One small step for an inflaton, one giant leap for inflation: A novel non-Gaussian tail and primordial black holes

Cai, Yi-Fu; Ma, Xiao-Han; Sasaki, Misao; Wang, Dong-Gang; Zhou, Zihan

doi:10.1016/j.physletb.2022.137461

Cited by 45 publications

(40 citation statements)

References 18 publications

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“…Models with an extremely flat feature fall in this category including those with an inflection point in the potential [7,. Other examples of feature are a tiny bump or dip [61][62][63][64][65][66], an upward or downward step [67][68][69][70][71][72], polynomial shape [73][74][75][76] and Coleman-Weinberg potential [39,77,78]. In these examples, modification of potential makes a sharp η transition on the inflaton dynamics.…”

mentioning

confidence: 99%

Ruling Out Primordial Black Hole Formation From Single-Field Inflation

Kristiano¹,

Yokoyama²

2022

Preprint

139

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mentioning

confidence: 99%

Ruling Out Primordial Black Hole Formation From Single-Field Inflation

Kristiano¹,

Yokoyama²

2022

Preprint

139

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“…[29,[41][42][43][44][45][46][47][48][49] for the first papers on this approach, and also Refs. [50][51][52][53][54][55][56][57] for its application to the exponential tail), qualitative features are often extracted by a simple assumption that only one noise gives a dominant contribution and the other dynamics is well approximated by the one without noise [19,[58][59][60]. Let us also focus on the extremely-flat-potential region, i.e., the ultra slow-roll phase to make perturbations large.…”

Section: Exponential-tailed Curvature Perturbations and Primordial Bl...mentioning

confidence: 99%

“…In the small perturbation region |ζ| 1, the full curvature perturbation is well approximated by the Gaussian part ζ g with perturbative corrections as can be seen in its series expansion, [19][20][21]). Heavier tails such that lim ζ→+∞ Λ = 0 have been also proposed [58][59][60].…”

Section: Exponential-tailed Curvature Perturbations and Primordial Bl...mentioning

confidence: 99%

Primordial black holes and gravitational waves induced by exponential-tailed perturbations

Abe¹,

Inui²,

Tada³

et al. 2022

Preprint

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Primordial black holes (PBHs) whose masses are in ∼ [10 −15 M , 10 −11 M ] have been extensively studied as a candidate of whole dark matter (DM). One of the probes to test such a PBH-DM scenario is scalar-induced stochastic gravitational waves (GWs) accompanied with the enhanced primordial fluctuations to form the PBHs with frequency peaked in the mHz band being targeted by the LISA mission. In order to utilize the stochastic GWs for checking the PBH-DM scenario, it needs to exactly relate the PBH abundance and the amplitude of the GWs spectrum. Recently in Kitajima et al. [1], the impact of the non-Gaussianity of the enhanced primordial curvature perturbations on the PBH abundance has been investigated based on the peak theory, and they found that a specific non-Gaussian feature called the exponential tail significantly increases the PBH abundance compared with the Gaussian case. In this work, we investigate the spectrum of the induced stochastic GWs associated with PBH DM in the exponential-tail case. In order to take into account the non-Gaussianity properly, we employ the diagrammatic approach for the calculation of the spectrum. We find that the amplitude of the stochastic GW spectrum is slightly lower than the one for the Gaussian case, but it can still be detectable with the LISA sensitivity. We also find that the non-Gaussian contribution can appear on the high-frequency side through their complicated momentum configurations. Although this feature emerges under the LISA sensitivity, it might be possible to obtain information about the non-Gaussianity from GW observation with a deeper sensitivity such as the DECIGO mission.

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“…However, alternative mechanisms have been proposed regarding single field inflation. One of them is models with a feature like steps in the potential [35][36][37][38]. Moreover, models with ultra slowroll inflation have been studied [39,40].…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from no-scale supergravity

Spanos

Stamou

2023

Eur. Phys. J. C

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In this paper we study four concrete models, based on no-scale supergravity with SU(2,1)/SU(2) $$\times $$ × U(1) symmetry. We modify either the Kähler potential or the superpotential, which are related to the no-scale theory with this symmetry. In this scenario, the induced Gravitational Waves, are calculated to be detectable by the future space-based observations such as LISA, BBO and DECIGO. The models under study are interrelated, as they all yield the Starobinsky effective-like scalar potential in the unmodified case. We evaluate numerically the scalar power spectrum and the stochastic background of the Gravitational Waves, satisfying the observational Planck cosmological constraints for inflation.

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One small step for an inflaton, one giant leap for inflation: A novel non-Gaussian tail and primordial black holes

Cited by 45 publications

References 18 publications

Ruling Out Primordial Black Hole Formation From Single-Field Inflation

Ruling Out Primordial Black Hole Formation From Single-Field Inflation

Primordial black holes and gravitational waves induced by exponential-tailed perturbations

Gravitational waves from no-scale supergravity

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