October
2024
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2024A&A...690A..30E
Authors
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Euclid Collaboration
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Dournac, F.
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Blanchard, A.
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Ilić, S.
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Lamine, B.
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Tutusaus, I.
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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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Baldi, M.
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Bardelli, S.
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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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Brinchmann, J.
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Camera, S.
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Capobianco, V.
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Carretero, J.
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Casas, S.
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Castellano, M.
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Cavuoti, S.
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Cimatti, A.
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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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Courbin, F.
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Courtois, H. M.
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Da Silva, A.
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Degaudenzi, H.
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Di Giorgio, A. M.
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Dinis, J.
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Douspis, M.
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Dubath, F.
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Dupac, X.
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Dusini, S.
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Ealet, A.
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Farina, M.
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Farrens, S.
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Ferriol, S.
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Frailis, M.
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Franceschi, E.
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Galeotta, S.
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Gillard, W.
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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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Haugan, S. V. H.
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Holmes, W.
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Hook, I.
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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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Keihänen, E.
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Kermiche, S.
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Kiessling, A.
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Kilbinger, M.
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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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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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Maino, D.
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Maiorano, E.
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Mansutti, O.
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Marggraf, O.
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Markovic, K.
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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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Medinaceli, E.
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Mei, S.
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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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Moresco, M.
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Moscardini, L.
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Munari, E.
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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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Saglia, R.
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Sapone, D.
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Schneider, P.
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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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Sirignano, C.
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Sirri, G.
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Stanco, L.
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Surace, C.
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Tallada-Crespí, P.
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Tavagnacco, D.
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Taylor, A. N.
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Tereno, I.
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Toledo-Moreo, R.
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Torradeflot, F.
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Valentijn, E. A.
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Valenziano, L.
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Vassallo, T.
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Veropalumbo, A.
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Wang, Y.
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Zacchei, A.
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Zamorani, G.
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Zoubian, J.
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Zucca, E.
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Biviano, A.
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Bolzonella, M.
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Boucaud, A.
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Bozzo, E.
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Burigana, C.
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Colodro-Conde, C.
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De Lucia, G.
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Di Ferdinando, D.
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Escartin Vigo, J. A.
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Farinelli, R.
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Gracia-Carpio, J.
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Mainetti, G.
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Martinelli, M.
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Mauri, N.
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Neissner, C.
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Sakr, Z.
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Scottez, V.
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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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Allevato, V.
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Anselmi, S.
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Baccigalupi, C.
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Balaguera-Antolinez, A.
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Ballardini, M.
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Blot, L.
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Borgani, S.
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Bruton, S.
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Cabanac, R.
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Calabro, A.
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Canas-Herrera, G.
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Cappi, A.
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Carvalho, C. S.
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Castignani, G.
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Castro, T.
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Chambers, K. C.
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Contarini, S.
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Cooray, A. R.
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Coupon, J.
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Davini, S.
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De Caro, B.
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de la Torre, S.
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Desprez, G.
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Díaz-Sánchez, A.
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Di Domizio, S.
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Dole, H.
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Escoffier, S.
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Ferrari, A. G.
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Ferreira, P. G.
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Ferrero, I.
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Finelli, F.
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Gabarra, L.
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Ganga, K.
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García-Bellido, J.
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Gaztanaga, E.
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Giacomini, F.
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Gozaliasl, G.
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Hildebrandt, H.
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Jimenez Munoz, A.
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Kajava, J. J. E.
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Kansal, V.
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Karagiannis, D.
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Kirkpatrick, C. C.
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Legrand, L.
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Libet, G.
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Loureiro, A.
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Macias-Perez, J.
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Maggio, G.
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Magliocchetti, M.
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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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Matthew, S.
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Maurin, L.
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Metcalf, R. B.
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Migliaccio, M.
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Monaco, P.
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Moretti, C.
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Morgante, G.
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Nadathur, S.
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Walton, N. A.
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Patrizii, L.
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Pezzotta, A.
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Pöntinen, M.
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Popa, V.
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Porciani, C.
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Potter, D.
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Risso, I.
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Rocci, P. -F.
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Sahlén, M.
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Sánchez, A. G.
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Schewtschenko, J. A.
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Schneider, A.
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Sefusatti, E.
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Sereno, M.
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Steinwagner, J.
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Tessore, N.
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Testera, G.
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Teyssier, R.
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Toft, S.
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Tosi, S.
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Troja, A.
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Tucci, M.
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Valiviita, J.
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Vergani, D.
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Verza, G.
Abstract
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Future data provided by the Euclid mission will allow us to better understand the cosmic history of the Universe. A metric of its performance is the figure-of-merit (FoM) of dark energy, usually estimated with Fisher forecasts. The expected FoM has previously been estimated taking into account the two main probes of Euclid, namely the three-dimensional clustering of the spectroscopic galaxy sample, and the so-called 3×2pt signal from the photometric sample (i.e., the weak lensing signal, the galaxy clustering, and their cross-correlation). So far, these two probes have been treated as independent. In this paper, we introduce a new observable given by the ratio of the (angular) two-point correlation function of galaxies from the two surveys. For identical (normalised) selection functions, this observable is unaffected by sampling noise, and its variance is solely controlled by Poisson noise. We present forecasts for Euclid where this multi-tracer method is applied and is particularly relevant because the two surveys will cover the same area of the sky. This method allows for the exploitation of the combination of the spectroscopic and photometric samples. When the correlation between this new observable and the other probes is not taken into account, a significant gain is obtained in the FoM, as well as in the constraints on other cosmological parameters. The benefit is more pronounced for a commonly investigated modified gravity model, namely the γ parametrisation of the growth factor. However, the correlation between the different probes is found to be significant and hence the actual gain is uncertain. We present various strategies for circumventing this issue and still extract useful information from the new observable.
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