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Evolution of cosmic filaments in the MTNG simulation?

Galárraga-Espinosa, Daniela ; Cadiou, Corentin LU orcid ; Gouin, Céline ; White, Simon D.M. ; Springel, Volker ; Pakmor, Rüdiger ; Hadzhiyska, Boryana ; Bose, Sownak ; Ferlito, Fulvio and Hernquist, Lars , et al. (2024) In Astronomy and Astrophysics 684.
Abstract

We present a study of the evolution of cosmic filaments across redshift with an emphasis on some important properties: filament lengths, growth rates, and radial profiles of galaxy densities. Following an observation-driven approach, we built cosmic filament catalogues at z = 0, 1, 2, 3, and 4 from the galaxy distributions of the large hydro-dynamical run of the MilleniumTNG project. We employed the extensively used DisPerSE cosmic web finder code, for which we provide a user-friendly guide, including the details of a physics-driven calibration procedure, with the hope of helping future users. We performed the first statistical measurements of the evolution of connectivity in a large-scale simulation, finding that the connectivity of... (More)

We present a study of the evolution of cosmic filaments across redshift with an emphasis on some important properties: filament lengths, growth rates, and radial profiles of galaxy densities. Following an observation-driven approach, we built cosmic filament catalogues at z = 0, 1, 2, 3, and 4 from the galaxy distributions of the large hydro-dynamical run of the MilleniumTNG project. We employed the extensively used DisPerSE cosmic web finder code, for which we provide a user-friendly guide, including the details of a physics-driven calibration procedure, with the hope of helping future users. We performed the first statistical measurements of the evolution of connectivity in a large-scale simulation, finding that the connectivity of cosmic nodes (defined as the number of filaments attached) globally decreases from early to late times. The study of cosmic filaments in proper coordinates reveals that filaments grow in length and radial extent, as expected from large-scale structures in an expanding Universe. But the most interesting results arise once the Hubble flow is factored out. We find remarkably stable comoving filament length functions and over-density profiles, showing only little evolution of the total population of filaments in the past ∼12.25 Gyr. However, by tracking the spatial evolution of individual structures, we demonstrate that filaments of different lengths actually follow different evolutionary paths. While short filaments preferentially contract, long filaments expand along their longitudinal direction with growth rates that are the highest in the early, matter-dominated Universe. Filament diversity at a fixed redshift is also shown by the different (∼5σ) density values between the shortest and longest filaments. Our results hint that cosmic filaments can be used as additional probes for dark energy, but further theoretical work is still needed.

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Contribution to journal
publication status
published
subject
keywords
cosmology: theory, galaxies: clusters: general, large-scale structure of Universe, methods: numerical, methods: statistical
in
Astronomy and Astrophysics
volume
684
publisher
EDP Sciences
external identifiers
  • scopus:85189655183
ISSN
0004-6361
DOI
10.1051/0004-6361/202347982
language
English
LU publication?
yes
id
0de7fb4d-2b1f-4918-aacb-965519dc342b
date added to LUP
2024-04-24 15:21:18
date last changed
2024-04-24 15:22:39
@article{0de7fb4d-2b1f-4918-aacb-965519dc342b,
  abstract     = {{<p>We present a study of the evolution of cosmic filaments across redshift with an emphasis on some important properties: filament lengths, growth rates, and radial profiles of galaxy densities. Following an observation-driven approach, we built cosmic filament catalogues at z = 0, 1, 2, 3, and 4 from the galaxy distributions of the large hydro-dynamical run of the MilleniumTNG project. We employed the extensively used DisPerSE cosmic web finder code, for which we provide a user-friendly guide, including the details of a physics-driven calibration procedure, with the hope of helping future users. We performed the first statistical measurements of the evolution of connectivity in a large-scale simulation, finding that the connectivity of cosmic nodes (defined as the number of filaments attached) globally decreases from early to late times. The study of cosmic filaments in proper coordinates reveals that filaments grow in length and radial extent, as expected from large-scale structures in an expanding Universe. But the most interesting results arise once the Hubble flow is factored out. We find remarkably stable comoving filament length functions and over-density profiles, showing only little evolution of the total population of filaments in the past ∼12.25 Gyr. However, by tracking the spatial evolution of individual structures, we demonstrate that filaments of different lengths actually follow different evolutionary paths. While short filaments preferentially contract, long filaments expand along their longitudinal direction with growth rates that are the highest in the early, matter-dominated Universe. Filament diversity at a fixed redshift is also shown by the different (∼5σ) density values between the shortest and longest filaments. Our results hint that cosmic filaments can be used as additional probes for dark energy, but further theoretical work is still needed.</p>}},
  author       = {{Galárraga-Espinosa, Daniela and Cadiou, Corentin and Gouin, Céline and White, Simon D.M. and Springel, Volker and Pakmor, Rüdiger and Hadzhiyska, Boryana and Bose, Sownak and Ferlito, Fulvio and Hernquist, Lars and Kannan, Rahul and Barrera, Monica and Delgado, Ana Maria and Hernández-Aguayo, César}},
  issn         = {{0004-6361}},
  keywords     = {{cosmology: theory; galaxies: clusters: general; large-scale structure of Universe; methods: numerical; methods: statistical}},
  language     = {{eng}},
  month        = {{04}},
  publisher    = {{EDP Sciences}},
  series       = {{Astronomy and Astrophysics}},
  title        = {{Evolution of cosmic filaments in the MTNG simulation<sup>?</sup>}},
  url          = {{http://dx.doi.org/10.1051/0004-6361/202347982}},
  doi          = {{10.1051/0004-6361/202347982}},
  volume       = {{684}},
  year         = {{2024}},
}