Large Angular Scale CMB Anisotropy Induced by Cosmic Strings

(2) University of Cambridge - DAMTP; (3) NASA/Fermilab Astrophysics Center; (4) NASA/Goddard Space Flight Center); A. Stebbins (3); B. Allen (1); E.P.S. Shellard (2); R.R. Caldwell (2); S. Veeraraghavan (4) ((1) University of Wisconsin - Milwaukee

RECORD

Large Angular Scale CMB Anisotropy Induced by Cosmic Strings

B. Allen (1), R.R. Caldwell (2), E.P.S. Shellard (2), A. Stebbins (3), S. Veeraraghavan (4) ((1) University of Wisconsin - Milwaukee, (2) University of Cambridge - DAMTP, (3) NASA/Fermilab Astrophysics Center, (4) NASA/Goddard Space Flight Center)

Astrophysics · Submitted 5 Sep 1996

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim By comparing with the observed temperature anisotropy, we set the normalization for the cosmic string mass-per-unit-length $\mu$, obtaining $G\mu/c^2=1.05 {}^{+0.35}_{-0.20} \times10^{-6}$, which is consistent with all other observational constraints on cosmic strings.

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arXiv IDastro-ph/9609038 (version 1)

Pith IDZ623NUGE, Pith's permanent record of this paper and its review

Citation(2) University of Cambridge - DAMTP, (3) NASA/Fermilab Astrophysics Center, (4) NASA/Goddard Space Flight Center), A. Stebbins (3), B. Allen (1), E.P.S. Shellard (2), R.R. Caldwell (2), S. Veeraraghavan (4) ((1) University of Wisconsin - Milwaukee. "Large Angular Scale CMB Anisotropy Induced by Cosmic Strings." arXiv:astro-ph/9609038 (1996). https://pith.science/paper/Z623NUGE

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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. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 4,301 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.14 · human participants 0.01 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.72 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

We simulate the anisotropy in the cosmic microwave background (CMB) induced by cosmic strings. By numerically evolving a network of cosmic strings we generate full-sky CMB temperature anisotropy maps. Based on $192$ maps, we compute the anisotropy power spectrum for multipole moments $\ell \le 20$. By comparing with the observed temperature anisotropy, we set the normalization for the cosmic string mass-per-unit-length $\mu$, obtaining $G\mu/c^2=1.05 {}^{+0.35}_{-0.20} \times10^{-6}$, which is consistent with all other observational constraints on cosmic strings. We demonstrate that the anisotropy pattern is consistent with a Gaussian random field on large angular scales.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We simulate the anisotropy in the cosmic microwave background (CMB) induced by cosmic strings.	contribution 0.94	0.96	0.04	asserted 0.84
s1	By numerically evolving a network of cosmic strings we generate full-sky CMB temperature anisotropy maps.	method 0.99	0.96	0.03	asserted 1.00
s2	Based on $192$ maps, we compute the anisotropy power spectrum for multipole moments $\ell \le 20$.	method 0.94	0.97	0.05	asserted 1.00
s3	By comparing with the observed temperature anisotropy, we set the normalization for the cosmic string mass-per-unit-length $\mu$, obtaining $G\mu/c^2=1.05 {}^{+0.35}_{-0.20} \times10^{-6}$, which is consistent with all other observational constraints on cosmic strings.	result 0.99	0.96	0.76	asserted 0.91
s4	We demonstrate that the anisotropy pattern is consistent with a Gaussian random field on large angular scales.	result 0.91	0.94	0.20	asserted 0.91

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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arXiv listing abstract v1

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full text
figures and tables
references and citing sentences
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P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We simulate the anisotropy in the cosmic microwave background (CMB) induced by cosmic strings. By numerically evolving a network of cosmic strings we generate full-sky CMB temperature anisotropy maps. Based on $192$ maps, we compute the anisotropy power spectrum for multipole moments $\ell \le 20$. By comparing with the observed temperature anisotropy, we set the normalization for the cosmic string mass-per-unit-length $\mu$, obtaining $G\mu/c^2=1.05 {}^{+0.35}_{-0.20} \times10^{-6}$, which is consistent with all other observational constraints on cosmic strings. We demonstrate that the anisotropy pattern is consistent with a Gaussian random field on large angular scales.

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References

Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

CMB power spectrum contribution from cosmic strings using field-evolution simulations of the Abelian Higgs model
astro-ph 2006-04 conditional novelty 7.0 of 10

Field-theory simulations of Abelian Higgs cosmic strings produce a CMB temperature power spectrum whose shape differs from idealized-string models and whose WMAP-3 normalization implies a string tension 2-3 times high...
Limits on Black Hole Formation from Cosmic String Loops
astro-ph 1997-07 conditional novelty 6.0 of 10

Gamma-ray and antiproton data bound the fraction of cosmic string loops that collapse into black holes, and combined with a simulated collapse efficiency they cap the string tension at Gmu/c^2 of order 2e-6, close to ...
Cosmic String constraints from WMAP and the South Pole Telescope
astro-ph.CO 2011-09 accept novelty 5.0 of 10

WMAP plus South Pole Telescope temperature data cap the cosmic string contribution to the CMB at 1.75% of the total power, giving G mu < 1.7e-7 at 95% confidence.
Signals of Inflationary Models with Cosmic Strings
astro-ph.CO 2011-06 accept novelty 3.0 of 10

A review of the observational signatures of cosmic strings produced at the end of inflation, concluding that CMB data already bound the string tension G-mu below roughly 10^-6, while the loop population and hence the ...

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3 arXiv papers cite this in 3 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 2 sentences without a confident label

Cites it as background 1 paper

Bounds on phenomenological parameters such as the string tension and number density have also been obtained using the predicted effects of strings on CMB anisotropy [ref] , the expected emission of high-energy rays from cusps and kinks [ref] and possible signatures in the 21cm line [ref] .

Evolution of FLRW spacetime after the birth of a cosmic string · Introduction · 0.83

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