The cosmic web from perturbation theory

Kitaura, F.-S.; Sinigaglia, F.; Balaguera-Antolínez, A.; Favole, G.

doi:10.1051/0004-6361/202345876

A&A

2024

DOI: 10.1051/0004-6361/202345876

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The cosmic web from perturbation theory

F.-S. Kitaura,

F. Sinigaglia,

A. Balaguera-Antolínez

et al.

Abstract: Analysing the large-scale structure (LSS) in the Universe with galaxy surveys demands accurate structure formation models. Such models should ideally be fast and have a clear theoretical framework in order to rapidly scan a variety of cosmological parameter spaces without requiring large training data sets. This study aims to extend Lagrangian perturbation theory (LPT), including viscosity and vorticity, to reproduce the cosmic evolution from dark matter $N$-body calculations at the field level. We extend LPT … Show more

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2024

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Cited by 4 publications

References 60 publications

(56 reference statements)

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Fast simulation mapping: From standard to modified gravity cosmologies using the bias assignment method

García-Farieta,

Balaguera-Antolínez,

Kitaura

2024

A&A

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We assess the effectiveness of a non-parametric bias model in generating mock halo catalogues for modified gravity (MG) cosmologies, relying on the distribution of dark matter from either MG or Lambda cold dark matter ( simulations. We aim to generate halo catalogues that effectively capture the distinct impact of MG, ensuring high accuracy in both two- and three-point statistics for a comprehensive analysis of large-scale structures. We investigated the inclusion of MG in non-local bias to directly map the tracers onto fields, which would significantly reduce computational costs. We employed the bias assignment method ( BAM ) to model halo distribution statistics by leveraging seven high-resolution COLA simulations of MG cosmologies. Taking cosmic-web dependences into account when learning the bias relations, we designed two experiments to map the MG effects: one utilising the consistent MG density fields and the other employing the benchmark \ density field. BAM generates MG halo catalogues from both calibration experiments with excellent summary statistics, achieving a $ 1<!PCT!>$ accuracy in the power spectrum across a wide range of $k$ modes, with minimal differences well below 10<!PCT!> for modes subject to cosmic variance, particularly below $k<0.07$ The reduced bispectrum remains consistent with the reference catalogues within 10<!PCT!> for the studied configuration. Our results demonstrate that a non-linear and non-local bias description can model the effects of MG starting from a field.

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Fast simulation mapping: From standard to modified gravity cosmologies using the bias assignment method

García-Farieta,

Balaguera-Antolínez,

Kitaura

2024

A&A

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Large-scale structure around the Fornax-Eridanus complex

Raj,

Awad,

Peletier

et al. 2024

A&A

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Our objectives are to map the filamentary network around the Fornax-Eridanus complex and probe the influence of the local environment on galaxy morphology. We employed the novel machine-learning tool, named, 1-Dimensional, Recovery, Extraction, and Analysis of Manifolds (1-DREAM) to detect and model filaments around the Fornax cluster. We then used the morphology-density relation of galaxies to examine the variation in the galaxies' morphology with respect to their distance from the central axis of the detected filaments. We detected 27 filaments that vary in length and galaxy-number density around the Fornax-Eridanus complex. We find that 81<!PCT!> of galaxies in our catalogue belong to filaments and 19<!PCT!> of galaxies are located outside filaments. The filaments around the Fornax-Eridanus complex showcase a variety of environments:\ some filaments encompass groups and clusters, while others are only inhabited by galaxies in pristine filamentary environments. In this context, we reveal a well-known structure, namely:\ the Fornax Wall, which passes through the Dorado group, Fornax cluster, and Eridanus supergroup. With regard to the morphology of galaxies, we find that early-type galaxies (ETGs) populate high-density filaments and high-density regions of the Fornax Wall. Furthermore, the fraction of the ETG-population decreases as the distance to the central axis of the filament increases. The fraction of late-type galaxies (LTGs; 8<!PCT!>) is lower than that of ETGs (12<!PCT!>) at 0.5 Mpc/$h$ from the filament spine. Of the total galaxy population in filaments around the Fornax-Eridanus complex, sim 7<!PCT!> are ETGs and sim 24<!PCT!> are LTGs located in pristine environments of filaments, while sim 27<!PCT!> are ETGs and sim 42<!PCT!> are LTGs in groups and clusters within filaments. Among the galaxies in the filamentary network around the Fornax-Eridanus complex, 44<!PCT!> of them belong to the Fornax Wall. This study reveals the cosmic web around the Fornax cluster, which exhibits a variety of filamentary environments. With this, our research asserts that filamentary environments are heterogeneous in nature. When investigating the role of the environment on galaxy morphology, it is essential to consider both the local number-density and a galaxy's proximity to the filament spine (i.e. the filament core). Within this framework, we ascribe the observed morphological segregation in the Fornax Wall to the pre-processing of galaxies among groups embedded in it.

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CosmoMIA: cosmic web-based redshift space halo distribution

Forero Sánchez,

Kitaura,

Sinigaglia

et al. 2024

J. Cosmol. Astropart. Phys.

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Modern galaxy surveys demand extensive survey volumes and resolutions surpassing current dark matter-only simulations' capabilities. To address this, many methods employ effective bias models on the dark matter field to approximate object counts on a grid. However, realistic catalogs necessitate specific coordinates and velocities for a comprehensive understanding of the Universe. In this research, we explore sub-grid modeling to create accurate catalogs, beginning with coarse grid number counts at resolutions of approximately 5.5 h -1 Mpc per side. These resolutions strike a balance between modeling nonlinear damping of baryon acoustic oscillations and facilitating large-volume simulations. Augmented Lagrangian Perturbation Theory (ALPT) is utilized to model the dark matter field and motions, replicating the clustering of a halo catalog derived from a massive simulation at z = 1.1. Our approach involves four key stages: Tracer Assignment: Allocating dark matter particles to tracers based on grid cell counts, generating additional particles to address discrepancies. Attractor Identification: Defining attractors based on particle cosmic web environments, acting as gravitational focal points. Tracer Collapse: Guiding tracers towards attractors, simulating structure collapse. Redshift Space Distortions: Introducing redshift space distortions to simulated catalogs using ALPT and a random dispersion term. Results demonstrate accurate reproduction of monopoles and quadrupoles up to wave numbers of approximately k = 0.6 h Mpc-1. This method holds significant promise for galaxy surveys like DESI, EUCLID, and LSST, enhancing our understanding of the cosmos across scales.

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The cosmic web from perturbation theory

Cited by 4 publications

References 60 publications

Fast simulation mapping: From standard to modified gravity cosmologies using the bias assignment method

Fast simulation mapping: From standard to modified gravity cosmologies using the bias assignment method

Large-scale structure around the Fornax-Eridanus complex

CosmoMIA: cosmic web-based redshift space halo distribution

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