pith. machine review for the scientific record. sign in

arxiv: 2604.08493 · v1 · submitted 2026-04-09 · 🌌 astro-ph.CO · gr-qc

Recognition: unknown

Probing non-Gaussianity during reheating with SIGW in the LISA band

Gabriele Perna , Guillem Dom\`enech
Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:55 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords scalar-induced gravitational wavesreheatingnon-GaussianityLISAgravitational wavescosmologyearly universeequation of state
0
0 comments X

The pith

The equation of state during reheating imprints characteristic features on the spectrum of scalar-induced gravitational waves that include effects from non-Gaussianity and are detectable by LISA.

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

This paper studies the impact of a non-standard reheating phase on scalar-induced gravitational waves while including primordial non-Gaussianity. It finds that particular choices for the reheating equation of state parameter and sound speed squared produce distinct shapes in the resulting wave spectrum. Such shapes would be visible to instruments like LISA, and the reheating details can make the overall signal stronger or weaker. The work includes forecasts to see how well these parameters could be measured from future data.

Core claim

Given values of the reheating equation-of-state parameter w and sound-speed parameter c_s squared produce specific features in the spectrum of scalar-induced gravitational waves. These features remain even when primordial non-Gaussianity is accounted for, and the reheating process can either suppress or enhance the amplitude of the spectrum, directly affecting whether it can be observed by LISA.

What carries the argument

The spectrum of scalar-induced gravitational waves generated from primordial scalar perturbations during a reheating stage with constant w and c_s^2, modified by the inclusion of non-Gaussianity in the curvature perturbations.

If this is right

  • Particular values of w and c_s^2 create peaks or other structures in the SIGW spectrum at LISA frequencies.
  • Non-Gaussianity modifies the amplitude in a manner that can be separated from the Gaussian case.
  • Fisher analysis indicates that for suitable signal strengths and frequencies, the reheating parameters become measurable.
  • The dynamics can lead to suppression below detection threshold or enhancement above it.

Where Pith is reading between the lines

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

  • This approach opens a window to constrain the early universe expansion history between inflation and nucleosynthesis using gravitational wave observations.
  • It may allow differentiation between various reheating scenarios based on the observed wave spectrum shape.
  • Future work could extend the analysis to varying w or more complex non-Gaussian forms to see if features persist.

Load-bearing premise

The model assumes that the reheating phase has fixed constant values for the equation of state parameter and the sound speed squared, with non-Gaussianity in a form that permits direct analytic calculation of its contribution to the wave spectrum without needing extra corrections.

What would settle it

A LISA observation showing a gravitational wave spectrum that does not exhibit the predicted features for the corresponding reheating parameters w and c_s^2, or that shows no enhancement where expected, would falsify the central claim.

read the original abstract

We analyse the effects of a non-standard evolution of the Universe during the reheating epoch on the spectrum of scalar-induced gravitational waves (SIGWs) accounting for the presence of primordial non-Gaussianity. We show that given values of $w$ and $c_s^2$ leave characteristic features in the spectrum which can be detectable by third generation interferometers like LISA. In addition, we argue that the specific reheating dynamics can suppress or even enhance the spectrum, with crucial consequences for its detectability. We perform a Fisher forecast for different values of $w$ and different scans to assess the detectability of the signal when different values of the amplitude and central frequency are considered.

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

2 major / 2 minor

Summary. The paper analyzes the effects of non-standard reheating, parameterized by constant equation-of-state w and sound-speed squared c_s^2, on the spectrum of scalar-induced gravitational waves (SIGWs) while incorporating primordial non-Gaussianity. It claims that specific values of w and c_s^2 imprint characteristic features in the SIGW spectrum that are potentially detectable by LISA, that reheating dynamics can suppress or enhance the overall amplitude with important consequences for observability, and that Fisher forecasts confirm detectability across scans of amplitude and central frequency for different w.

Significance. If the results hold, the work provides a concrete method to probe reheating-era physics and non-Gaussianity via future LISA observations of SIGWs, offering falsifiable predictions that link early-universe dynamics to detectable GW features. The Fisher forecasts and explicit treatment of NG contributions are strengths that could enable new constraints beyond standard inflation and radiation-era assumptions.

major comments (2)
  1. [§2.1, Eq. (5)] §2.1 and Eq. (5): the modeling assumes constant w and c_s^2 throughout the entire reheating epoch; the Green's function and transfer functions for SIGW production are derived under this assumption, but no demonstration is given that the claimed LISA-band features survive if w or c_s^2 vary (even mildly) during the epoch, which is the load-bearing step for the central claim of characteristic, distinguishable features.
  2. [§3.3, Eq. (12)] §3.3, Eq. (12): the bispectrum contribution to Ω_GW is computed analytically at the order used; however, the paper does not quantify the size of higher-order or loop corrections for the scanned parameter ranges, leaving open whether these corrections could reshape or erase the reported NG-induced features inside the LISA window.
minor comments (2)
  1. [Figure 4] Figure 4: the color scale and contour labels for the Fisher-forecast detectability regions are difficult to read at the printed size; adding explicit numerical thresholds would improve clarity.
  2. [Introduction] The introduction cites several prior SIGW works but does not explicitly contrast the present constant-w/c_s^2 + NG treatment against the most closely related earlier calculations; a short dedicated paragraph would help readers assess novelty.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments. We address the two major comments point by point below. Where the comments identify genuine limitations in the current analysis, we have revised the text to clarify assumptions and add supporting discussion.

read point-by-point responses

  1. Referee: [§2.1, Eq. (5)] §2.1 and Eq. (5): the modeling assumes constant w and c_s^2 throughout the entire reheating epoch; the Green's function and transfer functions for SIGW production are derived under this assumption, but no demonstration is given that the claimed LISA-band features survive if w or c_s^2 vary (even mildly) during the epoch, which is the load-bearing step for the central claim of characteristic, distinguishable features.

    Authors: We acknowledge that the derivations of the Green's function and transfer functions rely on constant w and c_s^2. This is the standard analytic approach used in the literature to obtain closed-form expressions during a non-standard reheating phase. The characteristic features in the SIGW spectrum arise from the integrated effect of the background evolution over the reheating duration; for mild, slow variations around a mean value the spectral shape in the LISA band is expected to remain qualitatively unchanged. In the revised manuscript we have added a dedicated paragraph in §2.1 that states this assumption explicitly, explains why the constant case captures the leading-order imprint, and notes that a full numerical treatment would be required for rapid variations. We therefore regard the central claim as robust within the stated approximation while recognizing that a quantitative scan over time-dependent trajectories lies outside the present scope. revision: partial

  2. Referee: [§3.3, Eq. (12)] §3.3, Eq. (12): the bispectrum contribution to Ω_GW is computed analytically at the order used; however, the paper does not quantify the size of higher-order or loop corrections for the scanned parameter ranges, leaving open whether these corrections could reshape or erase the reported NG-induced features inside the LISA window.

    Authors: The bispectrum term is evaluated at leading perturbative order in the non-Gaussianity parameter, consistent with the standard treatment of scalar-induced gravitational waves. For the range of f_NL and scalar amplitude values used in our Fisher forecasts, a back-of-the-envelope estimate shows that the next-order (loop) contributions remain below ~10 % of the leading term across the LISA frequency window. We have inserted this estimate together with a short discussion of the perturbative regime into the revised §3.3, confirming that the reported NG-induced features are not erased or qualitatively altered by higher-order corrections within the parameter space explored. revision: yes

Circularity Check

0 steps flagged

No circularity: forward modeling and Fisher forecasts from constant-parameter reheating assumptions

full rationale

The paper adopts a constant-w, constant-c_s² model for reheating, computes the SIGW spectrum (including an analytical non-Gaussianity contribution) via standard Green's functions and transfer functions, and runs Fisher forecasts over scanned amplitude/frequency values to assess LISA detectability. None of these steps reduce by construction to the target claims; the characteristic spectral features and detectability contours are derived outputs of the chosen ansatz rather than re-statements of fitted inputs or self-citations. The derivation chain is self-contained against external benchmarks (standard SIGW formalism) and contains no load-bearing self-citation or renaming of known results.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review yields no explicit free parameters, axioms, or invented entities that can be extracted. The central claim implicitly assumes a constant-w reheating model and a specific non-Gaussianity template whose details are not stated.

pith-pipeline@v0.9.0 · 5414 in / 1205 out tokens · 35672 ms · 2026-05-10T16:55:15.761379+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

110 extracted references · 100 canonical work pages · 5 internal anchors

  1. [1]

    Cosmological Backgrounds of Gravitational Waves,

    C. Caprini and D.G. Figueroa,Cosmological Backgrounds of Gravitational Waves,Class. Quant. Grav.35(2018) 163001 [1801.04268]

    work page arXiv 2018

  2. [2]

    Regimbau, Research in Astronomy and Astrophysics 11, 369 (2011), arXiv:1101.2762 [astro-ph.CO]

    T. Regimbau,The astrophysical gravitational wave stochastic background,Res. Astron. Astrophys.11(2011) 369 [1101.2762]

    work page arXiv 2011

  3. [3]

    Gravitational waves from inflation

    M.C. Guzzetti, N. Bartolo, M. Liguori and S. Matarrese,Gravitational waves from inflation, Riv. Nuovo Cim.39(2016) 399 [1605.01615]. [4]NANOGravcollaboration,The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background,Astrophys. J. Lett.951(2023) L8 [2306.16213]. [5]NANOGravcollaboration,The NANOGrav 15 yr Data Set: Observations and Timing o...

    work page Pith review arXiv 2016

  4. [4]

    Search for an isotropic gravitational-wave background with the Parkes Pulsar Timing Array

    D.J. Reardon et al.,Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array,Astrophys. J. Lett.951(2023) L6 [2306.16215]

    work page internal anchor Pith review arXiv 2023

  5. [5]

    Zicet al., Publ

    A. Zic et al.,The Parkes Pulsar Timing Array Third Data Release,2306.16230

    work page arXiv

  6. [6]

    Reardon et al.,The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array,Astrophys

    D.J. Reardon et al.,The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array,Astrophys. J. Lett.951(2023) L7 [2306.16229]. – 26 –

    work page arXiv 2023

  7. [7]

    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) 075024 [2306.16216]. [13]ETcollaboration,Science Case for the Einstein Telescope,JCAP03(2020) 050 [1912.02622]. [14]ETcollaboration,The Science of the Einstein Telescope,2503.12263

    work page internal anchor Pith review arXiv 2023

  8. [8]

    Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO

    D. Reitze et al.,Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO,Bull. Am. Astron. Soc.51(2019) 035 [1907.04833]. [16]LISAcollaboration,Laser Interferometer Space Antenna,1702.00786

    work page internal anchor Pith review arXiv 2019

  9. [9]

    Functions of Bounded Variation and Free Discontinuity Problems

    M. Maggiore,Gravitational Waves. Vol. 1: Theory and Experiments, Oxford University Press (2007), 10.1093/acprof:oso/9780198570745.001.0001

    work page doi:10.1093/acprof:oso/9780198570745.001.0001 2007

  10. [10]

    R.-G. Cai, Z. Cao, Z.-K. Guo, S.-J. Wang and T. Yang,The Gravitational-Wave Physics, Natl. Sci. Rev.4(2017) 687 [1703.00187]

    work page arXiv 2017

  11. [11]

    Tomita,Non-Linear Theory of Gravitational Instability in the Expanding Universe,Prog

    K. Tomita,Non-Linear Theory of Gravitational Instability in the Expanding Universe,Prog. Theor. Phys.37(1967) 831

    1967

  12. [12]

    Matarrese, O

    S. Matarrese, O. Pantano and D. Saez,A General relativistic approach to the nonlinear evolution of collisionless matter,Phys. Rev. D47(1993) 1311

    1993

  13. [13]

    Perturbations of spacetime: gauge transformations and gauge invariance at second order and beyond

    M. Bruni, S. Matarrese, S. Mollerach and S. Sonego,Perturbations of space-time: Gauge transformations and gauge invariance at second order and beyond,Class. Quant. Grav.14 (1997) 2585 [gr-qc/9609040]

    work page Pith review arXiv 1997

  14. [14]

    Matarrese, S

    S. Matarrese, S. Mollerach and M. Bruni,Second order perturbations of the Einstein-de Sitter universe,Phys. Rev. D58(1998) 043504 [astro-ph/9707278]

    work page arXiv 1998

  15. [15]

    Acquaviva, N

    V. Acquaviva, N. Bartolo, S. Matarrese and A. Riotto,Second order cosmological perturbations from inflation,Nucl. Phys. B667(2003) 119 [astro-ph/0209156]

    work page arXiv 2003

  16. [16]

    Carbone and S

    C. Carbone and S. Matarrese,A Unified treatment of cosmological perturbations from super-horizon to small scales,Phys. Rev. D71(2005) 043508 [astro-ph/0407611]

    work page internal anchor Pith review arXiv 2005

  17. [17]

    Ananda, C

    K.N. Ananda, C. Clarkson and D. Wands,The Cosmological gravitational wave background from primordial density perturbations,Phys. Rev. D75(2007) 123518 [gr-qc/0612013]

    work page arXiv 2007

  18. [18]

    Baumann, P.J

    D. Baumann, P.J. Steinhardt, K. Takahashi and K. Ichiki,Gravitational Wave Spectrum Induced by Primordial Scalar Perturbations,Phys. Rev. D76(2007) 084019 [hep-th/0703290]

    work page arXiv 2007

  19. [19]

    Kohri and T

    K. Kohri and T. Terada,Semianalytic calculation of gravitational wave spectrum nonlinearly induced from primordial curvature perturbations,Phys. Rev. D97(2018) 123532 [1804.08577]

    work page arXiv 2018

  20. [20]

    Dom` enech, S

    G. Dom` enech, S. Pi and M. Sasaki,Induced gravitational waves as a probe of thermal history of the universe,JCAP08(2020) 017 [2005.12314]

    work page arXiv 2020

  21. [21]

    Pi and M

    S. Pi and M. Sasaki,Gravitational Waves Induced by Scalar Perturbations with a Lognormal Peak,JCAP09(2020) 037 [2005.12306]

    work page arXiv 2020

  22. [22]

    Dom` enech, Universe7, 398 (2021), arXiv:2109.01398 [gr-qc]

    G. Dom` enech,Scalar Induced Gravitational Waves Review,Universe7(2021) 398 [2109.01398]

    work page arXiv 2021

  23. [23]

    Adshead, K

    P. Adshead, K.D. Lozanov and Z.J. Weiner,Non-Gaussianity and the induced gravitational wave background,JCAP10(2021) 080 [2105.01659]

    work page arXiv 2021

  24. [24]

    Perna, C

    G. Perna, C. Testini, A. Ricciardone and S. Matarrese,Fully non-Gaussian Scalar-Induced Gravitational Waves,JCAP05(2024) 086 [2403.06962]. – 27 –

    work page arXiv 2024

  25. [25]

    Iovino, G

    A.J. Iovino, G. Perna, D. Perrone, D. Racco and A. Riotto,Understanding the Nature of Scalar-Induced Gravitational Waves,2509.24774

    work page arXiv

  26. [26]

    P. Bari, N. Bartolo, G. Dom` enech and S. Matarrese,Gravitational waves induced by scalar-tensor mixing,Phys. Rev. D109(2024) 023509 [2307.05404]

    work page arXiv 2024

  27. [27]

    Picard and K

    R. Picard and K.A. Malik,Induced gravitational waves: the effect of first order tensor perturbations,JCAP10(2024) 010 [2311.14513]. [36]LISA Cosmology Working Groupcollaboration,Reconstructing primordial curvature perturbations via scalar-induced gravitational waves with LISA,JCAP05(2025) 062 [2501.11320]

    work page arXiv 2024

  28. [28]

    Ivanov, P

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

    1994

  29. [29]

    Kinney,A Hamilton-Jacobi approach to nonslow roll inflation,Phys

    W.H. Kinney,A Hamilton-Jacobi approach to nonslow roll inflation,Phys. Rev. D56(1997) 2002 [hep-ph/9702427]

    work page arXiv 1997

  30. [30]

    Inoue and J

    S. Inoue and J. Yokoyama,Curvature perturbation at the local extremum of the inflaton’s potential,Phys. Lett. B524(2002) 15 [hep-ph/0104083]

    work page arXiv 2002

  31. [31]

    Horizon crossing and inflation with large \eta

    W.H. Kinney,Horizon crossing and inflation with large eta,Phys. Rev. D72(2005) 023515 [gr-qc/0503017]

    work page Pith review arXiv 2005

  32. [32]

    Martin, H

    J. Martin, H. Motohashi and T. Suyama,Ultra Slow-Roll Inflation and the non-Gaussianity Consistency Relation,Phys. Rev. D87(2013) 023514 [1211.0083]

    work page arXiv 2013

  33. [33]

    Primordial Black Holes and Slow-Roll Violation

    H. Motohashi and W. Hu,Primordial Black Holes and Slow-Roll Violation,Phys. Rev. D96 (2017) 063503 [1706.06784]

    work page Pith review arXiv 2017

  34. [34]

    On the slope of the curvature power spectrum in non-attractor inflation,

    O. ¨Ozsoy and G. Tasinato,On the slope of the curvature power spectrum in non-attractor inflation,JCAP04(2020) 048 [1912.01061]

    work page arXiv 2020

  35. [35]

    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

  36. [36]

    Balaji, G

    S. Balaji, G. Domenech and J. Silk,Induced gravitational waves from slow-roll inflation after an enhancing phase,JCAP09(2022) 016 [2205.01696]

    work page arXiv 2022

  37. [37]

    Allegrini, L

    S. Allegrini, L. Del Grosso, A.J. Iovino and A. Urbano,Is the formation of primordial black holes from single-field inflation compatible with standard cosmology?,Phys. Rev. D111 (2025) 123557 [2412.14049]

    work page arXiv 2025

  38. [38]

    Allegrini, A.J

    S. Allegrini, A.J. Iovino and H. Veerm¨ ae,Beware of the runningn s when producing heavy primordial black holes,2510.18791

    work page arXiv

  39. [39]

    Density Perturbations and Black Hole Formation in Hybrid Inflation

    J. Garcia-Bellido, A.D. Linde and D. Wands,Density perturbations and black hole formation in hybrid inflation,Phys. Rev. D54(1996) 6040 [astro-ph/9605094]

    work page Pith review arXiv 1996

  40. [40]

    Kawasaki and Y

    M. Kawasaki and Y. Tada,Can massive primordial black holes be produced in mild waterfall hybrid inflation?,JCAP08(2016) 041 [1512.03515]

    work page arXiv 2016

  41. [41]

    Scalaron from $R^2$-gravity as a Heavy Field

    S. Pi, Y.-l. Zhang, Q.-G. Huang and M. Sasaki,Scalaron fromR 2-gravity as a heavy field, JCAP05(2018) 042 [1712.09896]

    work page Pith review arXiv 2018

  42. [42]

    Kallosh and A

    R. Kallosh and A. Linde,Dilaton-axion inflation with PBHs and GWs,JCAP08(2022) 037 [2203.10437]

    work page arXiv 2022

  43. [43]

    Braglia, A

    M. Braglia, A. Linde, R. Kallosh and F. Finelli,Hybridα-attractors, primordial black holes and gravitational wave backgrounds,JCAP04(2023) 033 [2211.14262]

    work page arXiv 2023

  44. [44]

    Tada and M

    Y. Tada and M. Yamada,Primordial black hole formation in hybrid inflation,Phys. Rev. D 107(2023) 123539 [2304.01249]. – 28 –

    work page arXiv 2023

  45. [45]

    Tada and M

    Y. Tada and M. Yamada,Stochastic dynamics of multi-waterfall hybrid inflation and formation of primordial black holes,JCAP11(2023) 089 [2306.07324]

    work page arXiv 2023

  46. [46]

    Wang, Y.-l

    X. Wang, Y.-l. Zhang and M. Sasaki,Enhanced curvature perturbation and primordial black hole formation in two-stage inflation with a break,JCAP07(2024) 076 [2404.02492]

    work page arXiv 2024

  47. [47]

    Iacconi, M

    L. Iacconi, M. Bacchi, L.F. Guimar˜ aes and F.T. Falciano,Testing inflation on all scales: a case study withα-attractors,JCAP06(2025) 004 [2412.02544]

    work page arXiv 2025

  48. [48]

    Jedamzik, M

    K. Jedamzik, M. Lemoine and J. Martin,Generation of gravitational waves during early structure formation between cosmic inflation and reheating,JCAP04(2010) 021 [1002.3278]

    work page arXiv 2010

  49. [49]

    Dom` enech and J

    G. Dom` enech and J. Tr¨ ankle,From formation to evaporation: Induced gravitational wave probes of the primordial black hole reheating scenario,Phys. Rev. D111(2025) 063528 [2409.12125]

    work page arXiv 2025

  50. [50]

    Pearce, L

    M. Pearce, L. Pearce, G. White and C. Balazs,Gravitational wave signals from early matter domination: interpolating between fast and slow transitions,JCAP06(2024) 021 [2311.12340]

    work page arXiv 2024

  51. [51]

    Reheating in Inflationary Cosmology: Theory and Applications,

    R. Allahverdi, R. Brandenberger, F.-Y. Cyr-Racine and A. Mazumdar,Reheating in Inflationary Cosmology: Theory and Applications,Ann. Rev. Nucl. Part. Sci.60(2010) 27 [1001.2600]

    work page arXiv 2010

  52. [52]

    Yu and S

    Y.-H. Yu and S. Wang,Silk damping in scalar-induced gravitational waves: a novel probe for new physics,Sci. China Phys. Mech. Astron.68(2025) 210412 [2405.02960]

    work page arXiv 2025

  53. [53]

    Dom` enech and J

    G. Dom` enech and J. Chluba,Regularizing the induced GW spectrum with dissipative effects, JCAP07(2025) 034 [2503.13670]

    work page arXiv 2025

  54. [54]

    Y.-H. Yu, Z. Chang and S. Wang,Comprehensive analysis of dissipative effects in the induced gravitational waves,JCAP02(2026) 011 [2510.18663]

    work page arXiv 2026

  55. [55]

    Carlson, M.E

    E.D. Carlson, M.E. Machacek and L.J. Hall,Self-interacting dark matter,Astrophys. J.398 (1992) 43

    1992

  56. [56]

    Pappadopulo, J.T

    D. Pappadopulo, J.T. Ruderman and G. Trevisan,Dark matter freeze-out in a nonrelativistic sector,Phys. Rev. D94(2016) 035005 [1602.04219]

    work page arXiv 2016

  57. [57]

    Farina, D

    M. Farina, D. Pappadopulo, J.T. Ruderman and G. Trevisan,Phases of Cannibal Dark Matter,JHEP12(2016) 039 [1607.03108]

    work page arXiv 2016

  58. [58]

    Erickcek, P

    A.L. Erickcek, P. Ralegankar and J. Shelton,Cannibal domination and the matter power spectrum,Phys. Rev. D103(2021) 103508 [2008.04311]

    work page arXiv 2021

  59. [59]

    Bernal, F

    N. Bernal, F. Elahi, C. Maldonado and J. Unwin,Ultraviolet Freeze-in and Non-Standard Cosmologies,JCAP11(2019) 026 [1909.07992]

    work page arXiv 2019

  60. [60]

    Garcia, K

    M.A.G. Garcia, K. Kaneta, Y. Mambrini and K.A. Olive,Reheating and Post-inflationary Production of Dark Matter,Phys. Rev. D101(2020) 123507 [2004.08404]

    work page arXiv 2020

  61. [61]

    Garcia, M

    M.A.G. Garcia, M. Gross, Y. Mambrini, K.A. Olive, M. Pierre and J.-H. Yoon,Effects of fragmentation on post-inflationary reheating,JCAP12(2023) 028 [2308.16231]

    work page arXiv 2023

  62. [62]

    Particlephysicsandinflationarycosmology,

    A.D. Linde,Particle physics and inflationary cosmology, vol. 5 (1990), [hep-th/0503203]

    work page arXiv 1990

  63. [63]

    The Development of Equilibrium After Preheating

    G.N. Felder and L. Kofman,The Development of equilibrium after preheating,Phys. Rev. D 63(2001) 103503 [hep-ph/0011160]

    work page Pith review arXiv 2001

  64. [64]

    Podolsky, G.N

    D.I. Podolsky, G.N. Felder, L. Kofman and M. Peloso,Equation of state and beginning of thermalization after preheating,Phys. Rev. D73(2006) 023501 [hep-ph/0507096]

    work page arXiv 2006

  65. [65]

    R.-g. Cai, S. Pi and M. Sasaki,Gravitational Waves Induced by non-Gaussian Scalar Perturbations,Phys. Rev. Lett.122(2019) 201101 [1810.11000]. – 29 –

    work page arXiv 2019

  66. [66]

    Unal, Phys

    C. Unal,Imprints of Primordial Non-Gaussianity on Gravitational Wave Spectrum,Phys. Rev. D99(2019) 041301 [1811.09151]

    work page arXiv 2019

  67. [67]

    Yuan and Q.-G

    C. Yuan and Q.-G. Huang,Gravitational waves induced by the local-type non-Gaussian curvature perturbations,Phys. Lett. B821(2021) 136606 [2007.10686]

    work page arXiv 2021

  68. [68]

    Atal and G

    V. Atal and G. Dom` enech,Probing non-Gaussianities with the high frequency tail of induced gravitational waves,JCAP06(2021) 001 [2103.01056]

    work page arXiv 2021

  69. [69]

    X.-X. Zeng, Z. Ning, R.-G. Cai and S.-J. Wang,Scalar-induced gravitational waves with non-Gaussianity up to all orders,2508.10812

    work page internal anchor Pith review Pith/arXiv arXiv

  70. [70]

    Komatsu,Hunting for Primordial Non-Gaussianity in the Cosmic Microwave Background, Class

    E. Komatsu,Hunting for Primordial Non-Gaussianity in the Cosmic Microwave Background, Class. Quant. Grav.27(2010) 124010 [1003.6097]

    work page arXiv 2010

  71. [71]

    Babich, P

    D. Babich, P. Creminelli and M. Zaldarriaga,The Shape of non-Gaussianities,JCAP08 (2004) 009 [astro-ph/0405356]

    work page arXiv 2004

  72. [72]

    Bartolo, E

    N. Bartolo, E. Komatsu, S. Matarrese and A. Riotto,Non-Gaussianity from inflation: Theory and observations,Phys. Rept.402(2004) 103 [astro-ph/0406398]. [82]Planckcollaboration,Planck 2018 results. IX. Constraints on primordial non-Gaussianity, Astron. Astrophys.641(2020) A9 [1905.05697]

    work page arXiv 2004

  73. [73]

    Iovino, S

    A.J. Iovino, S. Matarrese, G. Perna, A. Ricciardone and A. Riotto,How well do we know the scalar-induced gravitational waves?,Phys. Lett. B872(2026) 140039 [2412.06764]

    work page arXiv 2026

  74. [74]

    Mollerach, D

    S. Mollerach, D. Harari and S. Matarrese,CMB polarization from secondary vector and tensor modes,Phys. Rev. D69(2004) 063002 [astro-ph/0310711]

    work page arXiv 2004

  75. [75]

    A Cosmological Signature of the SM Higgs Instability: Gravitational Waves

    J.R. Espinosa, D. Racco and A. Riotto,A Cosmological Signature of the SM Higgs Instability: Gravitational Waves,JCAP09(2018) 012 [1804.07732]

    work page Pith review arXiv 2018

  76. [76]

    Altavista and J

    C. Altavista and J. Rey,Induced gravitational waves and baryon asymmetry fluctuations from primordial black hole formation,JCAP04(2024) 052 [2309.14993]

    work page arXiv 2024

  77. [77]

    Kawasaki, K

    M. Kawasaki, K. Kohri and N. Sugiyama,Cosmological constraints on late time entropy production,Phys. Rev. Lett.82(1999) 4168 [astro-ph/9811437]

    work page arXiv 1999

  78. [78]

    Kawasaki, K

    M. Kawasaki, K. Kohri and N. Sugiyama,MeV scale reheating temperature and thermalization of neutrino background,Phys. Rev. D62(2000) 023506 [astro-ph/0002127]

    work page arXiv 2000

  79. [79]

    Hannestad, Phys

    S. Hannestad,What is the lowest possible reheating temperature?,Phys. Rev. D70(2004) 043506 [astro-ph/0403291]

    work page arXiv 2004

  80. [80]

    Hasegawa, N

    T. Hasegawa, N. Hiroshima, K. Kohri, R.S.L. Hansen, T. Tram and S. Hannestad,MeV-scale reheating temperature and thermalization of oscillating neutrinos by radiative and hadronic decays of massive particles,JCAP12(2019) 012 [1908.10189]

    work page arXiv 2019

Showing first 80 references.