Cosmology and Nongalactic Astrophysics · arXiv:1203.2307 v3 · submitted 11 Mar 2012
The 21 cm Signature of Shock Heated and Diffuse Cosmic String Wakes
The paper says
“Finally we compare the size of these signals compared to the expected thermal noise per pixel which dominates over the background cosmic gas brightness temperature and find that the cosmic string signal will exceed the thermal noise of an individual pixel in the Square Kilometre Array for string tensions Gμ > 2.5 × 10−8.”
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Abstract
The analysis of the 21 cm signature of cosmic string wakes is extended in several ways. First we consider the constraints on Gμ from the absorption signal of shock heated wakes laid down much later than matter radiation equality. Secondly we analyze the signal of diffuse wake, that is those wakes in which there is a baryon overdensity but which have not shock heated. Finally we compare the size of these signals compared to the expected thermal noise per pixel which dominates over the background cosmic gas brightness temperature and find that the cosmic string signal will exceed the thermal noise of an individual pixel in the Square Kilometre Array for string tensions Gμ > 2.5 × 10−8.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 1.00
What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.27 · human participants 0.01 · controlled comparison 0.24 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.58 · mentions code or data availability 0.02
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v3). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| The analysis of the 21 cm signature of cosmic string wakes is extended in several ways. | contribution 0.88 | 0.72 | 0.02 | asserted 0.91 |
| First we consider the constraints on $G\mu$ from the absorption signal of shock heated wakes laid down much later than matter radiation equality. | contribution 0.99 | 0.68 | 0.04 | asserted 0.58 |
| Secondly we analyze the signal of diffuse wake, that is those wakes in which there is a baryon overdensity but which have not shock heated. | contribution 1.00 | 0.86 | 0.03 | asserted 0.75 |
| Finally we compare the size of these signals compared to the expected thermal noise per pixel which dominates over the background cosmic gas brightness temperature and find that the cosmic string signal will exceed the thermal noise of an individual pixel in the Square Kilometre Array for string tensions $G\mu > 2.5 \times 10^{-8}$. | result 0.99 | 0.90 | 0.81 | asserted 1.00 |
What kind of paper the classifier reports this is: theoretical result 0.97 · evidence from proof or derivation 0.66
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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,642 input tokens, $0.0002 reported.
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Cited by 1 Pith paper
Reviewed papers on Pith that cite this one. The full citation record
- Searching for Cosmic Strings in New Observational Windows astro-ph.CO · Jan 2013
How the literature uses it
16 arXiv papers cite this in 36 sentences
Papers citing it · 29 sentences without a confident label
Uses its method or tool 1 paper
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In this section, we calculate the broadening and the brightness temperature of a diffuse wake following [ref] .
Extracting the Signal of Cosmic String Wakes from 21-cm Observations · Diffuse Wakes · 0.97
Uses its data or values 1 paper
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This is depicted in Figure 8 (taken from [ref] ) which shows the string wave signal as a function of $G μ$ for various values in the redshift $z_i$ when the wake is laid down, and for a fixed reshift $z = 20$ when our past light cone intersects the wake, compared to the noise (the almost horizontal lines to the top and bottom of the horizontal axis).
Probing Particle Physics from Top Down with Cosmic Strings · Imprints of Cosmic Strings in 21cm Surveys · 0.81
Cites it as background 4 papers
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Several papers have investigated redshifted 21 cm signatures from string wakes produced by long strings [ref] and filaments created by string loops [ref] .
High redshift signatures in the 21 cm forest due to cosmic string wakes · Introduction · 0.97
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Cosmological 21 cm signatures due to cosmic strings have been investigated in several papers [ref] .
21 cm Angular Spectrum of Cosmic String Loops · Introduction · 0.96
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These include the anisotropy of the CMB temperature [ref] and B-mode plarization [ref] , gravitational waves [ref] , gravitational lensing [ref] , wakes in the 21cm maps [ref] , early structure formation [ref] , early reionization due to early structure formation [ref] , and formation of dark matter clumps [ref] .
Constraints on Superconducting Cosmic Strings from Early Reionization · Introduction · 0.94
What it cites · 24 sentences without a confident label
Uses the method or tool of 3 papers
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To derive this noise temperature per pixel in [ref] we began with the thermal noise per visibility as given by Morales [ref] to arrive at the thermal noise per pixel for the brightness temperature.
The High-Redshift Neutral Hydrogen Signature of an Anisotropic Matter Power Spectrum · Diffuse Cosmic String Wakes · 0.90
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To derive this noise temperature per pixel in [ref] we began with the thermal noise per visibility as given by Morales [ref] to arrive at the thermal noise per pixel for the brightness temperature.
Power Spectrum Sensitivity and the Design of Epoch of Reionization Observatories · Diffuse Cosmic String Wakes · 0.90
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This is determined using the Zel'dovich approximation [ref] .The result obtained in [ref] is
The 21 cm Signature of Cosmic String Wakes · Cosmic Strings, Their Wakes and 21 cm Signatures · 0.85
Uses data or values from 2 papers
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The system temperature is given by ARCADE 2 [ref] .
ARCADE 2 Measurement of the Extra-Galactic Sky Temperature at 3-90 GHz · Diffuse Cosmic String Wakes · 0.99
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Here, $z_e$ is the redshift of 21 cm emission or absorption, $T_γ$ is the CMB temperature, $θ$ is the angle of the 21 cm ray with respect to the vertical to the wake, and $x_c$ are the collision coefficients whose values can be obtained from the tables listed in [ref] .
Spin Exchange Rates in Electron-Hydrogen Collisions · Diffuse Cosmic String Wakes · 0.93
Compares with 2 papers
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Demanding that the relative brightness temperature exceeds the pixel thermal noise in a future 21cm experiment such as the Square Kilometre Array (SKA) (with the pixel size chosen to be able to identify the wake signal, as described in the text) leads to a limit of $G μ> 2.5 ×10^-8$, an improvement over the current limit of Eq. ([ref]) obtained from CMB anisotropy maps [ref] .
Cosmic String constraints from WMAP and the South Pole Telescope · Conclusions · 0.98
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Limits based only on WMAP data gives a bound larger than this by a factor of two [ref] .
Observational Constraints on Cosmic String Production During Brane Inflation · Introduction · 0.90
Cites as support 1 paper
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This approximate analytical analysis has been confirmed in detailed hydrodynamical simulations [ref] .
The Structure of Cosmic String Wakes · Cosmic Strings, Their Wakes and 21 cm Signatures · 0.97
Cites as background 2 papers
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Cosmic strings can be used as a cosmological probe of New Physics because any particle physics model which admits stable cosmic strings as a solution inevitably results in a a network of such strings forming during a symmetry breaking phase transition in the early universe (see [ref] for reviews on cosmic strings and cosmology).
Topological Defects and Structure Formation · Cosmic Strings, Their Wakes and 21 cm Signatures · 0.99
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Cosmic strings can be used as a cosmological probe of New Physics because any particle physics model which admits stable cosmic strings as a solution inevitably results in a a network of such strings forming during a symmetry breaking phase transition in the early universe (see [ref] for reviews on cosmic strings and cosmology).
Cosmic strings · Cosmic Strings, Their Wakes and 21 cm Signatures · 0.99
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