Euclid: Constraining linearly scale-independent modifications of gravity with the spectroscopic and photometric primary probes

Article
Report number	arXiv:2306.12368
Title	Euclid: Constraining linearly scale-independent modifications of gravity with the spectroscopic and photometric primary probes
Author(s)	Frusciante, N. (Naples U.) ; Pace, F. (Turin U. ; INFN, Turin ; Turin Observ.) ; Cardone, V.F. (Rome Observ. ; Rome U.) ; Casas, S. (Unlisted, GE) ; Tutusaus, I. (Geneva U. ; Barcelona, IEEC ; IRAP, Toulouse) ; Ballardini, M. (Ferrara U. ; Bologna U. ; Bologna Observ. ; INFN, Bologna) ; Bellini, E. (INFN, Trieste ; SISSA, Trieste ; IFPU, Trieste ; Geneva U.) ; Benevento, G. (Johns Hopkins U.) ; Bose, B. (Edinburgh U., Inst. Astron. ; Geneva U. ; Zurich U.) ; Valageas, P. (IPhT, Saclay) ; Bartolo, N. (U. Padua, Dept. Phys. Astron. ; INFN, Padua ; Padua Observ.) ; Brax, P. (IPhT, Saclay ; CERN) ; Ferreira, P.G. (Oxford U.) ; Finelli, F. (Bologna Observ. ; INFN, Bologna) ; Koyama, K. (Portsmouth U., ICG) ; Legrand, L. (Geneva U.) ; Lombriser, L. (Geneva U.) ; Paoletti, D. (Bologna Observ. ; INFN, Bologna) ; Pietroni, M. (ICJ, Lyon ; Parma U.) ; Rozas-Fernández, A. (Lisbon U.) ; Sakr, Z. (Paris, Inst. Astrophys. ; U. Heidelberg, ITP ; USJ, Beirut) ; Silvestri, A. (Leiden U.) ; Vernizzi, F. (IPhT, Saclay) ; Winther, H.A. (Inst. Theor. Astrophys., Oslo) ; Aghanim, N. (Orsay, IAS) ; Amendola, L. (U. Heidelberg, ITP) ; Auricchio, N. (Bologna Observ.) ; Azzollini, R. (Mullard Space Sci. Lab.) ; Baldi, M. (Bologna U. ; Bologna Observ. ; INFN, Bologna) ; Bonino, D. (Turin Observ.) ; Branchini, E. (Genoa U. ; INFN, Genoa ; INFN, Rome3) ; Brescia, M. (Naples U. ; Capodimonte Observ.) ; Brinchmann, J. (Porto U., Astron. Dept.) ; Camera, S. (Turin U. ; INFN, Turin ; Turin Observ.) ; Capobianco, V. (Turin Observ.) ; Carbone, C. (IASF, Milan) ; Carretero, J. (Barcelona, IFAE) ; Castellano, M. (Rome Observ.) ; Cavuoti, S. (Capodimonte Observ. ; INFN, Naples) ; Cimatti, A. (Bologna U. ; Trieste Observ.) ; Cledassou, R. (CNES, Toulouse ; Paris, IN2P3) ; Congedo, G. (Edinburgh U., Inst. Astron.) ; Conversi, L. (European Space Agency ; ESA, Madrid) ; Copin, Y. (IP2I, Lyon) ; Corcione, L. (Turin Observ.) ; Courbin, F. (LASTRO Observ.) ; Cropper, M. (Mullard Space Sci. Lab.) ; Da Silva, A. (Lisbon U.) ; Degaudenzi, H. (U. Geneva (main)) ; Dinis, J. (Lisbon U.) ; Dubath, F. (U. Geneva (main)) ; Dupac, X. (ESA, Madrid) ; Dusini, S. (INFN, Padua) ; Farrens, S. (AIM, Saclay) ; Ferriol, S. (IP2I, Lyon) ; Fosalba, P. (Barcelona, IEEC) ; Frailis, M. (Trieste Observ.) ; Franceschi, E. (Bologna Observ.) ; Galeotta, S. (Trieste Observ.) ; Gillis, B. (Edinburgh U., Inst. Astron.) ; Giocoli, C. (Bologna Observ. ; INFN, Bologna) ; Grazian, A. (Padua Observ.) ; Grupp, F. (Garching, Max Planck Inst., MPE ; Munich U.) ; Guzzo, L. (Milan U. ; INFN, Milan ; Brera Observ.) ; Haugan, S.V. H. (Inst. Theor. Astrophys., Oslo) ; Holmes, W. (Caltech, JPL) ; Hormuth, F. (Unlisted, DE) ; Hornstrup, A. (Denmark, Tech. U.) ; Jahnke, K. (Heidelberg, Max Planck Inst. Astron.) ; Kermiche, S. (Marseille, CPPM) ; Kiessling, A. (Caltech, JPL) ; Kilbinger, M. (AIM, Saclay) ; Kitching, T. (Mullard Space Sci. Lab.) ; Kunz, M. (Geneva U.) ; Kurki-Suonio, H. (Helsinki Inst. of Phys.) ; Ligori, S. (Turin Observ.) ; Lilje, P.B. (Inst. Theor. Astrophys., Oslo) ; Lloro, I. (ASTRON, Dwingeloo) ; Maiorano, E. (Bologna Observ.) ; Mansutti, O. (Trieste Observ.) ; Marggraf, O. (Argelander Inst. Astron.) ; Markovic, K. (Caltech, JPL) ; Marulli, F. (U. Bologna, DIFA ; Bologna Observ. ; INFN, Bologna) ; Massey, R. (Durham U., ICC) ; Medinaceli, E. (Bologna Observ.) ; Meneghetti, M. (INFN, Bologna ; Bologna Observ.) ; Meylan, G. (LASTRO Observ.) ; Moresco, M. (U. Bologna, DIFA ; Bologna Observ.) ; Moscardini, L. (U. Bologna, DIFA ; Bologna Observ. ; INFN, Bologna) ; Munari, E. (Trieste Observ.) ; Niemi, S.M. (ESTEC, Noordwijk) ; Nightingale, J. (Durham U., ICC) ; Padilla, C. (Barcelona, IFAE) ; Paltani, S. (U. Geneva (main)) ; Pasian, F. (Trieste Observ.) ; Pedersen, K. (Aarhus U.) ; Percival, W.J. (Waterloo U., Math. Dept. ; Waterloo U. ; Perimeter Inst. Theor. Phys.) ; Pettorino, V. (AIM, Saclay) ; Polenta, G. (ASI, Rome) ; Poncet, M. (CNES, Toulouse) ; Popa, L. (Bucharest, Inst. Space Science) ; Raison, F. (Garching, Max Planck Inst., MPE) ; Rebolo, R. (IAC, La Laguna ; Laguna U., Tenerife) ; Renzi, A. (U. Padua, Dept. Phys. Astron. ; INFN, Padua) ; Rhodes, J. (Caltech, JPL) ; Riccio, G. (Capodimonte Observ.) ; Romelli, E. (Trieste Observ.) ; Saglia, R. (Garching, Max Planck Inst., MPE ; Munich U.) ; Sapone, D. (Chile U., Beauchef) ; Sartoris, B. (Munich U. ; Trieste Observ.) ; Secroun, A. (Marseille, CPPM) ; Seidel, G. (Heidelberg, Max Planck Inst. Astron.) ; Sirignano, C. (U. Padua, Dept. Phys. Astron. ; INFN, Padua) ; Sirri, G. (INFN, Bologna) ; Stanco, L. (INFN, Padua) ; Surace, C. (Marseille, Lab. Astrophys.) ; Tallada-Crespí, P. (Madrid, CIEMAT ; Madrid, Escuela Tec. Sup. Ing. Ind. ; Barcelona, IFAE) ; Taylor, A.N. (Edinburgh U., Inst. Astron.) ; Tereno, I. (Lisbon U. ; Lisbon Astron. Observ.) ; Toledo-Moreo, R. (Cartagena Politecnica U.) ; Torradeflot, F. (Madrid, CIEMAT ; Madrid, Escuela Tec. Sup. Ing. Ind. ; Barcelona, IFAE) ; Valentijn, E.A. (Kapteyn Astron. Inst., Groningen) ; Valenziano, L. (Bologna Observ. ; INFN, Bologna) ; Vassallo, T. (Trieste Observ.) ; Kleijn, G.A. Verdoes (Kapteyn Astron. Inst., Groningen) ; Wang, Y. (Caltech) ; Zacchei, A. (Trieste Observ.) ; Zamorani, G. (Bologna Observ.) ; Zoubian, J. (Marseille, CPPM) ; Scottez, V. (Paris, Inst. Astrophys.)
Publication	2024-10-01
Imprint	2023-06-21
Number of pages	22
In:	Astron. Astrophys. 690 (2024) A133
DOI	10.1051/0004-6361/202347526 (publication)
Subject category	gr-qc ; General Relativity and Cosmology ; astro-ph.CO ; Astrophysics and Astronomy
Accelerator/Facility, Experiment	EUCLID
Abstract	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, $\omega_{\rm BD}$, $\Omega_{\rm rc}$ and $\epsilon_{2,0}$. 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 $\log_{10}{\omega_{\rm BD}}$, with a fiducial value of $\omega_{\rm BD}=800$, 27.1% using GCsp alone, 3.6% using GCph+WL+XC and 3.2% using GCph+WL+XC+GCsp; for $\log_{10}{\Omega_{\rm rc}}$, with a fiducial value of $\Omega_{\rm rc}=0.25$, we find 93.4%, 20% and 15% respectively; and finally, for $\epsilon_{2,0}=-0.04$, we find 3.4%, 0.15%, and 0.14%. (abridged)
Copyright/License	preprint: (License: CC BY 4.0) publication: © 2024 The Authors (License: CC BY 4.0)

$Large-scale structure observables for the different MG models considered in this work evaluated at the fiducial values of the model parameters used for the Fisher matrix analysis. {\bf Top Left}: The linear (dashed) and nonlinear (solid lines) matter power spectrum $P_{\delta \delta}(z,k)$ entering Eqs.~(\ref{eq:pk_dw}) and (\ref{eq:ISTrecipe}), respectively, evaluated at redshift $z=0$, for KM1 ($\epsilon_{2,0}=-0.04$, blue), JBD1 ($\omega_{\rm BD}=800$, red) and nDGP1 ($\Omega_{\rm rc}=0.25$, green). {\bf Top Right}: Ratio of the matter power spectra for the above mentioned models with respect to their \lcdm\ counterpart with the same value of $\sigma_8$ today, both for the linear (dashed) and nonlinear (solid) cases. While for nDGP1 and JBD1 the linear ratio remains constant, in the case of KM1 the ratio shows large-scale damping and oscillatory features that appear at scales around $k \approx 0.1\,h\, \mathrm{Mpc}^{-1}$. {\bf Bottom Left}: Cosmic shear (WL) angular power spectra for the first bin $i=j=1$, defined in Eq.~(\ref{eq:ISTrecipe}) for the three models considered above, with the same legend labels. {\bf Bottom Right}: Ratio of the cosmic shear $C_{i,j}(\ell)$ to their \lcdm\ counterpart, for the bin combination $i=j=1$. For JBD1 and nDGP1 the suppression in the nonlinear power spectrum can also be seen as a suppression of the lensing angular spectra. For KM1, however, although the nonlinear power spectrum is also decreased at small scales the lensing enhancement function $\Sigma$ defined in Eq.~(\ref{mu_Sigma_KM}) is larger than 1 at $z$ 0$, giving an overall increase in the lensing $C_{i,j}(\ell)$ when compared to \lcdm." width="200px"/> $Large-scale structure observables for the different MG models evaluated at the fiducial values of the model parameters used for the Fisher matrix analysis. {\bf Top left}: Linear (dashed) and non-linear (solid lines) matter power spectrum $P_{\delta \delta}(z,k)$ entering Eqs.~(\ref{eq:pk_dw}) and (\ref{eq:ISTrecipe}), respectively, evaluated at redshift $z=0$, for KM1 ($\epsilon_{2,0}=-0.04$, blue), JBD1 ($\omega_{\rm BD}=800$, red) and nDGP1 ($\Omega_{\rm rc}=0.25$, green). {\bf Top right}: Ratio of the matter power spectra for the above mentioned models with respect to their \lcdm\ counterpart with the same value of $\sigma_8$ today, for the linear (dashed) and non-linear (solid) cases. {\bf Bottom left}: Cosmic shear (WL) angular power spectra for the auto-correlation of the first photometric bin $C^{\rm WL}_{1,1}(\ell)$ (solid line) and the cross-correlation of the first and last bin $C^{\rm WL}_{1,10}(\ell)$ (dotted line), defined in Eq.~(\ref{eq:ISTrecipe}) for the three models considered above, with the same colour labelling. {\bf Bottom right}: Ratio of the cosmic shear $C_{i,j}(\ell)$ to their \lcdm\ counterpart, for the bin combination $i=j=1$ and $i=1; j=10$.$ $Marginalised $1\sigma$ errors on the models' parameters relative to their corresponding fiducial values, for JBD (case 1 in blue and case 2 in cyan), nDGP (case 1 in green and case 2 in light green) and KM (case 1 in red and case 2 in light red). We show the marginalised $1\sigma$ errors for \GCsp\ in the optimistic (dotted area), pessimistic (dashed area) and quasi-linear (filled area) scenarios (top panel), for WL+XC+\GCph\ in the optimistic and pessimistic cases (central panel) and for the \GCsp+WL+XC+\GCph\ in the the optimistic and pessimistic cases.$ Show more plots

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