Primordial black holes in non-Gaussian regimes

Young, Sam; Byrnes, Christian T.

doi:10.1088/1475-7516/2013/08/052

Cited by 174 publications

(217 citation statements)

References 64 publications

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“…Indeed we have briefly checked that the local non-linearity parameter f NL is as small as ∼ 0.1 and for such a small NG it is known that the predicted PBH abundance is hardly affected [43][44][45]. However the second peak on ∼ 30M which we will show later might be modified by NG effects since it corresponds with the phase of the beginning of the new inflation.…”

Section: Formation Of Primordial Black Holesmentioning

confidence: 83%

Primordial black holes as dark matter in supergravity inflation models

et al. 2016

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We propose a novel scenario to produce abundant primordial black holes (PBHs) in new inflation which is a second phase of a double inflation in the supergravity frame work. In our model, some preinflation phase before the new inflation is assumed and it would be responsible for the primordial curvature perturbations on the cosmic microwave background scale, while the new inflation produces only the small scale perturbations. Our new inflation model has linear, quadratic, and cubic terms in its potential and PBH production corresponds with its flat inflection point. The linear term can be interpreted to come from a supersymmetry-breaking sector, and with this assumption, the vanishing cosmological constant condition after inflation and the flatness condition for the inflection point can be consistently satisfied.

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Section: Formation Of Primordial Black Holesmentioning

confidence: 83%

Primordial black holes as dark matter in supergravity inflation models

et al. 2016

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“…[147] and the many references listed in Section II therein, as well as [148,149]). In particular, their abundance is believed to be intrinsically related to a possible non-Gaussianity of the density perturbations [150,151]. Moreover, it has been argued that a potential detection of a PBH might rule out several WIMP models [152][153][154][155][156][157].…”

Section: Evaporation Of Primordial Black Holesmentioning

confidence: 99%

The synergy between CMB spectral distortions and anisotropies

Lucca

Schöneberg

Hooper

et al. 2020

J. Cosmol. Astropart. Phys.

159

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Spectral distortions and anisotropies of the CMB provide independent and complementary probes to study energy injection processes in the early universe. Here we discuss the synergy between these observables, and show the promising future of spectral distortion missions to constrain both exotic and non-exotic energy injections. We show that conventional probes such as Big Bang Nucleosynthesis and CMB anisotropies can benefit from and even be surpassed by future spectral distortion experiments. For this, we have implemented a unified framework within the Boltzmann code class to consistently treat the thermal evolution of photons and baryons. Furthermore, we give an extensive and pedagogical introduction into the topic of spectral distortions and energy injections throughout the thermal history of the universe, highlighting some of their unique features and potential as a novel probe for cosmology and particle physics.1 This quantity should not be confused with the actual photon temperature Tγ , which may have a more complicated evolution. The precise normalization of Tz is arbitrary, but T0 ≡ Tz(0) will be chosen close to the actual temperature today, Tγ(0) = (2.7255 ± 0.0005)K [65,66], in order to have Tγ Tz at least in the late universe.2 Note that with perturbations in the PPSD this is not true anymore as shown in [51].

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“…The relative height ν (more specifically, the critical value ν c = δ c / δ 2 1/2 ) is the crucial parameter for determining PBH abundance. The full calculation will not be discussed here, and can be significantly affected by primordial non-Gaussianity [20,21], and the non-linear relations between the density contrast and the curvature perturbation (discussed briefly in section VII, readers are directed to recent papers [22][23][24][25]). In equation (15), δ 2 is the variance of perturbations, which can be found by integrating over the power spectrum:…”

Section: Timing Is Everythingmentioning

confidence: 99%

The primordial black hole formation criterion re-examined: Parametrisation, timing and the choice of window function

Young

2019

Int. J. Mod. Phys. D

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127

134

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In this paper, the criterion used to determine whether a density perturbation will collapse to form a primordial black hole (PBH) is re-examined, in respect of its use to determine the abundance of PBHs. There is particular focus on which parameter to use, the time at which the abundance should be calculated, and the use of different smoothing functions. It is concluded that, with the tools currently available, the smoothed density contrast should be used rather than the peak value, and should be calculated from the time-independent component of the density contrast in the super-horizon limit (long before perturbations enter the horizon) rather than at horizon crossing. For the first time the effect of the choice of smoothing function upon the formation criterion is calculated, and, for a given abundance of PBHs, it is found that the uncertainty in the amplitude of the power spectrum due to this is O(10%), an order of magnitude smaller than previous calculations suggest. The relation between the formation criterion stated in terms of the density contrast and the curvature perturbation R is also discussed.

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Primordial black holes in non-Gaussian regimes

Cited by 174 publications

References 64 publications

Primordial black holes as dark matter in supergravity inflation models

Primordial black holes as dark matter in supergravity inflation models

The synergy between CMB spectral distortions and anisotropies

The primordial black hole formation criterion re-examined: Parametrisation, timing and the choice of window function

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