Cosmology and Nongalactic Astrophysics · arXiv:2009.01539 v2 · submitted 3 Sep 2020
Simulations and observational tests of primordial magnetic fields from Cosmic Microwave Background constraints
The paper says
“However, several statistical full-sky analyses, such as the cross-correlation between galaxies and diffuse synchrotron power, the Faraday Rotation structure functions from background radio galaxies, or the analysis of arrival direction of Ultra-High-Energy Cosmic Rays, can already be used to constrain these primordial field models.”
from the abstract · picked out as the main claim by a classifier
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The paper
Abstract
We present the first cosmological simulations of primordial magnetic fields derived from the constraints by the Cosmic Microwave Background observations, based on the fields' gravitational effect on cosmological perturbations. We evolved different primordial magnetic field models with the {\enzo} code and compared their observable signatures (and relative differences) in galaxy clusters, filaments and voids. The differences in synchrotron radio powers and Faraday Rotation measure from galaxy clusters are generally too small to be detected, whereas differences present in filaments will be testable with the higher sensitivity of the Square Kilometre Array. However, several statistical full-sky analyses, such as the cross-correlation between galaxies and diffuse synchrotron power, the Faraday Rotation structure functions from background radio galaxies, or the analysis of arrival direction of Ultra-High-Energy Cosmic Rays, can already be used to constrain these primordial field models.
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. No sentence in this record was written by a model.
abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 0.64
What the abstract itself states, as probabilities: claims first 0.95 · states limitation 0.83 · human participants 0.01 · controlled comparison 0.16 · randomized assignment 0.01 · states quantitative result 0.09 · compares with prior results 0.31 · mentions code or data availability 0.03
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v2). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| We present the first cosmological simulations of primordial magnetic fields derived from the constraints by the Cosmic Microwave Background observations, based on the fields' gravitational effect on cosmological perturbations. | contribution 1.00 | 0.94 | 0.09 | asserted 1.00 |
| We evolved different primordial magnetic field models with the {\enzo} code and compared their observable signatures (and relative differences) in galaxy clusters, filaments and voids. | method 0.90 | 0.95 | 0.05 | asserted 0.99 |
| The differences in synchrotron radio powers and Faraday Rotation measure from galaxy clusters are generally too small to be detected, whereas differences present in filaments will be testable with the higher sensitivity of the Square Kilometre Array. | result 0.86 | 0.82 | 0.31 | asserted 0.90 |
| However, several statistical full-sky analyses, such as the cross-correlation between galaxies and diffuse synchrotron power, the Faraday Rotation structure functions from background radio galaxies, or the analysis of arrival direction of Ultra-High-Energy Cosmic Rays, can already be used to constrain these primordial field models. | interpretation 0.58 | 0.16 | 0.37 | asserted 0.64 |
What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00
What was examined, and what was not
Sources read
- arXiv listing abstract v2
Not examined
- full text
- figures and tables
- references and citing sentences
- relations to other papers
Levels run
- P abstract
Not run
- S sections
- T body sentences
- C citations
- R cross-paper relations
How the labels were made
Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,760 input tokens.
Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON
Cited by 5 Pith papers
Reviewed papers on Pith that cite this one. The full citation record
- Non-Gaussian matter fluctuations from primordial magnetic fields and galaxy luminosity function astro-ph.CO · Nov 2026
- The driving mode of turbulence in disc galaxy simulations with adaptive mesh refinement astro-ph.GA · Sep 2026
- The impact of primordial magnetic fields on the formation of galaxies astro-ph.GA · Sep 2026
- Forward cascade of large-scale primordial magnetic fields during structure formation astro-ph.CO · Aug 2025
- Progress on Cosmological Magnetic Fields astro-ph.CO · Oct 2020
How the literature uses it
6 arXiv papers cite this in 6 sentences
Papers citing it · 2 sentences without a confident label
Cites it as support 1 paper
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Indeed, a direct link between PMFs (as constrained by the CMB anisotropy power spectra) and the nowadays cosmic magnetism was also confirmed by simulations [ref] .
The amplification of cosmological magnetic fields in Extended $f(T,B)$ Teleparallel Gravity · Discussion and Conclusions · 0.99
Cites it as background 3 papers
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A similar – although smaller – investigation was carried out in [ref] and [ref] , where the impact of the primordial seed strength on the properties of galaxies has been studied in the context of a uniform seeding at $z ≳100$, and in [ref] , where the effects of the seed field power spectrum were investigated.
Magnetogenesis around the first galaxies: the impact of different field seeding processes on galaxy formation · Introduction · 0.81
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This PMF evolution depends upon the helicity and homogeneity of the magnetic fields [ref] , and its behavior in the late non-linear structure formation phase has been investigated in a number of recent three-dimensional simulations [ref] .
Distribution function of nuclei from $e^\pm$ scattering in the presence of a strong primordial magnetic field · Introduction · 0.83
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The amplitude and topology of magnetic fields simulated for six different variations of input primoridal seed fields was also studied in detail in [ref] .
Synchrotron emission and neutral hydrogen in the simulated cosmic web · Other results and future perspectives · 0.92
What it cites · 3 sentences without a confident label
Uses the method or tool of 1 paper
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For the identification of up-stream magnetic field values and of the local shock propagation direction, we rely on our velocity-based shock finder [ref] .
2006.10063 · Global properties · 1.00
Challenges and discussion
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