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Observational constraints on cosmic strings: Bayesian analysis in a three dimensional parameter space
Astrophysics · Submitted 10 Mar 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Already, varying only three parameters -- the spectral index and the amplitudes of the adiabatic and string contributions -- we find that the upper bound on the cosmic string contribution is of order 10%.
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The abstract, sentence by sentence
Current data exclude cosmic strings as the primary source of primordial density fluctuations. However, in a wide class of inflationary models, strings can form at later stages of inflation and have potentially detectable observational signatures. We study the constraints from WMAP and SDSS data on the fraction of primordial fluctuations sourced by local cosmic strings. The Bayesian analysis presented in this brief report is restricted to the minimal number of parameters. Yet it is useful for two reasons. It confirms the results of Pogosian et al (2003) using an alternative statistical method. Secondly, it justifies the more costly multi-parameter analysis. Already, varying only three parameters -- the spectral index and the amplitudes of the adiabatic and string contributions -- we find that the upper bound on the cosmic string contribution is of order 10%. We expect that the full multi-parameter study, currently underway, will likely loosen this bound.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Current data exclude cosmic strings as the primary source of primordial density fluctuations. | background 0.99 | 0.12 | 0.14 | asserted 1.00 |
| s1 | However, in a wide class of inflationary models, strings can form at later stages of inflation and have potentially detectable observational signatures. | background 0.94 | 0.06 | 0.04 | hedged possibility 0.96 |
| s2 | We study the constraints from WMAP and SDSS data on the fraction of primordial fluctuations sourced by local cosmic strings. | contribution 0.93 | 0.89 | 0.04 | asserted 0.80 |
| s3 | The Bayesian analysis presented in this brief report is restricted to the minimal number of parameters. | limitation 0.95 | 0.84 | 0.02 | asserted 1.00 |
| s4 | Yet it is useful for two reasons. | interpretation 0.62 | 0.27 | 0.02 | asserted 0.94 |
| s5 | It confirms the results of Pogosian et al (2003) using an alternative statistical method. | interpretation 0.43 | 0.72 | 0.06 | asserted 1.00 |
| s6 | Secondly, it justifies the more costly multi-parameter analysis. | interpretation 0.47 | 0.63 | 0.04 | asserted 0.99 |
| s7 | Already, varying only three parameters -- the spectral index and the amplitudes of the adiabatic and string contributions -- we find that the upper bound on the cosmic string contribution is of order 10%. | result 1.00 | 0.96 | 0.77 | asserted 1.00 |
| s8 | We expect that the full multi-parameter study, currently underway, will likely loosen this bound. | future work 0.93 | 0.38 | 0.07 | hedged possibility 1.00 |
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The paper
Original abstract
Current data exclude cosmic strings as the primary source of primordial density fluctuations. However, in a wide class of inflationary models, strings can form at later stages of inflation and have potentially detectable observational signatures. We study the constraints from WMAP and SDSS data on the fraction of primordial fluctuations sourced by local cosmic strings. The Bayesian analysis presented in this brief report is restricted to the minimal number of parameters. Yet it is useful for two reasons. It confirms the results of Pogosian et al (2003) using an alternative statistical method. Secondly, it justifies the more costly multi-parameter analysis. Already, varying only three parameters -- the spectral index and the amplitudes of the adiabatic and string contributions -- we find that the upper bound on the cosmic string contribution is of order 10%. We expect that the full multi-parameter study, currently underway, will likely loosen this bound.
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References
How the literature uses it
9 arXiv papers cite this in 10 sentences
Papers citing it · 7 sentences without a confident label
Uses its data or values 2 papers
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The current CMB bound on the tension is $G μ<6.1×10^-7$ [ref] .
Gravitational-Wave Stochastic Background from Kinks and Cusps on Cosmic Strings · Introduction · 0.99
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The current CMB bound on the tension is $G μ<6.1×10^-7$ [ref] .
Anisotropies in the Gravitational-Wave Stochastic Background · Introduction · 0.97
Cites it as background 1 paper
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They can produce various effects, most of which are gravitational, such as CMB anisotropies [ref] , non-Gaussianity [ref] , B-mode polarization [ref] and gravitational waves [ref] .
CMB Distortions from Damping of Acoustic Waves Produced by Cosmic Strings · Introduction · 0.91
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