Euclid: Constraining linearly scale-independent modifications of gravity with the spectroscopic and photometric primary probes
Creators: name: Frusciante, N.
name: Pace, F.
name: Cardone, V. F.
name: Casas, S.
name: Tutusaus, I.
name: Ballardini, M.
name: Bellini, E.
name: Benevento, G.
name: Bose, B.
name: Valageas, P.
name: Bartolo, N.
name: Brax, P.
name: Ferreira, P. G.
name: Finelli, F.
name: Koyama, K.
name: Legrand, L.
name: Lombriser, L.
name: Paoletti, D.
name: Pietroni, M.
name: Rozas-Fernández, A.
name: Sakr, Z.
name: Silvestri, A.
name: Vernizzi, F.
name: Winther, H. A.
name: Aghanim, N.
name: Amendola, L.
name: Auricchio, N.
name: Azzollini, R.
name: Baldi, M.
name: Bonino, D.
name: Branchini, E.
name: Brescia, M.
name: Brinchmann, J.
name: Camera, S.
name: Capobianco, V.
name: Carbone, C.
name: Carretero, J.
name: Castellano, M.
name: Cavuoti, S.
name: Cimatti, A.
name: Cledassou, R.
name: Congedo, G.
name: Conversi, L.
name: Copin, Y.
name: Corcione, L.
name: Courbin, F.
name: Cropper, M.
name: Da Silva, A.
name: Degaudenzi, H.
name: Dinis, J.
name: Dubath, F.
name: Dupac, X.
name: Dusini, S.
name: Farrens, S.
name: Ferriol, S.
name: Fosalba, P.
name: Frailis, M.
name: Franceschi, E.
name: Galeotta, S.
name: Gillis, B.
name: Giocoli, C.
name: Grazian, A.
name: Grupp, F.
name: Guzzo, L.
name: Haugan, S. V. H.
name: Holmes, W.
name: Hormuth, F.
name: Hornstrup, A.
name: Jahnke, K.
name: Kermiche, S.
name: Kiessling, A.
name: Kilbinger, M.
name: Kitching, T.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Ligori, S.
name: Lilje, P. B.
name: Lloro, I.
name: Maiorano, E.
name: Mansutti, O.
name: Marggraf, O.
name: Markovic, K.
name: Marulli, F.
name: Massey, R.
name: Medinaceli, E.
name: Meneghetti, M.
name: Meylan, G.
name: Moresco, M.
name: Moscardini, L.
name: Munari, E.
name: Niemi, S. M.
name: Nightingale, J.
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.
name: Raison, F.
name: Rebolo, R.
name: Renzi, A.
name: Rhodes, J.
name: Riccio, G.
name: Romelli, E.
name: Saglia, R.
name: Sapone, D.
name: Sartoris, B.
name: Secroun, A.
name: Seidel, G.
name: Sirignano, C.
name: Sirri, G.
name: Stanco, L.
name: Surace, C.
name: Tallada-Crespí, P.
name: Taylor, A. N.
name: Tereno, I.
name: Toledo-Moreo, R.
name: Torradeflot, F.
name: Valentijn, E. A.
name: Valenziano, L.
name: Vassallo, T.
name: Kleijn, G. A. Verdoes
name: Wang, Y.
name: Zacchei, A.
name: Zamorani, G.
name: Zoubian, J.
name: Scottez, V.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: General Relativity and Quantum Cosmology (gr-qc)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The future Euclid space satellite mission will offer an invaluable opportunity to constrain modifications to Einstein's general relativity at cosmic scales. We focus on modified gravity models characterised, at linear scales, by a scale-independent growth of perturbations while featuring different testable types of derivative screening mechanisms at smaller non-linear scales. We considered three specific models, namely JBD, a scalar-tensor theory with a flat potential, the nDGP gravity, a braneworld model in which our Universe is a four-dimensional brane embedded in a five-dimensional Minkowski space-time, and $k$-mouflage (KM) gravity, an extension of $k$-essence scenarios with a universal coupling of the scalar field to matter. In preparation for real data, we provide forecasts from spectroscopic and photometric primary probes by Euclid on the cosmological parameters and the additional parameters of the models, respectively, $ω_{\rm BD}$, $Ω_{\rm rc}$ and $ε_{2,0}$. The forecast analysis employs the Fisher matrix method applied to weak lensing (WL); photometric galaxy clustering (GCph), spectroscopic galaxy clustering (GCsp) and the cross-correlation (XC) between GCph and WL. In an optimistic setting at 68.3\% confidence interval, we find the following percentage relative errors with Euclid alone: for $\log_{10}{ω_{\rm BD}}$, with a fiducial value of $ω_{\rm BD}=800$, 27.1\% using GCsp alone, 3.6\% using GCph+WL+XC and 3.2\% using GCph+WL+XC+GCsp; for $\log_{10}{Ω_{\rm rc}}$, with a fiducial value of $Ω_{\rm rc}=0.25$, we find 93.4\%, 20\% and 15\% respectively; and finally, for $ε_{2,0}=-0.04$, we find 3.4\%, 0.15\%, and 0.14\%. (abridged)
description: 23 pages, 8 figures, 4 tables, 1 appendix, matches Journal version