Constraints on amplitudes of curvature perturbations from primordial black holes

Bugaev, É. V.; Klimai, Peter

doi:10.1103/physrevd.79.103511

Cited by 56 publications

(86 citation statements)

References 94 publications

(153 reference statements)

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“…On the second count, assuming that the formation of the PBHs coincided with the end of inflation, then the arguments we presented in section (I A) apply. Thus, using N as a discriminator we rule out A 0 > 3 and µ This model has also been analysed by [70], in which the authors use neutrino and γ− ray background data to constrain the PBH mass spectrum, which determines the spectral index on small scales k ∼ 15 Mpc −1 . Then assuming that the running mass model is correct they reconstruct the power spectrum, finding that on these small scales the spectrum is highly sensitive to the running of the spectral index.…”

Section: Discussionmentioning

confidence: 99%

Generating primordial black holes via hilltop-type inflation models

Alabidi

Kohri

2009

Phys. Rev. D

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It has been shown that black holes would have formed in the early Universe if, on any given scale, the spectral amplitude of the Cosmic Microwave Background (CMB) exceeds P ζ ∼ 10 −4 . This value is within the bounds allowed by astrophysical phenomena for the small scale spectrum of the CMB, corresponding to scales which exit the horizon at the end of slow-roll inflation. Previous work by Kohri et. al. (2007) showed that for black holes to form from a single field model of inflation, the slope of the potential at the end of inflation must be flatter than it was at horizon exit. In this work we show that a phenomenological Hilltop model of inflation, satisfying the Kohri et. al. criteria, could lead to the production of black holes, if the power of the inflaton self-interaction is less than or equal to 3, with a reasonable number or e−folds. We extend our analysis to the running mass model, and confirm that this model results in the production of black holes, and by using the latest WMAP year 5 bounds on the running of the spectral index, and the black hole constraint we update the results of Leach et. al. (2000) excluding more of parameter space.

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Section: Discussionmentioning

confidence: 99%

Generating primordial black holes via hilltop-type inflation models

Alabidi

Kohri

2009

Phys. Rev. D

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“…[4,5], we investigated this case, and argued there that the relative large amplitude of the potential Ψ can be achieved on subhorizon scales and may lead to the overproduction of PBHs at the end of inflation. The constraint on the amplitude of the curvature perturbation is then tighter than the current bound from the PBHs formed throughout the radiation epoch [5] (for the constraints on the "standard" formation of PBHs see [6][7][8][9][10][11][12][13][14][15][16]). …”

Section: Introductionmentioning

confidence: 99%

Boosted perturbations at the end of inflation

Zaballa

Sasaki²

2010

J. Cosmol. Astropart. Phys.

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We study the effect on the primordial cosmological perturbations of a sharp transition from inflationary to a radiation and matter dominated epoch respectively. We assume that the perturbations are generated by the vacuum fluctuations of a scalar field slowly rolling down its potential, and that the transition into the subsequent epoch takes place much faster than a Hubble time. The behaviour of the superhorizon perturbations corresponding to cosmological scales in this case is well known. However, it is not clear how perturbations on scales of and smaller than the Hubble horizon scale at the end of inflation may evolve through such a transition. We derive the evolution equation for the gravitational potential Ψ, which allows us to study the evolution of the perturbations on all scales under these circumstances. We show that for a certain range of scales inside the horizon at the end of inflation, the amplitude of the perturbations are enhanced relative to the superhorizon scales. This enhancement may lead to the overproduction of Primordial Black Holes (PBHs), and therefore constrain the dynamics of the transitions that take place at the end of inflation.

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“…At the time, highly peaked spectra for the primordial black holes was what was mostly considered and hence the effect of critical collapse scaling was thought to be roughly degenerate with more realistic initial mass spectra. In the literature, therefore, with notable exceptions such as [31], one mostly approximates the primordial black-hole mass to be identical with the horizon mass -or one simply scales the overall spectrum by some constant. Both approaches yield a specific functional form for the predictions of β in any given model.…”

Section: Introductionmentioning

confidence: 99%

Effects of critical collapse on primordial black-hole mass spectra

2016

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Certain inflationary models as well as realisations of phase transitions in the early Universe predict the formation of primordial black holes. For most mass ranges, the fraction of matter in the form of primordial black holes is limited by many different observations on various scales. Primordial black holes are assumed to be formed when overdensities that cross the horizon have Schwarzschild radii larger than the horizon. Traditionally it was therefore assumed that primordial black-hole masses were equal to the horizon mass at their time of formation. However, detailed calculations of their collapse show that primordial black holes formed at each point in time should rather form a spectrum of different masses, obeying critical scaling. Though this has been known for more than 15 years, the effect of this scaling behaviour is largely ignored when considering predictions for primordial black-hole mass spectra. In this paper we consider the critical collapse scaling for a variety of models which produce primordial black holes, and find that it generally leads to a shift, broadening and an overall decrease of the mass contained in primordial black holes. This effect is model and parameter dependent and cannot be contained by a constant rescaling of the spectrum; it can become important and should be taken into account when comparing to observational constraints.

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Constraints on amplitudes of curvature perturbations from primordial black holes

Cited by 56 publications

References 94 publications

Generating primordial black holes via hilltop-type inflation models

Generating primordial black holes via hilltop-type inflation models

Boosted perturbations at the end of inflation

Effects of critical collapse on primordial black-hole mass spectra

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