REVIEW 9 cited by
The exponential tail of inflationary fluctuations: consequences for primordial black holes
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
The curvature perturbations produced during an early era of inflation are known to have quasi-Gaussian distribution functions close to their maximum, where they are well constrained by measurements of the cosmic microwave background anisotropies and of the large-scale structures. In contrast, the tails of these distributions are poorly known, although this part is the relevant one for rare, extreme objects such as primordial black holes. We show that these tails are highly non-Gaussian, and cannot be described with standard non-Gaussian expansions, that are designed to approximate the distributions close to their maximum only. Using the stochastic-$\delta N$ formalism, we develop a generic framework to compute the tails, which are found to have an exponential, rather than Gaussian, decay. These exponential tails are inevitable, and do not require any non-minimal feature as they simply result from the quantum diffusion of the inflaton field along its potential. We apply our formalism to a few relevant single-field, slow-roll inflationary potentials, where our analytical treatment is confirmed by comparison with numerical results. We discuss the implications for the expected abundance of primordial black holes in these models, and highlight that it can differ from standard results by several orders of magnitude. In particular, we find that potentials with an inflection point overproduce primordial black holes, unless slow roll is violated.
Forward citations
Cited by 9 Pith papers
-
Nonlinear Lattice Framework for Inflation: Bridging stochastic inflation and the $\delta{N}$ formalism
A shear-free locally FLRW lattice framework for single-field inflation captures spatially varying expansion, curvature corrections, and nonlinear δN observables at a fraction of the cost of full numerical relativity.
-
Confronting infrared divergences in de Sitter: loops, logarithms and the stochastic formalism
The authors show that loop corrections do not alter tree-level time dependence in de Sitter correlators, so secular growth is a regularization artifact, not a physical effect.
-
The gravitational-wave fingerprint of dynamically assembled primordial black hole cluster seeds in JWST's Little Red Dots
Strongly clustered PBHs with a QCD-broad mass function form IMBH nuclei plus light-PBH swarms that assemble LRD-scale seeds in 10-50 Myr and radiate a truncated f^{2/3} GW background topped by a ringdown comb.
-
Primordial black holes forming during kination: the trapped, the overdense, and the void
In one non-attractor inflation model, initially similar field fluctuations produce three distinct black-hole formation channels—trapped, overdense, void—with collapse thresholds determined by the full density profile,...
-
Deviations from Gaussian White Noise in Stochastic Inflation
Relaxing the sharp cutoff or the Bunch-Davies initial state in stochastic inflation makes the noise colored, and relaxing the initial state also makes it non-Gaussian.
-
Friction in Stochastic Inflation
Adding a constant drift to time-reversed stochastic inflation in a flat potential yields an exact curvature distribution with exponential tails; forward and reverse delta-N formalisms differ by a factor of two in the ...
-
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.
-
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.
-
Little Red Dots from Small-Scale Primordial Black Hole Clustering
Densely clustered 30-solar-mass primordial black holes can sequentially merge into ~10^6 solar-mass seeds by redshift 6, possibly explaining JWST little red dots, with high spin from tidal torques and a two-peak gravi...
Discussion (0). Sign in to comment.