G. de Lucia

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Co-Authors

H. Kurki‐Suonio

University of Helsinki

M. Moresco

University of Bologna

M. Pöntinen

University of Helsinki

M. Ballardini

Istituto Nazionale di Fisica Nucleare, Sezione di Ferrara

E. Franceschi

Osservatorio di Astrofisica e Scienza dello Spazio

J. Carretero

Institute for High Energy Physics

S. Escoffier

Centre de physique des particules de Marseille

I. Tutusaus

Institut de Recherche en Astrophysique et Planétologie

D. Di Ferdinando

Istituto Nazionale di Fisica Nucleare, Sezione di Bologna

E. A. Valentijn

University of Groningen

Cooperative Institutions

Centre National de la Recherche Scientifique

275

University College London

169

University of Copenhagen

133

National Institute for Astrophysics

121

Flatiron Health (United States)

120

Flatiron Institute

117

Royal Holloway University of London

110

University of California, Davis

106

New York University

106

Princeton University

106

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Euclid Preparation XXIX: Forecasts for 10 different higher-order weak lensing statistics

HAL (Le Centre pour la Communication Scientifique Directe) (2023)

V. Ajani M. Baldi A. Barthelemy Aoife Boyle Peter Rolf Burger

Recent cosmic shear studies have shown that higher-order statistics (HOS) developed by independent teams now outperform standard two-point estimators in terms of statistical precision thanks to their sensitivity to the non-Gaussian features of large-scale structure. The aim of the Higher-Order Weak Lensing Statistics (HOWLS) project is to assess, compare, and combine the constraining power of $10$ different HOS on a common set of $Euclid$-like mocks, derived from N-body simulations. In this first paper of the HOWLS series we compute the non-tomographic ($\Omega_{\rm m}$, $\sigma_8$) Fisher information for one-point probability distribution function, peak counts, Minkowski functionals, Betti numbers, persistent homology Betti numbers and heatmap, and scattering transform coefficients, and compare them to the shear and convergence two-point correlation functions in the absence of any systematic bias. We also include forecasts for three implementations of higher-order moments, but these cannot be robustly interpreted as the Gaussian likelihood assumption breaks down for these statistics. Taken individually, we find that each HOS outperforms the two-point statistics by a factor of around $2$ in the precision of the forecasts with some variations across statistics and cosmological parameters. When combining all the HOS, this increases to a $4.5$ times improvement, highlighting the immense potential of HOS for cosmic shear cosmological analyses with $Euclid$. The data used in this analysis are publicly released with the paper.

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Euclid. I. Overview of the Euclid mission

Y. Mellier J. A. Acevedo Barroso A. Achúcarro Jiřı́ Adámek R. Adam

10.48550/arxiv.2405.13491

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Euclid preparation XXVI: The Euclid Morphology Challenge. Towards structural parameters for billions of galaxies

HAL (Le Centre pour la Communication Scientifique Directe) (2022)

H. Bretonnière Ulrike Kuchner M. Huertas-Company E Merlin M. Castellano

The various Euclid imaging surveys will become a reference for studies of galaxy morphology by delivering imaging over an unprecedented area of 15 000 square degrees with high spatial resolution. In order to understand the capabilities of measuring morphologies from Euclid-detected galaxies and to help implement measurements in the pipeline, we have conducted the Euclid Morphology Challenge, which we present in two papers. While the companion paper by Merlin et al. focuses on the analysis of photometry, this paper assesses the accuracy of the parametric galaxy morphology measurements in imaging predicted from within the Euclid Wide Survey. We evaluate the performance of five state-of-the-art surface-brightness-fitting codes DeepLeGATo, Galapagos-2, Morfometryka, Profit and SourceXtractor++ on a sample of about 1.5 million simulated galaxies resembling reduced observations with the Euclid VIS and NIR instruments. The simulations include analytic S\'ersic profiles with one and two components, as well as more realistic galaxies generated with neural networks. We find that, despite some code-specific differences, all methods tend to achieve reliable structural measurements (10% scatter on ideal S\'ersic simulations) down to an apparent magnitude of about 23 in one component and 21 in two components, which correspond to a signal-to-noise ratio of approximately 1 and 5 respectively. We also show that when tested on non-analytic profiles, the results are typically degraded by a factor of 3, driven by systematics. We conclude that the Euclid official Data Releases will deliver robust structural parameters for at least 400 million galaxies in the Euclid Wide Survey by the end of the mission. We find that a key factor for explaining the different behaviour of the codes at the faint end is the set of adopted priors for the various structural parameters.

Morphology

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Euclid preparation. XXIV. Calibration of the halo mass function in $\Lambda(\nu)$CDM cosmologies

HAL (Le Centre pour la Communication Scientifique Directe) (2022)

T. Castro A. Fumagalli R. E. Angulo S. Bocquet S. Borgani

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo-finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein--de Sitter and standard $\Lambda$CDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the $\Lambda$CDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass-observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference.

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