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

Context . The future Euclid space satellite mission will offer an invaluable opportunity to constrain modifications to Einstein’s general relativity at cosmic scales. In this paper, 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. Aims . We considered three specific models, namely Jordan-Brans-Dicke, a scalar-tensor theory with a flat potential, the normal branch of Dvali-Gabadadze-Porrati (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 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 BD , Ω гc and ϵ 2,0 , which quantify the deviations from general relativity. This analysis will improve our knowledge of the cosmology of these modified gravity models. Methods . The forecast analysis employs the Fisher matrix method applied to weak lensing (WL); photometric galaxy clustering (GC ph ), spectroscopic galaxy clustering (GC sp ) and the cross-correlation (XC) between GC ph and WL. For the Euclid survey specifications, we define three scenarios that are characterised by different cuts in the maximum multipole and wave number, to assess the constraining power of non-linear scales. For each model we considered two fiducial values for the corresponding model parameter. Results . In an optimistic setting at 68.3% confidence interval, we find the following percentage relative errors with Euclid alone: for log 10 ω BD , with a fiducial value of ω BD = 800, 27.1% using GC sp alone, 3.6% using GC ph +WL+XC and 3.2% using GC ph +WL+XC+GC sp ; for log 10 Ω гc , with a fiducial value of Ω гc = 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%. From the relative errors for fiducial values closer to their ΛCDM limits, we find that most of the constraining power is lost. Our results highlight the importance of the constraining power from non-linear scales.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-10-01
DOI
https://doi.org/10.1051/0004-6361/202347526
Citations
14
Primary Topic
Cosmology and Gravitation Theories
Type
article
Field-Weighted Citation Impact
4.64

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article

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

G. Seidel, J. Brinchmann, M. Ballardini, Emilio Bellini et al.
14 citations
Astronomy and Astrophysics
Cosmology and Gravitation Theories
4.64
article

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

G. Seidel, J. Brinchmann, M. Ballardini, Emilio Bellini, R. P. Saglia, G. Riccio, C. Sirignano, M. Brescia, M. Kunz, L. Amendola, J. Carretero, F. Marulli, O. Marggraf, V. F. Cardone, F. Courbin, Y. Copin, D. Paoletti, Santiago Casas, A. Grazian, G. Sirri, E Maiorano, Noemi Frusciante, E. Munari, R. Azzollini, Lucas Lombriser, V. Capobianco, S. Farrens, S. Cavuoti, A. Kiessling, S. V. H. Haugan, R. Massey, T. Vassallo, R. Toledo-Moreo, M. Moresco, D. Sapone, S. M. Niemi, M. Meneghetti, D. Bonino, J.W Nightingale, M. Poncet, L. Valenziano, Alberto Rozas-Fernández, A. Cimatti, O. Mansutti, G. Zamorani, P. Tallada-Crespí, A. N. Taylor, C. Padilla Aranda, B. Gillis, C. Giocoli, F. Dubath, H. Degaudenzi, A. Hornstrup, Benjamin Bose, E. Medinaceli, Patrick Valageas, Massimo Pietroni, R. Cledassou, F. Pasian, L. Guzzo, S. Ligori, M. Castellano, T. Kitching, F. Grupp, A. Zacchei, S. Galeotta, F. Raison, E. Franceschi, E. A. Valentijn, K Jahnke, Marco Baldi, K. Pedersen, S. Dusini, K. Koyama, K. Markovič, Philippe Brax, S. Camera, Hans A. Winther, L. Legrand, Giampaolo Benevento, M. Kilbinger, F. Finelli⋆, J. Dinis, Jason Rhodes, R. Rébolo, L. Conversi, M. Cropper, P. G. Ferreira, E. Romelli, N. Auricchio, M. Frailis, C. Carbone, S. Kermiche, L. Corcione, S. Ferriol, W.J Percival, P. B. Lilje, F. Torradeflot, G. Polenta, E. Branchini, A. Secroun, Yun Wang, A. Da Silva, L. Stančo, Francesco Pace, Alessandra Silvestri, I. Tutusaus, N. Aghanim, B. Sartoris, J. Zoubian, F. Hormuth, I. Tereno, V. Pettorino, A. Renzi, L. A. Popa, G. Meylan, F. Vernizzi, V. Scottez, H. Kurki‐Suonio, Z. Sakr, W. A. Holmes, P. Fosalba, N. Bartolo, X Dupac, S. Paltani, G. A. Verdoes Kleijn, L. Moscardini, I. Lloro, G. Congedo
article en
14 citations

Abstract

Context . The future Euclid space satellite mission will offer an invaluable opportunity to constrain modifications to Einstein’s general relativity at cosmic scales. In this paper, 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. Aims . We considered three specific models, namely Jordan-Brans-Dicke, a scalar-tensor theory with a flat potential, the normal branch of Dvali-Gabadadze-Porrati (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 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 BD , Ω гc and ϵ 2,0 , which quantify the deviations from general relativity. This analysis will improve our knowledge of the cosmology of these modified gravity models. Methods . The forecast analysis employs the Fisher matrix method applied to weak lensing (WL); photometric galaxy clustering (GC ph ), spectroscopic galaxy clustering (GC sp ) and the cross-correlation (XC) between GC ph and WL. For the Euclid survey specifications, we define three scenarios that are characterised by different cuts in the maximum multipole and wave number, to assess the constraining power of non-linear scales. For each model we considered two fiducial values for the corresponding model parameter. Results . In an optimistic setting at 68.3% confidence interval, we find the following percentage relative errors with Euclid alone: for log 10 ω BD , with a fiducial value of ω BD = 800, 27.1% using GC sp alone, 3.6% using GC ph +WL+XC and 3.2% using GC ph +WL+XC+GC sp ; for log 10 Ω гc , with a fiducial value of Ω гc = 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%. From the relative errors for fiducial values closer to their ΛCDM limits, we find that most of the constraining power is lost. Our results highlight the importance of the constraining power from non-linear scales.

Astronomy and AstrophysicsVol. 690
Université Claude Bernard Lyon 1 (FR), University of Geneva (CH), Leiden University (NL), California Institute of Technology (US), University of Parma (IT), Centre National de la Recherche Scientifique (FR), Institute of Space Sciences (ES), Jet Propulsion Laboratory (US), University of Helsinki (FI), Université Toulouse III - Paul Sabatier (FR), University of Bonn (DE), Scuola Internazionale Superiore di Studi Avanzati (IT), University of Padua (IT), University of Lisbon (PT), University of Trieste (IT), Johns Hopkins University (US), University of Waterloo (CA), Universidad de La Laguna (ES), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Universidade do Porto (PT), Perimeter Institute (CA), Saint Joseph University (LB), University of Oslo (NO), Institute for High Energy Physics (ES), University of Milan (IT), Durham University (GB), University of Ferrara (IT), University of Zurich (CH), Aarhus University (DK), Université Paris Cité (FR), Aix-Marseille Université (FR), Heidelberg University (DE), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris-Saclay (FR), Centre National d'Études Spatiales (FR), Arcetri Astrophysical Observatory (IT), Helsinki Institute of Physics (FI), Astronomical Observatory of Rome (IT), Agenzia Spaziale Italiana (IT), Trieste Astronomical Observatory (IT), Institut d'Astrophysique de Paris (FR), Astronomical Observatory of Capodimonte (IT), European Space Agency (FR), Brera Astronomical Observatory (IT), Universidad Politécnica de Cartagena (ES), Sorbonne Université (FR), University of Oxford (GB), Astrophysique, Instrumentation et Modélisation (FR), Institute of Astrophysics and Space Sciences (PT), Istituto Nazionale di Fisica Nucleare, Sezione di Roma Tre (IT), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Centre de physique des particules de Marseille (FR), Laboratoire d’Astrophysique de Marseille (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institut d'Astrophysique Spatiale (FR), Institut Camille Jordan (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Padova (IT), Osservatorio Astrofisico di Torino (IT), Royal Observatory (GB), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Max Planck Institute for Astronomy (DE), Château Gombert (FR), Université Bourgogne Franche-Comté (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), CEA Paris-Saclay (FR), Instituto de Astrofísica de Canarias (ES), Institut National de Physique Nucléaire et de Physique des Particules (FR), von Hoerner & Sulger (Germany) (DE), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Institute of Space Science - INFLPR Subsidiary (RO), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (IT), Port d'Informació Científica (ES), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (IT), Institute for Fundamental Physics of the Universe (IT), Institute of Nuclear Physics of Lyon (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Roma I (IT), Osservatorio Astronomico di Padova (IT), Institut de Physique Théorique (FR), European Space Research Institute (IT), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), Institut de Recherche en Astrophysique et Planétologie (FR), Infrared Processing and Analysis Center (US), Osservatorio di Astrofisica e Scienza dello Spazio, Institut de Physique des 2 Infinis de Lyon (FR), European Space Research and Technology Centre (NL), University College London (GB), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), University of Portsmouth (GB), European Organization for Nuclear Research (CH), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), Ludwig-Maximilians-Universität München (DE), National Institute for Astrophysics (IT), RWTH Aachen University (DE), Netherlands Institute for Radio Astronomy (NL), University of Bologna (IT), Technical University of Denmark (DK), University of Edinburgh (GB)
National Science Foundation, National Aeronautics and Space Administration, Ministerio de Ciencia, Innovación y Universidades, Dipartimenti di Eccellenza, European Space Agency, European Commission, Deutsche Forschungsgemeinschaft, Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, Academy of Finland, Ministero dell’Istruzione, dell’Università e della Ricerca, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación, Universidade de Lisboa, National Astronomical Observatory of Japan, Agenția Spațială Română, Istituto Nazionale di Fisica Nucleare, Norsk Romsenter, Horizon 2020 Framework Programme, Science and Technology Facilities Council, Fundação para a Ciência e a Tecnologia, Staatssekretariat für Bildung, Forschung und Innovation
Openalex Percentile: Top 5%
Cosmology and Gravitation Theories
4.64
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