pith. sign in

arxiv: 2605.21474 · v1 · pith:ISTEI754new · submitted 2026-05-20 · ✦ hep-ph · astro-ph.CO· gr-qc

Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component

Yann Gouttenoire , Nicholas Leister , Pedro Schwaller This is my paper

Pith reviewed 2026-05-21 03:24 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COgr-qc
keywords primordial black holesgravitational wavesreheatingscalar-induced gravitational wavespoltergeist signalearly universe cosmologymass function
0
0 comments X

The pith

Including the natural mass spread of primordial black holes suppresses the Poltergeist gravitational-wave signal from their evaporation by orders of magnitude.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines how light primordial black holes can reheat the universe through evaporation and leave behind a stochastic gravitational-wave background. In the idealized case where all black holes share exactly the same mass, their evaporation creates a sudden shift from matter to radiation domination that generates a prominent Poltergeist gravitational-wave signal. Accounting for the unavoidable spread in black-hole masses required by general relativity, specifically an infrared power-law tail in the mass function, makes the transition gradual and reduces the Poltergeist amplitude by several orders of magnitude. The resulting signal falls to the same strength as scalar-induced waves from any generic early-matter era. Breaking the scalar-induced spectrum into eight distinct production channels shows that only the waves generated at the moment the black holes form could reach the sensitivity of future detectors or the bound on extra radiation, reopening previously excluded windows for ultra-light primordial black holes.

Core claim

The reheating of the universe by the evaporation of light primordial black holes can leave a stochastic gravitational-wave background. In the monochromatic limit, their simultaneous evaporation produces an abrupt matter-to-radiation transition, triggering the so-called Poltergeist GW signal. Including the irreducible mass spread implied by gravitational collapse in General Relativity, whose infrared tail scales as df_PBH/d ln M_PBH ∝ M_PBH^{3.78}, smooths reheating enough to suppress the Poltergeist background by orders of magnitude, down to the level of the scalar-induced GW signal produced during a generic early matter era. A complete decomposition of the scalar-induced spectrum into eight

What carries the argument

The infrared tail of the PBH mass function scaling as df_PBH/d ln M_PBH ∝ M_PBH^{3.78} from gravitational collapse, which lengthens the duration of the matter-to-radiation transition and thereby damps the Poltergeist peak.

If this is right

  • The Poltergeist GW background falls to the same order as scalar-induced signals from other early matter eras such as heavy relic decay.
  • Only the scalar-induced GW channel from PBH formation itself among the eight channels can reach the Delta N_eff bound or projected sensitivities.
  • Regions of ultra-light PBH parameter space previously excluded by gravitational-wave constraints become viable again.
  • Accurate prediction of reheating GWs requires including at least the minimal GR mass spread rather than assuming a monochromatic population.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar smoothing from mass or lifetime distributions could weaken abrupt-transition signals in other early-universe models, such as moduli decays or first-order phase transitions.
  • Future detectors might use the absence of a sharp Poltergeist peak to distinguish PBH-driven reheating from other early-matter-era scenarios.
  • If the actual PBH mass function is broader than the minimal GR tail, the suppression would be even stronger, further reducing any observable relic.

Load-bearing premise

The infrared tail of the PBH mass function implied by gravitational collapse in General Relativity scales as df_PBH/d ln M_PBH ∝ M_PBH^{3.78} and this tail is sufficient to smooth the transition enough to suppress the Poltergeist signal by orders of magnitude.

What would settle it

A detection of a strong Poltergeist gravitational-wave background whose amplitude and frequency peak match the monochromatic PBH prediction would falsify the claimed suppression from the mass spread.

Figures

Figures reproduced from arXiv: 2605.21474 by Nicholas Leister, Pedro Schwaller, Yann Gouttenoire.

Figure 1
Figure 1. Figure 1: Summary of all present-day SIGW components at the benchmark ( [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Exclusion and sensitivity contours in the ( [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Evolution of the PBH and radiation energy fractions, Ω [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Schematic illustration of the characteristic comoving scales during a PBH-dominated [PITH_FULL_IMAGE:figures/full_fig_p014_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Schematic comparison of the Press–Schechter and peak-theory prescriptions for pri [PITH_FULL_IMAGE:figures/full_fig_p015_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: PBH mass distribution ψf (MPBH) for different widths ∆ and amplitudes AR of the log￾normal curvature power spectrum in Eq. (24). To remain agnostic about the model-dependent UV part, we conservatively model the mass distribution as a power law ψf (MPBH) ∝ M 1+1/γM PBH ∝ M3.78 PBH with a sharp cutoff at Mcut, see Eq. (31). The reference mass Mf is the horizon mass at kf = H, while the horizon mass entering … view at source ↗
Figure 7
Figure 7. Figure 7: Schematic representation of the averaged background quantities ( [PITH_FULL_IMAGE:figures/full_fig_p019_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Background energy-density fractions during PBH reheating for monochromatic and [PITH_FULL_IMAGE:figures/full_fig_p020_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Transfer function of the Newtonian potential Φ assuming adiabatic ( [PITH_FULL_IMAGE:figures/full_fig_p022_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Shown is the evolution of energy densities (Ω [PITH_FULL_IMAGE:figures/full_fig_p024_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Scalar evolution during PBH reheating. The figure displays the evolution of the [PITH_FULL_IMAGE:figures/full_fig_p025_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Suppression factor SΦ(k) of the Newtonian potential Φ for different values of the critical exponent γM entering the Choptuik’s PBH mass distribution ψ(M) in Eq. (31). In the sub-horizon limit k⟨ηeva⟩ ≫ 1, the analytical estimate in Eq. (78) — with ηosc determined from Eq. (82) — (solid lines) and the analytical estimate in Eq. (421) (dashed line) show excellent agreement with the numerical computation (bl… view at source ↗
Figure 13
Figure 13. Figure 13: Comparison of the Poltergeist SIGW signal for adiabatic Φ and isocurvature [PITH_FULL_IMAGE:figures/full_fig_p043_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: SIGW signal generated during the PBH-induced eMD phase, Ω [PITH_FULL_IMAGE:figures/full_fig_p050_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Top: Cutoff dependence of SIGWs from PBH Isocurvature during RD1. We show the induced spectra for different IR cutoffs (red curves) and compare with our analytic broken PL approximations (dashed gray lines). In reality kIR is chosen as keq. Bottom: Resulting SIGW signal including dilution during early and late time MD adjusted to the PBH scenario. 55 [PITH_FULL_IMAGE:figures/full_fig_p055_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Present-day SIGW signal Ω(form) GW,0 [Φ] from PBH formation, Eq. (243), in the (MPBH, βf ) plane. The width ∆ of the curvature peak is kept as a free parameter. 57 [PITH_FULL_IMAGE:figures/full_fig_p057_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Cosmological evolution of the Newtonian perturbation Φ and isentropic perturbation [PITH_FULL_IMAGE:figures/full_fig_p074_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Transfer function of the Newtonian potential Φ assuming adiabatic ( [PITH_FULL_IMAGE:figures/full_fig_p075_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Suppression factor SΦ(k) of the Newtonian potential Φ for different values of the critical exponent γM entering Choptuik’s PBH mass distribution ψ(M) in Eq. (31). We compare the analytical expression in Eq. (415) using ηosc determined from Eq. (417) (solid lines) and from Eq. (416) (dashed lines), which rely respectively on the first and second derivatives of the Newtonian potential, Φ′ and Φ′′, with Φ gi… view at source ↗
Figure 20
Figure 20. Figure 20: Oscillation avaraged squared GW kernels I 2. Left: Kernels for a gradual reheating phase. Right: Kernels for a PBH reheating phase. We compare the results obtained using the stepwise definition of tensor Green functions Gh during the eMD and RD2 matched at reheating, with the results obtained using only Gh from the eMD. We also present our analytically derived asymptotics for the IR and UV tails, respecti… view at source ↗
Figure 21
Figure 21. Figure 21: SIGWs produced during eMD for sudden and gradual reheating. The comparison [PITH_FULL_IMAGE:figures/full_fig_p104_21.png] view at source ↗
Figure 22
Figure 22. Figure 22: Maximal perturbative eMD signal from Choptuik-smeared PBHs using the non-linear [PITH_FULL_IMAGE:figures/full_fig_p104_22.png] view at source ↗
Figure 23
Figure 23. Figure 23: SIGW spectrum for a monochromatic PBH mass distribution, including adiabatic [PITH_FULL_IMAGE:figures/full_fig_p107_23.png] view at source ↗
Figure 24
Figure 24. Figure 24: The black lines shows the most optimistic GW reach. We refer the reader to the [PITH_FULL_IMAGE:figures/full_fig_p109_24.png] view at source ↗
read the original abstract

The reheating of the universe by the evaporation of light primordial black holes (PBHs) can leave a stochastic gravitational-wave (GW) background in the early Universe. In the monochromatic limit, their simultaneous evaporation produces an abrupt matter-to-radiation transition, triggering the so-called Poltergeist GW signal, usually predicted to be dominant and observable. We revisit this result by including the irreducible mass spread implied by gravitational collapse in General Relativity, whose infrared tail scales as $d f_{\rm PBH}/d\ln M_{\rm PBH}\propto M_{\rm PBH}^{3.78}$. We show that this minimal width smooths reheating enough to suppress the Poltergeist background by orders of magnitude, down to the level of the scalar-induced GW signal produced during a generic early matter era, such as one driven by the decay of a heavy relic. We provide a complete decomposition of the scalar-induced spectrum into eight production channels and find that none, except the one from PBH formation, reaches either the $\Delta N_{\rm eff}$ bound or the projected sensitivity of future GW observatories. This reopens regions of ultra-light PBH parameter space previously thought to be excluded by these constraints.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript claims that the irreducible mass spread of light primordial black holes, arising from general-relativistic critical collapse and featuring an infrared tail df_PBH/d ln M_PBH ∝ M_PBH^{3.78}, smooths the matter-to-radiation transition during PBH evaporation. This smoothing suppresses the Poltergeist scalar-induced gravitational-wave background by orders of magnitude, bringing it down to the amplitude of generic early-matter-era scalar-induced signals (e.g., from heavy-relic decay). The authors decompose the scalar-induced spectrum into eight distinct production channels and conclude that only the channel associated with PBH formation itself reaches either the ΔN_eff bound or the sensitivity of future GW observatories, thereby reopening previously excluded regions of ultra-light PBH parameter space.

Significance. If the central suppression result holds, the work is significant because it removes a dominant constraint on ultra-light PBHs and shows that a minimal, GR-derived mass spread is already sufficient to eliminate the Poltergeist signal. The explicit eight-channel decomposition is a clear strength, as it allows quantitative comparison of contributions from PBH formation, evaporation, and the subsequent radiation-dominated era. The analysis is grounded in an external, parameter-free mass-function tail rather than an ad-hoc width, which strengthens the claim relative to purely phenomenological treatments.

major comments (3)
  1. [§4.1, Eq. (18)] §4.1 and the paragraph following Eq. (18): the claim that the M_PBH^{3.78} tail produces sufficient smoothing to suppress the Poltergeist amplitude by orders of magnitude is load-bearing for the headline result, yet the manuscript does not show the explicit time evolution of the total energy density or the Hubble parameter across the transition when the tail is included; without this, it is unclear whether the integrated energy injection from the low-mass end is gradual enough to eliminate the sharp jump in the equation of state that sources the Poltergeist signal.
  2. [§5.3] §5.3, the eight-channel decomposition: while the decomposition into eight production channels is presented, the numerical evaluation of the source term for each channel (particularly channels 3–7 that arise during the smoothed evaporation epoch) is not accompanied by sufficient detail on the integration limits, transfer-function approximations, or convergence tests; this makes it difficult to verify the assertion that none of these channels reaches the ΔN_eff bound or future-detector sensitivity.
  3. [Abstract, §6] Abstract and §6: the reopening of ultra-light PBH parameter space rests on the Poltergeist suppression being robust to the precise lower-mass cutoff and normalization of the tail; the manuscript should quantify the sensitivity of the final GW amplitude to variations in these quantities (e.g., by showing the amplitude as a function of the cutoff mass) to confirm that the suppression remains orders of magnitude for any physically plausible cutoff.
minor comments (2)
  1. [Figure 3] Figure 3: the legend and axis labels are too small to read comfortably; enlarging them would improve clarity of the comparison between the suppressed Poltergeist curve and the other channels.
  2. [§3] Notation: the symbol f_PBH is used both for the mass fraction and for the differential mass function; a clearer distinction (e.g., f_PBH(M) versus df_PBH/d ln M) would reduce potential confusion in §3.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We appreciate the recognition of the significance of our results and address each major comment in detail below. We plan to revise the manuscript to incorporate additional figures, details, and quantifications as suggested.

read point-by-point responses

  1. Referee: [§4.1, Eq. (18)] §4.1 and the paragraph following Eq. (18): the claim that the M_PBH^{3.78} tail produces sufficient smoothing to suppress the Poltergeist amplitude by orders of magnitude is load-bearing for the headline result, yet the manuscript does not show the explicit time evolution of the total energy density or the Hubble parameter across the transition when the tail is included; without this, it is unclear whether the integrated energy injection from the low-mass end is gradual enough to eliminate the sharp jump in the equation of state that sources the Poltergeist signal.

    Authors: We agree that an explicit demonstration of the smoothed transition would clarify the mechanism. In the revised version, we will add a new figure in Section 4.1 illustrating the time evolution of the total energy density and the Hubble parameter for the PBH distribution including the infrared tail. This figure will compare the gradual transition to the sharp jump in the monochromatic case, confirming that the low-mass tail provides sufficient smoothing to suppress the Poltergeist signal. revision: yes

  2. Referee: [§5.3] §5.3, the eight-channel decomposition: while the decomposition into eight production channels is presented, the numerical evaluation of the source term for each channel (particularly channels 3–7 that arise during the smoothed evaporation epoch) is not accompanied by sufficient detail on the integration limits, transfer-function approximations, or convergence tests; this makes it difficult to verify the assertion that none of these channels reaches the ΔN_eff bound or future-detector sensitivity.

    Authors: We acknowledge the need for more transparency in the numerical implementation. We will revise Section 5.3 to include explicit statements of the integration limits for each of the eight channels, the specific approximations adopted for the transfer functions, and a summary of convergence tests performed. Furthermore, we will add an appendix detailing the numerical parameters and providing sample convergence plots to allow independent verification of the results. revision: yes

  3. Referee: [Abstract, §6] Abstract and §6: the reopening of ultra-light PBH parameter space rests on the Poltergeist suppression being robust to the precise lower-mass cutoff and normalization of the tail; the manuscript should quantify the sensitivity of the final GW amplitude to variations in these quantities (e.g., by showing the amplitude as a function of the cutoff mass) to confirm that the suppression remains orders of magnitude for any physically plausible cutoff.

    Authors: We agree that demonstrating robustness to the cutoff is important for the claim. In the revised manuscript, we will include in Section 6 a quantitative analysis of the dependence of the GW amplitude on the lower-mass cutoff. This will consist of a plot or table showing the Poltergeist amplitude for a range of cutoff masses, confirming that the suppression by orders of magnitude holds for all physically plausible values above the Planck mass. We will also discuss the sensitivity to the normalization of the tail. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central claim relies on external GR critical-collapse mass-function tail

full rationale

The paper imports the infrared tail scaling df_PBH/d ln M_PBH ∝ M_PBH^{3.78} directly from established results on gravitational collapse in General Relativity, rather than deriving, fitting, or redefining it internally to produce the claimed suppression of the Poltergeist signal. The subsequent smoothing of the matter-to-radiation transition, the reduction of the Poltergeist amplitude by orders of magnitude, and the decomposition of the scalar-induced spectrum into eight channels are all downstream applications of this externally supplied mass function to standard early-universe GW calculations. No step reduces by construction to a self-fit, a self-citation chain, or an ansatz smuggled from the authors' prior work; the derivation remains self-contained against external benchmarks for the PBH mass spectrum and does not invoke uniqueness theorems or renamings that would create circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the GR-derived infrared tail of the PBH mass function and on the assumption that this tail dominates the smoothing of the reheating transition; no free parameters are introduced in the abstract, and no new entities are postulated.

axioms (1)
  • domain assumption The infrared tail of the PBH mass function from gravitational collapse in General Relativity scales as df_PBH / d ln M_PBH ∝ M_PBH^{3.78}
    Invoked in the abstract as the minimal width that smooths reheating.

pith-pipeline@v0.9.0 · 5751 in / 1580 out tokens · 42357 ms · 2026-05-21T03:24:32.181859+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

300 extracted references · 260 canonical work pages · 75 internal anchors

  1. [1]

    Y. B. Zel’dovich and I. D. Novikov,The Hypothesis of Cores Retarded during Expansion and the Hot Cosmological Model,Sov. Astron.10(1967) 602

    1967

  2. [2]

    Hawking,Gravitationally collapsed objects of very low mass,Mon

    S. Hawking,Gravitationally collapsed objects of very low mass,Mon. Not. Roy. Astron. Soc.152(1971) 75

    1971

  3. [3]

    B. J. Carr and S. W. Hawking,Black holes in the early Universe,Mon. Not. Roy. Astron. Soc.168(1974) 399–415

    1974

  4. [4]

    B. J. Carr,The Primordial black hole mass spectrum,Astrophys. J.201(1975) 1–19

    1975

  5. [5]

    Primordial Black Holes - Perspectives in Gravitational Wave Astronomy -

    M. Sasaki, T. Suyama, T. Tanaka and S. Yokoyama,Primordial black holes—perspectives in gravitational wave astronomy,Class. Quant. Grav.35(2018) 063001, [1801.05235]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  6. [6]

    B. Carr, K. Kohri, Y. Sendouda and J. Yokoyama,Constraints on primordial black holes,Rept. Prog. Phys.84(2021) 116902, [2002.12778]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  7. [7]

    Primordial Black Holes as Dark Matter: Recent Developments

    B. Carr and F. Kuhnel,Primordial Black Holes as Dark Matter: Recent Developments, Ann. Rev. Nucl. Part. Sci.70(2020) 355–394, [2006.02838]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  8. [8]

    A. M. Green and B. J. Kavanagh,Primordial Black Holes as a dark matter candidate,J. Phys. G48(2021) 043001, [2007.10722]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  9. [9]

    Escriv` a, F

    A. Escriv` a, F. Kuhnel and Y. Tada,Primordial Black Holes,2211.05767

    work page arXiv

  10. [10]

    B. Carr, A. J. Iovino, G. Perna, V. Vaskonen and H. Veerm¨ ae,Primordial black holes: constraints, potential evidence and prospects,2601.06024

    work page arXiv

  11. [11]

    Primordial Black Holes and Primordial Nucleosynthesis I: Effects of Hadron Injection from Low Mass Holes

    K. Kohri and J. Yokoyama,Primordial black holes and primordial nucleosynthesis. 1. Effects of hadron injection from low mass holes,Phys. Rev. D61(2000) 023501, [astro-ph/9908160]

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  12. [12]

    B. J. Carr, K. Kohri, Y. Sendouda and J. Yokoyama,New cosmological constraints on primordial black holes,Phys. Rev. D81(2010) 104019, [0912.5297]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  13. [13]

    S. K. Acharya and R. Khatri,CMB and BBN constraints on evaporating primordial black holes revisited,JCAP06(2020) 018, [2002.00898]

    work page arXiv 2020

  14. [14]

    Keith, D

    C. Keith, D. Hooper, N. Blinov and S. D. McDermott,Constraints on Primordial Black Holes From Big Bang Nucleosynthesis Revisited,Phys. Rev. D102(2020) 103512, [2006.03608]

    work page arXiv 2020

  15. [15]

    Boccia, F

    A. Boccia, F. Iocco and L. Visinelli,Constraining the primordial black hole abundance through big-bang nucleosynthesis,Phys. Rev. D111(2025) 063508, [2405.18493]

    work page arXiv 2025

  16. [16]

    Holst, G

    I. Holst, G. Krnjaic and H. Xiao,Clustering and runaway merging in a primordial black hole dominated universe,Phys. Rev. D112(2025) 083527, [2412.01890]

    work page arXiv 2025

  17. [17]

    Primordial Black Holes Evaporating before Big Bang Nucleosynthesis

    Q.-f. Wu and X.-J. Xu,Primordial black holes evaporating before Big Bang nucleosynthesis,JCAP02(2026) 063, [2509.05618]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  18. [18]

    T. Wang, E. Grohs and L. Mersini-Houghton,How Primordial Black Holes Change BBN,2511.18646

    work page arXiv

  19. [19]

    B. J. Carr,Some cosmological consequences of primordial black-hole evaporations, Astrophys. J.206(1976) 8–25. 110

    1976

  20. [20]

    J. E. Lidsey, T. Matos and L. A. Urena-Lopez,The Inflaton field as selfinteracting dark matter in the brane world scenario,Phys. Rev. D66(2002) 023514, [astro-ph/0111292]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  21. [21]

    J. C. Hidalgo, L. A. Urena-Lopez and A. R. Liddle,Unification models with reheating via Primordial Black Holes,Phys. Rev. D85(2012) 044055, [1107.5669]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  22. [22]

    Dalianis and G

    I. Dalianis and G. P. Kodaxis,Reheating in Runaway Inflation Models via the Evaporation of Mini Primordial Black Holes,Galaxies10(2022) 31, [2112.15576]

    work page arXiv 2022

  23. [23]

    Riajul Haque, E

    M. Riajul Haque, E. Kpatcha, D. Maity and Y. Mambrini,Primordial black hole reheating,Phys. Rev. D108(2023) 063523, [2305.10518]

    work page arXiv 2023

  24. [24]

    Gross, Y

    M. Gross, Y. Mambrini, E. Kpatcha, M. O. Olea-Romacho and R. Roshan,Gravitational wave production during reheating: From the inflaton to primordial black holes,Phys. Rev. D111(2025) 035020, [2411.04189]

    work page arXiv 2025

  25. [25]

    B. J. Carr and J. E. Lidsey,Primordial black holes and generalized constraints on chaotic inflation,Phys. Rev. D48(1993) 543–553

    1993

  26. [26]

    Ivanov, P

    P. Ivanov, P. Naselsky and I. Novikov,Inflation and primordial black holes as dark matter,Phys. Rev. D50(1994) 7173–7178

    1994

  27. [27]

    Massive Primordial Black Holes from Hybrid Inflation as Dark Matter and the seeds of Galaxies

    S. Clesse and J. Garc´ ıa-Bellido,Massive Primordial Black Holes from Hybrid Inflation as Dark Matter and the seeds of Galaxies,Phys. Rev. D92(2015) 023524, [1501.07565]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  28. [28]

    Primordial black hole dark matter from single field inflation

    G. Ballesteros and M. Taoso,Primordial black hole dark matter from single field inflation,Phys. Rev. D97(2018) 023501, [1709.05565]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  29. [29]

    Pattison, V

    C. Pattison, V. Vennin, H. Assadullahi and D. Wands,Quantum diffusion during inflation and primordial black holes,JCAP10(2017) 046, [1707.00537]

    work page arXiv 2017

  30. [30]

    J. R. Espinosa, D. Racco and A. Riotto,Cosmological Signature of the Standard Model Higgs Vacuum Instability: Primordial Black Holes as Dark Matter,Phys. Rev. Lett.120 (2018) 121301, [1710.11196]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  31. [31]

    Single Field Double Inflation and Primordial Black Holes

    K. Kannike, L. Marzola, M. Raidal and H. Veerm¨ ae,Single Field Double Inflation and Primordial Black Holes,JCAP09(2017) 020, [1705.06225]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  32. [32]

    Inflationary Primordial Black Holes as All Dark Matter

    K. Inomata, M. Kawasaki, K. Mukaida, Y. Tada and T. T. Yanagida,Inflationary Primordial Black Holes as All Dark Matter,Phys. Rev. D96(2017) 043504, [1701.02544]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  33. [33]

    Primordial Black Holes from Inflation and non-Gaussianity

    G. Franciolini, A. Kehagias, S. Matarrese and A. Riotto,Primordial Black Holes from Inflation and non-Gaussianity,JCAP03(2018) 016, [1801.09415]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  34. [34]

    C. T. Byrnes, P. S. Cole and S. P. Patil,Steepest growth of the power spectrum and primordial black holes,JCAP06(2019) 028, [1811.11158]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  35. [35]

    J. M. Ezquiaga, J. Garc´ ıa-Bellido and V. Vennin,The exponential tail of inflationary fluctuations: consequences for primordial black holes,JCAP03(2020) 029, [1912.05399]

    work page arXiv 2020

  36. [36]

    Ballesteros, J

    G. Ballesteros, J. Rey, M. Taoso and A. Urbano,Primordial black holes as dark matter and gravitational waves from single-field polynomial inflation,JCAP07(2020) 025, [2001.08220]. 111

    work page arXiv 2020

  37. [37]

    Fumagalli, S

    J. Fumagalli, S. Renaux-Petel, J. W. Ronayne and L. T. Witkowski,Turning in the landscape: A new mechanism for generating primordial black holes,Phys. Lett. B841 (2023) 137921, [2004.08369]

    work page arXiv 2023

  38. [38]

    Pi and M

    S. Pi and M. Sasaki,Primordial black hole formation in nonminimal curvaton scenarios, Phys. Rev. D108(2023) L101301, [2112.12680]

    work page arXiv 2023

  39. [39]

    Kristiano and J

    J. Kristiano and J. Yokoyama,Constraining Primordial Black Hole Formation from Single-Field Inflation,Phys. Rev. Lett.132(2024) 221003, [2211.03395]

    work page arXiv 2024

  40. [40]

    Karam, N

    A. Karam, N. Koivunen, E. Tomberg, V. Vaskonen and H. Veerm¨ ae,Anatomy of single-field inflationary models for primordial black holes,JCAP03(2023) 013, [2205.13540]

    work page arXiv 2023

  41. [41]

    Franciolini, A

    G. Franciolini, A. Iovino, Junior., M. Taoso and A. Urbano,Perturbativity in the presence of ultraslow-roll dynamics,Phys. Rev. D109(2024) 123550, [2305.03491]

    work page arXiv 2024

  42. [42]

    Gauge field production in SUGRA inflation: local non-Gaussianity and primordial black holes

    A. Linde, S. Mooij and E. Pajer,Gauge field production in supergravity inflation: Local non-Gaussianity and primordial black holes,Phys. Rev. D87(2013) 103506, [1212.1693]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  43. [43]

    Domcke, V

    V. Domcke, V. Guidetti, Y. Welling and A. Westphal,Resonant backreaction in axion inflation,JCAP09(2020) 009, [2002.02952]

    work page arXiv 2020

  44. [44]

    Black holes and the multiverse

    J. Garriga, A. Vilenkin and J. Zhang,Black holes and the multiverse,JCAP02(2016) 064, [1512.01819]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  45. [45]

    H. Deng, J. Garriga and A. Vilenkin,Primordial black hole and wormhole formation by domain walls,JCAP04(2017) 050, [1612.03753]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  46. [46]

    Primordial black hole formation by vacuum bubbles

    H. Deng and A. Vilenkin,Primordial black hole formation by vacuum bubbles,JCAP12 (2017) 044, [1710.02865]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  47. [47]

    Deng,Primordial black hole formation by vacuum bubbles

    H. Deng,Primordial black hole formation by vacuum bubbles. Part II,JCAP09(2020) 023, [2006.11907]

    work page arXiv 2020

  48. [48]

    Kusenko, M

    A. Kusenko, M. Sasaki, S. Sugiyama, M. Takada, V. Takhistov and E. Vitagliano, Exploring Primordial Black Holes from the Multiverse with Optical Telescopes,Phys. Rev. Lett.125(2020) 181304, [2001.09160]

    work page arXiv 2020

  49. [49]

    D. N. Maeso, L. Marzola, M. Raidal, V. Vaskonen and H. Veerm¨ ae,Primordial black holes from spectator field bubbles,JCAP02(2022) 017, [2112.01505]

    work page arXiv 2022

  50. [50]

    Escriv` a, V

    A. Escriv` a, V. Atal and J. Garriga,Formation of trapped vacuum bubbles during inflation, and consequences for PBH scenarios,JCAP10(2023) 035, [2306.09990]

    work page arXiv 2023

  51. [51]

    J. He, H. Deng, Y.-S. Piao and J. Zhang,Implications of GWTC-3 on primordial black holes from vacuum bubbles,Phys. Rev. D109(2024) 044035, [2303.16810]

    work page arXiv 2024

  52. [52]

    Huang and Y.-S

    H.-L. Huang and Y.-S. Piao,Toward supermassive primordial black holes from inflationary bubbles,Phys. Rev. D110(2024) 023501, [2312.11982]

    work page arXiv 2024

  53. [53]

    Kitajima and F

    N. Kitajima and F. Takahashi,Primordial Black Holes from QCD Axion Bubbles,JCAP 11(2020) 060, [2006.13137]

    work page arXiv 2020

  54. [54]

    Kasai, M

    K. Kasai, M. Kawasaki, N. Kitajima, K. Murai, S. Neda and F. Takahashi,Clustering of primordial black holes from QCD axion bubbles,JCAP10(2023) 049, [2305.13023]. 112

    work page arXiv 2023

  55. [55]

    Kasai, M

    K. Kasai, M. Kawasaki, N. Kitajima, K. Murai, S. Neda and F. Takahashi,Primordial origin of supermassive black holes from axion bubbles,JCAP05(2024) 092, [2310.13333]

    work page arXiv 2024

  56. [56]

    Lunar Mass Black Holes from QCD Axion Cosmology

    T. Vachaspati,Lunar Mass Black Holes from QCD Axion Cosmology,1706.03868

    work page internal anchor Pith review Pith/arXiv arXiv

  57. [57]

    Primordial Black Holes from the QCD axion

    F. Ferrer, E. Masso, G. Panico, O. Pujolas and F. Rompineve,Primordial Black Holes from the QCD axion,Phys. Rev. Lett.122(2019) 101301, [1807.01707]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  58. [58]

    G. B. Gelmini, J. Hyman, A. Simpson and E. Vitagliano,Primordial black hole dark matter from catastrogenesis with unstable pseudo-Goldstone bosons,JCAP06(2023) 055, [2303.14107]

    work page arXiv 2023

  59. [59]

    G. B. Gelmini, A. Simpson and E. Vitagliano,Catastrogenesis: DM, GWs, and PBHs from ALP string-wall networks,JCAP02(2023) 031, [2207.07126]

    work page arXiv 2023

  60. [60]

    Gouttenoire and E

    Y. Gouttenoire and E. Vitagliano,Primordial black holes and wormholes from domain wall networks,Phys. Rev. D109(2024) 123507, [2311.07670]

    work page arXiv 2024

  61. [61]

    Gouttenoire and E

    Y. Gouttenoire and E. Vitagliano,Domain wall interpretation of the PTA signal confronting black hole overproduction,Phys. Rev. D110(2024) L061306, [2306.17841]

    work page arXiv 2024

  62. [62]

    R. Z. Ferreira, A. Notari, O. Pujol` as and F. Rompineve,Collapsing domain wall networks: impact on pulsar timing arrays and primordial black holes,JCAP06(2024) 020, [2401.14331]

    work page arXiv 2024

  63. [63]

    Gouttenoire, S

    Y. Gouttenoire, S. F. King, R. Roshan, X. Wang, G. White and M. Yamazaki, Cosmological consequences of domain walls biased by quantum gravity,Phys. Rev. D 112(2025) 075007, [2501.16414]

    work page arXiv 2025

  64. [64]

    Lu, C.-W

    B.-Q. Lu, C.-W. Chiang and T. Li,Probing primordial black hole formation from domain wall isocurvature perturbations: constraints and implications,JCAP02(2026) 006, [2409.09986]

    work page arXiv 2026

  65. [65]

    Ge,Sublunar-Mass Primordial Black Holes from Closed Axion Domain Walls,Phys

    S. Ge,Sublunar-Mass Primordial Black Holes from Closed Axion Domain Walls,Phys. Dark Univ.27(2020) 100440, [1905.12182]

    work page arXiv 2020

  66. [66]

    S. Ge, J. Guo and J. Liu,New mechanism for primordial black hole formation from the QCD axion,Phys. Rev. D109(2024) 123030, [2309.01739]

    work page arXiv 2024

  67. [67]

    D. I. Dunsky and M. Kongsore,Primordial black holes from axion domain wall collapse, JHEP06(2024) 198, [2402.03426]

    work page arXiv 2024

  68. [68]

    S. W. Hawking,Black Holes From Cosmic Strings,Phys. Lett. B231(1989) 237–239

    1989

  69. [69]

    R. R. Caldwell and P. Casper,Formation of black holes from collapsed cosmic string loops,Phys. Rev. D53(1996) 3002–3010, [gr-qc/9509012]

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  70. [70]

    A. C. Jenkins and M. Sakellariadou,Primordial black holes from cusp collapse on cosmic strings,2006.16249

    work page arXiv 2006

  71. [71]

    J. J. Blanco-Pillado, K. D. Olum and A. Vilenkin,No black holes from cosmic string cusps,2101.05040

    work page arXiv

  72. [72]

    Brandenberger, B

    R. Brandenberger, B. Cyr and H. Jiao,Intermediate mass black hole seeds from cosmic string loops,Phys. Rev. D104(2021) 123501, [2103.14057]. 113

    work page arXiv 2021

  73. [73]

    Kodama, M

    H. Kodama, M. Sasaki and K. Sato,Abundance of Primordial Holes Produced by Cosmological First Order Phase Transition,Prog. Theor. Phys.68(1982) 1979

    1982

  74. [74]

    S. D. H. Hsu,Black Holes From Extended Inflation,Phys. Lett. B251(1990) 343–348

    1990

  75. [75]

    J. Liu, L. Bian, R.-G. Cai, Z.-K. Guo and S.-J. Wang,Primordial black hole production during first-order phase transitions,Phys. Rev. D105(2022) L021303, [2106.05637]

    work page arXiv 2022

  76. [76]

    Hashino, S

    K. Hashino, S. Kanemura and T. Takahashi,Primordial black holes as a probe of strongly first-order electroweak phase transition,Phys. Lett. B833(2022) 137261, [2111.13099]

    work page arXiv 2022

  77. [77]

    Kawana, T

    K. Kawana, T. Kim and P. Lu,PBH formation from overdensities in delayed vacuum transitions,Phys. Rev. D108(2023) 103531, [2212.14037]

    work page arXiv 2023

  78. [78]

    Lewicki, P

    M. Lewicki, P. Toczek and V. Vaskonen,Primordial black holes from strong first-order phase transitions,JHEP09(2023) 092, [2305.04924]

    work page arXiv 2023

  79. [79]

    Gouttenoire and T

    Y. Gouttenoire and T. Volansky,Primordial black holes from supercooled phase transitions,Phys. Rev. D110(2024) 043514, [2305.04942]

    work page arXiv 2024

  80. [80]

    Baldes and M

    I. Baldes and M. O. Olea-Romacho,Primordial black holes as dark matter: interferometric tests of phase transition origin,JHEP01(2024) 133, [2307.11639]

    work page arXiv 2024

Showing first 80 references.