arxiv: 2512.03959 · v2 · submitted 2025-12-03 · 🌌 astro-ph.CO · gr-qc· hep-th

Recognition: 3 theorem links

· Lean Theorem

Primary gravitational waves at high frequencies I: Origin of suppression in the power spectrum

Alipriyo Hoory , Jerome Martin , Arnab Paul , L. Sriramkumar

Authors on Pith no claims yet

Pith reviewed 2026-05-17 02:10 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-th

keywords primary gravitational wavespower spectrum regularizationadiabatic regularizationinflationary transitionshigh-frequency gravitational wavessmooth transitionssmall-scale power spectrum

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The pith

Smoothing the inflation-to-radiation transition suppresses the amplitude of high-frequency oscillations in the regularized power spectrum of primary gravitational waves.

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

The paper examines the power spectrum of primary gravitational waves at very small scales that never exit the Hubble radius during inflation. After showing that adiabatic regularization truncates the unphysical k squared rise and produces oscillations of fixed amplitude around zero mean for abrupt transitions, it introduces a linear smoothing of the effective potential. This smoothing is shown to convert the fixed-amplitude oscillations into a power-law decay in amplitude at high wave numbers. The result matters because it indicates that both regularization and smooth transitions are needed to keep real-space correlation functions of these waves well behaved.

Core claim

When the effective potential in the mode equation for primary gravitational waves is smoothed with a linear function across the transition from inflation to radiation domination, the amplitude of the oscillations (around the zero mean) in the regularized power spectrum at high frequencies is suppressed by a power law, in contrast to the constant amplitude obtained with instantaneous transitions.

What carries the argument

A linear smoothing function applied to the effective potential that governs the equation of motion for PGW modes, which controls how the regularized power spectrum behaves over scales that remain inside the Hubble radius.

If this is right

Regularization alone eliminates the k squared divergence but leaves persistent oscillations of constant amplitude.
Smoothing the transition converts those oscillations into a decaying power-law envelope at small scales.
Well-behaved real-space correlation functions require both regularization and smooth transitions when modeling epochs after inflation.
The same smoothing effect must be checked for the subsequent radiation-to-matter transition.

Where Pith is reading between the lines

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

High-frequency tails of the PGW spectrum could be further suppressed in models with gradual reheating, altering expected signals for detectors sensitive to those frequencies.
The power-law index of the suppression may depend on the precise shape and duration of the smoothing function, suggesting a family of possible decay behaviors.
Similar regularization-plus-smoothing analyses could be applied to scalar curvature perturbations to compare their high-frequency behavior with that of tensor modes.

Load-bearing premise

The effective potential for the PGW modes can be replaced by a simple linear smoothing function without breaking the validity of adiabatic regularization during the transition epochs.

What would settle it

Numerical evaluation of the regularized power spectrum using a non-linear smoothing profile or a different transition width, to check whether the oscillation amplitude still follows the predicted power-law suppression.

read the original abstract

[Abridged] The primary gravitational waves (PGWs) are generated in the early universe from the quantum vacuum during inflation. In slow roll inflation, the power spectrum (PS) of PGWs over large scales, which leave the Hubble radius during inflation, is nearly scale-invariant. However, over very small scales, which never leave the Hubble radius, the PS of PGWs behaves as k^2, where k denotes the wave number. We examine the PS of PGWs at such high wave numbers or frequencies when the PGWs are evolved post-inflation, through the epochs of radiation and matter domination. Firstly, we argue that the PS has to be regularized in order to truncate the unphysical k^2 rise at high frequencies. Assuming instantaneous transitions from inflation to the epochs of radiation and matter domination, we carry out the method of adiabatic regularization to arrive at the PS of PGWs over a wide range of frequencies. We show that the process of regularization truncates the k^2 rise and the PS of PGWs oscillates with a fixed amplitude about a vanishing mean value over small scales or, equivalently, at high frequencies. Secondly, we smooth the transition from inflation to radiation domination (to be precise, we smooth the 'effective potential' governing the equation of motion of PGWs) and examine the impact of the smoothing on the regularized PS of PGWs. With the help of a linear smoothing function, we explicitly show that the smoother transition leads to a power-law suppression in the amplitude of the oscillations (about the zero mean value) of the regularized PS of PGWs over small scales that never leave the Hubble radius during inflation. Our analysis indicates that, when transitions are involved, regularization as well as smooth transitions seem essential to ensure that the correlation functions of the PGWs in real space are well behaved. We discuss the directions in which our results need to be extended.

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.

Desk Editor's Note private letter to a colleague

Smoothing the transition with a linear function produces a power-law suppression in the high-k oscillations of the regularized PGW spectrum, but the C^0 matching raises real questions about whether adiabatic regularization still holds at those frequencies.

read the letter

The paper's central result is that a linear smoothing of the effective potential across the inflation-to-radiation transition suppresses the amplitude of oscillations in the regularized high-frequency power spectrum by a power law, unlike the fixed-amplitude oscillations seen with instantaneous transitions. This comes after they first apply adiabatic regularization to remove the unphysical k^2 rise for modes that stay inside the Hubble radius. The regularization step itself is standard and does what they claim: it truncates the growth and leaves oscillations around a zero mean. That part is clean and addresses a practical issue for keeping real-space correlation functions finite. The smoothing extension is the new piece, and they show explicitly how the width parameter controls the suppression strength. That demonstration is useful for anyone thinking about how transition details affect ultraviolet behavior in inflationary spectra. The stress-test concern about differentiability is on target. A linear smoothing function is continuous but has jumps in the first derivative at the matching points. Adiabatic regularization relies on the background varying slowly enough for the WKB subtraction to work; those derivative discontinuities can source extra high-k contributions that the subtraction may not fully remove. The abstract gives no numerical mode evolution or error estimates to check whether the suppression survives once the full equations are integrated. Without those checks, the result stays plausible but not yet solid. The paper is aimed at specialists in primordial gravitational waves and early-universe regularization methods. Readers who care about high-frequency tails for future detectors or about consistency of correlation functions will find the explicit calculation worth looking at. It is not a broad review but a focused technical point. I would send it to peer review. The method is laid out clearly enough that referees can test the smoothing assumption and ask for the missing numerical cross-checks.

Referee Report

1 major / 2 minor

Summary. The manuscript analyzes the power spectrum of primary gravitational waves (PGWs) at high frequencies for modes that never exit the Hubble radius during inflation. It first applies adiabatic regularization under instantaneous transitions to truncate the unphysical k² rise, resulting in oscillations of fixed amplitude around a zero mean. It then smooths the effective potential governing the PGW mode equation during the inflation-to-radiation transition using a linear function and shows that this produces a power-law suppression in the amplitude of those oscillations.

Significance. If the central results hold, the work clarifies the combined roles of adiabatic regularization and transition smoothing in taming high-frequency PGW spectra and ensuring well-behaved real-space correlation functions. The explicit analytic demonstration of suppression via a concrete smoothing choice is a concrete contribution, though the absence of error estimates or cross-checks against full numerical mode evolution limits immediate applicability to observational forecasts.

major comments (1)

[Smoothing of the effective potential] The linear smoothing of the effective potential (described in the abstract and the section on smoothed transitions) is only C⁰ continuous, with discontinuous first derivatives at the matching points. Adiabatic regularization relies on the background varying sufficiently slowly and smoothly; these derivative jumps can source additional non-adiabatic contributions to the mode functions at high k, potentially altering the subtracted terms and the resulting suppression. A quantitative estimate of the size of any contamination or an explicit check that the regularization procedure remains valid across the smoothed interval is required.

minor comments (2)

Include error estimates or direct comparisons against numerical integration of the mode equations to quantify the accuracy of the regularized spectrum and the suppression result.
Specify the exact functional form of the linear smoothing function, the value(s) chosen for the smoothing width parameter, and the range of k over which the power-law suppression is observed.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of our manuscript and for the constructive comment on the smoothness of the effective potential. We address this point in detail below and indicate the revisions we intend to incorporate.

read point-by-point responses

Referee: The linear smoothing of the effective potential (described in the abstract and the section on smoothed transitions) is only C⁰ continuous, with discontinuous first derivatives at the matching points. Adiabatic regularization relies on the background varying sufficiently slowly and smoothly; these derivative jumps can source additional non-adiabatic contributions to the mode functions at high k, potentially altering the subtracted terms and the resulting suppression. A quantitative estimate of the size of any contamination or an explicit check that the regularization procedure remains valid across the smoothed interval is required.

Authors: We thank the referee for highlighting this important technical point. The linear smoothing function we adopted is indeed only C⁰ continuous, with discontinuous first derivatives at the endpoints of the smoothing interval. This choice was made to permit an explicit analytic calculation demonstrating the power-law suppression of the high-frequency oscillations. We agree that, in principle, the derivative discontinuities could generate additional non-adiabatic contributions at sufficiently high k and that a quantitative assessment is desirable. In the revised manuscript we will add a dedicated subsection that (i) compares the present C⁰ results with those obtained using a C¹ smoothing function of comparable width and (ii) provides a numerical check of the mode functions across the smoothed interval to confirm that the adiabatic subtraction remains valid for the k-range of interest. These additions will include order-of-magnitude estimates of any residual contamination to the subtracted terms. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained

full rationale

The paper derives the power-law suppression in the oscillation amplitude of the regularized PGW power spectrum by applying standard adiabatic regularization to the mode equation after inserting an externally chosen linear smoothing function into the effective potential. This is an explicit calculation from the differential equation rather than a redefinition, a fit renamed as a prediction, or a result justified solely by self-citation. The regularization procedure and smoothing ansatz are introduced as standard tools with stated assumptions; the suppression emerges from solving the smoothed system and is not presupposed by the inputs. No load-bearing step reduces to its own definition or to prior work by the same authors.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the applicability of adiabatic regularization to the PGW mode equation across cosmic transitions and on the validity of a linear smoothing of the effective potential; no new free parameters or invented entities are introduced beyond the choice of smoothing function.

free parameters (1)

linear smoothing width parameter
The width of the linear smoothing function applied to the effective potential is chosen by hand to model a gradual transition.

axioms (2)

domain assumption Adiabatic regularization removes the ultraviolet divergence in the power spectrum while preserving the physical content of the mode functions.
Invoked to truncate the k^2 rise at high frequencies.
domain assumption The effective potential in the PGW equation of motion can be smoothed without altering the underlying quantum field theory framework.
Used when replacing instantaneous transitions with a linear smoothing function.

pith-pipeline@v0.9.0 · 5666 in / 1257 out tokens · 27430 ms · 2026-05-17T02:10:02.645147+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

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IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel echoes

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echoes
ECHOES: this paper passage has the same mathematical shape or conceptual pattern as the Recognition theorem, but is not a direct formal dependency.

With the help of a linear smoothing function, we explicitly show that the smoother transition leads to a power-law suppression in the amplitude of the oscillations ... of the regularized PS of PGWs over small scales
IndisputableMonolith/Foundation/AlphaCoordinateFixation.lean alpha_pin_under_high_calibration unclear

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unclear
Relation between the paper passage and the cited Recognition theorem.

we smooth the 'effective potential' governing the equation of motion of PGWs

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

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Inflationary magnetic fields induce curvature perturbations that form ultralight PBHs, generating a stochastic GW background with model-specific features.

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Works this paper leans on

88 extracted references · 88 canonical work pages · cited by 1 Pith paper · 38 internal anchors

[1]

V. F. Mukhanov, H. A. Feldman, and R. H. Brandenberger,Theory of cosmological perturbations. Part 1. Classical perturbations. Part 2. Quantum theory of perturbations. Part

work page
[2]

Rept.215(1992) 203–333

Extensions,Phys. Rept.215(1992) 203–333

work page 1992
[3]

Inflation and Precision Cosmology

J. Martin,Inflation and precision cosmology,Braz. J. Phys.34(2004) 1307–1321, [astro-ph/0312492]

work page internal anchor Pith review Pith/arXiv arXiv 2004
[4]

Inflationary Cosmological Perturbations of Quantum-Mechanical Origin

J. Martin,Inflationary cosmological perturbations of quantum-mechanical origin,Lect. Notes Phys.669(2005) 199–244, [hep-th/0406011]

work page internal anchor Pith review Pith/arXiv arXiv 2005
[5]

B. A. Bassett, S. Tsujikawa, and D. Wands,Inflation dynamics and reheating,Rev. Mod. Phys.78(May, 2006) 537–589

work page 2006
[6]

Sriramkumar,An introduction to inflation and cosmological perturbation theory,Curr

L. Sriramkumar,An introduction to inflation and cosmological perturbation theory,Curr. Sci. 97(2009) 868, [arXiv:0904.4584]

work page arXiv 2009
[7]

Cosmological Inflation: Theory and Observations

D. Baumann and H. V. Peiris,Cosmological Inflation: Theory and Observations,Adv. Sci. Lett.2(2009) 105–120, [arXiv:0810.3022]

work page internal anchor Pith review Pith/arXiv arXiv 2009
[8]

TASI Lectures on Inflation

D. Baumann,Inflation, inTheoretical Advanced Study Institute in Elementary Particle Physics: Physics of the Large and the Small, 7, 2009.arXiv:0907.5424

work page internal anchor Pith review Pith/arXiv arXiv 2009
[9]

Sriramkumar,On the generation and evolution of perturbations during inflation and reheating, pp

L. Sriramkumar,On the generation and evolution of perturbations during inflation and reheating, pp. 207–249. 2012. – 49 – 10−6 10−1 104 109 1014 1019 f Hz 10−34 10−30 10−26 10−22 10−18 10−14 10−10 hc(f ) LISA BBO CE ET DECIGO L VK SKA TianQin PTA ARCADE ADMX SQMS IAXO HET+SPD BA W GB JURA IAXO OSQAR CAST Figure 10. The sensitivity curves for the dimension...

work page 2012
[10]

Inflationary Cosmology after Planck 2013

A. Linde,Inflationary Cosmology after Planck 2013, in100e Ecole d’Ete de Physique: Post-Planck Cosmology, 2, 2014.arXiv:1402.0526

work page internal anchor Pith review Pith/arXiv arXiv 2013
[11]

The Observational Status of Cosmic Inflation after Planck

J. Martin,The Observational Status of Cosmic Inflation after Planck,Astrophys. Space Sci. Proc.45(2016) 41–134, [arXiv:1502.05733]. [11]PlanckCollaboration, P. A. R. Ade et al.,Planck 2015 results. XX. Constraints on inflation, Astron. Astrophys.594(2016) A20, [arXiv:1502.02114]. [12]PlanckCollaboration, Y. Akrami et al.,Planck 2018 results. X. Constraint...

work page internal anchor Pith review Pith/arXiv arXiv 2016
[12]

L. P. Grishchuk,Amplification of gravitational waves in an istropic universe,Zh. Eksp. Teor. – 50 – Fiz.67(1974) 825–838

work page 1974
[13]

A. A. Starobinsky,Spectrum of relict gravitational radiation and the early state of the universe,JETP Lett.30(1979) 682–685

work page 1979
[14]

M. C. Guzzetti, N. Bartolo, M. Liguori, and S. Matarrese,Gravitational waves from inflation, Riv. Nuovo Cim.39(2016), no. 9 399–495, [arXiv:1605.01615]

work page internal anchor Pith review Pith/arXiv arXiv 2016
[15]

Cosmological Backgrounds of Gravitational Waves

C. Caprini and D. G. Figueroa,Cosmological Backgrounds of Gravitational Waves,Class. Quant. Grav.35(2018), no. 16 163001, [arXiv:1801.04268]

work page internal anchor Pith review Pith/arXiv arXiv 2018
[16]

Scalar induced gravitational waves review

G. Dom` enech,Scalar Induced Gravitational Waves Review,Universe7(2021), no. 11 398, [arXiv:2109.01398]

work page internal anchor Pith review arXiv 2021
[17]

Roshan and G

R. Roshan and G. White,Using gravitational waves to see the first second of the Universe, Rev. Mod. Phys.97(2025), no. 1 015001, [arXiv:2401.04388]

work page arXiv 2025
[18]

Giovannini,Gravitational wave astronomy and the expansion history of the Universe, arXiv:2412.13968

M. Giovannini,Gravitational wave astronomy and the expansion history of the Universe, arXiv:2412.13968

work page arXiv
[19]

Bernal and F

N. Bernal and F. Hajkarim,Primordial Gravitational Waves in Nonstandard Cosmologies, Phys. Rev. D100(2019), no. 6 063502, [arXiv:1905.10410]

work page arXiv 2019
[20]

Bernal, A

N. Bernal, A. Ghoshal, F. Hajkarim, and G. Lambiase,Primordial Gravitational Wave Signals in Modified Cosmologies,JCAP11(2020) 051, [arXiv:2008.04959]

work page arXiv 2020
[21]

M. R. Haque, D. Maity, T. Paul, and L. Sriramkumar,Decoding the phases of early and late time reheating through imprints on primordial gravitational waves,Phys. Rev. D104(2021), no. 6 063513, [arXiv:2105.09242]

work page arXiv 2021
[22]

The Quest for B Modes from Inflationary Gravitational Waves

M. Kamionkowski and E. D. Kovetz,The Quest for B Modes from Inflationary Gravitational Waves,Ann. Rev. Astron. Astrophys.54(2016) 227–269, [arXiv:1510.06042]. [28]PlanckCollaboration, P. A. R. Ade et al.,Planck intermediate results. XLI. A map of lensing-induced B-modes,Astron. Astrophys.596(2016) A102, [arXiv:1512.02882]

work page internal anchor Pith review Pith/arXiv arXiv 2016
[23]

Namikawa et al.,Simons Observatory: Constraining inflationary gravitational waves with multitracer B-mode delensing,Phys

T. Namikawa et al.,Simons Observatory: Constraining inflationary gravitational waves with multitracer B-mode delensing,Phys. Rev. D105(2022), no. 2 023511, [arXiv:2110.09730]

work page arXiv 2022
[24]

Paoletti, F

D. Paoletti, F. Finelli, J. Valiviita, and M. Hazumi,Planck and BICEP/Keck Array 2018 constraints on primordial gravitational waves and perspectives for future B-mode polarization measurements,Phys. Rev. D106(2022), no. 8 083528, [arXiv:2208.10482]. [31]BICEP, KeckCollaboration, P. A. R. Ade et al.,Improved Constraints on Primordial Gravitational Waves us...

work page arXiv 2018
[25]

Zic et al.,The Parkes Pulsar Timing Array third data release,Publ

A. Zic et al.,The Parkes Pulsar Timing Array third data release,Publ. Astron. Soc. Austral. 40(2023) e049, [arXiv:2306.16230]

work page arXiv 2023
[26]

D. J. Reardon et al.,Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array,Astrophys. J. Lett.951(2023), no. 1 L6, [arXiv:2306.16215]

work page internal anchor Pith review Pith/arXiv arXiv 2023
[27]

Searching for the nano-Hertz stochastic gravitational wave background with the Chinese Pulsar Timing Array Data Release I

H. Xu et al.,Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I,Res. Astron. Astrophys.23(2023), no. 7 075024, [arXiv:2306.16216]

work page internal anchor Pith review Pith/arXiv arXiv 2023
[28]

Yokoyama,Implication of pulsar timing array experiments on cosmological gravitational wave detection,AAPPS Bull.31(2021), no

J. Yokoyama,Implication of pulsar timing array experiments on cosmological gravitational wave detection,AAPPS Bull.31(2021), no. 1 17, [arXiv:2105.07629]

work page arXiv 2021
[29]

Gravitational wave astronomy with the SKA

G. Janssen et al.,Gravitational wave astronomy with the SKA,PoSAASKA14(2015) 037, [arXiv:1501.00127]

work page internal anchor Pith review Pith/arXiv arXiv 2015
[30]

Science with the space-based interferometer LISA. IV: Probing inflation with gravitational waves

N. Bartolo et al.,Science with the space-based interferometer LISA. IV: Probing inflation with gravitational waves,JCAP12(2016) 026, [arXiv:1610.06481]. [51]LISA Cosmology Working GroupCollaboration, P. Auclair et al.,Cosmology with the Laser Interferometer Space Antenna,Living Rev. Rel.26(2023), no. 1 5, [arXiv:2204.05434]

work page internal anchor Pith review Pith/arXiv arXiv 2016
[31]

Hu and Y.-L

W.-R. Hu and Y.-L. Wu,The Taiji Program in Space for gravitational wave physics and the nature of gravity,Natl. Sci. Rev.4(2017), no. 5 685–686. [53]TianQinCollaboration, J. Mei et al.,The TianQin project: current progress on science and technology,PTEP2021(2021), no. 5 05A107, [arXiv:2008.10332]. – 52 –

work page arXiv 2017
[32]

Y. Gong, J. Luo, and B. Wang,Concepts and status of Chinese space gravitational wave detection projects,Nature Astron.5(2021), no. 9 881–889, [arXiv:2109.07442]

work page arXiv 2021
[33]

Beyond LISA: Exploring Future Gravitational Wave Missions

J. Crowder and N. J. Cornish,Beyond LISA: Exploring future gravitational wave missions, Phys. Rev.D72(2005) 083005, [gr-qc/0506015]

work page internal anchor Pith review Pith/arXiv arXiv 2005
[34]

Detecting the Cosmic Gravitational Wave Background with the Big Bang Observer

V. Corbin and N. J. Cornish,Detecting the cosmic gravitational wave background with the big bang observer,Class. Quant. Grav.23(2006) 2435–2446, [gr-qc/0512039]

work page internal anchor Pith review Pith/arXiv arXiv 2006
[35]

G. M. Harry, P. Fritschel, D. A. Shaddock, W. Folkner, and E. S. Phinney,Laser interferometry for the big bang observer,Class. Quant. Grav.23(2006) 4887–4894. [Erratum: Class.Quant.Grav. 23, 7361 (2006)]

work page 2006
[36]

Space Based Gravitational Wave Astronomy Beyond LISA

J. Baker et al.,Space Based Gravitational Wave Astronomy Beyond LISA,Bull. Am. Astron. Soc.51(2019), no. 7 243, [arXiv:1907.11305]. [59]DECIGO working groupCollaboration, S. Kawamura,Primordial gravitational wave and DECIGO,PoSKMI2019(2019) 019

work page internal anchor Pith review Pith/arXiv arXiv 2019
[37]

Current status of space gravitational wave antenna DECIGO and B-DECIGO

S. Kawamura et al.,Current status of space gravitational wave antenna DECIGO and B-DECIGO,PTEP2021(2021), no. 5 05A105, [arXiv:2006.13545]. [61]MAGIS-100Collaboration, J. Coleman,Matter-wave Atomic Gradiometer InterferometricSensor (MAGIS-100) at Fermilab,PoSICHEP2018(2019) 021, [arXiv:1812.00482]

work page internal anchor Pith review arXiv 2021
[38]

A Horizon Study for Cosmic Explorer: Science, Observatories, and Community

M. Evans et al.,A Horizon Study for Cosmic Explorer: Science, Observatories, and Community,arXiv:2109.09882

work page internal anchor Pith review Pith/arXiv arXiv
[39]

Evans et al.,Cosmic Explorer: A Submission to the NSF MPSAC ngGW Subcommittee, arXiv:2306.13745

M. Evans et al.,Cosmic Explorer: A Submission to the NSF MPSAC ngGW Subcommittee, arXiv:2306.13745

work page arXiv
[40]

Scientific Objectives of Einstein Telescope

B. Sathyaprakash et al.,Scientific Objectives of Einstein Telescope,Class. Quant. Grav.29 (2012) 124013, [arXiv:1206.0331]. [Erratum: Class.Quant.Grav. 30, 079501 (2013)]

work page internal anchor Pith review Pith/arXiv arXiv 2012
[41]

Branchesi et al.,Science with the Einstein Telescope: a comparison of different designs, JCAP07(2023) 068, [arXiv:2303.15923]

M. Branchesi et al.,Science with the Einstein Telescope: a comparison of different designs, JCAP07(2023) 068, [arXiv:2303.15923]

work page arXiv 2023
[42]

The Science of the Einstein Telescope

A. Abac et al.,The Science of the Einstein Telescope,arXiv:2503.12263

work page internal anchor Pith review Pith/arXiv arXiv
[43]

Observation of Rayleigh phonon scattering through excitation of extremely high overtones in low-loss cryogenic acoustic cavities for hybrid quantum systems

M. Goryachev, D. L. Creedon, S. Galliou, and M. E. Tobar,Observation of Rayleigh phonon scattering through excitation of extremely high overtones in low-loss cryogenic acoustic cavities for hybrid quantum systems,Phys. Rev. Lett.111(2013) 085502, [arXiv:1309.4830]

work page internal anchor Pith review Pith/arXiv arXiv 2013
[44]

Extremely Low Loss Phonon-Trapping Cryogenic Acoustic Cavities for Future Physical Experiments

S. Galliou, M. Goryachev, R. Bourquin, P. Abb´ e, J. P. Aubry, and M. E. Tobar,Extremely Low Loss Phonon-Trapping Cryogenic Acoustic Cavities for Future Physical Experiments,Sci. Rep.3(2013) 2132, [arXiv:1309.4832]

work page internal anchor Pith review Pith/arXiv arXiv 2013
[45]

D. J. Fixsen et al.,ARCADE 2 Measurement of the Extra-Galactic Sky Temperature at 3-90 GHz,Astrophys. J.734(2011) 5, [arXiv:0901.0555]. [70]OSQARCollaboration, R. Ballou et al.,New exclusion limits on scalar and pseudoscalar axionlike particles from light shining through a wall,Phys. Rev. D92(2015), no. 9 092002, [arXiv:1506.08082]. [71]CASTCollaboration,...

work page internal anchor Pith review Pith/arXiv arXiv 2011
[46]

M.-l. Tong, Y. Zhang, and F.-Y. Li,Using polarized maser to detect high-frequency relic gravitational waves,Phys. Rev. D78(2008) 024041, [arXiv:0807.0885]

work page internal anchor Pith review Pith/arXiv arXiv 2008
[47]

Domcke, C

V. Domcke, C. Garcia-Cely, and N. L. Rodd,Novel Search for High-Frequency Gravitational Waves with Low-Mass Axion Haloscopes,Phys. Rev. Lett.129(2022), no. 4 041101, [arXiv:2202.00695]. – 53 –

work page arXiv 2022
[48]

Bringmann, V

T. Bringmann, V. Domcke, E. Fuchs, and J. Kopp,High-frequency gravitational wave detection via optical frequency modulation,Phys. Rev. D108(2023), no. 6 L061303, [arXiv:2304.10579]

work page arXiv 2023
[49]

Y. Kahn, J. Sch¨ utte-Engel, and T. Trickle,Searching for high-frequency gravitational waves with phonons,Phys. Rev. D109(2024), no. 9 096023, [arXiv:2311.17147]

work page arXiv 2024
[50]

Kanno, J

S. Kanno, J. Soda, and A. Taniguchi,Search for high-frequency gravitational waves with Rydberg atoms,Eur. Phys. J. C85(2025), no. 1 31, [arXiv:2311.03890]. [77]ADMXCollaboration, C. Bartram et al.,Search for Invisible Axion Dark Matter in the 3.3–4.2µeV Mass Range,Phys. Rev. Lett.127(2021), no. 26 261803, [arXiv:2110.06096]

work page arXiv 2025
[51]

Berlin, D

A. Berlin, D. Blas, R. Tito D’Agnolo, S. A. R. Ellis, R. Harnik, Y. Kahn, and J. Sch¨ utte-Engel,Detecting high-frequency gravitational waves with microwave cavities,Phys. Rev. D105(2022), no. 11 116011, [arXiv:2112.11465]

work page arXiv 2022
[52]

Ringwald, J

A. Ringwald, J. Sch¨ utte-Engel, and C. Tamarit,Gravitational Waves as a Big Bang Thermometer,JCAP03(2021) 054, [arXiv:2011.04731]

work page arXiv 2021
[53]

Electromagnetic response of a Gaussian beam to high-frequency relic gravitational waves in quintessential inflationary models

F.-Y. Li, M.-X. Tang, and D.-P. Shi,Electromagnetic response of a Gaussian beam to high frequency relic gravitational waves in quintessential inflationary models,Phys. Rev. D67 (2003) 104008, [gr-qc/0306092]

work page internal anchor Pith review Pith/arXiv arXiv 2003
[54]

Beacham et al.,Physics Beyond Colliders at CERN: Beyond the Standard Model Working Group Report,J

J. Beacham et al.,Physics Beyond Colliders at CERN: Beyond the Standard Model Working Group Report,J. Phys. G47(2020), no. 1 010501, [arXiv:1901.09966]

work page arXiv 2020
[55]

Ruz et al.,Next Generation Search for Axion and ALP Dark Matter with the International Axion Observatory, in2018 IEEE Nuclear Science Symposium and Medical Imaging Conference, p

J. Ruz et al.,Next Generation Search for Axion and ALP Dark Matter with the International Axion Observatory, in2018 IEEE Nuclear Science Symposium and Medical Imaging Conference, p. 8824640, 2018

work page 2018
[56]

D.-G. Wang, Y. Zhang, and J.-W. Chen,Vacuum and gravitons of relic gravitational waves and the regularization of the spectrum and energy-momentum tensor,Phys. Rev. D94(2016), no. 4 044033, [arXiv:1512.03134]

work page internal anchor Pith review Pith/arXiv arXiv 2016
[57]

Amplitude of Perturbations from Inflation

L. Parker,Amplitude of Perturbations from Inflation,hep-th/0702216

work page internal anchor Pith review Pith/arXiv arXiv
[58]

The Power Spectrum in de Sitter Inflation, Revisited

I. Agullo, J. Navarro-Salas, G. J. Olmo, and L. Parker,Reexamination of the Power Spectrum in De Sitter Inflation,Phys. Rev. Lett.101(2008) 171301, [arXiv:0806.0034]

work page internal anchor Pith review Pith/arXiv arXiv 2008
[59]

Revising the predictions of inflation for the cosmic microwave background anisotropies

I. Agullo, J. Navarro-Salas, G. J. Olmo, and L. Parker,Revising the predictions of inflation for the cosmic microwave background anisotropies,Phys. Rev. Lett.103(2009) 061301, [arXiv:0901.0439]

work page internal anchor Pith review Pith/arXiv arXiv 2009
[60]

Revising the observable consequences of slow-roll inflation

I. Agullo, J. Navarro-Salas, G. J. Olmo, and L. Parker,Revising the observable consequences of slow-roll inflation,Phys. Rev. D81(2010) 043514, [arXiv:0911.0961]

work page internal anchor Pith review Pith/arXiv arXiv 2010
[61]

Urakawa and A

Y. Urakawa and A. A. Starobinsky,Adiabatic regularization of primordial perturbations generated during inflation, in19th Workshop on General Relativity and Gravitation in Japan, 2009

work page 2009
[62]

Spacetime correlators of perturbations in slow-roll de Sitter inflation

A. del Rio and J. Navarro-Salas,Spacetime correlators of perturbations in slow-roll de Sitter inflation,Phys. Rev. D89(2014), no. 8 084037, [arXiv:1401.6912]

work page internal anchor Pith review Pith/arXiv arXiv 2014
[63]

Pla and B

S. Pla and B. A. Stefanek,Renormalization of the primordial inflationary power spectra, Phys. Lett. B856(2024) 138926, [arXiv:2402.14910]

work page arXiv 2024
[64]

The Impact of Ultraviolet Regularization on the Spectrum of Curvature Perturbations During Inflation

F. Finelli, G. Marozzi, G. P. Vacca, and G. Venturi,The Impact of ultraviolet regularization on the spectrum of curvature perturbations during inflation,Phys. Rev. D76(2007) 103528, [arXiv:0707.1416]

work page internal anchor Pith review Pith/arXiv arXiv 2007
[65]

Precision calculations of the gravitational wave background spectrum from inflation

S. Kuroyanagi, T. Chiba, and N. Sugiyama,Precision calculations of the gravitational wave background spectrum from inflation,Phys. Rev. D79(2009) 103501, [arXiv:0804.3249]. – 54 –

work page internal anchor Pith review Pith/arXiv arXiv 2009
[66]

Ringwald and C

A. Ringwald and C. Tamarit,Revealing the cosmic history with gravitational waves,Phys. Rev. D106(2022), no. 6 063027, [arXiv:2203.00621]

work page arXiv 2022
[67]

A. Ito, J. Soda, and M. Yamaguchi,Analytic formula for the dynamics around inflation end and implications on primordial gravitational waves,JCAP03(2021) 033, [arXiv:2009.03611]

work page arXiv 2021
[68]

S. Pi, M. Sasaki, A. Wang, and J. Wang,Revisiting the ultraviolet tail of the primordial gravitational wave,Phys. Rev. D110(2024), no. 10 103529, [arXiv:2407.06066]

work page arXiv 2024
[69]

Weinberg,Cosmology

S. Weinberg,Cosmology. 2008

work page 2008
[70]

Gravitational Wave Experiments and Early Universe Cosmology

M. Maggiore,Gravitational wave experiments and early universe cosmology,Phys. Rept.331 (2000) 283–367, [gr-qc/9909001]

work page internal anchor Pith review Pith/arXiv arXiv 2000
[71]

Maggiore,Gravitational Waves

M. Maggiore,Gravitational Waves. Vol. 1: Theory and Experiments. Oxford University Press, 2007

work page 2007
[72]

I. S. Gradshteyn and I. M. Ryzhik,Table of integrals, series, and products. Elsevier/Academic Press, Amsterdam, seventh ed., 2007. Translated from the Russian, Translation edited and with a preface by Alan Jeffrey and Daniel Zwillinger, With one CD-ROM (Windows, Macintosh and UNIX)

work page 2007
[73]

T. S. Bunch and P. C. W. Davies,Quantum Field Theory in de Sitter Space: Renormalization by Point Splitting,Proc. Roy. Soc. Lond. A360(1978) 117–134. [101]PlanckCollaboration, N. Aghanim et al.,Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641(2020) A6, [arXiv:1807.06209]. [Erratum: Astron.Astrophys. 652, C4 (2021)]

work page internal anchor Pith review Pith/arXiv arXiv 1978
[74]

C. J. Moore, R. H. Cole, and C. P. L. Berry,Gravitational-wave sensitivity curves,Class. Quant. Grav.32(2015), no. 1 015014, [arXiv:1408.0740]

work page internal anchor Pith review Pith/arXiv arXiv 2015
[75]

Franciolini, A

G. Franciolini, A. Maharana, and F. Muia,Hunt for light primordial black hole dark matter with ultrahigh-frequency gravitational waves,Phys. Rev. D106(2022), no. 10 103520, [arXiv:2205.02153]

work page arXiv 2022
[76]

Weinberg,The Quantum theory of fields

S. Weinberg,The Quantum theory of fields. Vol. 1: Foundations. Cambridge University Press, 6, 2005

work page 2005
[77]

Weinberg,The quantum theory of fields

S. Weinberg,The quantum theory of fields. Vol. 2: Modern applications. Cambridge University Press, 8, 2013

work page 2013
[78]

N. D. Birrell and P. C. W. Davies,Quantum Fields in Curved Space. Cambridge Monographs on Mathematical Physics. Cambridge University Press, Cambridge, UK, 1982

work page 1982
[79]

L. E. Parker and D. Toms,Quantum Field Theory in Curved Spacetime: Quantized Field and Gravity. Cambridge Monographs on Mathematical Physics. Cambridge University Press, 8, 2009

work page 2009
[80]

S. A. Fulling and L. Parker,Renormalization in the theory of a quantized scalar field interacting with a robertson-walker spacetime,Annals Phys.87(1974) 176–204

work page 1974

Showing first 80 references.