Pith. sign in

REVIEW 3 major objections 4 minor 85 references

Light PIDM in Warped Extra Dimensions

T0 review · 3 major / 4 minor · reviewed 2026-08-07 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read A warped five-dimensional construction with an extra dark brane allows light composite dark matter (1 MeV–1 TeV) to be produced by freeze-in with Planck-suppressed gravitational couplings and reheating temperatures as low as about 10 GeV.

desk verdict New warped-extra-dimension setup for light Planck-interacting DM, with a coherent freeze-in calculation, but the central coupling is scanned rather than derived. read the letter →

arxiv 2506.09135 v2 pith:IUUBMBHG submitted 2025-06-10 hep-ph astro-ph.COhep-th

Mathew T Arun , Prachiti P. Athalye , Basabendu Barman This is my paper
classification hep-phastro-ph.COhep-th
keywords lightdarkmatterPlanckianinteractingwarpedextradimensionsfreeze-inKaluza-Kleingravitonbranereheatingtemperaturecomposite
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that the usual view of Planckian interacting dark matter (PIDM)—that it must be heavy, with mass between $10^{3}$ and $10^{15}$ GeV, and require reheating temperatures near $10^{15}$ GeV—can be overturned in a warped five-dimensional universe. The construction adds a 'dark brane' between the usual ultraviolet and infrared branes and confines the dark matter on it, near the UV brane, so the dark matter's coupling to every graviton mode stays Planck suppressed. The paper then shows that annihilations of infrared-localized Standard Model fields and their Kaluza-Klein towers through KK gravitons can produce the observed relic abundance via freeze-in, for dark matter masses from 1 MeV to 1 TeV. This works with reheating temperatures as low as about 10 GeV, and the paper maps the allowed regions in the reheating-temperature/coupling plane. A variant with partially composite dark matter is also analyzed and found to overproduce dark matter unless annihilation runs near a resonance.

What carries the argument

The machine of the paper is the warped extra dimension with three branes and the Kaluza-Klein tower of the graviton. In this geometry the fifth dimension is an interval with an exponential warp factor; the zero-mode graviton has a flat profile while the massive KK gravitons are peaked near the infrared brane. The dark brane's position is chosen so that the dark-matter field localized on it has a coupling C000 around $10^{{-15}}$ $GeV^{{-1}}$ to all graviton states. The production calculation combines the KK graviton propagator sum, the $s^{3}$-scaling cross-sections for scalar, fermion, and vector dark matter, and the freeze-in Boltzmann equation, with analytic reaction-density scalings ($T^{12}$ off resonance at low temperature, $T^{8}$ at high temperature, and K_1 Bessel-function bumps at resonances) that let the yield be integrated analytically.

What would settle it

Solving the five-dimensional stabilization equations for the dark brane position would settle the model: if the brane position that yields C000 around $10^{{-15}}$ $GeV^{{-1}}$ is not a stable minimum, the claimed parameter space in the T_rh–C000 and T_rh–Λ_π planes disappears.

Watch

Extended reading notes

Core claim

The central discovery is that the location of the dark brane in a warped five-dimensional background converts the old PIDM obstruction into an advantage. Because the dark brane sits close to the UV brane, a localized composite dark-matter state avoids strong coupling to the KK gravitons; its interactions with all graviton states are of order 1/M_P. The heavy Standard Model fields needed for the fermion-mass hierarchy, however, are IR-localized, so they couple with $TeV^{{-1}}$ strength to the same KK gravitons. The graviton-mediated 2-to-2 scatterings, with cross-sections growing like $s^{3}$ and resonances at the KK masses, produce dark matter with a UV freeze-in yield that scales as m_DM times $T_rh^{7}$ (for T_rh below the KK masses) or $T_rh^{3}$ (above), allowing the relic density to be matched for light dark matter and TeV-scale reheating.

Load-bearing premise

The entire calculation rests on the assumption that a third 'dark brane' can be positioned in the warped extra dimension near the UV brane—and held there—so that dark matter's coupling to every graviton state is Planck suppressed, with no stabilization mechanism supplied.

Editorial extensions

If this is right

  • Dark matter masses from 1 MeV to 1 TeV can be produced with the observed relic abundance for reheating temperatures ranging from about 10 GeV to 10^10 GeV, removing the traditional PIDM need for near-Planck-scale reheating.
  • The same geometry preserves the geometric fermion-mass hierarchy, because light Standard Model fermions stay UV-localized while the top quark and all heavy KK modes are IR-localized and couple strongly to KK gravitons.
  • For a fixed DM-graviton coupling, heavier dark matter requires a lower reheating temperature, and dark matter cannot be heavier than the reheating temperature under the instantaneous-reheating assumption.
  • In the partially composite variant, the heavier KK excitations of dark matter freeze out early and overproduce the stable zero mode, so that scenario only works if their annihilation to Standard Model states runs near a KK graviton resonance.
  • Existing collider bounds on KK graviton masses around 3–5 TeV are compatible with the allowed parameter space shown in the paper.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the dark brane's position were derived from a stabilization potential instead of imposed by hand, the Planck-suppressed coupling C000 would become a prediction of the model, and the scanned parameter space of the paper would reduce to a narrower physical slice.
  • The instantaneous-reheating assumption fixes T_rh as the maximum temperature of the bath; a full reheating-phase treatment could alter the UV freeze-in yield in the high-temperature T^8 regime, potentially reshaping the allowed contours in Figs. 4 and 5.
  • A dedicated search for KK graviton resonances decaying to top pairs or dijets in the few-TeV window would directly test the IR-localized couplings that the freeze-in mechanism relies on, independent of the dark sector.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. This paper proposes a warped five-dimensional Randall-Sundrum setup with an additional 'dark brane' between the UV and IR branes, on which a light composite dark-matter state is localized. The dark sector interacts with the Standard Model only through the graviton and its Kaluza-Klein excitations, with an effective DM-graviton coupling taken to be Planck-suppressed. The authors compute freeze-in production of scalar, fermion, and vector DM from SM and KK initial states, derive analytic scalings for the reaction density and relic yield (Eqs. 3.11, 3.12), and present relic-density contours in the effective-coupling/reheating-temperature and Lambda_pi/reheating-temperature planes (Figs. 4, 5). They claim that the observed relic abundance can be reproduced for DM masses from 1 MeV to 1 TeV with reheating temperatures as low as TeV scale or below. A second 'partially composite' DM scenario is analyzed and found to overclose unless a resonant annihilation channel is invoked.

Significance. If the quantitative results survive scrutiny, the proposal is novel and of phenomenological interest: it would extend the PIDM framework to light DM and to much lower reheating temperatures by exploiting the warped geometry. The paper has real strengths: the analytic scaling of the reaction density in Eq. (3.11) is checked against the numerical curves in Fig. 3, the treatment covers three DM spins, and the discussion of thermalization bounds and of non-instantaneous reheating is candid. However, the central quantitative claim currently depends on an effective DM-graviton coupling that is not derived from the construction, and there are serious normalization inconsistencies in the equations behind the relic-density contours. The result is therefore promising but not yet reliably established.

major comments (3)
  1. [Sec. 2.2.1 and Eq. (3.7)] The DM-graviton coupling C000, which controls the entire freeze-in yield, is treated as an independent scanned parameter: Eq. (3.7) lists {Lambda_pi, mDM, Trh, C_phi phi G_mnq} as the independent set, and Figs. 4 and 5 scan C000 freely. But the construction in Sec. 2 does not specify the dark-brane position or the bulk mass parameter that enter the overlap integral Eq. (2.27); Table 1 quotes coupling values for 'a choice of the bulk mass parameter' without stating that choice, and no stabilization mechanism for the dark brane is discussed. Since the central claim is that the observed relic density can be obtained with TeV-scale Trh for a Planck-suppressed coupling, the paper must either derive the achievable range of C000 from the brane location and bulk profiles, or explicitly state that the allowed regions are conditional on an arbitrary tunable coupling.
  2. [Tables 1-3 and Figs. 3-4] There is a three-order-of-magnitude normalization inconsistency in the effective coupling. For Lambda_pi = 1 TeV, Table 1 gives the scalar 000-1 graviton coupling as 1.03298 x 10^-15 Lambda_pi^-1 = 1.03 x 10^-18 GeV^-1, whereas the caption of Fig. 3 and the text use C_phi phi G_000 = 10^-15 GeV^-1 as a benchmark. Because every cross-section and reaction density scales as (C000)^2, this ambiguity changes the predicted relic abundance by about six orders of magnitude. The paper should specify unambiguously whether C000 denotes the dimensionless overlap integral from Eq. (2.27) or the dimensionful physical coupling, and should make Table 1, Fig. 3, and Fig. 4 mutually consistent.
  3. [Eq. (3.5) with Eqs. (3.2)-(3.4)] The yield equation appears to have both a sign error and an incorrect coefficient. Differentiating YDM(T) = -MP integral_T^{Trh} C(T) gamma(T)/T^6 dT gives dY/dT = +MP C gamma / T^6, whereas Eq. (3.3), x H s dY/dx = gamma, together with dx/dT = -x/T, gives dY/dT = -gamma/(H s T). For T < Trh the printed integral is negative, contradicting the positive yields in Eq. (3.12) and Fig. 4. Moreover, substituting H(T) and s(T) from Eq. (3.4) yields C(T) = 135/(2 pi^3 sqrt(g*/10) g*_s), not C(T) = (2 pi^2/45) g*_s / sqrt(pi^2 g*/90). If the numerical integration behind Fig. 4 uses the printed Eq. (3.5), the relic-density contours need to be recomputed; if it uses a corrected version, that correction should be stated.
minor comments (4)
  1. [Sec. 2.1, Eq. (2.7)] The KK mass formula m_n approximately (n + (1/2) sqrt(4+a) - 3/4) pi is dimensionally unclear; the right-hand side should be multiplied by the appropriate warped scale (such as k e^{-k rc pi} or Lambda_pi) or the notation should state that the result is in units of that scale.
  2. [Sec. 3.2 and Fig. 7] The partially composite scenario is shown to overclose in Fig. 7; the text then suggests that a resonant annihilation channel could revive it, but does not demonstrate this. Since the abstract and conclusions present the scenario as one of the realizations, I recommend reformulating it as a channel that is not viable under the current assumptions, with the resonance possibility left as an outlook.
  3. [Sec. 2, cutoff Lambda/MKK = 4] The restriction to the first four KK levels is asserted rather than justified. The observation in Fig. 3 that the q=4 graviton contribution is smaller than q=2 is not a general proof of convergence for q >> 4; a comment on the convergence of the KK sum, or an estimate of the truncation error, would strengthen the analysis.
  4. [Throughout] There are several typos and small inconsistencies: 'femrion' in Sec. 2.2.2, 'Froggatt-Neilsen' in the abstract, 'is is' in Sec. 4, and the caption of Fig. 4 describing the shading order. These do not affect the physics but should be corrected in the final version.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: freeze-in abundance is computed from explicit overlap-integral couplings and then the DM-graviton coupling is scanned and constrained by the relic density; co-author self-citations are background only.

full rationale

The paper's derivation chain is: 5D warped geometry (Sec. 2) determines field profiles and overlap integrals for DM-SM-graviton couplings (Eqs. 2.27-2.29, Tables 1-3); these couplings enter the Boltzmann freeze-in equations (Sec. 3.1) and the relic abundance is obtained by integrating the reaction density (Eqs. 3.5, 3.11-3.12). The central object C000 is explicitly declared to be an independent parameter (Eq. 3.7) and Figs. 4-5 show contours where the computed abundance equals the observed value. This is a standard parameter-scan constraint, not a fitted input renamed as a prediction: the paper does not first fit C000 to the relic density and then present that same quantity as a derived result. The few citations that overlap with a co-author (refs. [12], [26], [73]) are background references for UVFI and reheating behavior; none is invoked as a uniqueness theorem or as the sole justification for the model's central premise. The admitted gaps - the dark-brane position and bulk mass parameter behind Table 1 are not specified quantitatively, and no brane stabilization mechanism is provided - are model-building incompleteness, not circularity, because the abundance calculation is a well-defined function of the stated parameters and the paper honestly reports that the partially-composite fallback overcloses (Sec. 3.2, Fig. 7). The central claim therefore has independent content and does not reduce to its inputs by construction.

Assumptions & free parameters 5 free parameters · 6 assumptions · 3 invented entities

The model's phenomenology depends on a handful of free parameters (C000, Lambda_pi, mDM, Trh) plus unstated bulk mass parameters. The key entity, the dark brane, is introduced to realize the Planck-suppressed DM coupling and is not stabilized or independently evidenced. The freeze-in calculation assumes equilibrium SM bath and instantaneous reheating, both standard but load-bearing.

free parameters (5)
  • C000 (DM-graviton coupling) = scanned over 1e-20 to 1e-9 GeV^-1 in Fig. 4
    The effective strength of the DM interaction with the zero-mode and KK gravitons. Treated as an independent parameter in Eq. (3.7) and plotted on the x-axis of the relic-density contours; the brane position is adjusted to realize it.
  • Lambda_pi (warped-down scale) = 1 TeV (benchmark choice)
    Adopted as the benchmark in the figures and used to fix KK graviton masses; chosen by hand within the allowed 3-4 TeV range discussed in Sec. 2.3.
  • mDM = scanned over 1 MeV - 1 TeV
    DM mass is an input parameter of the dark sector.
  • Trh = scanned over 10 GeV - 10^10 GeV
    Reheating temperature is a cosmological input in the freeze-in integral (Eq. 3.5).
  • Bulk mass parameters (scalar, fermion, DM localization) = not specified numerically
    Values of the bulk mass parameters determine the wavefunction overlap integrals in Tables 1-3, but the paper only states qualitative localization choices (UV/IR). The computed couplings depend on these unstated choices.
assumptions (6)
  • domain assumption Existence and stability of the Randall-Sundrum warped 5D background with three branes (UV, Dark, IR)
    The line element (2.1) and the placement of an additional dark brane are assumed; no stabilization mechanism for the dark brane is provided (Sec. 2).
  • domain assumption DM sector couples only through gravity
    The PIDM ethos, stated in the abstract and Sec. 1, fixes the DM-graviton coupling to be Planck suppressed and forbids other portals.
  • domain assumption SM particles and their KK modes are in thermal equilibrium at Trh
    Used in Sec. 3.1 for the freeze-in calculation; justified by the footnote on page 11 (KK modes have SM gauge interactions), but still an assumption about the early universe.
  • domain assumption Instantaneous reheating
    Used to identify Trh with the maximal bath temperature (Eq. 3.5); the paper discusses non-instantaneous effects qualitatively and argues they are O(1) for the T^12 scaling.
  • ad hoc to paper Cutoff at the fourth KK level: Lambda/MKK = 4
    Introduced in Sec. 2 to regulate the infinite KK tower; contributions from q>4 are argued to be subdominant (Sec. 3.1).
  • domain assumption Radion contributions can be neglected
    Justified in Sec. 2.3 by the smallness of radion couplings to UV-localized fields and the s vs s^3 scaling; still an approximation.
invented entities (3)
  • Dark brane (DB)
    purpose: A third brane in the warped bulk where the DM is localized; its position sets the DM-graviton coupling strength
    No dynamical stabilization or observational handle for an additional brane is proposed; it is a model-building input.
  • Dark brane composite DM state
    purpose: A light (1 MeV-1 TeV) scalar, fermion, or vector state localized on the dark brane, interacting only via gravity
    The DM particle is the subject of the paper and is not independently observed; its mass and spin are free inputs.
  • Dark brane partially composite DM state
    purpose: A bulk scalar whose zero mode is localized on the dark brane and whose KK partners are IR-localized
    Used in Sec. 3.2 to study the alternative production channel; shown to overclose the universe in the benchmark considered.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Light PIDM in Warped Extra Dimensions." pith.science (2026). https://pith.science/paper/IUUBMBHG

@misc{pith2026250609135,
  author       = {Pith},
  title        = {Pith review of: Light PIDM in Warped Extra Dimensions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/IUUBMBHG}},
  note         = {Machine review of arXiv:2506.09135}
}
abstract

Traditional Planckian Interacting Dark Matter (PIDM), which interacts exclusively through gravity, typically requires heavy DM candidates (with mass $10^3-10^{15}$ GeV) and very high reheating temperature ($T_{\rm rh}\gtrsim 10^{15}$ GeV). In this article, we explore a novel realization of PIDM in warped five-dimensions, consisting of an "Ultra Violet"$-$"Dark"$-$"Infra Red" (UV-DB-IR) brane setup, where the DM can be a Dark brane composite light state with mass 1 MeV $-$ 1 TeV. The DM sector is assumed to interact solely via gravity in five-dimensions. After orbifolding and performing a Kaluza-Klein (KK) decomposition, the DM is assumed to be localized onto the DB, which is positioned in the extra-dimension such that the DM interacts with both the massless graviton and its massive KK excitations, with suppressed couplings to remain consistent with the ethos of the PIDM framework. The light (heavy) Standard Model matter is assumed to be localized near UV (IR) branes for the geometric Froggatt-Nielsen mechanism, while their KK modes are localized close to the IR brane. We show that this construction allows for a viable and efficient freeze-in production mechanism for light composite PIDM, consistent with TeV-scale reheating temperature.

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

85 extracted references · 12 canonical work pages

  1. [1]

    Planck collaboration, Planck 2018 results. VI. Cosmological parameters , Astron. Astrophys. 641 (2020) A6 [ 1807.06209]

    arXiv 2020

  2. [2]

    Jungman, M

    G. Jungman, M. Kamionkowski and K. Griest, Supersymmetric dark matter , Phys. Rept. 267 (1996) 195 [ hep-ph/9506380]

    arXiv 1996

  3. [3]

    Bertone and D

    G. Bertone and D. Hooper, History of dark matter , Rev. Mod. Phys. 90 (2018) 045002 [1605.04909]

    arXiv 2018

  4. [4]

    de Swart, G

    J. de Swart, G. Bertone and J. van Dongen, How Dark Matter Came to Matter , Nature Astron. 1 (2017) 0059 [ 1703.00013]

    arXiv 2017

  5. [5]

    Roszkowski, E.M

    L. Roszkowski, E.M. Sessolo and S. Trojanowski, WIMP dark matter candidates and searches—current status and future prospects, Rept. Prog. Phys. 81 (2018) 066201 [1707.06277]

    arXiv 2018

  6. [6]

    Arcadi, M

    G. Arcadi, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini, M. Pierre et al., The waning of the WIMP? A review of models, searches, and constraints , Eur. Phys. J. C 78 (2018) 203 [1703.07364]

    arXiv 2018

  7. [7]

    Arcadi, D

    G. Arcadi, D. Cabo-Almeida, M. Dutra, P. Ghosh, M. Lindner, Y. Mambrini et al., The Waning of the WIMP: Endgame? , Eur. Phys. J. C 85 (2025) 152 [ 2403.15860]

    arXiv 2025

  8. [8]

    McDonald, Thermally generated gauge singlet scalars as selfinteracting dark matter , Phys.Rev.Lett

    J. McDonald, Thermally generated gauge singlet scalars as selfinteracting dark matter , Phys.Rev.Lett. 88 (2002) 091304 [ hep-ph/0106249]

    arXiv 2002

Show all 85 references
  1. [9]

    L.J. Hall, K. Jedamzik, J. March-Russell and S.M. West, Freeze-In Production of FIMP Dark Matter, JHEP 03 (2010) 080 [ 0911.1120]

    2010 arXiv

  2. [10]

    Bernal, M

    N. Bernal, M. Heikinheimo, T. Tenkanen, K. Tuominen and V. Vaskonen, The Dawn of FIMP Dark Matter: A Review of Models and Constraints , Int. J. Mod. Phys. A 32 (2017) 1730023 [1706.07442]

    2017 arXiv

  3. [11]

    Elahi, C

    F. Elahi, C. Kolda and J. Unwin, UltraViolet Freeze-in, JHEP 03 (2015) 048 [ 1410.6157]

    2015 arXiv

  4. [12]

    Barman, D

    B. Barman, D. Borah and R. Roshan, Effective Theory of Freeze-in Dark Matter , JCAP 11 (2020) 021 [ 2007.08768]

    2020 arXiv

  5. [13]

    Y. Ema, R. Jinno, K. Mukaida and K. Nakayama, Gravitational Effects on Inflaton Decay , JCAP 05 (2015) 038 [ 1502.02475]

    2015 arXiv

  6. [14]

    Garny, M

    M. Garny, M. Sandora and M.S. Sloth, Planckian Interacting Massive Particles as Dark Matter, Phys. Rev. Lett. 116 (2016) 101302 [ 1511.03278]

    2016 arXiv

  7. [15]

    Tang and Y.-L

    Y. Tang and Y.-L. Wu, Pure Gravitational Dark Matter, Its Mass and Signatures , Phys. Lett. B 758 (2016) 402 [ 1604.04701]

    2016 arXiv

  8. [16]

    Y. Ema, R. Jinno, K. Mukaida and K. Nakayama, Gravitational particle production in oscillating backgrounds and its cosmological implications , Phys. Rev. D 94 (2016) 063517 [1604.08898]

    2016 arXiv

  9. [17]

    Garny, A

    M. Garny, A. Palessandro, M. Sandora and M.S. Sloth, Theory and Phenomenology of Planckian Interacting Massive Particles as Dark Matter , JCAP 02 (2018) 027 [ 1709.09688]

    2018 arXiv

  10. [18]

    Tang and Y.-L

    Y. Tang and Y.-L. Wu, On Thermal Gravitational Contribution to Particle Production and Dark Matter , Phys. Lett. B 774 (2017) 676 [ 1708.05138]

    2017 arXiv

  11. [19]

    Bernal, M

    N. Bernal, M. Dutra, Y. Mambrini, K. Olive, M. Peloso and M. Pierre, Spin-2 Portal Dark Matter, Phys. Rev. D 97 (2018) 115020 [ 1803.01866]. – 24 –

    2018 arXiv

  12. [20]

    Y. Ema, K. Nakayama and Y. Tang, Production of Purely Gravitational Dark Matter , JHEP 09 (2018) 135 [ 1804.07471]

    2018 arXiv

  13. [21]

    Y. Ema, K. Nakayama and Y. Tang, Production of purely gravitational dark matter: the case of fermion and vector boson , JHEP 07 (2019) 060 [ 1903.10973]

    2019 arXiv

  14. [22]

    M. Redi, A. Tesi and H. Tillim, Gravitational Production of a Conformal Dark Sector , JHEP 05 (2021) 010 [ 2011.10565]

    2021 arXiv

  15. [23]

    Chianese, B

    M. Chianese, B. Fu and S.F. King, Impact of Higgs portal on gravity-mediated production of superheavy dark matter , JCAP 06 (2020) 019 [ 2003.07366]

    2020 arXiv

  16. [24]

    Chianese, B

    M. Chianese, B. Fu and S.F. King, Interplay between neutrino and gravity portals for FIMP dark matter , JCAP 01 (2021) 034 [ 2009.01847]

    2021 arXiv

  17. [25]

    Mambrini and K.A

    Y. Mambrini and K.A. Olive, Gravitational Production of Dark Matter during Reheating , Phys. Rev. D 103 (2021) 115009 [ 2102.06214]

    2021 arXiv

  18. [26]

    Barman and N

    B. Barman and N. Bernal, Gravitational SIMPs, JCAP 06 (2021) 011 [ 2104.10699]

    2021 arXiv

  19. [27]

    Haque and D

    M.R. Haque and D. Maity, Gravitational dark matter: Free streaming and phase space distribution, Phys. Rev. D 106 (2022) 023506 [ 2112.14668]

    2022 arXiv

  20. [28]

    Clery, Y

    S. Clery, Y. Mambrini, K.A. Olive and S. Verner, Gravitational portals in the early Universe , Phys. Rev. D 105 (2022) 075005 [ 2112.15214]

    2022 arXiv

  21. [29]

    Clery, Y

    S. Clery, Y. Mambrini, K.A. Olive, A. Shkerin and S. Verner, Gravitational portals with nonminimal couplings, Phys. Rev. D 105 (2022) 095042 [ 2203.02004]

    2022 arXiv

  22. [30]

    Ahmed, B

    A. Ahmed, B. Grzadkowski and A. Socha, Higgs boson induced reheating and ultraviolet frozen-in dark matter , JHEP 02 (2023) 196 [ 2207.11218]

    2023 arXiv

  23. [31]

    Kolb and A.J

    E.W. Kolb and A.J. Long, Cosmological gravitational particle production and its implications for cosmological relics, Rev. Mod. Phys. 96 (2024) 045005 [ 2312.09042]

    2024 arXiv

  24. [32]

    Ohanian, Gravitons as goldstone bosons , Phys

    H.C. Ohanian, Gravitons as goldstone bosons , Phys. Rev. 184 (1969) 1305

    1969

  25. [33]

    Phillips, Is the Graviton a Goldstone Boson? , Phys

    P.R. Phillips, Is the Graviton a Goldstone Boson? , Phys. Rev. 146 (1966) 966

    1966

  26. [34]

    Chkareuli, C.D

    J.L. Chkareuli, C.D. Froggatt and H.B. Nielsen, Lorentz invariance and origin of symmetries , Phys. Rev. Lett. 87 (2001) 091601 [ hep-ph/0106036]

    2001 arXiv

  27. [35]

    Berezhiani, D

    Z. Berezhiani, D. Comelli, F. Nesti and L. Pilo, Spontaneous Lorentz Breaking and Massive Gravity, Phys. Rev. Lett. 99 (2007) 131101 [ hep-th/0703264]

    2007 arXiv

  28. [36]

    Berezhiani and O.V

    Z. Berezhiani and O.V. Kancheli, Spontaneous Breaking of Lorentz-Invariance and Gravitons as Goldstone Particles , in Low dimensional physics and gauge principles , 8, 2008, DOI [0808.3181]

    2008 arXiv

  29. [37]

    Carroll, H

    S.M. Carroll, H. Tam and I.K. Wehus, Lorentz Violation in Goldstone Gravity , Phys. Rev. D 80 (2009) 025020 [ 0904.4680]

    2009 arXiv

  30. [38]

    Tomboulis, General Relativity as the effective theory of GL(4,R) spontaneous symmetry breaking, Phys

    E.T. Tomboulis, General Relativity as the effective theory of GL(4,R) spontaneous symmetry breaking, Phys. Rev. D 84 (2011) 084018 [ 1105.5848]

    2011 arXiv

  31. [39]

    H.M. Lee, M. Park and V. Sanz, Gravity-mediated (or Composite) Dark Matter , Eur. Phys. J. C 74 (2014) 2715 [ 1306.4107]

    2014 arXiv

  32. [40]

    H.M. Lee, M. Park and V. Sanz, Gravity-Mediated Dark Matter at a low reheating temperature , JHEP 05 (2025) 126 [ 2412.07850]

    2025 arXiv

  33. [41]

    Bernal, A

    N. Bernal, A. Donini, M.G. Folgado and N. Rius, Kaluza-Klein FIMP Dark Matter in Warped Extra-Dimensions, JHEP 09 (2020) 142 [ 2004.14403]

    2020 arXiv

  34. [42]

    Bernal, A

    N. Bernal, A. Donini, M.G. Folgado and N. Rius, FIMP Dark Matter in Clockwork/Linear Dilaton Extra-Dimensions, JHEP 04 (2021) 061 [ 2012.10453]. – 25 –

    2021 arXiv

  35. [43]

    Froggatt and H.B

    C.D. Froggatt and H.B. Nielsen, Hierarchy of Quark Masses, Cabibbo Angles and CP Violation, Nucl. Phys. B 147 (1979) 277

    1979

  36. [44]

    Randall and R

    L. Randall and R. Sundrum, A Large mass hierarchy from a small extra dimension , Phys. Rev. Lett. 83 (1999) 3370 [ hep-ph/9905221]

    1999 arXiv

  37. [45]

    Randall and R

    L. Randall and R. Sundrum, An Alternative to compactification , Phys. Rev. Lett. 83 (1999) 4690 [hep-th/9906064]

    1999 arXiv

  38. [46]

    Davoudiasl, J.L

    H. Davoudiasl, J.L. Hewett and T.G. Rizzo, Experimental probes of localized gravity: On and off the wall , Physical Review D 63 (2001)

    2001

  39. [47]

    Davoudiasl, J.L

    H. Davoudiasl, J.L. Hewett and T.G. Rizzo, Phenomenology of the Randall-Sundrum Gauge Hierarchy Model, Phys. Rev. Lett. 84 (2000) 2080 [ hep-ph/9909255]

    2000 arXiv

  40. [48]

    Davoudiasl, S

    H. Davoudiasl, S. Gopalakrishna, E. Ponton and J. Santiago, Warped 5-Dimensional Models: Phenomenological Status and Experimental Prospects , New J. Phys. 12 (2010) 075011 [0908.1968]

    2010 arXiv

  41. [49]

    CMS collaboration, Search for Narrow Resonances Using the Dijet Mass Spectrum in pp Collisions at √s=8 TeV, Phys. Rev. D 87 (2013) 114015 [ 1302.4794]

    2013 arXiv

  42. [50]

    S.A. Li, C.S. Li, H.T. Li and J. Gao, Constraints on Randall-Sundrum model from the events of dijet production with QCD next-to-leading order accuracy at the LHC , Phys. Rev. D 91 (2015) 014027 [1408.2762]

    2015 arXiv

  43. [51]

    G. Das, P. Mathews, V. Ravindran and S. Seth, RS resonance in di-final state production at the LHC to NLO+PS accuracy , JHEP 10 (2014) 188 [ 1408.3970]

    2014 arXiv

  44. [52]

    Agashe, A

    K. Agashe, A. Delgado, M.J. May and R. Sundrum, RS1, custodial isospin and precision tests , JHEP 08 (2003) 050 [ hep-ph/0308036]

    2003 arXiv

  45. [53]

    Agashe, R

    K. Agashe, R. Contino, L. Da Rold and A. Pomarol, A Custodial symmetry for Zb¯b, Phys. Lett. B 641 (2006) 62 [ hep-ph/0605341]

    2006 arXiv

  46. [54]

    Huber, Flavor violation and warped geometry , Nucl

    S.J. Huber, Flavor violation and warped geometry , Nucl. Phys. B 666 (2003) 269 [hep-ph/0303183]

    2003 arXiv

  47. [55]

    Agashe, G

    K. Agashe, G. Perez and A. Soni, Flavor structure of warped extra dimension models , Phys. Rev. D 71 (2005) 016002 [ hep-ph/0408134]

    2005 arXiv

  48. [56]

    Santiago, Minimal Flavor Protection: A New Flavor Paradigm in Warped Models , JHEP 12 (2008) 046 [ 0806.1230]

    J. Santiago, Minimal Flavor Protection: A New Flavor Paradigm in Warped Models , JHEP 12 (2008) 046 [ 0806.1230]

    2008 arXiv

  49. [57]

    H.M. Lee, M. Park and V. Sanz, Gravity-mediated (or Composite) Dark Matter Confronts Astrophysical Data, JHEP 05 (2014) 063 [ 1401.5301]

    2014 arXiv

  50. [58]

    Rueter, T.G

    T.D. Rueter, T.G. Rizzo and J.L. Hewett, Gravity-Mediated Dark Matter Annihilation in the Randall-Sundrum Model, JHEP 10 (2017) 094 [ 1706.07540]

    2017 arXiv

  51. [59]

    Rizzo, Kinetic mixing, dark photons and extra dimensions

    T.G. Rizzo, Kinetic mixing, dark photons and extra dimensions. Part II: fermionic dark matter, JHEP 10 (2018) 069 [ 1805.08150]

    2018 arXiv

  52. [60]

    Rizzo, Kinetic mixing, dark photons and an extra dimension

    T.G. Rizzo, Kinetic mixing, dark photons and an extra dimension. Part I , JHEP 07 (2018) 118 [1801.08525]

    2018 arXiv

  53. [61]

    Carrillo-Monteverde, Y.-J

    A. Carrillo-Monteverde, Y.-J. Kang, H.M. Lee, M. Park and V. Sanz, Dark Matter Direct Detection from new interactions in models with spin-two mediators , JHEP 06 (2018) 037 [1803.02144]

    2018 arXiv

  54. [62]

    P. Brax, S. Fichet and P. Tanedo, The Warped Dark Sector , Phys. Lett. B 798 (2019) 135012 [1906.02199]

    2019 arXiv

  55. [63]

    Folgado, A

    M.G. Folgado, A. Donini and N. Rius, Gravity-mediated Scalar Dark Matter in Warped Extra-Dimensions, 1907.04340. – 26 –

    1907 arXiv

  56. [64]

    M. Duch, B. Grzadkowski and D. Huang, Strongly self-interacting vector dark matter via freeze-in, JHEP 01 (2018) 020 [ 1710.00320]

    2018 arXiv

  57. [65]

    Particle Data Groupcollaboration, Review of Particle Physics , PTEP 2022 (2022) 083C01

    2022

  58. [66]

    Giudice, E.W

    G.F. Giudice, E.W. Kolb and A. Riotto, Largest temperature of the radiation era and its cosmological implications, Phys. Rev. D 64 (2001) 023508 [ hep-ph/0005123]

    2001 arXiv

  59. [67]

    E.W. Kolb, A. Notari and A. Riotto, On the reheating stage after inflation , Phys. Rev. D 68 (2003) 123505 [ hep-ph/0307241]

    2003 arXiv

  60. [68]

    Garcia, Y

    M.A.G. Garcia, Y. Mambrini, K.A. Olive and M. Peloso, Enhancement of the Dark Matter Abundance Before Reheating: Applications to Gravitino Dark Matter , Phys. Rev. D 96 (2017) 103510 [1709.01549]

    2017 arXiv

  61. [69]

    Bernal, F

    N. Bernal, F. Elahi, C. Maldonado and J. Unwin, Ultraviolet Freeze-in and Non-Standard Cosmologies, JCAP 11 (2019) 026 [ 1909.07992]

    2019

  62. [70]

    Garcia, K

    M.A.G. Garcia, K. Kaneta, Y. Mambrini and K.A. Olive, Reheating and Post-inflationary Production of Dark Matter , Phys. Rev. D 101 (2020) 123507 [ 2004.08404]

    2020 arXiv

  63. [71]

    R.T. Co, E. Gonzalez and K. Harigaya, Increasing Temperature toward the Completion of Reheating, JCAP 11 (2020) 038 [ 2007.04328]

    2020 arXiv

  64. [72]

    Ahmed, B

    A. Ahmed, B. Grzadkowski and A. Socha, Implications of time-dependent inflaton decay on reheating and dark matter production , Phys. Lett. B 831 (2022) 137201 [ 2111.06065]

    2022 arXiv

  65. [73]

    Barman, N

    B. Barman, N. Bernal, Y. Xu and ´O. Zapata, Ultraviolet freeze-in with a time-dependent inflaton decay, JCAP 07 (2022) 019 [ 2202.12906]

    2022 arXiv

  66. [74]

    Sarkar, Big bang nucleosynthesis and physics beyond the standard model , Rept

    S. Sarkar, Big bang nucleosynthesis and physics beyond the standard model , Rept. Prog. Phys. 59 (1996) 1493 [ hep-ph/9602260]

    1996 arXiv

  67. [75]

    Kawasaki, K

    M. Kawasaki, K. Kohri and N. Sugiyama, MeV scale reheating temperature and thermalization of neutrino background , Phys. Rev. D 62 (2000) 023506 [ astro-ph/0002127]

    2000 arXiv

  68. [76]

    Hannestad, What is the lowest possible reheating temperature? , Phys

    S. Hannestad, What is the lowest possible reheating temperature? , Phys. Rev. D 70 (2004) 043506 [astro-ph/0403291]

    2004 arXiv

  69. [77]

    De Bernardis, L

    F. De Bernardis, L. Pagano and A. Melchiorri, New constraints on the reheating temperature of the universe after WMAP-5 , Astropart. Phys. 30 (2008) 192

    2008

  70. [78]

    de Salas, M

    P. de Salas, M. Lattanzi, G. Mangano, G. Miele, S. Pastor and O. Pisanti, Bounds on very low reheating scenarios after Planck , Phys. Rev. D 92 (2015) 123534 [ 1511.00672]

    2015 arXiv

  71. [79]

    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 , JCAP 12 (2019) 012 [ 1908.10189]

    2019 arXiv

  72. [80]

    Linde, Particle physics and inflationary cosmology , vol

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

    1990 arXiv

  73. [81]

    Moroi, H

    T. Moroi, H. Murayama and M. Yamaguchi, Cosmological constraints on the light stable gravitino, Phys. Lett. B 303 (1993) 289

    1993

  74. [82]

    Asaka, K

    T. Asaka, K. Ishiwata and T. Moroi, Right-handed sneutrino as cold dark matter of the universe, Phys. Rev. D 75 (2007) 065001 [ hep-ph/0612211]

    2007 arXiv

  75. [83]

    J.L. Feng, A. Rajaraman and F. Takayama, Superweakly interacting massive particles , Phys. Rev. Lett. 91 (2003) 011302

    2003

  76. [84]

    Garny and J

    M. Garny and J. Heisig, Interplay of super-WIMP and freeze-in production of dark matter , Phys. Rev. D 98 (2018) 095031 [ 1809.10135]

    2018 arXiv

  77. [85]

    Patel, Package-X 2.0: A Mathematica package for the analytic calculation of one-loop integrals, Comput

    H.H. Patel, Package-X 2.0: A Mathematica package for the analytic calculation of one-loop integrals, Comput. Phys. Commun. 218 (2017) 66 [ 1612.00009]. – 27 –

    2017 arXiv

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.