June
2026
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2026A&A...711A..10E
Authors
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Euclid Collaboration
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Marleau, F. R.
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Habas, R.
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Carollo, D.
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Tortora, C.
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Duc, P.-A.
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Sola, E.
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Saifollahi, T.
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Fügenschuh, M.
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Walmsley, M.
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Zöller, R.
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Ferré-Mateu, A.
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Cantiello, M.
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Urbano, M.
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Saremi, E.
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Ragusa, R.
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Laureijs, R.
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Hilker, M.
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Müller, O.
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Poulain, M.
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Peletier, R. F.
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Sprenger, S. J.
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Marchal, O.
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Aghanim, N.
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Altieri, B.
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Amara, A.
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Andreon, S.
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Auricchio, N.
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Aussel, H.
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Baccigalupi, C.
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Baldi, M.
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Balestra, A.
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Bardelli, S.
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Basset, A.
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Battaglia, P.
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Bender, R.
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Biviano, A.
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Bonchi, A.
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Bonino, D.
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Branchini, E.
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Brescia, M.
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Brinchmann, J.
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Camera, S.
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Cañas-Herrera, G.
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Capobianco, V.
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Carbone, C.
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Carretero, J.
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Casas, S.
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Castellano, M.
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Castignani, G.
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Cavuoti, S.
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Chambers, K. C.
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Cimatti, A.
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Colodro-Conde, C.
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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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Courbin, F.
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Courtois, H. M.
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Cropper, M.
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Cuillandre, J.-C.
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Da Silva, A.
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Degaudenzi, H.
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De Lucia, G.
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Di Giorgio, A. M.
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Dolding, C.
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Dole, H.
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Dubath, F.
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Dupac, X.
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Dusini, S.
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Escoffier, S.
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Fabricius, M.
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Farina, M.
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Faustini, F.
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Ferriol, S.
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Fosalba, P.
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Fotopoulou, S.
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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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Galeotta, S.
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George, K.
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Gillis, B.
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Giocoli, C.
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Granett, B. R.
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Grazian, A.
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Grupp, F.
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Gwyn, S.
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Haugan, S. V. H.
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Hoar, J.
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Hoekstra, H.
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Holmes, W.
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Hormuth, F.
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Hornstrup, A.
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Hudelot, P.
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Jahnke, K.
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Jhabvala, M.
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Joachimi, B.
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Keihänen, E.
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Kermiche, S.
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Kiessling, A.
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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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Le Boulc'h, Q.
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Le Brun, A. M. C.
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Le Mignant, D.
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Ligori, S.
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Lilje, P. B.
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Lindholm, V.
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Lloro, I.
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Mainetti, G.
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Maino, D.
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Maiorano, E.
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Mansutti, O.
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Marcin, S.
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Marggraf, O.
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Martinelli, M.
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Martinet, N.
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Marulli, F.
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Massey, R.
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Maurogordato, S.
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McCracken, H. J.
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Medinaceli, E.
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Mei, S.
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Melchior, M.
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Mellier, Y.
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Meneghetti, M.
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Merlin, E.
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Meylan, G.
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Mora, A.
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Moresco, M.
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Moscardini, L.
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Nakajima, R.
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Neissner, C.
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Niemi, S.-M.
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Nightingale, J. W.
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Padilla, C.
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Paltani, S.
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Pasian, F.
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Pedersen, K.
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Percival, W. J.
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Pettorino, V.
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Pires, S.
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Polenta, G.
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Poncet, M.
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Popa, L. A.
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Pozzetti, L.
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Raison, F.
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Rebolo, R.
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Renzi, A.
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Rhodes, J.
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Riccio, G.
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Romelli, E.
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Roncarelli, M.
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Rossetti, E.
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Rusholme, B.
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Saglia, R.
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Sakr, Z.
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Sánchez, A. G.
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Sapone, D.
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Sartoris, B.
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Sauvage, M.
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Schewtschenko, J. A.
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Schirmer, M.
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Schneider, P.
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Scodeggio, M.
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Secroun, A.
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Seidel, G.
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Seiffert, M.
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Serrano, S.
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Simon, P.
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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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Steinwagner, J.
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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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Tereno, I.
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Toft, S.
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Toledo-Moreo, R.
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Torradeflot, F.
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Tutusaus, I.
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Valenziano, L.
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Valiviita, J.
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Vassallo, T.
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Verdoes Kleijn, G.
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Veropalumbo, A.
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Wang, Y.
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Weller, J.
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Zacchei, A.
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Zamorani, G.
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Zerbi, F. M.
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Zucca, E.
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Ballardini, M.
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Bolzonella, M.
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Burigana, C.
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Cabanac, R.
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Cappi, A.
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Di Ferdinando, D.
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Escartin Vigo, J. A.
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Gabarra, L.
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Huertas-Company, M.
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Martín-Fleitas, J.
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Matthew, S.
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Mauri, N.
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Metcalf, R. B.
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Pöntinen, M.
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Scottez, V.
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Sereno, M.
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Tenti, M.
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Viel, M.
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Wiesmann, M.
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Akrami, Y.
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Andika, I. T.
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Anselmi, S.
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Archidiacono, M.
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Atrio-Barandela, F.
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Bertacca, D.
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Bethermin, M.
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Blanchard, A.
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Borgani, S.
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Brown, M. L.
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Bruton, S.
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Buitrago, F.
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Calabro, A.
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Camacho Quevedo, B.
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Caro, F.
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Carvalho, C. S.
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Castro, T.
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Cogato, F.
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Conseil, S.
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Cooray, A. R.
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Davini, S.
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De Paolis, F.
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Desprez, G.
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Díaz-Sánchez, A.
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Di Domizio, S.
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Diego, J. M.
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Dimauro, P.
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Enia, A.
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Franco, A.
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Ganga, K.
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García-Bellido, J.
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Gasparetto, T.
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Gaztanaga, E.
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Gianotti, F.
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Gozaliasl, G.
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Guidi, M.
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Gutierrez, C. M.
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Hall, A.
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Hernández-Monteagudo, C.
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Hildebrandt, H.
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Kajava, J. J. E.
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Kang, Y.
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Kansal, V.
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Karagiannis, D.
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Kiiveri, K.
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Kirkpatrick, C. C.
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Kruk, S.
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Legrand, L.
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Lepori, F.
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Leroy, G.
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Lesci, G. F.
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Lesgourgues, J.
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Liaudat, T. I.
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Liu, S. J.
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Macias-Perez, J.
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Mannucci, F.
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Maoli, R.
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Martins, C. J. A. P.
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Maurin, L.
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Miluzio, M.
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Monaco, P.
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Moretti, C.
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Morgante, G.
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Navarro-Alsina, A.
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Nicastro, L.
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Paterson, K.
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Patrizii, L.
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Potter, D.
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Quai, S.
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Radovich, M.
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Rocci, P.-F.
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Sacquegna, S.
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Sahlén, M.
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Sanders, D. B.
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Sarpa, E.
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Schultheis, M.
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Sciotti, D.
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Sellentin, E.
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Tanidis, K.
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Tao, C.
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Testera, G.
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Teyssier, R.
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Tosi, S.
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Troja, A.
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Tucci, M.
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Venhola, A.
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Vergani, D.
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Verza, G.
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Scott, D.
Abstract
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The Euclid Q1 fields were selected for calibration purposes in cosmology and are therefore relatively devoid of nearby galaxies. However, this is precisely what makes them interesting fields in which to search for dwarf galaxies in local density environments. We took advantage of the unprecedented depth, spatial resolution, and field of view of the Euclid Quick Release (Q1) to build a census of dwarf galaxies in these regions. We have identified dwarf galaxies in a representative sample of 25 contiguous tiles in the Euclid Deep Field North (EDF-N) covering an area of 14.25 deg2. The dwarf galaxy candidates were identified using a semi-automatic detection method based on properties measured by the Euclid pipeline and released as part of the catalogue produced by the MERge Processing Function (MER PF) pipeline. A selection cut in surface brightness and magnitude was used to produce an initial dwarf candidate catalogue, and this was followed by a cut in morphology (removing background spirals) and IE − HE colour (removing red ellipticals). This catalogue was then visually classified to produce a final sample of dwarf candidates, including their morphology, number of nuclei, globular cluster (GC) richness, and presence of a blue compact centre. We identified 2674 dwarf candidates, corresponding to 188 dwarfs per square degree. The visual classification of the dwarfs reveals a slightly uneven morphological mix of 58% ellipticals and 42% irregulars, with very few potentially GC-rich (1.0%) and nucleated (4.0%) candidates but a noticeable fraction (6.9%) of dwarfs with blue compact centres. The distance distribution of 388 (15%) of the dwarf candidates with spectroscopic redshifts peaks at about 400 Mpc. Their stellar mass distribution confirms that our selection effectively identifies dwarfs while minimising contamination. The most prominent dwarf overdensities are dominated by dwarf ellipticals, while dwarf irregulars are more evenly distributed across the field of view. This work highlights Euclid's remarkable ability to detect and characterise dwarf galaxies across diverse masses, distances, and environments.
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