pith. machine review for the scientific record. sign in

arxiv: 2604.22013 · v1 · submitted 2026-04-23 · 🌌 astro-ph.GA

Recognition: unknown

An Extended Parametric Model for Self-interacting Dark Matter Halos

Siddhesh Raut , Ethan Nadler , Andrew Benson
Authors on Pith no claims yet

Pith reviewed 2026-05-09 20:33 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords self-interacting dark matterSIDM halosparametric modelgravothermal evolutionmass accretionNFW profileV_maxcore collapse
0
0 comments X

The pith

An extended parametric model for SIDM halos incorporates mass accretion to reduce overpredictions of V_max at z=0.

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

The paper extends an earlier parametric model of self-interacting dark matter halo evolution by adding the effects of smooth mass accretion. The original model overpredicts the maximum circular velocity V_max for some field halos at the present day because it evolves them too quickly compared with cosmological simulations. The extension assumes that ongoing accretion drives the halo density profile back toward the Navarro-Frenk-White form that would apply in cold dark matter, thereby slowing the gravothermal core-collapse process. This produces substantially smaller errors in predicted V_max while keeping the model simple enough for use in semi-analytic calculations. A reader would care because accurate halo templates are needed to translate observations of galaxy rotation curves and strong lensing into constraints on the dark-matter self-interaction cross section.

Core claim

We improve upon the parametric model for the evolution of the density profiles of self-interacting dark matter (SIDM) halos introduced in Yang et al. (2024b), by considering the effects of mass accretion on a SIDM halo's gravothermal evolution. The original parametric model accurately predicts parameters V_max and R_max, but with a tendency to overpredict V_max at z=0 for a subset of field halos. This discrepancy results from the parametric model predicting a faster rate of gravothermal evolution for these field halos compared to that measured in cosmological zoom-in simulations. We propose that the effects of mass accretion on the evolution of SIDM halos are not fully captured by the orignl

What carries the argument

The assumption that smooth mass accretion delays core-collapse by driving the SIDM halo density profile back toward a Navarro-Frenk-White (NFW) shape.

If this is right

  • The model yields smaller residuals in V_max for field halos at z=0 while retaining analytic simplicity.
  • Predicted halo density profiles remain close to those measured in simulations across a broader range of accretion rates.
  • The framework can be inserted into semi-analytic galaxy-formation codes without requiring full N-body runs for each halo.
  • Core-collapse timescales become longer for halos that continue to accrete mass, altering the expected abundance of dense SIDM cores today.

Where Pith is reading between the lines

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

  • The same accretion-reset logic might be applied to other parametric SIDM models to improve their agreement with simulations at earlier redshifts.
  • If the reset assumption holds, observed samples of field dwarf galaxies could be used to place tighter limits on the SIDM cross section by comparing their measured V_max values to the extended model's predictions.
  • The approach suggests a concrete test: halos with recent major mergers should show less core collapse than isolated halos of similar mass and age.

Load-bearing premise

Smooth mass accretion on SIDM halos can be modeled as resetting their profiles toward NFW shapes and thereby delaying core collapse.

What would settle it

Comparing the extended model's V_max predictions against an independent suite of zoom-in simulations that span a wide range of mass-accretion histories would show whether the reduction in error persists or disappears.

Figures

Figures reproduced from arXiv: 2604.22013 by Andrew Benson, Ethan Nadler, Siddhesh Raut.

Figure 1
Figure 1. Figure 1: — Examples of the evolution of Vmax in SIDM halos as a function of lookback time, shown by purple lines. Black dashed lines show the evolution of Vmax in the matched CDM halo, while the blue line indicates the predictions of the original parametric model, computed using the assembly history of the matched CDM halo. Left and right panels show cases where the original parameter model provides an accurate mat… view at source ↗
Figure 2
Figure 2. Figure 2: — The distribution of fractional offsets in Vmax at z = 0, δVmax , between the original parametric model and field halos se￾lected from the Group simulation is shown by the blue histogram. The solid blue line shows a kernel density estimation (KDE) ap￾proximation to this distribution [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: — The distribution of fractional offsets in Vmax at z = 0, δVmax , between the extended parametric model (with α = 2.0 and C = 0.75) and field halos selected from the Group simulation is shown by the orange histogram. The solid orange line shows a KDE approximation to this distribution. For comparison, the results of the original parametric model are shown in blue. Vertical dashed lines indicate the mean o… view at source ↗
Figure 4
Figure 4. Figure 4: — The left panel shows halos for which the original parametric model predicted δVmax > 0.3, while the right panel shows those for which it predicted δVmax < 0.3. The distribution of δVmax for the original model and extended model is shown for both samples of halos to highlight how differently the predictions for δVmax change with the extended model for halos that are over-estimated vs well-estimated in the… view at source ↗
Figure 5
Figure 5. Figure 5: — The distribution of fractional offsets in Rmax at z = 0, δRmax , between the original parametric model and field halos selected from the Group simulation is shown by the blue histogram. The same is shown for the extended parametric model in orange. KDE of each histogram is shown to better illustrate the spread of δRmax values. Note that the mean of δRmax , ⟨δRmax ⟩ for the original model is ⟨δRmax ⟩ = 0.… view at source ↗
Figure 7
Figure 7. Figure 7: — The left panel shows Vmax values predicted by both original and extended models, and also those obtained from the N-body simulations. The center panel shows τ for the extended and original model, while the right panel shows τ for the extended model against the mass accretion rate to illustrate how our extended model drives τ to lower values during periods of rapid growth. 0.0 2.5 5.0 7.5 10.0 tLB (Gyr) 5… view at source ↗
Figure 8
Figure 8. Figure 8: — As [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: — 2D color maps measuring the performance of the extended parametric model in matching density profiles of SIDM halos in the Group simulation. The left panel shows ⟨δρ,tot⟩ for a range of C and α for the extended parametric model, while the right panel shows RMS(δρ,tot). The hatched area depicts the region of (C, α) parameters for which the extended parametric model performs better than the original parame… view at source ↗
Figure 10
Figure 10. Figure 10: — The distribution of δVmax for the original model and extended model for the sample of halos in the Milky Way simula￾tions. The original model has a mean of ⟨δVmax ⟩ = 0.021 and the extended model has a mean of ⟨δVmax ⟩ = −0.017 parameters, (C, α), predicts SIDM profiles across all ha￾los in our Group sample. It is also reassuring that the commonly used values for C in the literature, such as C = 0.75, o… view at source ↗
Figure 11
Figure 11. Figure 11: — The distribution of fractional offsets in Vmax at z = 0, δVmax , between the extended parametric model (with α = 2.0 and C = 0.75) and field halos selected from the Milky Way simulation is shown by the orange histogram. The solid orange line shows a KDE approximation to this distribution. For comparison, the results of the original parametric model are shown in blue. Vertical dashed lines indicate the m… view at source ↗
Figure 12
Figure 12. Figure 12: — The distribution of δRmax resulting from the original parametric model applied to halos from the Milky Way simulations is chosen by the blue histogram, with the blue line showing a kernel density estimate of this distribution function. The original model has a mean of ⟨δRmax ⟩ = 0.48 and the extended model has a mean of ⟨δRmax ⟩ = 0.62 the original model, merely being offset to negative values, but by a… view at source ↗
Figure 13
Figure 13. Figure 13: — 2D colormaps measuring the performance of the extended parametric model in matching density profiles of SIDM halos in the Milky Way simulation. The left panel shows ⟨δρ,tot⟩ as a function of C and α for the extended parametric model, while the right panel shows RMS(δρ,tot). The hatched area depicts the region of (C, α) parameters for which the extended parametric model performs better than the original … view at source ↗
Figure 14
Figure 14. Figure 14: — 2D color maps measuring the performance of the extended parametric model in predicting central densities of SIDM halos in the Group simulation. The left panel shows ⟨δρc ⟩ for a range of C and α for the extended parametric model, while the right panel shows RMS(δρc ). The hatched area depicts the region of (C, α) parameters for which the extended parametric model performs better than the original parame… view at source ↗
Figure 15
Figure 15. Figure 15: — 2D color maps measuring the performance of the extended parametric model in predicting central densities of SIDM halos in the Milky Way simulation. The left panel shows ⟨δρc ⟩ for a range of C and α for the extended parametric model, while the right panel shows RMS(δρc ). The hatched area depicts the region of (C, α) parameters for which the extended parametric model performs better than the original pa… view at source ↗
read the original abstract

We improve upon the parametric model for the evolution of the density profiles of self-interacting dark matter (SIDM) halos introduced in Yang et al. (2024b), by considering the effects of mass accretion on a SIDM halo's gravothermal evolution. The original parametric model accurately predicts parameters $V_{\max}$ and $R_{\max}$, but with a tendency to overpredict $V_{\max}$ at $z=0$ for a subset of field halos. This discrepancy results from the parametric model predicting a faster rate of gravothermal evolution for these field halos compared to that measured in cosmological zoom-in simulations. We propose that the effects of mass accretion on the evolution of SIDM halos are not fully captured by the original parametric model. Our extended parametric model assumes that smooth mass accretion delays core-collapse by driving the SIDM halo back toward a Navarro-Frenk-White (NFW) profile (as it would have in the case of cold dark matter). We find that this extended model is able to substantially reduce the error in predicted $V_{\max}$ for halos compared to the original model, providing a more accurate model of SIDM halo evolution.

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 paper extends the parametric model of Yang et al. (2024b) for the gravothermal evolution of SIDM halo density profiles by incorporating smooth mass accretion. The extension assumes that accretion delays core collapse by restoring the halo toward an NFW profile (as in CDM), and the authors report that this substantially reduces the overprediction of V_max at z=0 for a subset of field halos relative to the original model.

Significance. If the reported error reduction is robust, the extended model would provide a practical, computationally efficient improvement for predicting SIDM halo properties in cosmological contexts, particularly for matching zoom-in simulation results without full gravothermal integration. This could strengthen the use of parametric SIDM models in interpreting dwarf galaxy kinematics or other observables. The phenomenological calibration, however, limits its generality beyond the tuned simulation suite.

major comments (2)
  1. [Abstract] Abstract and central assumption: the claim that smooth mass accretion 'drives the SIDM halo back toward a Navarro-Frenk-White (NFW) profile' is introduced phenomenologically without derivation from the underlying gravothermal fluid equations or Boltzmann equation under continuous mass growth. No section demonstrates that the assumed instantaneous NFW reset is consistent with the coupled accretion+self-interaction dynamics; the reported V_max error reduction therefore rests on a functional form calibrated to the same zoom-in runs the model aims to reproduce.
  2. [Abstract] The abstract states that the extended model 'substantially reduce[s] the error in predicted V_max' but supplies no quantitative metrics (e.g., mean fractional error, RMS, or per-halo comparisons before/after the extension). Without these numbers or the corresponding simulation validation plots, the magnitude and statistical significance of the improvement cannot be assessed, undermining evaluation of the central claim.
minor comments (1)
  1. Notation for the accretion delay parameters should be defined explicitly with symbols and ranges when first introduced, rather than left implicit in the description of the extension.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed review of our manuscript. We address each major comment below in a point-by-point manner. We agree that the central assumption is phenomenological and will revise the text to clarify this while preserving the model's practical utility. We will also add quantitative metrics to the abstract.

read point-by-point responses

  1. Referee: [Abstract] Abstract and central assumption: the claim that smooth mass accretion 'drives the SIDM halo back toward a Navarro-Frenk-White (NFW) profile' is introduced phenomenologically without derivation from the underlying gravothermal fluid equations or Boltzmann equation under continuous mass growth. No section demonstrates that the assumed instantaneous NFW reset is consistent with the coupled accretion+self-interaction dynamics; the reported V_max error reduction therefore rests on a functional form calibrated to the same zoom-in runs the model aims to reproduce.

    Authors: We acknowledge that the assumption is introduced phenomenologically rather than derived directly from the gravothermal fluid or Boltzmann equations. The motivation arises from the well-established behavior in CDM, where smooth accretion maintains an NFW-like profile; we posit an analogous restoring effect in SIDM that delays core collapse. The original Yang et al. (2024b) model is itself a calibrated parametric fit, and our extension follows the same philosophy to achieve computational efficiency while improving agreement with the zoom-in suite. We will revise the manuscript to explicitly label the assumption as phenomenological, expand the discussion of its physical motivation and limitations, and note that full consistency with the coupled dynamics would require more expensive fluid simulations beyond the scope of this work. revision: partial

  2. Referee: [Abstract] The abstract states that the extended model 'substantially reduce[s] the error in predicted V_max' but supplies no quantitative metrics (e.g., mean fractional error, RMS, or per-halo comparisons before/after the extension). Without these numbers or the corresponding simulation validation plots, the magnitude and statistical significance of the improvement cannot be assessed, undermining evaluation of the central claim.

    Authors: We agree that the abstract would be strengthened by including explicit quantitative metrics. The full manuscript already contains per-halo comparisons, error reductions, and validation plots against the zoom-in simulations (see Figures 3–5 and associated tables). In the revised version we will update the abstract to report specific measures, such as the reduction in mean fractional error in V_max at z=0 and the RMS improvement relative to the original model, together with references to the relevant figures. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the extended parametric SIDM model derivation

full rationale

The paper extends the existing parametric model of Yang et al. (2024b) by introducing an explicit phenomenological assumption that smooth mass accretion drives SIDM halos back toward NFW profiles, thereby delaying core collapse. This assumption is presented as a modeling choice to address an observed discrepancy between the original model's gravothermal evolution rate and measurements from cosmological zoom-in simulations. The improvement in V_max accuracy is then demonstrated via direct comparison to those same external simulations. No quoted step reduces a claimed prediction or first-principles result to its own inputs by construction, nor does any load-bearing premise rest solely on overlapping-author self-citation. The derivation chain remains self-contained against the external simulation benchmarks, with the extension functioning as an added degree of freedom rather than a tautological redefinition or fitted renaming.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the domain assumption that mass accretion counteracts SIDM gravothermal evolution by restoring NFW profiles; no new particles or forces are introduced, but the parametric form itself depends on calibration choices not detailed in the abstract.

free parameters (1)
  • model parameters controlling accretion delay
    The extended parametric model necessarily introduces or adjusts parameters that encode the strength of the accretion restoring effect; these are fitted or chosen to match simulation trends.
axioms (1)
  • domain assumption Smooth mass accretion drives SIDM halos back toward NFW profiles and thereby delays core collapse
    This is the load-bearing physical assumption added to the original model and is invoked to explain the discrepancy with simulations.

pith-pipeline@v0.9.0 · 5510 in / 1485 out tokens · 45984 ms · 2026-05-09T20:33:07.336773+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

57 extracted references · 42 canonical work pages

  1. [1]

    The Astrophysical Journal , volume=

    Strong dark matter self-interactions diversify halo populations within and surrounding the milky way , author=. The Astrophysical Journal , volume=. 2023 , publisher=

    2023

  2. [2]

    The Astrophysical Journal Letters , volume=

    A Self-interacting Dark Matter Solution to the Extreme Diversity of Low-mass Halo Properties , author=. The Astrophysical Journal Letters , volume=. 2023 , publisher=

    2023

  3. [3]

    Journal of Cosmology and Astroparticle Physics , volume=

    Gravothermal evolution of dark matter halos with differential elastic scattering , author=. Journal of Cosmology and Astroparticle Physics , volume=. 2022 , publisher=

    2022

  4. [4]

    Monthly Notices of the Royal Astronomical Society , volume =

    Turner, Hannah C and Lovell, Mark R and Zavala, Jesús and Vogelsberger, Mark , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2021 , month =. doi:10.1093/mnras/stab1725 , url =

    work page doi:10.1093/mnras/stab1725 2021

  5. [5]

    The Astrophysical Journal , volume=

    Statistical properties of x-ray clusters: Analytic and numerical comparisons , author=. The Astrophysical Journal , volume=. 1998 , publisher=

    1998

  6. [6]

    Annual Review of Astronomy and Astrophysics , volume=

    Streams, substructures, and the early history of the Milky Way , author=. Annual Review of Astronomy and Astrophysics , volume=. 2020 , publisher=

    2020

  7. [7]

    Distinguishing dark matter annihilation enhancement scenarios via halo shapes , journal =

    Masahiro Ibe and Hai-Bo Yu , keywords =. Distinguishing dark matter annihilation enhancement scenarios via halo shapes , journal =. 2010 , issn =. doi:https://doi.org/10.1016/j.physletb.2010.07.026 , url =

    work page doi:10.1016/j.physletb.2010.07.026 2010

  8. [8]

    arXiv preprint arXiv:2406.10753 , year=

    Testing the parametric model for self-interacting dark matter using matched halos in cosmological simulations , author=. arXiv preprint arXiv:2406.10753 , year=

    work page arXiv

  9. [9]

    and Yu, Hai-Bo and Zhong, Yi-Ming , year=

    Yang, Daneng and Nadler, Ethan O. and Yu, Hai-Bo and Zhong, Yi-Ming , year=. A parametric model for self-interacting dark matter halos , volume=. Journal of Cosmology and Astroparticle Physics , publisher=. doi:10.1088/1475-7516/2024/02/032 , number=

    work page doi:10.1088/1475-7516/2024/02/032 2024

  10. [10]

    , keywords =

    Boylan-Kolchin, Michael and Bullock, James S. and Kaplinghat, Manoj , title =. Monthly Notices of the Royal Astronomical Society: Letters , volume =. 2011 , month =. doi:10.1111/j.1745-3933.2011.01074.x , url =

    work page doi:10.1111/j.1745-3933.2011.01074.x 2011

  11. [11]

    , keywords =

    Klypin, Anatoly and Kravtsov, Andrey V. and Valenzuela, Octavio and Prada, Francisco , title =. The Astrophysical Journal , abstract =. 1999 , month =. doi:10.1086/307643 , url =

    work page doi:10.1086/307643 1999

  12. [12]

    and Navarro, Julio F

    Ludlow, Aaron D. and Navarro, Julio F. and Boylan-Kolchin, Michael and Bett, Philip E. and Angulo, Raúl E. and Li, Ming and White, Simon D. M. and Frenk, Carlos and Springel, Volker , year=. The mass profile and accretion history of cold dark matter haloes , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/stt526 ...

    work page doi:10.1093/mnras/stt526

  13. [13]

    Observational Evidence for Self-Interacting Cold Dark Matter , author =. Phys. Rev. Lett. , volume =. 2000 , month =. doi:10.1103/PhysRevLett.84.3760 , url =

    work page doi:10.1103/physrevlett.84.3760 2000

  14. [14]

    Nature , volume=

    Evidence against dissipation-less dark matter from observations of galaxy haloes , author=. Nature , volume=. 1994 , publisher=

    1994

  15. [15]

    The Astrophysical Journal , volume=

    Self-interacting dark matter halos and the gravothermal catastrophe , author=. The Astrophysical Journal , volume=. 2002 , publisher=

    2002

  16. [16]

    Monthly Notices of the Royal Astronomical Society , volume=

    Simulations of X-ray clusters , author=. Monthly Notices of the Royal Astronomical Society , volume=. 1995 , publisher=

    1995

  17. [17]

    , year = 1997, month = dec, volume = 490, pages =

    Navarro, Julio F. and Frenk, Carlos S. and White, Simon D. M. , year=. A Universal Density Profile from Hierarchical Clustering , volume=. The Astrophysical Journal , publisher=. doi:10.1086/304888 , number=

    work page doi:10.1086/304888

  18. [18]

    A., Navarro, J

    Oman, Kyle A. and Navarro, Julio F. and Fattahi, Azadeh and Frenk, Carlos S. and Sawala, Till and White, Simon D. M. and Bower, Richard and Crain, Robert A. and Furlong, Michelle and Schaller, Matthieu and Schaye, Joop and Theuns, Tom , year=. The unexpected diversity of dwarf galaxy rotation curves , volume=. Monthly Notices of the Royal Astronomical Soc...

    work page doi:10.1093/mnras/stv1504

  19. [19]

    The Astrophysical Journal , volume=

    A universal mass profile for dwarf spheroidal galaxies? , author=. The Astrophysical Journal , volume=. 2009 , publisher=

    2009

  20. [20]

    S., Wechsler, R

    Behroozi, Peter S. and Wechsler, Risa H. and Wu, Hao-Yi and Busha, Michael T. and Klypin, Anatoly A. and Primack, Joel R. , year=. GRAVITATIONALLY CONSISTENT HALO CATALOGS AND MERGER TREES FOR PRECISION COSMOLOGY , volume=. The Astrophysical Journal , publisher=. doi:10.1088/0004-637x/763/1/18 , number=

    work page doi:10.1088/0004-637x/763/1/18

  21. [21]

    S., Wechsler , R

    Behroozi, Peter S. and Wechsler, Risa H. and Wu, Hao-Yi , year=. THE ROCKSTAR PHASE-SPACE TEMPORAL HALO FINDER AND THE VELOCITY OFFSETS OF CLUSTER CORES , volume=. The Astrophysical Journal , publisher=. doi:10.1088/0004-637x/762/2/109 , number=

    work page doi:10.1088/0004-637x/762/2/109

  22. [22]

    Velocity-dependent self-interacting dark matter from groups and clusters of galaxies , volume=

    Sagunski, Laura and Gad-Nasr, Sophia and Colquhoun, Brian and Robertson, Andrew and Tulin, Sean , year=. Velocity-dependent self-interacting dark matter from groups and clusters of galaxies , volume=. Journal of Cosmology and Astroparticle Physics , publisher=. doi:10.1088/1475-7516/2021/01/024 , number=

    work page doi:10.1088/1475-7516/2021/01/024 2021

  23. [23]

    Universal gravothermal evolution of isolated self-interacting dark matter halos for velocity-dependent cross-sections , volume=

    Outmezguine, Nadav Joseph and Boddy, Kimberly K and Gad-Nasr, Sophia and Kaplinghat, Manoj and Sagunski, Laura , year=. Universal gravothermal evolution of isolated self-interacting dark matter halos for velocity-dependent cross-sections , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/stad1705 , number=

    work page doi:10.1093/mnras/stad1705

  24. [24]

    and Yu, Hai-Bo and Zhong, Yi-Ming , year=

    Essig, Rouven and McDermott, Samuel D. and Yu, Hai-Bo and Zhong, Yi-Ming , year=. Constraining Dissipative Dark Matter Self-Interactions , volume=. Physical Review Letters , publisher=. doi:10.1103/physrevlett.123.121102 , number=

    work page doi:10.1103/physrevlett.123.121102

  25. [25]

    Theevolutionofbinaryfractionsinglobularclusters,

    Springel, Volker , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2005 , month =. doi:10.1111/j.1365-2966.2005.09655.x , url =

    work page doi:10.1111/j.1365-2966.2005.09655.x 2005

  26. [26]

    Nadler, Ethan O. and Mansfield, Philip and Wang, Yunchong and Du, Xiaolong and Adhikari, Susmita and Banerjee, Arka and Benson, Andrew and Darragh-Ford, Elise and Mao, Yao-Yuan and Wagner-Carena, Sebastian and Wechsler, Risa H. and Wu, Hao-Yi , year=. Symphony: Cosmological Zoom-in Simulation Suites over Four Decades of Host Halo Mass , volume=. The Astro...

    work page doi:10.3847/1538-4357/acb68c

  27. [27]

    , title =

    Zavala, Jesús and Vogelsberger, Mark and Walker, Matthew G. , title =. Monthly Notices of the Royal Astronomical Society: Letters , volume =. 2013 , month =. doi:10.1093/mnrasl/sls053 , url =

    work page doi:10.1093/mnrasl/sls053 2013

  28. [28]

    Dark Matter Halos as Particle Colliders: Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters , author =. Phys. Rev. Lett. , volume =. 2016 , month =. doi:10.1103/PhysRevLett.116.041302 , url =

    work page doi:10.1103/physrevlett.116.041302 2016

  29. [29]

    Comprehensiveanalyticformulaeforstellarevolutionasafunctionofmassandmetallicity,

    Hierarchical galaxy formation. , keywords =. doi:10.1046/j.1365-8711.2000.03879.x , archivePrefix =. astro-ph/0007281 , primaryClass =

    work page doi:10.1046/j.1365-8711.2000.03879.x 2000

  30. [30]

    The physical origin of the universal function

    Correa, Camila A. and Wyithe, J. Stuart B. and Schaye, Joop and Duffy, Alan R. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2015 , month =. doi:10.1093/mnras/stv689 , url =

    work page doi:10.1093/mnras/stv689 2015

  31. [31]

    Nature Astronomy , keywords =

    Baryonic solutions and challenges for cosmological models of dwarf galaxies , author=. Nature Astronomy , volume=. 2022 , publisher=. doi:10.1038/s41550-022-01689-w , number=

    work page doi:10.1038/s41550-022-01689-w 2022

  32. [32]

    Mao, Yao-Yuan and Williamson, Marc and Wechsler, Risa H. , year=. THE DEPENDENCE OF SUBHALO ABUNDANCE ON HALO CONCENTRATION , volume=. The Astrophysical Journal , publisher=. doi:10.1088/0004-637x/810/1/21 , number=

    work page doi:10.1088/0004-637x/810/1/21

  33. [33]

    and Kaplinghat, Manoj , year=

    Nishikawa, Hiroya and Boddy, Kimberly K. and Kaplinghat, Manoj , year=. Accelerated core collapse in tidally stripped self-interacting dark matter halos , volume=. Physical Review D , publisher=. doi:10.1103/physrevd.101.063009 , number=

    work page doi:10.1103/physrevd.101.063009

  34. [34]

    2025 , eprint=

    Calibrating the SIDM Gravothermal Catastrophe with N-body Simulations , author=. 2025 , eprint=

    2025

  35. [35]

    , keywords =

    Bullock, James S. and Boylan-Kolchin, Michael , year=. Small-Scale Challenges to the ΛCDM Paradigm , volume=. Annual Review of Astronomy and Astrophysics , publisher=. doi:10.1146/annurev-astro-091916-055313 , number=

    work page doi:10.1146/annurev-astro-091916-055313

  36. [36]

    Collins, Michelle L. M. and Read, Justin I. , year=. Observational constraints on stellar feedback in dwarf galaxies , volume=. Nature Astronomy , publisher=. doi:10.1038/s41550-022-01657-4 , number=

    work page doi:10.1038/s41550-022-01657-4

  37. [37]

    Baryonic clues to the puzzling diversity of dwarf galaxy rotation curves , volume=

    Santos-Santos, Isabel M E and Navarro, Julio F and Robertson, Andrew and Benítez-Llambay, Alejandro and Oman, Kyle A and Lovell, Mark R and Frenk, Carlos S and Ludlow, Aaron D and Fattahi, Azadeh and Ritz, Adam , year=. Baryonic clues to the puzzling diversity of dwarf galaxy rotation curves , volume=. Monthly Notices of the Royal Astronomical Society , p...

    work page doi:10.1093/mnras/staa1072

  38. [38]

    R., Hopkins P

    Wetzel, Andrew R. and Hopkins, Philip F. and Kim, Ji-hoon and Faucher-Giguère, Claude-André and Kereš, Dušan and Quataert, Eliot , year=. RECONCILING DWARF GALAXIES WITH ΛCDM COSMOLOGY: SIMULATING A REALISTIC POPULATION OF SATELLITES AROUND A MILKY WAY–MASS GALAXY , volume=. The Astrophysical Journal Letters , publisher=. doi:10.3847/2041-8205/827/2/l23 , number=

    work page doi:10.3847/2041-8205/827/2/l23 2041

  39. [39]

    The Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations , volume=

    Garrison-Kimmel, Shea and Hopkins, Philip F and Wetzel, Andrew and Bullock, James S and Boylan-Kolchin, Michael and Kereš, Dušan and Faucher-Giguère, Claude-André and El-Badry, Kareem and Lamberts, Astrid and Quataert, Eliot and Sanderson, Robyn , year=. The Local Group on FIRE: dwarf galaxy populations across a suite of hydrodynamic simulations , volume=...

    work page doi:10.1093/mnras/stz1317

  40. [40]

    and Kong, Demao and Yang, Daneng and Yu, Hai-Bo , year=

    Nadler, Ethan O. and Kong, Demao and Yang, Daneng and Yu, Hai-Bo , year=. SIDM Concerto: Compilation and Data Release of Self-interacting Dark Matter Zoom-in Simulations , volume=. The Astrophysical Journal , publisher=. doi:10.3847/1538-4357/adf553 , number=

    work page doi:10.3847/1538-4357/adf553

  41. [41]

    Reconciling the Diversity and Uniformity of Galactic Rotation Curves with Self-Interacting Dark Matter , volume=

    Ren, Tao and Kwa, Anna and Kaplinghat, Manoj and Yu, Hai-Bo , year=. Reconciling the Diversity and Uniformity of Galactic Rotation Curves with Self-Interacting Dark Matter , volume=. Physical Review X , publisher=. doi:10.1103/physrevx.9.031020 , number=

    work page doi:10.1103/physrevx.9.031020

  42. [42]

    Monthly Notices of the Royal Astronomical Society , volume =

    Silverman, Maya and Bullock, James S and Kaplinghat, Manoj and Robles, Victor H and Valli, Mauro , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =. doi:10.1093/mnras/stac3232 , url =

    work page doi:10.1093/mnras/stac3232 2022

  43. [43]

    Escalating core formation with dark matter self-heating , author =. Phys. Rev. D , volume =. 2020 , month =. doi:10.1103/PhysRevD.102.043009 , url =

    work page doi:10.1103/physrevd.102.043009 2020

  44. [44]

    A., et al

    Vegetti, S. and Koopmans, L. V. E. and Bolton, A. and Treu, T. and Gavazzi, R. , year=. Detection of a dark substructure through gravitational imaging: Detection of a dark substructure , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1111/j.1365-2966.2010.16865.x , number=

    work page doi:10.1111/j.1365-2966.2010.16865.x 2010

  45. [45]

    An unexpected high concentration for the dark substructure in the gravitational lens SDSSJ0946+1006 , volume=

    Minor, Quinn and Gad-Nasr, Sophia and Kaplinghat, Manoj and Vegetti, Simona , year=. An unexpected high concentration for the dark substructure in the gravitational lens SDSSJ0946+1006 , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/stab2247 , number=

    work page doi:10.1093/mnras/stab2247

  46. [46]

    and Fassnacht, Christopher D

    Despali, Giulia and Heinze, Felix M. and Fassnacht, Christopher D. and Vegetti, Simona and Spingola, Cristiana and Klessen, Ralf and Tajalli, Maryam , year=. Detecting low-mass haloes with strong gravitational lensing: II. Constraints on the density profiles of two detected subhaloes , volume=. doi:10.1051/0004-6361/202451546 , journal=

    work page doi:10.1051/0004-6361/202451546

  47. [47]

    SHARP–IX

    Tajalli, M and Vegetti, S and O’Riordan, C M and White, S D M and Fassnacht, C D and Powell, D M and McKean, J P and Despali, G , year=. SHARP–IX. The dense, low-mass perturbers in B1938+666 and J0946+1006: implications for cold and self-interacting dark matter , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/st...

    work page doi:10.1093/mnras/staf1357

  48. [48]

    Monthly Notices of the Royal Astronomical Society , volume=

    The overconcentrated dark halo in the strong lens SDSS J0946+ 1006 is a subhalo: evidence for self-interacting dark matter? , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2025 , publisher=. doi:10.1093/mnras/staf697 , number=

    work page doi:10.1093/mnras/staf697 2025

  49. [49]

    The Astrophysical Journal , volume=

    The Spur and the Gap in GD-1: Dynamical evidence for a dark substructure in the Milky Way halo , author=. The Astrophysical Journal , volume=. 2019 , publisher=

    2019

  50. [50]

    2025 , eprint=

    Strong Lensing Perturbers from the SIDM Concerto Suite , author=. 2025 , eprint=

    2025

  51. [51]

    2025 , eprint=

    Measurement of Dark Matter Substructure from the Kinematics of the GD-1 Stellar Stream , author=. 2025 , eprint=

    2025

  52. [52]

    2026 , eprint=

    MARVELously Dark: the gravothermal evolution of dwarf halos in velocity-dependent SIDM , author=. 2026 , eprint=

    2026

  53. [53]

    and An, Rui and Yang, Daneng and Yu, Hai-Bo and Benson, Andrew and Gluscevic, Vera , year=

    Nadler, Ethan O. and An, Rui and Yang, Daneng and Yu, Hai-Bo and Benson, Andrew and Gluscevic, Vera , year=. COZMIC. III. Cosmological Zoom-in Simulations of Self-interacting Dark Matter with Suppressed Initial Conditions , volume=. The Astrophysical Journal , publisher=. doi:10.3847/1538-4357/adce82 , number=

    work page doi:10.3847/1538-4357/adce82

  54. [54]

    Grant and Kaplinghat, Manoj and Valli, Mauro and Yu, Hai-Bo , year=

    Roberts, M. Grant and Kaplinghat, Manoj and Valli, Mauro and Yu, Hai-Bo , year=. Gravothermal collapse and the diversity of galactic rotation curves , volume=. Physical Review D , publisher=. doi:10.1103/physrevd.111.103041 , number=

    work page doi:10.1103/physrevd.111.103041

  55. [55]

    2018, Phys

    Tulin, Sean and Yu, Hai-Bo , year=. Dark matter self-interactions and small scale structure , volume=. doi:10.1016/j.physrep.2017.11.004 , journal=

    work page doi:10.1016/j.physrep.2017.11.004 2017

  56. [56]

    , title =

    Zhang, Xingyu and Yu, Hai-Bo and Yang, Daneng and Nadler, Ethan O. , title =. The Astrophysical Journal Letters , abstract =. 2025 , month =. doi:10.3847/2041-8213/ada02b , url =

    work page doi:10.3847/2041-8213/ada02b 2025

  57. [57]

    2025 , eprint=

    Three Birds with One Stone: Core-Collapsed SIDM Halos as the Common Origin of Dense Perturbers in Lenses, Streams, and Satellites , author=. 2025 , eprint=

    2025