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arxiv: 2605.20186 · v1 · pith:2SJKXET4new · submitted 2026-05-19 · ✦ hep-ph · astro-ph.CO· hep-th

WIMP-like Dark Matter Without Thermalization At Freeze-Out

Dan Hooper , Gordan Krnjaic , Gabriele Montefalcone This is my paper

Pith reviewed 2026-05-20 03:56 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COhep-th
keywords dark matterhidden sectorthermal relicfreeze-outdecouplingrelic densityWIMP
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The pith

Dark matter in hidden sectors can reach the observed relic density with extremely weak Standard Model couplings by decoupling early but sharing similar temperatures at freeze-out.

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

The paper establishes that hidden-sector dark matter can produce the standard thermal relic abundance even when it decouples from the Standard Model at temperatures much higher than the dark matter mass. In these models the two sectors evolve with independent thermal histories yet end up at comparable temperatures when freeze-out occurs around T ~ m_X/20. This setup yields the usual annihilation cross section of order 10^{-26} cm³/s without requiring ongoing chemical equilibrium between sectors. A reader would care because the approach allows the inter-sector coupling to be tiny enough that direct detection and collider signals fall below foreseeable experimental reach.

Core claim

In hidden-sector models the dark matter and Standard Model sectors decouple at T ≫ m_X and subsequently evolve with separate thermal histories, yet the sectors maintain similar temperatures during freeze-out, producing the observed relic density for annihilation cross sections of order 10^{-26} cm³/s.

What carries the argument

Hidden-sector models with early decoupling at T ≫ m_X but temperature alignment at freeze-out.

If this is right

  • The coupling between the Standard Model and hidden sectors can be extremely small.
  • Direct detection and collider signals can lie far below foreseeable sensitivities.
  • The observed relic density arises from the usual thermal mechanism despite the lack of late-time thermalization.
  • Comparable annihilation cross sections emerge naturally without fine-tuning the inter-sector interaction strength.

Where Pith is reading between the lines

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

  • This framework suggests that null results in current experiments may reflect early decoupling rather than the absence of dark matter interactions.
  • Cosmological probes of early-universe entropy injection or temperature ratios could test the required alignment of sector temperatures.
  • The mechanism opens parameter space for hidden-sector particles that interact too weakly for near-term detection but still satisfy the relic-density constraint.

Load-bearing premise

The decoupled sectors naturally reach similar temperatures at freeze-out through unspecified initial conditions or entropy production.

What would settle it

Continued non-observation of dark matter signals in direct detection experiments down to cross sections orders of magnitude below 10^{-26} cm³/s while the relic density is confirmed by cosmology would support the scenario; detection of a signal at standard WIMP strength would challenge it.

Figures

Figures reproduced from arXiv: 2605.20186 by Dan Hooper, Gabriele Montefalcone, Gordan Krnjaic.

Figure 1
Figure 1. Figure 1: FIG. 1. The ratio Γ [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The cosmological evolution of a hypercharge portal [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Viable parameter space in the ( [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
read the original abstract

In the standard thermal relic scenario, dark matter remains in chemical equilibrium with the Standard Model radiation bath until freeze-out occurs at $T \sim m_X/20$, where $m_X$ is the dark matter mass. In this familiar class of models, the observed relic density is obtained for annihilation cross sections of order $\sigma v \sim 10^{-26}$ cm$^3$/s. We show that comparable cross sections can naturally be realized in hidden-sector models in which the dark matter and Standard Model sectors decouple at a very high temperature, $T \gg m_X$, and subsequently evolve with separate thermal histories. Despite this decoupling, the two sectors have similar temperatures during freeze-out, leading to the usual thermal relic abundance. As a consequence, the coupling between the Standard Model and hidden sectors can be extremely small, potentially placing direct detection and collider signals far below foreseeable sensitivities.

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

1 major / 0 minor

Summary. The manuscript proposes a hidden-sector dark matter scenario in which the dark matter and Standard Model sectors decouple at T ≫ m_X and thereafter follow independent thermal histories, yet maintain comparable temperatures at the freeze-out epoch T ∼ m_X/20. This temperature alignment is asserted to occur naturally, permitting the standard thermal relic density for annihilation cross sections σv ∼ 10^{-26} cm³/s while allowing the inter-sector coupling to be extremely small.

Significance. If the temperature alignment can be shown to arise generically from the dynamics rather than from tuned initial conditions, the result would meaningfully enlarge the viable parameter space for WIMP-like dark matter by decoupling the relic-density requirement from the strength of direct-detection and collider signals. The approach highlights the role of separate entropy and temperature evolution in multi-sector models.

major comments (1)
  1. [Abstract] The central claim that the two sectors maintain similar temperatures at freeze-out after decoupling at T ≫ m_X is presented as natural in the abstract, yet the manuscript provides neither the coupled Boltzmann equations for the two temperatures nor any scan over initial temperature ratios or reheating scenarios that would establish the alignment as generic rather than dependent on specific initial conditions. This assumption is load-bearing for the assertion that comparable cross sections are 'naturally realized.'

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive comments and the opportunity to clarify aspects of our hidden-sector dark matter scenario. We address the major comment regarding the naturalness of the temperature alignment below.

read point-by-point responses

  1. Referee: [Abstract] The central claim that the two sectors maintain similar temperatures at freeze-out after decoupling at T ≫ m_X is presented as natural in the abstract, yet the manuscript provides neither the coupled Boltzmann equations for the two temperatures nor any scan over initial temperature ratios or reheating scenarios that would establish the alignment as generic rather than dependent on specific initial conditions. This assumption is load-bearing for the assertion that comparable cross sections are 'naturally realized.'

    Authors: We agree that the manuscript would benefit from a more explicit demonstration that the temperature alignment arises generically. After decoupling, each sector conserves its own comoving entropy, so the temperature ratio evolves according to the respective effective degrees of freedom and any subsequent entropy injections. To strengthen this point, we will add the explicit coupled equations governing the temperature evolution of the two sectors and include a scan over initial temperature ratios at decoupling together with representative reheating scenarios. These additions will show that comparable temperatures at T ∼ m_X/20 are achieved across a broad range of initial conditions without fine-tuning, thereby supporting the claim that standard thermal relic densities are naturally realized for WIMP-like cross sections. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central claim is a model-construction statement with independent content.

full rationale

The paper constructs hidden-sector scenarios in which the dark matter and SM sectors decouple early but maintain comparable temperatures at freeze-out, yielding the standard thermal relic density for WIMP-like cross sections. This is presented as a possible dynamical outcome rather than a derivation that reduces to its inputs by construction. No equations redefine a fitted quantity as a prediction, no self-citation chain bears the load of a uniqueness theorem, and no ansatz is smuggled in. The relic abundance calculation follows the usual Boltzmann equation once the temperature ratio is specified by the model, without tautological reduction. The temperature alignment is asserted to arise naturally in the constructed examples, but this is a statement about model viability rather than a self-referential loop.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The proposal rests on standard cosmological assumptions for relic-density calculations and the existence of a hidden sector with its own thermal bath; no new free parameters or invented particles with independent evidence are introduced in the abstract.

axioms (2)
  • standard math Standard thermal history of the universe and Boltzmann equations govern relic density
    Invoked to obtain the usual abundance once temperatures match at freeze-out.
  • domain assumption Hidden sector maintains its own thermal bath after early decoupling
    Core modeling choice enabling separate thermal histories.

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Reference graph

Works this paper leans on

84 extracted references · 84 canonical work pages · 58 internal anchors

  1. [1]

    Secluded Evolution.First, the hidden sector undergoes internal chemical freeze-out. The hidden- to-SM temperature ratio,ξ, evolves through entropy conservation in each sector, possibly modified by a transient cannibal phase once the mediator be- comes non-relativistic [ 14], but remains of order unity throughout. Since Γ Y ≪Hduring this entire epoch, the ...

    work page

  2. [2]

    Entropy T ransfer.In the second stage, the frozen- out mediator population, redshifting as matter, comes to dominate the total energy density before decaying into SM particles. These decays inject en- tropy into the visible sector, diluting all pre-existing comoving abundances by a factor of [13, 14] Sf Si = ρY (τY )3/4 T(τY )3 ,(13) where Si,f are the SM...

    work page

  3. [3]

    A History of Dark Matter

    G. Bertone and D. Hooper, Rev. Mod. Phys.90, 045002 (2018), arXiv:1605.04909 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  4. [4]

    Dark Matter Search Results from 4.2 Tonne-Years of Exposure of the LUX-ZEPLIN (LZ) Experiment

    J. Aalbers et al. (LZ), Phys. Rev. Lett.135, 011802 (2025), arXiv:2410.17036 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  5. [5]

    Aprile et al

    E. Aprile et al. (XENON), Phys. Rev. Lett.131, 041003 (2023), arXiv:2303.14729 [hep-ex]

    work page arXiv 2023

  6. [6]

    Dark Matter Search Results from the Complete Exposure of the PICO-60 C$_3$F$_8$ Bubble Chamber

    C. Amole et al. (PICO), Phys. Rev. D100, 022001 (2019), arXiv:1902.04031 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  7. [7]

    Search for dark matter and other new phenomena in events with an energetic jet and large missing transverse momentum using the ATLAS detector

    M. Aaboud et al. (ATLAS), JHEP01, 126 (2018), arXiv:1711.03301 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  8. [8]

    A. M. Sirunyan et al. (CMS), JHEP08, 130 (2018), arXiv:1806.00843 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  9. [9]

    Aad et al

    G. Aad et al. (ATLAS), Sci. Bull.69, 3005 (2024), arXiv:2306.00641 [hep-ex]

    work page arXiv 2024

  10. [10]

    Aad et al

    G. Aad et al. (ATLAS), Phys. Rev. D103, 112006 (2021), arXiv:2102.10874 [hep-ex]

    work page arXiv 2021

  11. [11]

    Search for dark matter and large extra dimensions in monojet events in pp collisions at sqrt(s) = 7 TeV

    S. Chatrchyan et al. (CMS), JHEP09, 094 (2012), arXiv:1206.5663 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  12. [12]

    Search for new phenomena with the monojet and missing transverse momentum signature using the ATLAS detector in sqrt(s) = 7 TeV proton-proton collisions

    G. Aad et al. (ATLAS), Phys. Lett. B705, 294 (2011), arXiv:1106.5327 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  13. [13]

    Secluded WIMP Dark Matter

    M. Pospelov, A. Ritz, and M. B. Voloshin, Phys. Lett. B 662, 53 (2008), arXiv:0711.4866 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  14. [14]

    A Theory of Dark Matter

    N. Arkani-Hamed, D. P. Finkbeiner, T. R. Slatyer, and N. Weiner, Phys. Rev. D79, 015014 (2009), arXiv:0810.0713 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  15. [15]

    Thermal Dark Matter From A Highly Decoupled Sector

    A. Berlin, D. Hooper, and G. Krnjaic, Phys. Rev. D94, 095019 (2016), arXiv:1609.02555 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  16. [16]

    PeV-Scale Dark Matter as a Thermal Relic of a Decoupled Sector

    A. Berlin, D. Hooper, and G. Krnjaic, Phys. Lett. B760, 106 (2016), arXiv:1602.08490 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  17. [17]

    Higgs-field Portal into Hidden Sectors

    B. Patt and F. Wilczek, (2006), arXiv:hep-ph/0605188

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  18. [18]

    McDonald, Phys

    J. McDonald, Phys. Rev. D50, 3637 (1994), arXiv:hep- ph/0702143

    work page arXiv 1994

  19. [19]

    Asymmetric Dark Matter from Leptogenesis

    A. Falkowski, J. T. Ruderman, and T. Volansky, JHEP 05, 106 (2011), arXiv:1101.4936 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  20. [20]

    J. M. Cline, G. Dupuis, Z. Liu, and W. Xue, JHEP08, 131 (2014), arXiv:1405.7691 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  21. [21]

    Sterile Neutrino portal to Dark Matter II: Exact Dark symmetry

    M. Escudero, N. Rius, and V. Sanz, Eur. Phys. J. C77, 397 (2017), arXiv:1607.02373 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [22]

    Sterile neutrino portal to Dark Matter I: The $U(1)_{B-L}$ case

    M. Escudero, N. Rius, and V. Sanz, JHEP02, 045 (2017), arXiv:1606.01258 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  23. [23]

    Hidden Sector Dark Matter and the Galactic Center Gamma-Ray Excess: A Closer Look

    M. Escudero, S. J. Witte, and D. Hooper, JCAP11, 042 (2017), arXiv:1709.07002 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  24. [24]

    J. A. Evans, S. Gori, and J. Shelton, JHEP02, 100 (2018), arXiv:1712.03974 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  25. [25]

    J. A. Evans, C. Gaidau, and J. Shelton, JHEP01, 032 (2020), arXiv:1909.04671 [hep-ph]

    work page arXiv 2020

  26. [26]

    Hooper, R

    D. Hooper, R. K. Leane, Y.-D. Tsai, S. Wegsman, and S. J. Witte, JHEP07, 163 (2020), arXiv:1912.08821 [hep- ph]

    work page arXiv 2020

  27. [27]

    A Comprehensive Study of WIMP Models Explaining the Fermi-LAT Galactic Center Excess

    C. Kong and M. Di Mauro, Phys. Rev. D113, 043031 (2026), arXiv:2511.21808 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  28. [28]

    Koechler and M

    J. Koechler and M. Di Mauro, Phys. Rev. D112, 115016 (2025), arXiv:2508.02775 [hep-ph]

    work page arXiv 2025

  29. [29]

    Y. Hu, C. Cesarotti, and T. R. Slatyer, (2025), arXiv:2509.08043 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  30. [30]

    LHC Signals for a SuperUnified Theory of Dark Matter

    N. Arkani-Hamed and N. Weiner, JHEP12, 104 (2008), arXiv:0810.0714 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  31. [31]

    Holdom, Phys

    B. Holdom, Phys. Lett. B178, 65 (1986)

    work page 1986

  32. [32]

    Vector Dark Matter through a Radiative Higgs Portal

    A. DiFranzo, P. J. Fox, and T. M. P. Tait, JHEP04, 135 (2016), arXiv:1512.06853 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  33. [33]

    Multi-component Dark Matter through a Radiative Higgs Portal

    A. DiFranzo and G. Mohlabeng, JHEP01, 080 (2017), arXiv:1610.07606 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  34. [34]

    Virtual signatures of dark sectors in Higgs couplings

    A. Voigt and S. Westhoff, JHEP11, 009 (2017), arXiv:1708.01614 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  35. [35]

    Dittmaier, S

    S. Dittmaier, S. Schuhmacher, and M. Stahlhofen, Eur. Phys. J. C81, 826 (2021), arXiv:2102.12020 [hep-ph]

    work page arXiv 2021

  36. [36]

    Frangipane, S

    E. Frangipane, S. Gori, and B. Shakya, JHEP09, 083 (2022), arXiv:2110.10711 [hep-ph]

    work page arXiv 2022

  37. [37]

    Bertuzzo, T

    E. Bertuzzo, T. Sassi, and A. Tesi, JHEP10, 109 (2024), arXiv:2406.14437 [hep-ph]

    work page arXiv 2024

  38. [38]

    Supersymmetric Dark Matter and the Reheating Temperature of the Universe

    N. Fornengo, A. Riotto, and S. Scopel, Phys. Rev. D67, 023514 (2003), arXiv:hep-ph/0208072

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  39. [39]

    The effect of a late decaying scalar on the neutralino relic density

    G. Gelmini, P. Gondolo, A. Soldatenko, and C. E. Yaguna, Phys. Rev. D74, 083514 (2006), arXiv:hep-ph/0605016

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  40. [40]

    G. Kane, K. Sinha, and S. Watson, Int. J. Mod. Phys. D 24, 1530022 (2015), arXiv:1502.07746 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  41. [41]

    Is the CMB telling us that dark matter is weaker than weakly interacting?

    D. Hooper, Phys. Rev. D88, 083519 (2013), arXiv:1307.0826 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  42. [42]

    A. V. Patwardhan, G. M. Fuller, C. T. Kishimoto, and A. Kusenko, Phys. Rev. D92, 103509 (2015), arXiv:1507.01977 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  43. [43]

    Flooded Dark Matter and S Level Rise

    L. Randall, J. Scholtz, and J. Unwin, JHEP03, 011 (2016), arXiv:1509.08477 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  44. [44]

    Nonthermal production of dark radiation and dark matter

    M. Reece and T. Roxlo, JHEP09, 096 (2016), arXiv:1511.06768 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  45. [45]

    D. H. Lyth and E. D. Stewart, Phys. Rev. D53, 1784 (1996), arXiv:hep-ph/9510204

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  46. [46]

    Inflatable Dark Matter

    H. Davoudiasl, D. Hooper, and S. D. McDermott, Phys. Rev. Lett.116, 031303 (2016), arXiv:1507.08660 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  47. [47]

    Changes in Dark Matter Properties After Freeze-Out

    T. Cohen, D. E. Morrissey, and A. Pierce, Phys. Rev. D 78, 111701 (2008), arXiv:0808.3994 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  48. [48]

    A little inflation at the cosmological QCD phase transition

    T. Boeckel and J. Schaffner-Bielich, Phys. Rev. D85, 103506 (2012), arXiv:1105.0832 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  49. [49]

    A little inflation in the early universe at the QCD phase transition

    T. Boeckel and J. Schaffner-Bielich, Phys. Rev. Lett.105, 041301 (2010), arXiv:0906.4520 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  50. [50]

    S. E. Hong, H.-J. Lee, Y. J. Lee, E. D. Stewart, and H. Zoe, JCAP06, 002 (2015), arXiv:1503.08938 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  51. [51]

    Aprile et al

    E. Aprile et al. (XENON), Phys. Rev. Lett.135, 221003 (2025), arXiv:2502.18005 [hep-ex]

    work page arXiv 2025

  52. [52]

    Planck Collaboration, A&A641, A6 (2020), arXiv:1807.06209 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  53. [53]

    Possible Evidence For Dark Matter Annihilation In The Inner Milky Way From The Fermi Gamma Ray Space Telescope

    L. Goodenough and D. Hooper, (2009), arXiv:0910.2998 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  54. [54]

    Dark Matter Annihilation in The Galactic Center As Seen by the Fermi Gamma Ray Space Telescope

    D. Hooper and L. Goodenough, Phys. Lett. B697, 412 (2011), arXiv:1010.2752 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  55. [55]

    On The Origin Of The Gamma Rays From The Galactic Center

    D. Hooper and T. Linden, Phys. Rev. D84, 123005 (2011), arXiv:1110.0006 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  56. [56]

    K. N. Abazajian and M. Kaplinghat, Phys. Rev. D86, 083511 (2012), [Erratum: Phys.Rev.D 87, 129902 (2013)], arXiv:1207.6047 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  57. [57]

    Two Emission Mechanisms in the Fermi Bubbles: A Possible Signal of Annihilating Dark Matter

    D. Hooper and T. R. Slatyer, Phys. Dark Univ.2, 118 (2013), arXiv:1302.6589 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  58. [58]

    Dark Matter and Pulsar Model Constraints from Galactic Center Fermi-LAT Gamma Ray Observations

    C. Gordon and O. Macias, Phys. Rev. D88, 083521 7 (2013), [Erratum: Phys.Rev.D 89, 049901 (2014)], arXiv:1306.5725 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  59. [59]

    The Characterization of the Gamma-Ray Signal from the Central Milky Way: A Compelling Case for Annihilating Dark Matter

    T. Daylan, D. P. Finkbeiner, D. Hooper, T. Linden, S. K. N. Portillo, N. L. Rodd, and T. R. Slatyer, Phys. Dark Univ.12, 1 (2016), arXiv:1402.6703 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  60. [60]

    Background model systematics for the Fermi GeV excess

    F. Calore, I. Cholis, and C. Weniger, JCAP03, 038 (2015), arXiv:1409.0042 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  61. [61]

    Fermi-LAT Observations of High-Energy Gamma-Ray Emission Toward the Galactic Center

    M. Ajello et al. (Fermi-LAT), Astrophys. J.819, 44 (2016), arXiv:1511.02938 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  62. [62]

    The Fermi Galactic Center GeV Excess and Implications for Dark Matter

    M. Ackermann et al. (Fermi-LAT), Astrophys. J.840, 43 (2017), arXiv:1704.03910 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  63. [63]

    Cholis, Y.-M

    I. Cholis, Y.-M. Zhong, S. D. McDermott, and J. P. Surdutovich, Phys. Rev. D105, 103023 (2022), arXiv:2112.09706 [astro-ph.HE]

    work page arXiv 2022

  64. [64]

    Di Mauro, Phys

    M. Di Mauro, Phys. Rev. D103, 063029 (2021), arXiv:2101.04694 [astro-ph.HE]

    work page arXiv 2021

  65. [65]

    Mertig, M

    R. Mertig, M. Bohm, and A. Denner, Comput. Phys. Commun.64, 345 (1991)

    work page 1991

  66. [66]

    New Developments in FeynCalc 9.0

    V. Shtabovenko, R. Mertig, and F. Orellana, Comput. Phys. Commun.207, 432 (2016), arXiv:1601.01167 [hep- ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  67. [67]

    FeynCalc 9.3: New features and improvements

    V. Shtabovenko, R. Mertig, and F. Orellana, Comput. Phys. Commun.256, 107478 (2020), arXiv:2001.04407 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  68. [68]

    Shtabovenko, R

    V. Shtabovenko, R. Mertig, and F. Orellana, Comput. Phys. Commun.306, 109357 (2025), arXiv:2312.14089 [hep-ph]

    work page arXiv 2025

  69. [69]

    HDECAY: a Program for Higgs Boson Decays in the Standard Model and its Supersymmetric Extension

    A. Djouadi, J. Kalinowski, and M. Spira, Comput. Phys. Commun.108, 56 (1998), arXiv:hep-ph/9704448

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  70. [70]

    HDECAY: Twenty++ Years After

    A. Djouadi, J. Kalinowski, M. Muehlleitner, and M. Spira (HDECAY), Comput. Phys. Commun.238, 214 (2019), arXiv:1801.09506 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  71. [71]

    M. W. Winkler, Phys. Rev. D99, 015018 (2019), arXiv:1809.01876 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  72. [72]

    Fernandez, Y

    N. Fernandez, Y. Kahn, and J. Shelton, JHEP07, 044 (2022), arXiv:2111.13709 [hep-ph]

    work page arXiv 2022

  73. [73]

    Searching for dilepton resonances below the Z mass at the LHC

    I. Hoenig, G. Samach, and D. Tucker-Smith, Phys. Rev. D90, 075016 (2014), arXiv:1408.1075 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  74. [74]

    Alenezi, C

    A. Alenezi, C. Cesarotti, S. Gori, and J. Shelton, JHEP 03, 177 (2026), arXiv:2504.00077 [hep-ph]

    work page arXiv 2026

  75. [75]

    Revisiting Big-Bang Nucleosynthesis Constraints on Long-Lived Decaying Particles

    M. Kawasaki, K. Kohri, T. Moroi, and Y. Takaesu, Phys. Rev. D97, 023502 (2018), arXiv:1709.01211 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  76. [76]

    C. D. Carone and H. Murayama, Phys. Rev. Lett.74, 3122 (1995), arXiv:hep-ph/9411256

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  77. [77]

    Baryon and Lepton Number as Local Gauge Symmetries

    P. Fileviez Perez and M. B. Wise, Phys. Rev. D82, 011901 (2010), [Erratum: Phys.Rev.D 82, 079901 (2010)], arXiv:1002.1754 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  78. [78]

    Gauge Theory for Baryon and Lepton Numbers with Leptoquarks

    M. Duerr, P. Fileviez Perez, and M. B. Wise, Phys. Rev. Lett.110, 231801 (2013), arXiv:1304.0576 [hep-ph]. 8 Supplementary Material for WIMP-like Dark Matter Without Thermalization At Freeze-Out Dan Hooper, Gordan Krnjaic, and Gabriele Montefalcone CONTENTS I. Details of the Numerical Implementation 8 A. Boltzmann Equations 8 B. Three-Phase Solver Strateg...

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  79. [79]

    Cross Sections and Rates In this model, the thermally averaged DM annihilation cross section takes the form ⟨σv⟩X ¯X→ϕϕ=a+ 6b xX ,(S39) where the coefficients a and b represent the s-wave and p-wave contributions, respectively, and are given by a= 2 √ 1−r2λ2 sλ2 p πm2 X (r2−2)2,(S40) b= 1 12m 2 Xπ √ 1−r2 (r2−2)4 [ −2(r2−1)3λ4 p + 3(r6−8r4 + 20r2−12)λ2 sλ2...

    work page

  80. [80]

    S1, we show the analogue of Fig

    Results In the top panel of Fig. S1, we show the analogue of Fig. 3 in the main text for the case of the Higgs portal, evaluated for λs = λp = 0.05 and for λs = λp = 0.1. The qualitative picture parallels that of the hypercharge portal, with direct detection bounding the relic line from above and BBN from below, leaving a large portion of viable parameter...

    work page

Showing first 80 references.