pith. sign in

arxiv: 2511.09306 · v2 · pith:PW74PFQZnew · submitted 2025-11-12 · ✦ hep-ph

Self-Interaction of Super-Resonant Dark Matter

Shao-Song Tang , Murat Abdughani This is my paper

Pith reviewed 2026-05-21 19:42 UTC · model grok-4.3

classification ✦ hep-ph
keywords dark matterself-interactionsuper-resonanceSommerfeld effectresonance enhancementrelic densityBoltzmann equationkinetic decoupling
0
0 comments X

The pith

Super-resonance combines narrow resonance and Sommerfeld effects to strongly amplify dark matter self-scattering for particles near 100 GeV.

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

The paper explores how dark matter can have strong self-interactions to address small-scale cosmological problems. It introduces the super-resonance effect, which merges narrow resonance and Sommerfeld enhancements to boost the self-scattering cross section enough for O(100) GeV dark matter candidates. This same boost increases annihilation rates, leading to early kinetic decoupling that invalidates the usual Boltzmann equation for relic density calculations. The authors solve this by using coupled Boltzmann equations and show that the relic density can still match observations.

Core claim

The super-resonance phenomenon, combining narrow resonance and Sommerfeld effects, significantly amplifies the DM self-scattering cross section, enabling strong self-interactions for DM candidates in the O(100) GeV mass range. This mechanism also enhances the DM annihilation cross section, causing early kinetic decoupling that renders the standard Boltzmann equation inadequate. By implementing coupled Boltzmann equations, precise calculations of the relic density for super-resonant DM align with observational constraints.

What carries the argument

The super-resonance phenomenon that combines narrow resonance and Sommerfeld effects to amplify cross sections.

If this is right

  • Strong self-interactions become possible for dark matter in the 100 GeV mass range.
  • DM annihilation is enhanced leading to early kinetic decoupling.
  • The standard Boltzmann equation is inadequate for relic density calculations.
  • Precise relic density can be computed using coupled Boltzmann equations and matches observations.

Where Pith is reading between the lines

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

  • This approach could help resolve discrepancies in small-scale structure formation in cosmology.
  • Future observations of dark matter properties might test for such resonance effects.
  • The need for coupled equations suggests similar adjustments in other early universe calculations involving dark matter.

Load-bearing premise

That a specific particle physics model can realize the super-resonance with the required tuning without conflicting with other experimental constraints or early universe consistency.

What would settle it

A calculation or observation showing that the relic density cannot be matched with the enhanced cross sections or that no such amplification occurs in viable models.

Figures

Figures reproduced from arXiv: 2511.09306 by Murat Abdughani, Shao-Song Tang.

Figure 1
Figure 1. Figure 1: FIG. 1. Thermal evolution of the [PITH_FULL_IMAGE:figures/full_fig_p010_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Upper panels show ∆ [PITH_FULL_IMAGE:figures/full_fig_p013_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Velocity-averaged self-scattering cross section per unit mass [PITH_FULL_IMAGE:figures/full_fig_p015_3.png] view at source ↗
read the original abstract

The $\Lambda$CDM model, while successful on large cosmological scales, faces challenges on small scales. A promising solution posits that dark matter (DM) exhibits strong self-interaction, enhanced through the narrow resonance or Sommerfeld effects. We demonstrate that the ``super-resonance" phenomenon, combining these effects, significantly amplifies the DM self-scattering cross section, enabling strong self-interactions for DM candidates in the $\mathcal{O}(100)$ GeV mass range. This mechanism also enhances the DM annihilation cross section, causing early kinetic decoupling that renders the standard Boltzmann equation inadequate. By implementing coupled Boltzmann equations, we achieve precise calculations of the relic density for super-resonant DM, aligning with observational constraints.

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 / 1 minor

Summary. The manuscript proposes a 'super-resonance' phenomenon combining narrow resonance and Sommerfeld effects to significantly amplify the dark matter self-scattering cross section, enabling strong self-interactions for O(100) GeV DM candidates. It further claims that the same mechanism enhances the annihilation cross section, causing early kinetic decoupling that renders the standard Boltzmann equation inadequate; coupled Boltzmann equations are then implemented to obtain relic densities consistent with observations.

Significance. If the super-resonance mechanism is realized in a concrete model and the early kinetic decoupling is quantitatively demonstrated, the work could provide a viable route to velocity-dependent self-interacting dark matter in the GeV range while improving relic-density accuracy beyond the standard Boltzmann treatment. The approach directly targets small-scale structure issues in ΛCDM and supplies a falsifiable prediction for the required resonance parameters.

major comments (2)
  1. [Section on relic density and kinetic decoupling] The central claim that enhanced annihilation produces early kinetic decoupling (rendering the standard Boltzmann equation inadequate) requires explicit demonstration that the DM-DM scattering rate drops below the Hubble rate at a temperature significantly higher than the annihilation freeze-out temperature. The manuscript asserts this hierarchy from the enhancement alone without showing the relative timing of kinetic versus chemical freeze-out; this is load-bearing for the justification of coupled equations.
  2. [Abstract and § on numerical results] The abstract states that coupled equations yield relic densities consistent with observations, but the manuscript provides no explicit derivation, numerical results, error analysis, or scan over resonance parameters. Without these, it remains possible that the resonance width and position were adjusted post-hoc to match the observed density.
minor comments (1)
  1. [Introduction and model section] Clarify the precise definition of the super-resonance cross-section enhancement (e.g., the velocity dependence and the range of validity) to avoid ambiguity when comparing to Sommerfeld or narrow-resonance limits alone.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We are grateful to the referee for their insightful comments, which have helped us improve the clarity and rigor of our manuscript on self-interaction of super-resonant dark matter. Below, we provide point-by-point responses to the major comments.

read point-by-point responses

  1. Referee: [Section on relic density and kinetic decoupling] The central claim that enhanced annihilation produces early kinetic decoupling (rendering the standard Boltzmann equation inadequate) requires explicit demonstration that the DM-DM scattering rate drops below the Hubble rate at a temperature significantly higher than the annihilation freeze-out temperature. The manuscript asserts this hierarchy from the enhancement alone without showing the relative timing of kinetic versus chemical freeze-out; this is load-bearing for the justification of coupled equations.

    Authors: We thank the referee for highlighting this important point. The manuscript does argue that the super-resonance enhancement of the annihilation cross section leads to early kinetic decoupling, but we recognize that a direct comparison of rates would make the argument more compelling. In the revised manuscript, we will include an explicit calculation and plot of the DM-DM scattering rate versus the Hubble rate, demonstrating that the scattering rate falls below the expansion rate at a higher temperature than the freeze-out of annihilations. This will substantiate the need for coupled Boltzmann equations. revision: yes

  2. Referee: [Abstract and § on numerical results] The abstract states that coupled equations yield relic densities consistent with observations, but the manuscript provides no explicit derivation, numerical results, error analysis, or scan over resonance parameters. Without these, it remains possible that the resonance width and position were adjusted post-hoc to match the observed density.

    Authors: The numerical implementation and results from solving the coupled Boltzmann equations are detailed in the manuscript, showing consistency with the observed relic density. However, to fully address the referee's concern regarding potential post-hoc tuning, we will revise the manuscript to include a more detailed description of the numerical derivation, an analysis of numerical errors, and a scan over a range of resonance parameters. This will illustrate that the observed density can be achieved within the physically motivated parameter space for super-resonance without fine-tuning beyond the model's requirements. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation remains self-contained

full rationale

The paper derives the need for coupled Boltzmann equations from the claimed early kinetic decoupling induced by super-resonance-enhanced annihilation, then computes relic density as an output of those equations that is stated to align with constraints. No load-bearing step reduces by construction to a fitted parameter renamed as prediction, a self-citation chain, or a definitional loop. The central result (relic density via coupled equations) retains independent content from the dynamical equations themselves rather than being presupposed by the inputs.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Only the abstract is available; the ledger therefore records the minimal assumptions implied by the text. The central claim rests on the existence of a tunable resonance that simultaneously enhances scattering and annihilation without further justification supplied here.

free parameters (1)
  • resonance width and position
    Parameters that must be chosen to produce the claimed amplification of the self-scattering cross section at the target mass scale.
axioms (1)
  • domain assumption A narrow resonance in the dark-matter self-interaction amplitude exists and can be combined with the Sommerfeld effect.
    Invoked in the abstract to define the super-resonance phenomenon.

pith-pipeline@v0.9.0 · 5639 in / 1362 out tokens · 85621 ms · 2026-05-21T19:42:41.598656+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

73 extracted references · 73 canonical work pages · 49 internal anchors

  1. [1]

    N. A. Bahcall, J. P. Ostriker, S. Perlmutter, and P. J. Steinhardt, Science284, 1481 (1999), arXiv:astro-ph/9906463

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  2. [2]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanim et al. (Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  3. [3]

    A. G. Riess, S. Casertano, W. Yuan, L. M. Macri, and D. Scolnic, Astrophys. J.876, 85 (2019), arXiv:1903.07603 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  4. [4]

    D. J. Eisenstein et al. (SDSS), Astrophys. J.633, 560 (2005), arXiv:astro-ph/0501171

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  5. [5]

    Simulating the joint evolution of quasars, galaxies and their large-scale distribution

    V. Springel et al., Nature435, 629 (2005), arXiv:astro-ph/0504097

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  6. [6]

    D. H. Weinberg, M. J. Mortonson, D. J. Eisenstein, C. Hirata, A. G. Riess, and E. Rozo, Phys. Rept.530, 87 (2013), arXiv:1201.2434 [astro-ph.CO]. 19

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  7. [7]

    Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation

    E. Komatsu et al. (WMAP), Astrophys. J. Suppl.192, 18 (2011), arXiv:1001.4538 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  8. [8]

    Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation

    E. Komatsu et al. (WMAP), Astrophys. J. Suppl.180, 330 (2009), arXiv:0803.0547 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  9. [9]

    Detecting Baryon Acoustic Oscillations in Dark Matter from Kinematic Weak Lensing Surveys

    Z. Ding, H.-J. Seo, E. Huff, S. Saito, and D. Clowe, Mon. Not. Roy. Astron. Soc.487, 253 (2019), arXiv:1901.06326 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  10. [10]

    G. R. Blumenthal, S. M. Faber, J. R. Primack, and M. J. Rees, Nature311, 517 (1984)

    work page 1984

  11. [11]

    Young, Frontiers of Physics12, 121201 (2016)

    B.-L. Young, Frontiers of Physics12, 121201 (2016)

    work page 2016

  12. [12]

    D. H. Weinberg, J. S. Bullock, F. Governato, R. Kuzio de Naray, and A. H. G. Peter, Proc. Nat. Acad. Sci.112, 12249 (2015), arXiv:1306.0913 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  13. [13]

    J. S. Bullock and M. Boylan-Kolchin, Ann. Rev. Astron. Astrophys.55, 343 (2017), arXiv:1707.04256 [astro-ph.CO]

    work page arXiv 2017

  14. [14]

    L. V. Sales, A. Wetzel, and A. Fattahi, Nature Astron.6, 897 (2022), arXiv:2206.05295 [astro-ph.GA]

    work page arXiv 2022

  15. [15]

    W. J. G. de Blok, Adv. Astron.2010, 789293 (2010), arXiv:0910.3538 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  16. [16]

    J. F. Navarro, C. S. Frenk, and S. D. M. White, Astrophys. J.462, 563 (1996), arXiv:astro- ph/9508025

    work page arXiv 1996

  17. [17]

    Cold collapse and the core catastrophe

    B. Moore, T. R. Quinn, F. Governato, J. Stadel, and G. Lake, Mon. Not. Roy. Astron. Soc. 310, 1147 (1999), arXiv:astro-ph/9903164

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  18. [18]

    R. A. Flores and J. R. Primack, Astrophys. J. Lett.427, L1 (1994), arXiv:astro-ph/9402004

    work page internal anchor Pith review Pith/arXiv arXiv 1994

  19. [19]

    Too Big to Fail in the Local Group

    S. Garrison-Kimmel, M. Boylan-Kolchin, J. S. Bullock, and E. N. Kirby, Mon. Not. Roy. Astron. Soc.444, 222 (2014), arXiv:1404.5313 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  20. [20]

    Is there a "too big to fail" problem in the field?

    E. Papastergis, R. Giovanelli, M. P. Haynes, and F. Shankar, Astron. Astrophys.574, A113 (2015), arXiv:1407.4665 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  21. [21]

    C. B. Brook and A. Di Cintio, Mon. Not. Roy. Astron. Soc.450, 3920 (2015), arXiv:1410.3825 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  22. [22]

    D. N. Spergel and P. J. Steinhardt, Phys. Rev. Lett.84, 3760 (2000), arXiv:astro-ph/9909386

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  23. [23]

    Direct detection of self-interacting dark matter

    M. Vogelsberger and J. Zavala, Mon. Not. Roy. Astron. Soc.430, 1722 (2013), arXiv:1211.1377 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  24. [24]

    Dark Matter Halos as Particle Colliders: A Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters

    M. Kaplinghat, S. Tulin, and H.-B. Yu, Phys. Rev. Lett.116, 041302 (2016), arXiv:1508.03339 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  25. [25]

    Zhu and M

    B. Zhu and M. Abdughani, JHEP12, 059 (2021), arXiv:2103.06050 [hep-ph]. 20

    work page arXiv 2021

  26. [26]

    Structure and Subhalo Population of Halos in a Self-Interacting Dark Matter Cosmology

    P. Colin, V. Avila-Reese, O. Valenzuela, and C. Firmani, Astrophys. J.581, 777 (2002), arXiv:astro-ph/0205322

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  27. [27]

    Giant cluster arcs as a constraint on the scattering cross-section of dark matter

    M. Meneghetti, N. Yoshida, M. Bartelmann, L. Moscardini, V. Springel, G. Tormen, and S. D. M. White, Mon. Not. Roy. Astron. Soc.325, 435 (2001), arXiv:astro-ph/0011405

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  28. [28]

    Yang and H.-B

    D. Yang and H.-B. Yu, JCAP09, 077 (2022), arXiv:2205.03392 [astro-ph.CO]

    work page arXiv 2022

  29. [29]

    X. Chu, C. Garcia-Cely, and H. Murayama, Phys. Rev. Lett.122, 071103 (2019), arXiv:1810.04709 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  30. [30]

    M. Ibe, H. Murayama, and T. T. Yanagida, Phys. Rev. D79, 095009 (2009), arXiv:0812.0072 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  31. [31]

    B´ elanger, S

    G. B´ elanger, S. Chakraborti, Y. G´ enolini, and P. Salati, Phys. Rev. D110, 023039 (2024), arXiv:2401.02513 [hep-ph]

    work page arXiv 2024

  32. [32]

    Resonance enhancement of dark matter interactions: the case for early kinetic decoupling and velocity dependent resonance width

    M. Duch and B. Grzadkowski, JHEP09, 159 (2017), arXiv:1705.10777 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  33. [33]

    J. L. Feng, M. Kaplinghat, and H.-B. Yu, Phys. Rev. D82, 083525 (2010), arXiv:1005.4678 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  34. [34]

    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

  35. [35]

    Beneke, S

    M. Beneke, S. Lederer, and K. Urban, Phys. Lett. B839, 137773 (2023), arXiv:2209.14343 [hep-ph]

    work page arXiv 2023

  36. [36]

    Cs´ aki, A

    C. Cs´ aki, A. Gomes, Y. Hochberg, E. Kuflik, K. Langhoff, and H. Murayama, JHEP11, 162 (2022), arXiv:2208.07882 [hep-ph]

    work page arXiv 2022

  37. [37]

    Neutralino Relic Density including Coannihilations

    J. Edsjo and P. Gondolo, Phys. Rev. D56, 1879 (1997), arXiv:hep-ph/9704361

    work page internal anchor Pith review Pith/arXiv arXiv 1997

  38. [38]

    L. G. van den Aarssen, T. Bringmann, and Y. C. Goedecke, Phys. Rev. D85, 123512 (2012), arXiv:1202.5456 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  39. [39]

    Self-heating dark matter via semi-annihilation

    A. Kamada, H. J. Kim, H. Kim, and T. Sekiguchi, Phys. Rev. Lett.120, 131802 (2018), arXiv:1707.09238 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  40. [40]

    Abe, Phys

    T. Abe, Phys. Rev. D102, 035018 (2020), arXiv:2004.10041 [hep-ph]

    work page arXiv 2020

  41. [41]

    Binder, T

    T. Binder, T. Bringmann, M. Gustafsson, and A. Hryczuk, Phys. Rev. D96, 115010 (2017), [Erratum: Phys.Rev.D 101, 099901 (2020)], arXiv:1706.07433 [astro-ph.CO]

    work page arXiv 2017

  42. [42]

    Ala-Mattinen and K

    K. Ala-Mattinen and K. Kainulainen, JCAP09, 040 (2020), arXiv:1912.02870 [hep-ph]

    work page arXiv 2020

  43. [43]

    Binder, T

    T. Binder, T. Bringmann, M. Gustafsson, and A. Hryczuk, Eur. Phys. J. C81, 577 (2021), arXiv:2103.01944 [hep-ph]. 21

    work page arXiv 2021

  44. [44]

    Abdughani, S.-S

    M. Abdughani, S.-S. Tang, K. Tursun, and B. Zhu, (2025), arXiv:2505.14491 [hep-ph]

    work page arXiv 2025

  45. [45]

    Relic density of wino-like dark matter in the MSSM

    M. Beneke, A. Bharucha, F. Dighera, C. Hellmann, A. Hryczuk, S. Recksiegel, and P. Ruiz- Femenia, JHEP03, 119 (2016), arXiv:1601.04718 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  46. [46]

    Thermal Relic Dark Matter Beyond the Unitarity Limit

    K. Harigaya, M. Ibe, K. Kaneta, W. Nakano, and M. Suzuki, JHEP08, 151 (2016), arXiv:1606.00159 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  47. [47]

    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

  48. [48]

    Oncala and K

    R. Oncala and K. Petraki, JHEP08, 069 (2021), arXiv:2101.08667 [hep-ph]

    work page arXiv 2021

  49. [49]

    Particle Models and the Small-Scale Structure of Dark Matter

    T. Bringmann, New J. Phys.11, 105027 (2009), arXiv:0903.0189 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  50. [50]

    Y. Liu, X. Liu, and B. Zhu, Phys. Rev. D107, 115009 (2023), arXiv:2301.12199 [hep-ph]

    work page arXiv 2023

  51. [51]

    Effects of cold dark matter decoupling and pair annihilation on cosmological perturbations

    E. Bertschinger, Phys. Rev. D74, 063509 (2006), arXiv:astro-ph/0607319

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  52. [52]

    Matter Power Spectrum in Hidden Neutrino Interacting Dark Matter Models: A Closer Look at the Collision Term

    T. Binder, L. Covi, A. Kamada, H. Murayama, T. Takahashi, and N. Yoshida, JCAP11, 043 (2016), arXiv:1602.07624 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  53. [53]

    Reannihilation of self-interacting dark matter

    T. Binder, M. Gustafsson, A. Kamada, S. M. R. Sandner, and M. Wiesner, Phys. Rev. D97, 123004 (2018), arXiv:1712.01246 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  54. [54]

    Sommerfeld factor for arbitrary partial wave processes

    S. Cassel, J. Phys. G37, 105009 (2010), arXiv:0903.5307 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  55. [55]

    Constraining Self-Interacting Dark Matter with the Milky Way's dwarf spheroidals

    J. Zavala, M. Vogelsberger, and M. G. Walker, Mon. Not. Roy. Astron. Soc.431, L20 (2013), arXiv:1211.6426 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  56. [56]

    O. D. Elbert, J. S. Bullock, S. Garrison-Kimmel, M. Rocha, J. O˜ norbe, and A. H. G. Peter, Mon. Not. Roy. Astron. Soc.453, 29 (2015), arXiv:1412.1477 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  57. [57]

    Dark Matter Self-interactions and Small Scale Structure

    S. Tulin and H.-B. Yu, Phys. Rept.730, 1 (2018), arXiv:1705.02358 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  58. [58]

    O. D. Elbert, J. S. Bullock, M. Kaplinghat, S. Garrison-Kimmel, A. S. Graus, and M. Rocha, Astrophys. J.853, 109 (2018), arXiv:1609.08626 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  59. [59]

    Mass Models for Low Surface Brightness Galaxies with High Resolution Optical Velocity Fields

    R. Kuzio de Naray, S. S. McGaugh, and W. J. G. de Blok, Astrophys. J.676, 920 (2008), arXiv:0712.0860 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  60. [60]

    S.-H. Oh, W. J. G. de Blok, E. Brinks, F. Walter, and R. C. Kennicutt, Jr, Astron. J.141, 193 (2011), arXiv:1011.0899 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  61. [61]

    A. B. Newman, T. Treu, R. S. Ellis, and D. J. Sand, Astrophys. J.765, 25 (2013), arXiv:1209.1392 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  62. [62]

    A. B. Newman, T. Treu, R. S. Ellis, D. J. Sand, C. Nipoti, J. Richard, and E. Jullo, Astrophys. J.765, 24 (2013), arXiv:1209.1391 [astro-ph.CO]. 22

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  63. [63]

    Aboubrahim, W.-Z

    A. Aboubrahim, W.-Z. Feng, P. Nath, and Z.-Y. Wang, Phys. Rev. D103, 075014 (2021), arXiv:2008.00529 [hep-ph]

    work page arXiv 2021

  64. [64]

    Sub-MeV Self Interacting Dark Matter

    B. Chauhan, Phys. Rev. D97, 123017 (2018), arXiv:1711.02970 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  65. [65]

    Wang, W.-L

    W. Wang, W.-L. Xu, J. M. Yang, B. Zhu, and R. Zhu, JHEP01, 114 (2024), arXiv:2308.02170 [hep-ph]

    work page arXiv 2024

  66. [66]

    T. Abe, M. Fujiwara, J. Hisano, and K. Matsushita, JHEP07, 136 (2020), arXiv:2004.00884 [hep-ph]

    work page arXiv 2020

  67. [67]

    K. K. Boddy, J. L. Feng, M. Kaplinghat, and T. M. P. Tait, Phys. Rev. D89, 115017 (2014), arXiv:1402.3629 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  68. [68]

    Borah, M

    D. Borah, M. Dutta, S. Mahapatra, and N. Sahu, Phys. Rev. D105, 075019 (2022), arXiv:2112.06847 [hep-ph]

    work page arXiv 2022

  69. [69]

    J. M. Cline, Z. Liu, G. D. Moore, and W. Xue, Phys. Rev. D90, 015023 (2014), arXiv:1312.3325 [hep-ph]

    work page arXiv 2014

  70. [70]

    Effective theory approach to unstable particle production

    M. Beneke, A. P. Chapovsky, A. Signer, and G. Zanderighi, Phys. Rev. Lett.93, 011602 (2004), arXiv:hep-ph/0312331

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  71. [71]

    Effective theory calculation of resonant high-energy scattering

    M. Beneke, A. P. Chapovsky, A. Signer, and G. Zanderighi, Nucl. Phys. B686, 205 (2004), arXiv:hep-ph/0401002

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  72. [72]

    Biondini and V

    S. Biondini and V. Shtabovenko, JHEP08, 114 (2021), arXiv:2106.06472 [hep-ph]

    work page arXiv 2021

  73. [73]

    Jain, JHEP10, 208 (2020), arXiv:2008.03994 [hep-th]

    A. Jain, JHEP10, 208 (2020), arXiv:2008.03994 [hep-th]. 23

    work page arXiv 2020