pith. sign in

arxiv: 2606.03487 · v1 · pith:TCSV67NUnew · submitted 2026-06-02 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

Probing Inelastic Dark Matter via Cosmic-Ray Upscattering in NGC 1068

Eung Jin Chun , Sanjoy Mandal , Abhishek Roy This is my paper

Pith reviewed 2026-06-28 09:29 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords inelastic dark mattercosmic raysactive galactic nucleiNGC 1068dark matter spikesdeep inelastic scatteringsub-GeV dark mattervector portal
0
0 comments X

The pith

Cosmic-ray cooling in NGC 1068 constrains sub-GeV inelastic dark matter.

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

The paper models how cosmic-ray protons in the active galactic nucleus NGC 1068 lose energy through scatterings with sub-GeV inelastic dark matter particles concentrated in a dense spike around the central black hole. It calculates the energy-loss rate in a minimal vector-portal model, incorporating both elastic scattering and deep inelastic scattering, and finds that the inelastic channel dominates at high momentum transfer. The analysis requires that this dark-matter-induced cooling remain compatible with the observed standard-model cooling timescale. A reader would care because the resulting limits reach dark-matter masses and interaction strengths that lie beyond the sensitivity of existing direct-detection experiments. The approach therefore supplies an independent astrophysical probe of light inelastic dark matter.

Core claim

In a minimal vector-portal inelastic dark matter framework, the cosmic-ray energy-loss rate from scatterings with dark matter in NGC 1068 includes dominant deep inelastic scattering contributions at high momentum transfer. Requiring compatibility with observed standard model cooling yields constraints that probe previously unexplored regions of sub-GeV inelastic dark matter parameter space inaccessible to direct-detection experiments.

What carries the argument

The cosmic-ray energy-loss rate due to elastic and deep inelastic scatterings with inelastic dark matter in dense dark matter spikes around the supermassive black hole.

Load-bearing premise

A dense dark matter spike exists around the supermassive black hole in NGC 1068 and the cosmic-ray flux and spectrum are known accurately enough to isolate any extra cooling from dark matter.

What would settle it

A measurement of the cosmic-ray spectrum or cooling timescale in NGC 1068 showing no excess cooling beyond standard-model processes would falsify the derived constraints.

Figures

Figures reproduced from arXiv: 2606.03487 by Abhishek Roy, Eung Jin Chun, Sanjoy Mandal.

Figure 1
Figure 1. Figure 1: FIG. 1: Ratio of DIS to elastic scattering (ES) energy loss rate [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Cooling timescales from CR protons scattering with DM, in terms of proton energy [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Sensitivity on mass splitting [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Comparison of elastic scattering (ES) with dipole form factor, ES with general form factors and deep [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: Left panel: DM distribution in NGC 1068, for different values of spike index [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
read the original abstract

We study constraints on sub-GeV inelastic dark matter (iDM) from cosmic-ray (CR) cooling in the active galactic nucleus (AGN) NGC 1068. In dense dark matter (DM) spikes surrounding supermassive black holes, high-energy CR protons can efficiently lose energy through scatterings with dark matter particles. We consider a minimal vector-portal iDM framework and consistently include both elastic and deep inelastic scattering (DIS) contributions to the CR energy-loss rate. We find that DIS processes dominate at high momentum transfer and substantially enhance the DM-induced cooling effect. By requiring the resulting cooling timescale to remain compatible with the observed Standard Model cooling in NGC 1068, we derive constraints on the iDM parameter space. Our results demonstrate that AGN cosmic-ray cooling probes previously unexplored regions of sub-GeV iDM parameter space inaccessible to current direct-detection experiments.

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 manuscript claims that cosmic-ray protons in NGC 1068 can lose energy via elastic and deep-inelastic scattering with sub-GeV inelastic dark matter in a dense DM spike around the central supermassive black hole; requiring that the resulting DM-induced cooling timescale remain compatible with the observed Standard Model cooling yields new constraints on the iDM mass and vector-portal coupling that reach parameter space inaccessible to direct-detection experiments.

Significance. If the central modeling assumptions hold, the result would be significant because it introduces AGN cosmic-ray cooling as a probe of light inelastic DM, with the consistent inclusion of DIS processes providing a concrete enhancement to the cooling rate at high momentum transfer. The approach is complementary to terrestrial searches and rests on independently observed SM cooling rather than a circular fit to the same data.

major comments (2)
  1. [DM spike modeling (near Eq. for energy-loss rate)] The central claim requires a steep DM density spike (typically ho ho r^{-7/3} from adiabatic contraction) whose existence is not directly observed and depends on assumptions about the initial halo profile, absence of major mergers, and negligible dynamical heating. No section quantifies how the derived limits degrade if the local DM density is reduced by even a factor of a few; this is load-bearing because the cooling rate scales linearly with ho_DM.
  2. [Cosmic-ray flux and spectrum section] The CR proton spectrum and normalization near the black hole are taken from propagation models rather than local data. The manuscript does not show the effect on the final bounds if this normalization is lowered by an order of magnitude, which would make the DM cooling timescale exceed the observed SM cooling time and erase the constraints.
minor comments (2)
  1. Notation for the inelastic splitting u and the vector-portal coupling should be defined explicitly at first use to avoid ambiguity with standard model parameters.
  2. [Abstract] The abstract states that DIS 'substantially enhance[s] the DM-induced cooling effect,' but a quantitative comparison (e.g., ratio of DIS to elastic loss rates at representative energies) would strengthen the presentation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments on our manuscript. We address each major point below and will revise the manuscript to incorporate sensitivity analyses where the comments identify gaps in the current presentation.

read point-by-point responses

  1. Referee: [DM spike modeling (near Eq. for energy-loss rate)] The central claim requires a steep DM density spike (typically ρ ∝ r^{-7/3} from adiabatic contraction) whose existence is not directly observed and depends on assumptions about the initial halo profile, absence of major mergers, and negligible dynamical heating. No section quantifies how the derived limits degrade if the local DM density is reduced by even a factor of a few; this is load-bearing because the cooling rate scales linearly with ρ_DM.

    Authors: We agree that the DM spike profile is a modeling assumption whose normalization is not directly observed and that the energy-loss rate scales linearly with ρ_DM. The ρ ∝ r^{-7/3} form follows from standard adiabatic contraction calculations in the literature, but we acknowledge the dependence on initial conditions and merger history. In the revised manuscript we will add an explicit discussion of this scaling, including a figure or table showing how the derived bounds on the vector coupling weaken for DM densities reduced by factors of 3 and 10 relative to the fiducial spike. This will make the load-bearing nature of the assumption transparent to readers. revision: yes

  2. Referee: [Cosmic-ray flux and spectrum section] The CR proton spectrum and normalization near the black hole are taken from propagation models rather than local data. The manuscript does not show the effect on the final bounds if this normalization is lowered by an order of magnitude, which would make the DM cooling timescale exceed the observed SM cooling time and erase the constraints.

    Authors: The CR spectrum is taken from published propagation models for NGC 1068 that are calibrated to multi-wavelength observations. We agree that an explicit sensitivity study to the overall normalization is warranted. In the revision we will add a paragraph and accompanying plot demonstrating the impact of lowering the CR flux normalization by a factor of 10; this will show that the DM-induced cooling time then exceeds the observed SM cooling time and the constraints are lost, as the referee notes. We will also state the minimum CR normalization required for any constraint to remain. revision: yes

Circularity Check

0 steps flagged

Derivation self-contained; no circular steps identified

full rationale

The paper derives constraints on sub-GeV iDM by modeling a DM spike and CR flux in NGC 1068, computing the additional energy-loss rate from elastic and DIS scattering, and requiring the resulting cooling timescale to remain compatible with independently observed SM cooling. This comparison uses external observational benchmarks rather than fitting parameters to the same dataset or redefining quantities by construction. No self-citations are load-bearing for the central result, and no equations reduce the predicted cooling to an input fit or ansatz smuggled via prior work. The derivation stands on modeled inputs tested against separate data.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Based solely on the abstract, the central claim rests on the existence of a dense DM spike, the accuracy of the vector-portal scattering model, and the ability to separate DM-induced cooling from Standard Model processes; no specific numerical free parameters are stated.

free parameters (1)
  • iDM mass and portal coupling
    The final constraints are placed on these quantities, but the abstract does not report any fitted numerical values.
axioms (2)
  • domain assumption Dense DM spike surrounds the supermassive black hole in NGC 1068
    Invoked to produce efficient CR-DM scattering rates.
  • domain assumption Vector-portal framework correctly describes iDM interactions
    Used to compute both elastic and DIS contributions.

pith-pipeline@v0.9.1-grok · 5686 in / 1233 out tokens · 33336 ms · 2026-06-28T09:29:02.726171+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

97 extracted references · 41 linked inside Pith

  1. [1]

    Particle dark matter: Evidence, candidates and constraints,

    G. Bertone, D. Hooper, and J. Silk, “Particle dark matter: Evidence, candidates and constraints,”Phys. Rept.405 (2005) 279–390,arXiv:hep-ph/0404175

    Pith/arXiv arXiv 2005

  2. [2]

    Dark Matter,

    M. Cirelli, A. Strumia, and J. Zupan, “Dark Matter,”arXiv:2406.01705 [hep-ph]

    Pith/arXiv arXiv

  3. [3]

    Nonbaryonic dark matter: Observational evidence and detection methods,

    L. Bergstr¨ om, “Nonbaryonic dark matter: Observational evidence and detection methods,”Rept. Prog. Phys.63(2000) 793,arXiv:hep-ph/0002126

    Pith/arXiv arXiv 2000

  4. [4]

    Cosmological Lower Bound on Heavy Neutrino Masses,

    B. W. Lee and S. Weinberg, “Cosmological Lower Bound on Heavy Neutrino Masses,”Phys. Rev. Lett.39(1977) 165–168

    1977

  5. [5]

    Supersymmetric dark matter,

    G. Jungman, M. Kamionkowski, and K. Griest, “Supersymmetric dark matter,”Phys. Rept.267(1996) 195–373, arXiv:hep-ph/9506380

    Pith/arXiv arXiv 1996

  6. [6]

    First Direct Detection Limits on sub-GeV Dark Matter from XENON10,

    R. Essig, A. Manalaysay, J. Mardon, P. Sorensen, and T. Volansky, “First Direct Detection Limits on sub-GeV Dark Matter from XENON10,”Phys. Rev. Lett.109(2012) 021301,arXiv:1206.2644 [astro-ph.CO]. [7]XENON1TCollaboration, E. Aprile, “The XENON1T Dark Matter Search Experiment,”Springer Proc. Phys.148 (2013) 93–96,arXiv:1206.6288 [astro-ph.IM]. [8]PandaX-I...

    Pith/arXiv arXiv 2012

  7. [7]

    Directly detecting sub-GeV dark matter with electrons from nuclear scattering,

    M. J. Dolan, F. Kahlhoefer, and C. McCabe, “Directly detecting sub-GeV dark matter with electrons from nuclear scattering,”Phys. Rev. Lett.121no. 10, (2018) 101801,arXiv:1711.09906 [hep-ph]

    Pith/arXiv arXiv 2018

  8. [8]

    Observing the Migdal effect from nuclear recoils of neutral particles with liquid xenon and argon detectors,

    N. F. Bell, J. B. Dent, R. F. Lang, J. L. Newstead, and A. C. Ritter, “Observing the Migdal effect from nuclear recoils of neutral particles with liquid xenon and argon detectors,”Phys. Rev. D105no. 9, (2022) 096015,arXiv:2112.08514 [hep-ph]

    arXiv 2022

  9. [9]

    Maximizing Direct Detection with Highly Interactive Particle Relic Dark Matter,

    G. Elor, R. McGehee, and A. Pierce, “Maximizing Direct Detection with Highly Interactive Particle Relic Dark Matter,”Phys. Rev. Lett.130no. 3, (2023) 031803,arXiv:2112.03920 [hep-ph]. [12]DAMIC-MCollaboration, I. Arnquistet al., “First Constraints from DAMIC-M on Sub-GeV Dark-Matter Particles Interacting with Electrons,”Phys. Rev. Lett.130no. 17, (2023) 1...

    arXiv 2023

  10. [10]

    Did IceCube discover dark matter around blazars?,

    A. G. De Marchi, A. Granelli, J. Nava, and F. Sala, “Did IceCube discover dark matter around blazars?,”Phys. Rev. D 112no. 4, (2025) 043042,arXiv:2412.07861 [astro-ph.HE]

    arXiv 2025

  11. [11]

    Extragalactic dark matter and direct detection experiments,

    A. N. Baushev, “Extragalactic dark matter and direct detection experiments,”Astrophys. J.771(2013) 117, arXiv:1208.0392 [astro-ph.CO]

    Pith/arXiv arXiv 2013

  12. [12]

    The highest-speed local dark matter particles come from the Large Magellanic Cloud,

    G. Besla, A. Peter, and N. Garavito-Camargo, “The highest-speed local dark matter particles come from the Large Magellanic Cloud,”JCAP11(2019) 013,arXiv:1909.04140 [astro-ph.GA]

    arXiv 2019

  13. [13]

    Direct detection of non-galactic light dark matter,

    G. Herrera and A. Ibarra, “Direct detection of non-galactic light dark matter,”Phys. Lett. B820(2021) 136551, arXiv:2104.04445 [hep-ph]

    arXiv 2021

  14. [14]

    Enhanced prospects for direct detection of inelastic dark matter from a non-galactic diffuse component,

    G. Herrera, A. Ibarra, and S. Shirai, “Enhanced prospects for direct detection of inelastic dark matter from a non-galactic diffuse component,”JCAP04(2023) 026,arXiv:2301.00870 [hep-ph]

    arXiv 2023

  15. [15]

    The impact of the Large Magellanic Cloud on dark matter direct detection signals,

    A. Smith-Orliket al., “The impact of the Large Magellanic Cloud on dark matter direct detection signals,”JCAP10 (2023) 070,arXiv:2302.04281 [astro-ph.GA]

    arXiv 2023

  16. [16]

    Novel direct detection constraints on light dark matter,

    T. Bringmann and M. Pospelov, “Novel direct detection constraints on light dark matter,”Phys. Rev. Lett.122no. 17, (2019) 171801,arXiv:1810.10543 [hep-ph]. 11

    Pith/arXiv arXiv 2019

  17. [17]

    Light Dark Matter at Neutrino Experiments,

    Y. Ema, F. Sala, and R. Sato, “Light Dark Matter at Neutrino Experiments,”Phys. Rev. Lett.122no. 18, (2019) 181802,arXiv:1811.00520 [hep-ph]

    Pith/arXiv arXiv 2019

  18. [18]

    Detecting Light Dark Matter via Inelastic Cosmic Ray Collisions,

    J. Alvey, M. Campos, M. Fairbairn, and T. You, “Detecting Light Dark Matter via Inelastic Cosmic Ray Collisions,” Phys. Rev. Lett.123(2019) 261802,arXiv:1905.05776 [hep-ph]

    arXiv 2019

  19. [19]

    Direct Detection Constraints on Blazar-Boosted Dark Matter,

    J.-W. Wang, A. Granelli, and P. Ullio, “Direct Detection Constraints on Blazar-Boosted Dark Matter,”Phys. Rev. Lett. 128no. 22, (2022) 221104,arXiv:2111.13644 [astro-ph.HE]

    arXiv 2022

  20. [20]

    (In)direct Detection of Boosted Dark Matter,

    K. Agashe, Y. Cui, L. Necib, and J. Thaler, “(In)direct Detection of Boosted Dark Matter,”JCAP10(2014) 062, arXiv:1405.7370 [hep-ph]

    Pith/arXiv arXiv 2014

  21. [21]

    Dark Matter “Collider

    D. Kim, J.-C. Park, and S. Shin, “Dark Matter “Collider” from Inelastic Boosted Dark Matter,”Phys. Rev. Lett.119 no. 16, (2017) 161801,arXiv:1612.06867 [hep-ph]

    Pith/arXiv arXiv 2017

  22. [22]

    Boosted dark matter from diffuse supernova neutrinos,

    A. Das and M. Sen, “Boosted dark matter from diffuse supernova neutrinos,”Phys. Rev. D104no. 7, (2021) 075029, arXiv:2104.00027 [hep-ph]

    arXiv 2021

  23. [23]

    Dark matter from Monogem,

    C. V. Cappiello, N. P. A. Kozar, and A. C. Vincent, “Dark matter from Monogem,”Phys. Rev. D107no. 3, (2023) 035003,arXiv:2210.09448 [hep-ph]

    arXiv 2023

  24. [24]

    Hadrophilic light dark matter from the atmosphere,

    C. A. Arg¨ uelles, V. Mu˜ noz, I. M. Shoemaker, and V. Takhistov, “Hadrophilic light dark matter from the atmosphere,” Phys. Lett. B833(2022) 137363,arXiv:2203.12630 [hep-ph]

    arXiv 2022

  25. [25]

    Searching for Afterglow: Light Dark Matter Boosted by Supernova Neutrinos,

    Y.-H. Lin, W.-H. Wu, M.-R. Wu, and H. T.-K. Wong, “Searching for Afterglow: Light Dark Matter Boosted by Supernova Neutrinos,”Phys. Rev. Lett.130no. 11, (2023) 111002,arXiv:2206.06864 [hep-ph]

    arXiv 2023

  26. [26]

    Mechanism for Thermal Relic Dark Matter of Strongly Interacting Massive Particles,

    Y. Hochberg, E. Kuflik, T. Volansky, and J. G. Wacker, “Mechanism for Thermal Relic Dark Matter of Strongly Interacting Massive Particles,”Phys. Rev. Lett.113(2014) 171301,arXiv:1402.5143 [hep-ph]

    Pith/arXiv arXiv 2014

  27. [27]

    New pathways to the relic abundance of vector-portal dark matter,

    P. J. Fitzpatrick, H. Liu, T. R. Slatyer, and Y.-D. Tsai, “New pathways to the relic abundance of vector-portal dark matter,”Phys. Rev. D106no. 8, (2022) 083517,arXiv:2011.01240 [hep-ph]

    arXiv 2022

  28. [28]

    Scalar and fermion two-component SIMP dark matter with an accidentalZ 4 symmetry,

    S.-Y. Ho, P. Ko, and C.-T. Lu, “Scalar and fermion two-component SIMP dark matter with an accidentalZ 4 symmetry,”JHEP03(2022) 005,arXiv:2201.06856 [hep-ph]

    arXiv 2022

  29. [29]

    Phenomenology of light fermionic asymmetric dark matter,

    B. Bhattacherjee, S. Matsumoto, S. Mukhopadhyay, and M. M. Nojiri, “Phenomenology of light fermionic asymmetric dark matter,”JHEP10(2013) 032,arXiv:1306.5878 [hep-ph]

    Pith/arXiv arXiv 2013

  30. [30]

    Analyzing the Discovery Potential for Light Dark Matter,

    E. Izaguirre, G. Krnjaic, P. Schuster, and N. Toro, “Analyzing the Discovery Potential for Light Dark Matter,”Phys. Rev. Lett.115no. 25, (2015) 251301,arXiv:1505.00011 [hep-ph]

    Pith/arXiv arXiv 2015

  31. [31]

    An asymmetric SIMP dark matter model,

    S.-Y. Ho, “An asymmetric SIMP dark matter model,”JHEP10(2022) 182,arXiv:2207.13373 [hep-ph]

    arXiv 2022

  32. [32]

    Dark matter freeze-in with a heavy mediator: beyond the EFT approach,

    E. Frangipane, S. Gori, and B. Shakya, “Dark matter freeze-in with a heavy mediator: beyond the EFT approach,” JHEP09(2022) 083,arXiv:2110.10711 [hep-ph]

    arXiv 2022

  33. [33]

    Freezing-in hadrophilic dark matter at low reheating temperatures,

    P. N. Bhattiprolu, G. Elor, R. McGehee, and A. Pierce, “Freezing-in hadrophilic dark matter at low reheating temperatures,”JHEP01(2023) 128,arXiv:2210.15653 [hep-ph]

    arXiv 2023

  34. [34]

    Inelastic dark matter,

    D. Tucker-Smith and N. Weiner, “Inelastic dark matter,”Phys. Rev. D64(2001) 043502,arXiv:hep-ph/0101138

    Pith/arXiv arXiv 2001

  35. [35]

    The Status of inelastic dark matter,

    D. Tucker-Smith and N. Weiner, “The Status of inelastic dark matter,”Phys. Rev. D72(2005) 063509, arXiv:hep-ph/0402065

    Pith/arXiv arXiv 2005

  36. [36]

    Inelastic Dark Matter in Light of DAMA/LIBRA,

    S. Chang, G. D. Kribs, D. Tucker-Smith, and N. Weiner, “Inelastic Dark Matter in Light of DAMA/LIBRA,”Phys. Rev. D79(2009) 043513,arXiv:0807.2250 [hep-ph]

    Pith/arXiv arXiv 2009

  37. [37]

    Final model independent result of DAMA/LIBRA-phase1,

    R. Bernabeiet al., “Final model independent result of DAMA/LIBRA-phase1,”Eur. Phys. J. C73(2013) 2648, arXiv:1308.5109 [astro-ph.GA]

    Pith/arXiv arXiv 2013

  38. [38]

    Signatures of Pseudo-Dirac Dark Matter at High-Intensity Neutrino Experiments,

    J. R. Jordan, Y. Kahn, G. Krnjaic, M. Moschella, and J. Spitz, “Signatures of Pseudo-Dirac Dark Matter at High-Intensity Neutrino Experiments,”Phys. Rev. D98no. 7, (2018) 075020,arXiv:1806.05185 [hep-ph]

    Pith/arXiv arXiv 2018

  39. [39]

    Dark Sectors at the Fermilab SeaQuest Experiment,

    A. Berlin, S. Gori, P. Schuster, and N. Toro, “Dark Sectors at the Fermilab SeaQuest Experiment,”Phys. Rev. D98 no. 3, (2018) 035011,arXiv:1804.00661 [hep-ph]

    Pith/arXiv arXiv 2018

  40. [40]

    Inelastic dark matter at the Fermilab Short Baseline Neutrino Program,

    B. Batell, J. Berger, L. Darm´ e, and C. Frugiuele, “Inelastic dark matter at the Fermilab Short Baseline Neutrino Program,”Phys. Rev. D104no. 7, (2021) 075026,arXiv:2106.04584 [hep-ph]

    arXiv 2021

  41. [41]

    Constraining light thermal inelastic dark matter with NA64,

    M. Mongillo, A. Abdullahi, B. B. Oberhauser, P. Crivelli, M. Hostert, D. Massaro, L. M. Bueno, and S. Pascoli, “Constraining light thermal inelastic dark matter with NA64,”Eur. Phys. J. C83no. 5, (2023) 391,arXiv:2302.05414 [hep-ph]

    arXiv 2023

  42. [42]

    Discovering Inelastic Thermal-Relic Dark Matter at Colliders,

    E. Izaguirre, G. Krnjaic, and B. Shuve, “Discovering Inelastic Thermal-Relic Dark Matter at Colliders,”Phys. Rev. D 93no. 6, (2016) 063523,arXiv:1508.03050 [hep-ph]. 12

    Pith/arXiv arXiv 2016

  43. [43]

    Dark Matter attempts for CoGeNT and DAMA,

    T. Schwetz and J. Zupan, “Dark Matter attempts for CoGeNT and DAMA,”JCAP08(2011) 008,arXiv:1106.6241 [hep-ph]

    Pith/arXiv arXiv 2011

  44. [44]

    Inelastic frontier: Discovering dark matter at high recoil energy,

    J. Bramante, P. J. Fox, G. D. Kribs, and A. Martin, “Inelastic frontier: Discovering dark matter at high recoil energy,” Phys. Rev. D94no. 11, (2016) 115026,arXiv:1608.02662 [hep-ph]

    Pith/arXiv arXiv 2016

  45. [45]

    Electromagnetic signals of inelastic dark matter scattering,

    M. Baryakhtar, A. Berlin, H. Liu, and N. Weiner, “Electromagnetic signals of inelastic dark matter scattering,”JHEP 06(2022) 047,arXiv:2006.13918 [hep-ph]

    arXiv 2022

  46. [46]

    Pushing the frontier of WIMPy inelastic dark matter: Journey to the end of the periodic table,

    N. Song, S. Nagorny, and A. C. Vincent, “Pushing the frontier of WIMPy inelastic dark matter: Journey to the end of the periodic table,”Phys. Rev. D104no. 10, (2021) 103032,arXiv:2104.09517 [hep-ph]

    arXiv 2021

  47. [47]

    Cosmic-ray upscattered inelastic dark matter,

    N. F. Bell, J. B. Dent, B. Dutta, S. Ghosh, J. Kumar, J. L. Newstead, and I. M. Shoemaker, “Cosmic-ray upscattered inelastic dark matter,”Phys. Rev. D104(2021) 076020,arXiv:2108.00583 [hep-ph]

    arXiv 2021

  48. [48]

    Earth-catalyzed detection of magnetic inelastic dark matter with photons in large underground detectors,

    J. Eby, P. J. Fox, and G. D. Kribs, “Earth-catalyzed detection of magnetic inelastic dark matter with photons in large underground detectors,”JHEP06(2024) 165,arXiv:2312.08478 [hep-ph]

    arXiv 2024

  49. [49]

    Explorations of pseudo-Dirac dark matter having keV splittings and interacting via transition electric and magnetic dipole moments,

    S. Chatterjee and R. Laha, “Explorations of pseudo-Dirac dark matter having keV splittings and interacting via transition electric and magnetic dipole moments,”Phys. Rev. D107no. 8, (2023) 083036,arXiv:2202.13339 [hep-ph]

    arXiv 2023

  50. [50]

    Low-mass constraints on WIMP effective models of inelastic scattering using the Migdal effect,

    S. Kang, S. Scopel, and G. Tomar, “Low-mass constraints on WIMP effective models of inelastic scattering using the Migdal effect,”JCAP01(2025) 035,arXiv:2407.16187 [hep-ph]

    arXiv 2025

  51. [51]

    Electron recoils from terrestrial upscattering of inelastic dark matter,

    T. Emken, J. Frerick, S. Heeba, and F. Kahlhoefer, “Electron recoils from terrestrial upscattering of inelastic dark matter,”Phys. Rev. D105no. 5, (2022) 055023,arXiv:2112.06930 [hep-ph]

    arXiv 2022

  52. [52]

    Not-so-inelastic Dark Matter,

    G. D. V. Garcia, F. Kahlhoefer, M. Ovchynnikov, and T. Schwetz, “Not-so-inelastic Dark Matter,”JHEP02(2025) 127,arXiv:2405.08081 [hep-ph]

    arXiv 2025

  53. [53]

    Snowmass2021 Cosmic Frontier: The landscape of low-threshold dark matter direct detection in the next decade,

    R. Essiget al., “Snowmass2021 Cosmic Frontier: The landscape of low-threshold dark matter direct detection in the next decade,” inSnowmass 2021. 3, 2022.arXiv:2203.08297 [hep-ph]

    arXiv 2021

  54. [54]

    Probing inelastic signatures of dark matter detection via polarized nucleus*,

    Z. Yun, J. Sun, B. Zhu, and X. Liu, “Probing inelastic signatures of dark matter detection via polarized nucleus*,” Chin. Phys. C48no. 10, (2024) 103106,arXiv:2309.01203 [hep-ph]

    arXiv 2024

  55. [55]

    Spin-dependent sub-GeV inelastic dark matter-electron scattering and Migdal effect. Part I. Velocity independent operator,

    J. Li, L. Su, L. Wu, and B. Zhu, “Spin-dependent sub-GeV inelastic dark matter-electron scattering and Migdal effect. Part I. Velocity independent operator,”JCAP04(2023) 020,arXiv:2210.15474 [hep-ph]

    arXiv 2023

  56. [56]

    Indirect detection of low mass dark matter in direct detection experiments with inelastic scattering,

    N. F. Bell, J. B. Dent, B. Dutta, J. Kumar, and J. L. Newstead, “Indirect detection of low mass dark matter in direct detection experiments with inelastic scattering,”Phys. Rev. D106no. 10, (2022) 103016,arXiv:2208.08020 [hep-ph]

    arXiv 2022

  57. [57]

    Detection of inelastic dark matter via electron recoils in SENSEI,

    Y. Gu, L. Wu, and B. Zhu, “Detection of inelastic dark matter via electron recoils in SENSEI,”Phys. Rev. D106no. 7, (2022) 075004,arXiv:2203.06664 [hep-ph]

    arXiv 2022

  58. [58]

    Active Galactic Nuclei as Potential Sources of Ultra-High Energy Cosmic Rays,

    F. M. Rieger, “Active Galactic Nuclei as Potential Sources of Ultra-High Energy Cosmic Rays,”Universe8no. 11, (2022) 607,arXiv:2211.12202 [astro-ph.HE]

    arXiv 2022

  59. [59]

    Chapter 10: High-Energy Neutrinos from Active Galactic Nuclei,

    K. Murase and F. W. Stecker, “Chapter 10: High-Energy Neutrinos from Active Galactic Nuclei,”arXiv:2202.03381 [astro-ph.HE]. [64]IceCubeCollaboration, R. Abbasiet al., “Evidence for neutrino emission from the nearby active galaxy NGC 1068,” Science378no. 6619, (2022) 538–543,arXiv:2211.09972 [astro-ph.HE]

    arXiv 2022

  60. [60]

    Disentangling the Hadronic Components in NGC 1068,

    M. Ajello, K. Murase, and A. McDaniel, “Disentangling the Hadronic Components in NGC 1068,”Astrophys. J. Lett. 954no. 2, (2023) L49,arXiv:2307.02333 [astro-ph.HE]. [66]IceCube, F ermi-LA T, MAGIC, AGILE, ASAS-SN, HA WC, H.E.S.S., INTEGRAL, Kanata, Kiso, Kapteyn, Liverpool T elescope, Subaru, Swift NuST AR, VERIT AS, VLA/17B-403Collaboration, M. G. Aartsen...

    arXiv 2023

  61. [61]

    A Multimessenger Picture of the Flaring Blazar TXS 0506+056: implications for High-Energy Neutrino Emission and Cosmic Ray Acceleration,

    A. Keivaniet al., “A Multimessenger Picture of the Flaring Blazar TXS 0506+056: implications for High-Energy Neutrino Emission and Cosmic Ray Acceleration,”Astrophys. J.864no. 1, (2018) 84,arXiv:1807.04537 [astro-ph.HE]

    Pith/arXiv arXiv 2018

  62. [62]

    TXS 0506+056, the first cosmic neutrino 13 source, is not a BL Lac,

    P. Padovani, F. Oikonomou, M. Petropoulou, P. Giommi, and E. Resconi, “TXS 0506+056, the first cosmic neutrino 13 source, is not a BL Lac,”Mon. Not. Roy. Astron. Soc.484no. 1, (2019) L104–L108,arXiv:1901.06998 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  63. [63]

    Dark matter annihilation at the galactic center,

    P. Gondolo and J. Silk, “Dark matter annihilation at the galactic center,”Phys. Rev. Lett.83(1999) 1719–1722, arXiv:astro-ph/9906391

    Pith/arXiv arXiv 1999

  64. [64]

    A Dark matter spike at the galactic center?,

    P. Ullio, H. Zhao, and M. Kamionkowski, “A Dark matter spike at the galactic center?,”Phys. Rev. D64(2001) 043504,arXiv:astro-ph/0101481

    Pith/arXiv arXiv 2001

  65. [65]

    Unique probe of dark matter in the core of M87 with the Event Horizon Telescope,

    T. Lacroix, M. Karami, A. E. Broderick, J. Silk, and C. Boehm, “Unique probe of dark matter in the core of M87 with the Event Horizon Telescope,”Phys. Rev. D96no. 6, (2017) 063008,arXiv:1611.01961 [astro-ph.GA]

    Pith/arXiv arXiv 2017

  66. [66]

    Probing light dark matter through cosmic-ray cooling in active galactic nuclei,

    G. Herrera and K. Murase, “Probing light dark matter through cosmic-ray cooling in active galactic nuclei,”Phys. Rev. D110no. 1, (2024) L011701,arXiv:2307.09460 [hep-ph]

    arXiv 2024

  67. [67]

    Cosmic-ray boosted inelastic dark matter from neutrino-emitting active galactic nuclei,

    R. A. Gustafson, G. Herrera, M. Mukhopadhyay, K. Murase, and I. M. Shoemaker, “Cosmic-ray boosted inelastic dark matter from neutrino-emitting active galactic nuclei,”arXiv:2508.20984 [hep-ph]

    Pith/arXiv arXiv

  68. [68]

    Enhanced Cosmic-Ray Cooling in AGN from Dark Matter Deep Inelastic Scattering,

    L. Li, C.-T. Lu, A. K. Mishra, L. Su, and L. Wu, “Enhanced Cosmic-Ray Cooling in AGN from Dark Matter Deep Inelastic Scattering,”arXiv:2509.11906 [hep-ph]

    arXiv

  69. [69]

    Cosmic-ray cooling in active galactic nuclei as a new probe of inelastic dark matter,

    R. A. Gustafson, G. Herrera, M. Mukhopadhyay, K. Murase, and I. M. Shoemaker, “Cosmic-ray cooling in active galactic nuclei as a new probe of inelastic dark matter,”Phys. Rev. D111no. 12, (2025) L121303,arXiv:2408.08947 [hep-ph]

    arXiv 2025

  70. [70]

    Probing gauged U(1) sub-GeV dark matter via cosmic ray cooling in active galactic nuclei,

    A. K. Mishra, N. Liu, and C.-T. Lu, “Probing gauged U(1) sub-GeV dark matter via cosmic ray cooling in active galactic nuclei,”Phys. Dark Univ.49(2025) 102050,arXiv:2504.03409 [hep-ph]

    arXiv 2025

  71. [71]

    Illuminating scalar dark matter co-scattering in EFT with monophoton signatures,

    G. B´ elanger, M. Mitra, R. Padhan, and A. Roy, “Illuminating scalar dark matter co-scattering in EFT with monophoton signatures,”JHEP01(2026) 007,arXiv:2508.06040 [hep-ph]

    arXiv 2026

  72. [72]

    Three exceptions in the calculation of relic abundances,

    K. Griest and D. Seckel, “Three exceptions in the calculation of relic abundances,”Phys. Rev. D43(1991) 3191–3203

    1991

  73. [73]

    Coannihilation without chemical equilibrium,

    M. Garny, J. Heisig, B. L¨ ulf, and S. Vogl, “Coannihilation without chemical equilibrium,”Phys. Rev. D96no. 10, (2017) 103521,arXiv:1705.09292 [hep-ph]

    Pith/arXiv arXiv 2017

  74. [74]

    Neutralino with the right cold dark matter abundance in (almost) any supersymmetric model,

    G. B. Gelmini and P. Gondolo, “Neutralino with the right cold dark matter abundance in (almost) any supersymmetric model,”Phys. Rev. D74(2006) 023510,arXiv:hep-ph/0602230

    Pith/arXiv arXiv 2006

  75. [75]

    Thermal dark matter with low-temperature reheating,

    N. Bernal, K. Deka, and M. Losada, “Thermal dark matter with low-temperature reheating,”JCAP09(2024) 024, arXiv:2406.17039 [hep-ph]

    arXiv 2024

  76. [76]

    Scrutinizing fermionic Dark Matter in scotogenic model with low reheating temperature,

    A. Roy and R. Sahu, “Scrutinizing fermionic Dark Matter in scotogenic model with low reheating temperature,”JCAP 03(2026) 014,arXiv:2508.14726 [hep-ph]

    arXiv 2026

  77. [77]

    Z’-mediated dark matter with low-temperature reheating,

    G. B´ elanger, N. Bernal, and A. Pukhov, “Z’-mediated dark matter with low-temperature reheating,”JHEP03(2025) 079,arXiv:2412.12303 [hep-ph]

    arXiv 2025

  78. [78]

    Cosmology with a primordial scaling field,

    P. G. Ferreira and M. Joyce, “Cosmology with a primordial scaling field,”Phys. Rev. D58(1998) 023503, arXiv:astro-ph/9711102

    Pith/arXiv arXiv 1998

  79. [79]

    Electroweak Baryogenesis and the Expansion Rate of the Universe,

    M. Joyce, “Electroweak Baryogenesis and the Expansion Rate of the Universe,”Phys. Rev. D55(1997) 1875–1878, arXiv:hep-ph/9606223

    Pith/arXiv arXiv 1997

  80. [80]

    When the Universe Expands Too Fast: Relentless Dark Matter,

    F. D’Eramo, N. Fernandez, and S. Profumo, “When the Universe Expands Too Fast: Relentless Dark Matter,”JCAP 05(2017) 012,arXiv:1703.04793 [hep-ph]

    Pith/arXiv arXiv 2017

Showing first 80 references.