Euclid preparation. Sensitivity to non-standard particle dark matter model
Creators: name: Euclid Collaboration
name: Lesgourgues, J.
name: Schwagereit, J.
name: Bucko, J.
name: Parimbelli, G.
name: Giri, S. K.
name: Hervas-Peters, F.
name: Schneider, A.
name: Archidiacono, M.
name: Pace, F.
name: Sakr, Z.
name: Amara, A.
name: Amendola, L.
name: Andreon, S.
name: Auricchio, N.
name: Aussel, H.
name: Baccigalupi, C.
name: Baldi, M.
name: Bardelli, S.
name: Bender, R.
name: Bodendorf, C.
name: Bonino, D.
name: Branchini, E.
name: Brescia, M.
name: Brinchmann, J.
name: Camera, S.
name: Capobianco, V.
name: Carbone, C.
name: Cardone, V. F.
name: Carretero, J.
name: Casas, S.
name: Castellano, M.
name: Castignani, G.
name: Cavuoti, S.
name: Cimatti, A.
name: Colodro-Conde, C.
name: Congedo, G.
name: Conselice, C. J.
name: Conversi, L.
name: Copin, Y.
name: Courbin, F.
name: Courtois, H. M.
name: Da Silva, A.
name: Degaudenzi, H.
name: De Lucia, G.
name: Di Giorgio, A. M.
name: Douspis, M.
name: Dubath, F.
name: Dupac, X.
name: Dusini, S.
name: Farina, M.
name: Farrens, S.
name: Ferriol, S.
name: Fosalba, P.
name: Frailis, M.
name: Franceschi, E.
name: Fumana, M.
name: Galeotta, S.
name: Gillis, B.
name: Giocoli, C.
name: Grazian, A.
name: Grupp, F.
name: Guzzo, L.
name: Haugan, S. V. H.
name: Hoekstra, H.
name: Holmes, W.
name: Hook, I.
name: Hormuth, F.
name: Hornstrup, A.
name: Ilić, S.
name: Jahnke, K.
name: Joachimi, B.
name: Keihänen, E.
name: Kermiche, S.
name: Kiessling, A.
name: Kubik, B.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Laureijs, R.
name: Ligori, S.
name: Lilje, P. B.
name: Lindholm, V.
name: Lloro, I.
name: Mainetti, G.
name: Maino, D.
name: Maiorano, E.
name: Mansutti, O.
name: Marggraf, O.
name: Markovic, K.
name: Martinelli, M.
name: Martinet, N.
name: Marulli, F.
name: Massey, R.
name: Medinaceli, E.
name: Mei, S.
name: Mellier, Y.
name: Meneghetti, M.
name: Merlin, E.
name: Meylan, G.
name: Moresco, M.
name: Moscardini, L.
name: Munari, E.
name: Nakajima, R.
name: Neissner, C.
name: Niemi, S. -M.
name: Nightingale, J. W.
name: Padilla, C.
name: Paltani, S.
name: Pasian, F.
name: Pedersen, K.
name: Percival, W. J.
name: Pettorino, V.
name: Polenta, G.
name: Poncet, M.
name: Popa, L. A.
name: Raison, F.
name: Rebolo, R.
name: Renzi, A.
name: Rhodes, J.
name: Riccio, G.
name: Romelli, E.
name: Roncarelli, M.
name: Saglia, R.
name: Sánchez, A. G.
name: Sapone, D.
name: Sartoris, B.
name: Scaramella, R.
name: Schewtschenko, J. A.
name: Schneider, P.
name: Schrabback, T.
name: Secroun, A.
name: Sefusatti, E.
name: Seidel, G.
name: Serrano, S.
name: Sirignano, C.
name: Sirri, G.
name: Stanco, L.
name: Steinwagner, J.
name: Tallada-Crespí, P.
name: Tereno, I.
name: Toledo-Moreo, R.
name: Torradeflot, F.
name: Tutusaus, I.
name: Valenziano, L.
name: Vassallo, T.
name: Veropalumbo, A.
name: Wang, Y.
name: Weller, J.
name: Zamorani, G.
name: Zucca, E.
name: Biviano, A.
name: Boucaud, A.
name: Bozzo, E.
name: Burigana, C.
name: Calabrese, M.
name: Di Ferdinando, D.
name: Vigo, J. A. Escartin
name: Fabbian, G.
name: Farinelli, R.
name: Gracia-Carpio, J.
name: Mauri, N.
name: Nucita, A. A.
name: Scottez, V.
name: Tenti, M.
name: Viel, M.
name: Wiesmann, M.
name: Akrami, Y.
name: Anselmi, S.
name: Ballardini, M.
name: Bertacca, D.
name: Blot, L.
name: Böhringer, H.
name: Borgani, S.
name: Bruton, S.
name: Cabanac, R.
name: Calabro, A.
name: Cappi, A.
name: Carvalho, C. S.
name: Castro, T.
name: Chambers, K. C.
name: Contarini, S.
name: Cooray, A. R.
name: Davini, S.
name: De Caro, B.
name: de la Torre, S.
name: Desprez, G.
name: Díaz-Sánchez, A.
name: Di Domizio, S.
name: Dole, H.
name: Escoffier, S.
name: Ferrari, A. G.
name: Ferreira, P. G.
name: Ferrero, I.
name: Finelli, F.
name: Fornari, F.
name: Gabarra, L.
name: Ganga, K.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Giacomini, F.
name: Gozaliasl, G.
name: Hildebrandt, H.
name: Hjorth, J.
name: Munñoz, A. Jimenez
name: Joudaki, S.
name: Kajava, J. J. E.
name: Kansal, V.
name: Karagiannis, D.
name: Kirkpatrick, C. C.
name: Legrand, L.
name: Libet, G.
name: Loureiro, A.
name: Macias-Perez, J.
name: Maggio, G.
name: Magliocchetti, M.
name: Mannucci, F.
name: Maoli, R.
name: Martins, C. J. A. P.
name: Matthew, S.
name: Maurin, L.
name: Metcalf, R. B.
name: Migliaccio, M.
name: Monaco, P.
name: Moretti, C.
name: Morgante, G.
name: Nadathur, S.
name: Walton, Nicholas A.
name: Patrizii, L.
name: Pezzotta, A.
name: Pöntinen, M.
name: Popa, V.
name: Porciani, C.
name: Potter, D.
name: Reimberg, P.
name: Risso, I.
name: Rocci, P. -F.
name: Sahlén, M.
name: Sereno, M.
name: Simon, P.
name: Mancini, A. Spurio
name: Tao, C.
name: Tessore, N.
name: Testera, G.
name: Teyssier, R.
name: Toft, S.
name: Tosi, S.
name: Troja, A.
name: Tucci, M.
name: Valieri, C.
name: Valiviita, J.
name: Vergani, D.
name: Verza, G.
Publisher: name: arXiv
Year: 2024
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The Euclid mission of the European Space Agency will provide weak gravitational lensing and galaxy clustering surveys that can be used to constrain the standard cosmological model and its extensions, with an opportunity to test the properties of dark matter beyond the minimal cold dark matter paradigm. We present forecasts from the combination of these surveys on the parameters describing four interesting and representative non-minimal dark matter models: a mixture of cold and warm dark matter relics; unstable dark matter decaying either into massless or massive relics; and dark matter experiencing feeble interactions with relativistic relics. We model these scenarios at the level of the non-linear matter power spectrum using emulators trained on dedicated N-body simulations. We use a mock Euclid likelihood to fit mock data and infer error bars on dark matter parameters marginalised over other parameters. We find that the Euclid photometric probe (alone or in combination with CMB data from the Planck satellite) will be sensitive to the effect of each of the four dark matter models considered here. The improvement will be particularly spectacular for decaying and interacting dark matter models. With Euclid, the bounds on some dark matter parameters can improve by up to two orders of magnitude compared to current limits. We discuss the dependence of predicted uncertainties on different assumptions: inclusion of photometric galaxy clustering data, minimum angular scale taken into account, modelling of baryonic feedback effects. We conclude that the Euclid mission will be able to measure quantities related to the dark sector of particle physics with unprecedented sensitivity. This will provide important information for model building in high-energy physics. Any hint of a deviation from the minimal cold dark matter paradigm would have profound implications for cosmology and particle physics.
description: 31 pages, 21 figures