dynamics

This paper describes the near-infrared processing function (NIR PF) that processes NIR images from the Near-Infrared Spectrometer and Photometer (NISP) instrument on board the Euclid satellite. NIR PF consists of three main components: (i) a common pre-processing stage for both photometric (NIR) and spectroscopic (SIR) data to remove instrumental effects; (ii) astrometric and photometric calibration of NIR data, along with catalogue extraction; and (iii) resampling and stacking. The necessary calibration products are generated using dedicated pipelines that process observations from both the early performance verification (PV) phase in 2023 and the nominal survey operations. After outlining the pipelineś structure and algorithms, we describe its application to Euclid Q1 images. For Q1, we achieved an astrometric accuracy of 5–8 mas, a relative photometric accuracy of 5 mmag, along with an absolute flux calibration limited by the 1% uncertainty of the Hubble Space Telescope (HST) CALSPEC database. We characterised the point spread function (PSF), which we found to be very stable across the focal plane. Finally, we discuss current limitations of NIR PF that will be improved upon for future data releases.