High Energy Physics - Phenomenology · arXiv:hep-ph/0403129 v2 · submitted 12 Mar 2004
Primordial fluctuations and cosmological inflation after WMAP 1.0
The paper says
“These observations allow us to constrain the physics of cosmological inflation: (i) The data show that the Hubble distance is almost constant during inflation.”
from the abstract · picked out as the main claim by a classifier
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The paper
Abstract
The observational constraints on the primordial power spectrum have tightened considerably with the release of the first year analysis of the WMAP observations, especially when combined with the results from other CMB experiments and galaxy redshift surveys. These observations allow us to constrain the physics of cosmological inflation: (i) The data show that the Hubble distance is almost constant during inflation. While observable modes cross the Hubble scale, it changes by less than 3% during one e-folding: d(d_H)/dt < 0.032 at 2 sigma. The distance scale of inflation itself remains poorly constrained: 1.2 x 10^-28 cm < d_H < 1 cm. (ii) We present a new classification of single-field inflationary scenarios (including scenarios beyond slow-roll inflation), based on physical criteria, namely the behaviour of the kinetic and total energy densities of the inflaton field. The current data show no preference for any of the scenarios. (iii) For the first time the slow-roll assumption could be dropped from the data analysis and replaced by the more general assumption that the Hubble scale is (almost) constant during the observable part of inflation. We present simple analytic expressions for the scalar and tensor power spectra for this very general class of inflation models and test their accuracy.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 0.82
What the abstract itself states, as probabilities: claims first 0.84 · states limitation 0.75 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.44 · mentions code or data availability 0.02
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 |
|---|---|---|---|---|
| The observational constraints on the primordial power spectrum have tightened considerably with the release of the first year analysis of the WMAP observations, especially when combined with the results from other CMB experiments and galaxy redshift surveys. | background 1.00 | 0.08 | 0.05 | asserted 1.00 |
| These observations allow us to constrain the physics of cosmological inflation: (i) The data show that the Hubble distance is almost constant during inflation. | result 0.74 | 0.37 | 0.23 | asserted 0.82 |
| While observable modes cross the Hubble scale, it changes by less than 3% during one e-folding: d(d_H)/dt < 0.032 at 2 sigma. | result 1.00 | 0.70 | 0.19 | asserted 1.00 |
| The distance scale of inflation itself remains poorly constrained: 1.2 x 10^{-28} cm < d_H < 1 cm. | result 0.92 | 0.69 | 0.08 | asserted 0.92 |
| (ii) We present a new classification of single-field inflationary scenarios (including scenarios beyond slow-roll inflation), based on physical criteria, namely the behaviour of the kinetic and total energy densities of the inflaton field. | contribution 0.99 | 0.93 | 0.09 | asserted 1.00 |
| The current data show no preference for any of the scenarios. | result 0.96 | 0.81 | 0.17 | asserted 1.00 |
| (iii) For the first time the slow-roll assumption could be dropped from the data analysis and replaced by the more general assumption that the Hubble scale is (almost) constant during the observable part of inflation. | contribution 0.88 | 0.87 | 0.25 | hedged possibility 0.95 |
| We present simple analytic expressions for the scalar and tensor power spectra for this very general class of inflation models and test their accuracy. | contribution 0.84 | 0.96 | 0.08 | asserted 0.97 |
What kind of paper the classifier reports this is: theoretical result 0.88 · evidence from analysis of existing data 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
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- P abstract
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- S sections
- T body sentences
- C citations
- R cross-paper relations
How the labels were made
Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,328 input tokens, $0.0003 reported.
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 14 Pith papers
Reviewed papers on Pith that cite this one. OpenAlex reports about 75 citations worldwide. The full citation record
- Cosmic Inflation at the Crossroads astro-ph.CO · Apr 2024
- Compatibility of Planck and BICEP2 in the Light of Inflation astro-ph.CO · May 2014
- Brane inflation and the WMAP data: a Bayesian analysis hep-th · Sep 2007
- Inflation after WMAP3: Confronting the Slow-Roll and Exact Power Spectra with CMB Data astro-ph · May 2006
- Low-frequency Gravitational Waves from Double-inflection-point Inflation astro-ph.CO · Jul 2019
- Inflation after Planck: Judgment Day astro-ph.CO · Feb 2019
- Stochastic inflation in phase space: Is slow roll a stochastic attractor? gr-qc · Mar 2017
- The Best Inflationary Models After Planck astro-ph.CO · Dec 2013
- The first WIMPy halos astro-ph · Mar 2005
- Second Order General Slow-Roll Power Spectrum hep-ph · May 2004
- Particle physics models of inflation and curvaton scenarios hep-ph · Jan 2010
- The exact numerical treatment of inflationary models astro-ph · Mar 2007
- Comment on: "Third-order corrections to the slow-roll expansion: Calculation and constraints with Planck, ACT, SPT, and BICEP/Keck [2025 PDU 47 101813]" astro-ph.CO · Mar 2026
- Viscous Cosmology for Early- and Late-Time Universe gr-qc · Jun 2017
How the literature uses it
15 arXiv papers cite this in 16 sentences
Papers citing it · 13 sentences without a confident label
Uses its method or tool 1 paper
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This set can be introduced by the horizon flow functions [ref] , providing model-independent quantities, valid even beyond the slow-roll approximation.
Quantum Effects in Cosmology · Classical Inflationary Dynamics · 0.82
Cites it as background 2 papers
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These parameters can be defined in terms of the Hubble parameter $H ≡ȧ/a$ (where the dot denotes the derivative with respect to cosmic time $t$) to yield what we refer to as the Hubble flow functions (HFF) [ref] : [equation] where $N ≡ln(a/a_ini)$ is the number of e-folds from the beginning of inflation.
Observational constraints on the second-order primordial power spectrum: Exploring a Continuous Spontaneous Localization inspired inflationary model · Slow roll model · 0.83
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Although there are many possible sets of slow-roll parameters, the mostly used in the literature are the so called Hubble-flow parameters [ref] , $ϵ_n$, defined iteratively through the following expression ϵ_n+1 = dln|ϵ_n|/dN, where $N$ is a time variable, called the e-fold number and it is defined as the logarithm of the scale factor, $N≡lna$.
Studying Aspects of the Early Universe with Primordial Black Holes · The Slow-Roll Regime · 0.81
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