Inflation model with lower multipoles of the CMB suppressed

Fuminobu Takahashi; Masahiro Kawasaki

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Inflation model with lower multipoles of the CMB suppressed

Masahiro Kawasaki, Fuminobu Takahashi

High Energy Physics - Phenomenology · Submitted 29 May 2003

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

The authors' main claim In this paper, we show that it is possible to explain the suppressed lower multipoles in the hybrid new inflation model.

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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, 3,535 input tokens, $0.0001 reported.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.10 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.05 · compares with prior results 0.26 · mentions code or data availability 0.01.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

The recent observation of the cosmic microwave background anisotropy by the WMAP confirmed that the lower multipoles are considerably suppressed. From the standpoint of the cosmic variance, it is nothing but a statistical accident. Alternatively, one can attribute the deficit of fluctuation on the large scale to the cosmic history, which might be explained in the context of the inflationary physics. In this paper, we show that it is possible to explain the suppressed lower multipoles in the hybrid new inflation model.

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	The recent observation of the cosmic microwave background anisotropy by the WMAP confirmed that the lower multipoles are considerably suppressed.	background 1.00	0.04	0.04	asserted 1.00
s1	From the standpoint of the cosmic variance, it is nothing but a statistical accident.	background 0.70	0.06	0.03	asserted 1.00
s2	Alternatively, one can attribute the deficit of fluctuation on the large scale to the cosmic history, which might be explained in the context of the inflationary physics.	background 0.91	0.05	0.05	speculative 0.68
s3	In this paper, we show that it is possible to explain the suppressed lower multipoles in the hybrid new inflation model.	contribution 0.91	0.93	0.92	asserted 0.61

What kind of paper the classifier reports this is: theoretical result 1.00 · evidence from proof or derivation 0.74.

What was examined, and what was not

sources read

arXiv listing abstract v2

not examined

full text
figures and tables
references and citing sentences
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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

The recent observation of the cosmic microwave background anisotropy by the WMAP confirmed that the lower multipoles are considerably suppressed. From the standpoint of the cosmic variance, it is nothing but a statistical accident. Alternatively, one can attribute the deficit of fluctuation on the large scale to the cosmic history, which might be explained in the context of the inflationary physics. In this paper, we show that it is possible to explain the suppressed lower multipoles in the hybrid new inflation model.

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References

Forward citations

Cited by 2 Pith papers

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

Running Spectral Index from Inflation with Modulations
astro-ph.CO 2010-11 conditional novelty 5.0 of 10

Superimposing periodic oscillations on a power-law inflaton potential reproduces the central value of the CMB running spectral index and predicts an enhanced, oscillatory small-scale power spectrum.
Multi-Natural Inflation in Supergravity and BICEP2
hep-ph 2014-03 conditional novelty 4.0 of 10

A two-sine-wave inflaton potential can span a broad region of (n_s, r) space, including n_s near or above unity with r around 0.1 to 0.2, so the model is not excluded by BICEP2.

How the literature uses it

4 arXiv papers cite this in 4 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 · 1 sentence without a confident label

Cites it as background 3 papers

Many models of inflation with broken scale-invariance have been compared to the low [ref] and/or high [ref] multipole anomalies.

Reconstruction of the primordial power spectrum of curvature perturbations using multiple data sets · Introduction · 0.83
Clearly this is not the case for many authors who investigated other possibilities as foreground or systematics not fully removed (see for example [ref] , [ref] ) or some effect of new physics (see [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] ).

A Complete Statistical Analysis for the Quadrupole Amplitude in an Ellipsoidal Universe · Introduction · 0.93
topologies of the universe [ref] , bouncing cosmologies [ref] , various inflationary scenarios (e.g. hybrid models of inflation [ref] , multi-field inflation [ref] , inflation which takes place in two stages [ref] just enough inflation [ref] which could take place in modified gravity theories [ref] or preceded by a fast roll phase [ref] ), etc.

Revisiting a pre-inflationary radiation era and its effect on the CMB power spectrum · Introduction · 1.00

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