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Primordial black holes as dark matter and gravitational waves from single-field polynomial inflation
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We consider the possibility that the majority of dark matter in our Universe consists of black holes of primordial origin. We determine the conditions under which such black holes may have originated from a single-field model of inflation characterized by a quartic polynomial potential. We also explore the effect of higher-dimensional operators. The large power spectrum of curvature perturbations that is needed for a large black hole abundance sources sizable second order tensor perturbations. The resulting stochastic background of primordial gravitational waves could be detected by the future space-based observatories LISA and DECIGO or --as long as we give up on the dark matter connection--by the ground-based Advanced LIGO-Virgo detector network.
Forward citations
Cited by 5 Pith papers
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Gravitational wave signatures of primordial black hole accretion during early matter domination
PBHs that form in a radiation era and accrete during an early matter era could produce a two-peak GW background detectable by LISA or BBO for asteroid-mass PBHs as all of dark matter.
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Scalar-induced gravitational waves from a box-shaped curvature power spectrum
Analytic SIGW spectra for a log-box curvature power spectrum: narrow-box geometric overlap factor turning IR slope k^{3}ln^{2}k into k^{2}ln^{2}k, plus broad-box product of universal edge functions.
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Evolution of Linear Perturbations under Time-Dependent Hubble Friction I: SR-USR-SR Inflation
Analytic asymptotics show the dip in the SR-USR-SR curvature power spectrum comes from cancellation between two growing modes, not a constant-versus-growing cancellation.
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Are Primordial Black Holes Truly Fine-Tuned?
Using a normalized sensitivity measure γ=c/c̄, the authors find γ≈1 for three single-field ultra-slow-roll inflation models and conclude PBH production is not technically unnatural.
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Cosmological constraints on small-scale primordial non-Gaussianity
Current pulsar-timing, CMB, BAO and PBH data constrain the small-scale local f_NL to -10.0 < f_NL < 1.2 for a monochromatic primordial power spectrum, with that constraint conditional on the spectral amplitude A_zeta = 10^-2.
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