June
2022
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2022A&A...662A.112E
Authors
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Euclid Collaboration
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Scaramella, R.
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Amiaux, J.
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Mellier, Y.
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Burigana, C.
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Carvalho, C. S.
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Cuillandre, J. -C.
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Da Silva, A.
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Derosa, A.
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Dinis, J.
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Maiorano, E.
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Maris, M.
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Tereno, I.
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Laureijs, R.
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Boenke, T.
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Buenadicha, G.
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Dupac, X.
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Gaspar Venancio, L. M.
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Gómez-Álvarez, P.
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Hoar, J.
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Lorenzo Alvarez, J.
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Racca, G. D.
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Saavedra-Criado, G.
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Schwartz, J.
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Vavrek, R.
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Schirmer, M.
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Aussel, H.
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Azzollini, R.
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Cardone, V. F.
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Cropper, M.
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Ealet, A.
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Garilli, B.
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Gillard, W.
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Granett, B. R.
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Guzzo, L.
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Hoekstra, H.
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Jahnke, K.
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Kitching, T.
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Maciaszek, T.
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Meneghetti, M.
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Miller, L.
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Nakajima, R.
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Niemi, S. M.
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Pasian, F.
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Percival, W. J.
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Pottinger, S.
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Sauvage, M.
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Scodeggio, M.
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Wachter, S.
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Zacchei, A.
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Aghanim, N.
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Amara, A.
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Auphan, T.
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Auricchio, N.
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Awan, S.
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Balestra, A.
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Bender, R.
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Bodendorf, C.
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Bonino, D.
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Branchini, E.
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Brau-Nogue, S.
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Brescia, M.
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Candini, G. P.
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Capobianco, V.
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Carbone, C.
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Carlberg, R. G.
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Carretero, J.
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Casas, R.
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Castander, F. J.
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Castellano, M.
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Cavuoti, S.
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Cimatti, A.
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Cledassou, R.
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Congedo, G.
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Conselice, C. J.
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Conversi, L.
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Copin, Y.
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Corcione, L.
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Costille, A.
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Courbin, F.
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Degaudenzi, H.
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Douspis, M.
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Dubath, F.
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Duncan, C. A. J.
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Dusini, S.
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Farrens, S.
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Ferriol, S.
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Fosalba, P.
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Fourmanoit, N.
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Frailis, M.
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Franceschi, E.
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Franzetti, P.
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Fumana, M.
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Gillis, B.
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Giocoli, C.
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Grazian, A.
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Grupp, F.
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Haugan, S. V. H.
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Holmes, W.
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Hormuth, F.
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Hudelot, P.
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Kermiche, S.
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Kiessling, A.
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Kilbinger, M.
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Kohley, R.
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Kubik, B.
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Kümmel, M.
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Kunz, M.
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Kurki-Suonio, H.
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Lahav, O.
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Ligori, S.
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Lilje, P. B.
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Lloro, I.
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Mansutti, O.
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Marggraf, O.
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Markovic, K.
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Marulli, F.
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Massey, R.
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Maurogordato, S.
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Melchior, M.
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Merlin, E.
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Meylan, G.
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Mohr, J. J.
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Moresco, M.
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Morin, B.
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Moscardini, L.
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Munari, E.
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Nichol, R. C.
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Padilla, C.
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Paltani, S.
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Peacock, J.
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Pedersen, K.
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Pettorino, V.
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Pires, S.
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Poncet, M.
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Popa, L.
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Pozzetti, L.
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Raison, F.
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Rebolo, R.
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Rhodes, J.
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Rix, H. -W.
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Roncarelli, M.
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Rossetti, E.
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Saglia, R.
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Schneider, P.
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Schrabback, T.
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Secroun, A.
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Seidel, G.
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Serrano, S.
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Sirignano, C.
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Sirri, G.
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Skottfelt, J.
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Stanco, L.
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Starck, J. L.
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Tallada-Crespí, P.
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Tavagnacco, D.
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Taylor, A. N.
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Teplitz, H. I.
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Toledo-Moreo, R.
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Torradeflot, F.
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Trifoglio, M.
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Valentijn, E. A.
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Valenziano, L.
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Verdoes Kleijn, G. A.
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Wang, Y.
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Welikala, N.
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Weller, J.
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Wetzstein, M.
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Zamorani, G.
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Zoubian, J.
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Andreon, S.
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Baldi, M.
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Bardelli, S.
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Boucaud, A.
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Camera, S.
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Di Ferdinando, D.
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Fabbian, G.
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Farinelli, R.
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Galeotta, S.
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Graciá-Carpio, J.
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Maino, D.
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Medinaceli, E.
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Mei, S.
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Neissner, C.
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Polenta, G.
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Renzi, A.
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Romelli, E.
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Rosset, C.
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Sureau, F.
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Tenti, M.
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Vassallo, T.
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Zucca, E.
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Baccigalupi, C.
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Balaguera-Antolínez, A.
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Battaglia, P.
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Biviano, A.
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Borgani, S.
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Bozzo, E.
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Cabanac, R.
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Cappi, A.
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Casas, S.
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Castignani, G.
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Colodro-Conde, C.
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Coupon, J.
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Courtois, H. M.
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Cuby, J.
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de la Torre, S.
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Desai, S.
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Dole, H.
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Fabricius, M.
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Farina, M.
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Ferreira, P. G.
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Finelli, F.
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Flose-Reimberg, P.
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Fotopoulou, S.
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Ganga, K.
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Gozaliasl, G.
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Hook, I. M.
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Keihanen, E.
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Kirkpatrick, C. C.
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Liebing, P.
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Lindholm, V.
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Mainetti, G.
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Martinelli, M.
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Martinet, N.
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Maturi, M.
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McCracken, H. J.
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Metcalf, R. B.
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Morgante, G.
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Nightingale, J.
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Nucita, A.
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Patrizii, L.
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Potter, D.
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Riccio, G.
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Sánchez, A. G.
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Sapone, D.
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Schewtschenko, J. A.
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Schultheis, M.
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Scottez, V.
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Teyssier, R.
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Tutusaus, I.
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Valiviita, J.
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Viel, M.
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Vriend, W.
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Whittaker, L.
Abstract
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Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 deg2 of extragalactic sky in six years. The wide-field telescope and instruments are optimised for pristine point spread function and reduced stray light, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, deep fields, and calibration fields, as well as spacecraft movements followed by Euclid as it operates in a step-and-stare mode from its orbit around the Lagrange point L2. Each EWS pointing has four dithered frames; we simulated the dither pattern at the pixel level to analyse the effective coverage. We used up-to-date models for the sky background to define the Euclid region-of-interest (RoI). The building of the reference survey is highly constrained from calibration cadences, spacecraft constraints, and background levels; synergies with ground-based coverage were also considered. Via purposely built software, we first generated a schedule for the calibrations and deep fields observations. On a second stage, the RoI was tiled and scheduled with EWS observations, using an algorithm optimised to prioritise the best sky areas, produce a compact coverage, and ensure thermal stability. The result is the optimised reference survey RSD_2021A, which fulfils all constraints and is a good proxy for the final solution. The current EWS covers ≈14 500 deg2. The limiting AB magnitudes (5σ point-like source) achieved in its footprint are estimated to be 26.2 (visible band IE) and 24.5 (for near infrared bands YE, JE, HE); for spectroscopy, the Hα line flux limit is 2 × 10−16 erg−1 cm−2 s−1 at 1600 nm; and for diffuse emission, the surface brightness limits are 29.8 (visible band) and 28.4 (near infrared bands) mag arcsec−2.
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