<i>Euclid</i> preparation

Context . Deviations from Gaussianity in the distribution of the fields probed by large-scale structure surveys generate additional terms in the data covariance matrix, increasing the uncertainties in the measurement of the cosmological parameters. Super-sample covariance (SSC) is among the largest of these non-Gaussian contributions, with the potential to significantly degrade constraints on some of the parameters of the cosmological model under study – especially for weak-lensing cosmic shear. Aims . We compute and validate the impact of SSC on the forecast uncertainties on the cosmological parameters for the Euclid photo-metric survey, and investigate how its impact depends on the specific details of the forecast. Methods . We followed the recipes outlined by the Euclid Collaboration (EC) to produce 1 σ constraints through a Fisher matrix analysis, considering the Gaussian covariance alone and adding the SSC term, which is computed through the public code PySSC . The constraints are produced both by using Euclid ’s photometric probes in isolation and by combining them in the ‘3×2pt’ analysis. Results . We meet EC requirements on the forecasts validation, with an agreement at the 10% level between the mean results of the two pipelines considered, and find the SSC impact to be non-negligible - halving the figure of merit (FoM) of the dark energy parameters ( w 0 , w a ) in the 3×2pt case and substantially increasing the uncertainties on Ω m,0 , w 0 , w 0 , and σ 8 for the weak-lensing probe. We find photometric galaxy clustering to be less affected as a consequence of the lower probe response. The relative impact of SSC, while highly dependent on the number and type of nuisance parameters varied in the analysis, does not show significant changes under variations of the redshift binning scheme. Finally, we explore how the use of prior information on the shear and galaxy bias changes the impact of SSC. We find that improving shear bias priors has no significant influence, while galaxy bias must be calibrated to a subpercent level in order to increase the FoM by the large amount needed to achieve the value when SSC is not included.

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Publication Details

Journal
Astronomy and Astrophysics
Published
2024-09-30
DOI
https://doi.org/10.1051/0004-6361/202348389
Citations
6
Primary Topic
Statistical and numerical algorithms
Type
article
Field-Weighted Citation Impact
5.85

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article

Euclid preparation

J. Graciá‐Carpio, M. Ballardini, R. P. Saglia, L. Moscardini et al.
6 citations
Astronomy and Astrophysics
Statistical and numerical algorithms
5.85
article

Euclid preparation

J. Graciá‐Carpio, M. Ballardini, R. P. Saglia, L. Moscardini, G. Riccio, N. Auricchio, M. Brescia, I. Hook, A. Boucaud, C. Baccigalupi, Jean‐Luc Starck, A. Boucaud, J. Carretero, M. Schirmer, J. Steinwagner, M. Baldi, B. Garilli, N. Mauri, M. Martinelli, S. Gouyou Beauchamps, S. Casas, J. F. Macías–Pérez, F. Courbin, C. Valieri, Y. Copin, S. Paltani, A Renzi, Joachim Stadel, M Aubert, A. Díaz‐Sánchez, G. Gozaliasl, Pierluigi Monaco, S. Mei, S. Bardelli, G. Desprez, Francisco Javier Castander, M. Magliocchetti, L. Gabarra, S. Andreon, Alexandre Barreira, S. V. H. Haugan, R. Massey, T. Vassallo, S. Farrens, J. Garcia-Bellido, R. Scaramella, C.J. Conselice, G. Castignani, R. Toledo-Moreo, M. Moresco, G Sirri, D. Sapone, T. Castro, M. Meneghetti, N. Martinet, L. Patrizii, F. Lacasa, J. J. E. Kajava, S. Ilić, A. Veropalumbo, K. Ganga, H. Hildebrandt, B Gillis, E. Romelli, A. Da Silva, Adélie Gorce, C. Burigana, A. Biviano, E Medinaceli, H. Degaudenzi, G. Morgante, B. Joachimi, V. Allevato, J. Väliviita, W. Gillard, L. Conversi, S. Escoffier, J Brinchmann, C. Padilla Aranda, C. Porciani, M. Roncarelli, F. Dubath, Marco Bonici, M. Migliaccio, A. Hornstrup, E. Medinaceli, H. M. Courtois, A. Amara, M. Pöntinen, J. Jacobson, S. Di Domizio, M Viel, E. Branchini, M. Farina, G. Zamorani, O. Cucciati, F. Pasian, L. Guzzo, E. Sefusatti, V. Kansal, J. Weller, M. Castellano, Robin Upham, R. Farinelli, F. Giacomini, A. Zacchei, W. Holmes, S. Galeotta, F. Raison, Kim Steenstrup Pedersen, E. Franceschi, O. Marggraf, K Jahnke, ENRIQUE GAZTAÑAGA, R Teyssier, Philippe Baratta, A. A. Nucita, A. Kiessling, K. Markovič, R. Cabanac, S. Camera, L. Legrand, K. C. Chambers, F. Finelli⋆, R. Rébolo, E. Sefusatti, M. Sereno, M. Cropper, E. Keihänen, B. Sartoris, P. C. Schneider, S. Cavuoti, V Scottez, M. Fumana, A. Spurio Mancini, P. Šimon, G. Seidel, S. Kermiche, J. Graciá-Carpio, L. Corcione, G. Meylan, S. Davini, Sune Toft, O. Mansutti, E. Bozzo, S Dusini, M. Schirmer, A. G. Sánchez, S. Serrano, M. Kunz, Aurel Schneider, D. Potter, C. Porciani, J. Dinis, L. Corcione, Y. Akrami, F Grupp, S Andreon, D Sciotti, Yun Wang, Pedro G. Ferreira, L. Maurin, G de Lucia, I. Tutusaus, S. Pires, Y. Mellier, A. G. Sánchez, S.-M. Niemi, A. Cappi, C Neissner, C.C Kirkpatrick, D. Di Ferdinando, I. Tereno, V. Pettorino, L. A. Popa, V. Popa, J. Rhodes, P Fosalba, M. Béthermin, L. Valenziano, L. Stanco, Z Sakr, R. Cledassou, E. Munari, H. Kurki‐Suonio, P. Hudelot, A Zacchei, S. Davini, M. Tenti, W. A. Holmes, N. Aghanim, C. Padilla, F. Hormuth, F Torradeflot, J.A. Escartin Vigo, A Grazian, A. Cimatti, G Mainetti, X Dupac, M. D. Seiffert, M. Tucci, V. F. Cardone, A. N. Taylor, J. Coupon, E Zucca, I. Lloro, A. Pourtsidou
article en
6 citations

Abstract

Context . Deviations from Gaussianity in the distribution of the fields probed by large-scale structure surveys generate additional terms in the data covariance matrix, increasing the uncertainties in the measurement of the cosmological parameters. Super-sample covariance (SSC) is among the largest of these non-Gaussian contributions, with the potential to significantly degrade constraints on some of the parameters of the cosmological model under study – especially for weak-lensing cosmic shear. Aims . We compute and validate the impact of SSC on the forecast uncertainties on the cosmological parameters for the Euclid photo-metric survey, and investigate how its impact depends on the specific details of the forecast. Methods . We followed the recipes outlined by the Euclid Collaboration (EC) to produce 1 σ constraints through a Fisher matrix analysis, considering the Gaussian covariance alone and adding the SSC term, which is computed through the public code PySSC . The constraints are produced both by using Euclid ’s photometric probes in isolation and by combining them in the ‘3×2pt’ analysis. Results . We meet EC requirements on the forecasts validation, with an agreement at the 10% level between the mean results of the two pipelines considered, and find the SSC impact to be non-negligible - halving the figure of merit (FoM) of the dark energy parameters ( w 0 , w a ) in the 3×2pt case and substantially increasing the uncertainties on Ω m,0 , w 0 , w 0 , and σ 8 for the weak-lensing probe. We find photometric galaxy clustering to be less affected as a consequence of the lower probe response. The relative impact of SSC, while highly dependent on the number and type of nuisance parameters varied in the analysis, does not show significant changes under variations of the redshift binning scheme. Finally, we explore how the use of prior information on the shear and galaxy bias changes the impact of SSC. We find that improving shear bias priors has no significant influence, while galaxy bias must be calibrated to a subpercent level in order to increase the FoM by the large amount needed to achieve the value when SSC is not included.

Astronomy and AstrophysicsVol. 691
Université Claude Bernard Lyon 1 (FR), Institut polytechnique de Grenoble (FR), University of Geneva (CH), University of Rome Tor Vergata (IT), Leiden University (NL), California Institute of Technology (US), University of Copenhagen (DK), Ames Research Center (US), Centre National de la Recherche Scientifique (FR), Institute of Space Sciences (ES), University of Hawaii System (US), Jet Propulsion Laboratory (US), University of Helsinki (FI), Université Toulouse III - Paul Sabatier (FR), Consejo Superior de Investigaciones Científicas (ES), University of Bonn (DE), Scuola Internazionale Superiore di Studi Avanzati (IT), University of Padua (IT), University of Lisbon (PT), University of Trieste (IT), University of Salento (IT), University of Turku (FI), Scuola Normale Superiore (IT), Universidad de La Laguna (ES), Stockholm University (SE), University of Groningen (NL), Université Fédérale de Toulouse Midi-Pyrénées (FR), Universidade do Porto (PT), Saint Joseph University (LB), University of Oslo (NO), Institute for High Energy Physics (ES), University of Milan (IT), Durham University (GB), Université Clermont Auvergne (FR), Princeton University (US), University of Ferrara (IT), Université Côte d'Azur (FR), University of Zurich (CH), University of California, Irvine (US), 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 Sciences et Lettres (FR), Université Paris-Saclay (FR), Centre National d'Études Spatiales (FR), 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), Laboratoire AstroParticule et Cosmologie (FR), Brera Astronomical Observatory (IT), University of Manchester (GB), École Normale Supérieure - PSL (FR), Universidad Politécnica de Cartagena (ES), Sorbonne Université (FR), Astrophysique, Instrumentation et Modélisation (FR), Institute of Astrophysics and Space Sciences (PT), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), European Space Astronomy Centre (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Istituto Nazionale di Fisica Nucleare, Sezione di Lecce (IT), Excellence Cluster Origins (DE), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT), Institute for Space Astrophysics and Planetology (IT), Laboratoire de Physique de Clermont Auvergne (FR), Institut d'Astrophysique Spatiale (FR), École Normale Supérieure (BI), Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères (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 Ferrara (IT), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (IT), Centro de Astrofísica da Universidade do Porto (PT), Max Planck Institute for Astronomy (DE), Istituto di Radioastronomia di Bologna (IT), Université Bourgogne Franche-Comté (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), Observatoire de la Côte d’Azur (FR), 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), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (FR), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (IT), Institute of Space Science - INFLPR Subsidiary (RO), Centre de Calcul de l’Institut National de Physique Nucléaire et de Physique des Particules (FR), 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), Damien Foundation (BD), 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), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), 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, European Space Research and Technology Centre (NL), University College London (GB), Imperial College London (GB), McGill University (CA), École Polytechnique Fédérale de Lausanne (CH), University of Turin (IT), Case Western Reserve University (US), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Saint Mary's University (CA), Lancaster University (GB), University of Chile (CL), Heidelberg Institute for Theoretical Studies (DE), Ludwig-Maximilians-Universität München (DE), University of Genoa (IT), Sapienza University of Rome (IT), National Institute for Astrophysics (IT), RWTH Aachen University (DE), Université Grenoble Alpes (FR), Ruhr University Bochum (DE), Netherlands Institute for Radio Astronomy (NL), University of Bologna (IT), Universitat Politècnica de Catalunya (ES), Technical University of Denmark (DK), Stanford University (US), University of Edinburgh (GB), Aalto University (FI)
National Aeronautics and Space Administration, Aix-Marseille Université, Ministerio de Ciencia, Innovación y Universidades, Dipartimenti di Eccellenza, European Space Agency, European Commission, Centre National d’Etudes Spatiales, Magyar Tudományos Akadémia, Agenzia Spaziale Italiana, National Astronomical Observatory of Japan, Agenția Spațială Română, Norsk Romsenter, Horizon 2020 Framework Programme, Fundação para a Ciência e a Tecnologia
Openalex Percentile: Top 3%
Statistical and numerical algorithms
5.85
DOIOpen Access PDFOpenAlex
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