Pith. sign in

REVIEW 1 major objections 5 minor 172 references

A new AREPO-2 SIDM module decouples scattering from gravity so multiple collisions per step stay conserved and cheap.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · grok-4.5

2026-07-11 06:36 UTC pith:OGBCXMAG

load-bearing objection Solid methods paper: dedicated DM tree + multi-scatter MPI makes AREPO-2 SIDM practical for hierarchical gravity and deep core collapse, with thorough validation and real speedups. the 1 major comments →

arxiv 2607.05504 v1 pith:OGBCXMAG submitted 2026-07-06 astro-ph.CO astro-ph.HEhep-phhep-th

A Novel Implementation of Self-Interacting Dark Matter in AREPO

Oliver Zier , Xuejian Shen , Vinh Tran , Martin Rosenlyst , Mark Vogelsberger , Rongrong Liu This is my paper
classification astro-ph.CO astro-ph.HEhep-phhep-th
keywords self-interacting dark matterMonte-Carlo N-bodyAREPOgravothermal core collapsehierarchical time integrationneighbour treevelocity-dependent cross-sectioncosmological simulations
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Self-interacting dark matter can reshape galaxy cores and later drive dense core collapse, but simulating it accurately and cheaply has been hard, especially once many particles scatter more than once in a single time step. This paper presents a Monte-Carlo SIDM solver for the moving-mesh code AREPO-2 whose central design is a dedicated dark-matter-only neighbour tree, so scattering no longer reuses the gravity tree. That change keeps the code compatible with hierarchical gravity time integration and lets the optimized gravity solver run unconstrained. A pairwise MPI exchange updates particle velocities after every accepted scatter, conserving momentum and energy to machine precision while allowing multiple events per step; a per-pair time-step criterion then avoids the far stricter total-probability limits of earlier schemes. The module supports velocity-dependent and inelastic cross-sections through a four-function user interface that hides the parallel layer. Idealized beam, thermalization, isolated-halo and cosmological tests match analytic or fluid benchmarks and the previous AREPO-1 implementation, while wall-clock cost stays only modestly above pure cold dark matter except deep in core collapse, where the new code remains far cheaper.

Core claim

The authors show that a Monte-Carlo SIDM implementation built around a dedicated DM-only neighbour tree, ordered pairwise MPI communication that reloads the latest particle state after every accepted scatter, and a per-pair time-step criterion (C_SIDM = 0.1) conserves momentum and energy to machine precision, reproduces analytic and gravothermal-fluid benchmarks, matches the legacy AREPO-1 SIDM results, and incurs only modest overhead relative to CDM except in late core collapse (where it remains substantially faster than AREPO-1).

What carries the argument

Dedicated DM-only neighbour-search tree plus pairwise MPI protocol: the tree decouples scattering from gravity so hierarchical time integration remains usable; the protocol processes remote pairs one task-pair at a time, reloading the export-buffer state before each successive scatter on an imported particle, thereby keeping multi-scatter kinematics self-consistent and conserving momentum and energy by construction.

Load-bearing premise

That the one-sided cubic-spline kernel with a fixed neighbour count of roughly 32, together with the continuum Monte-Carlo rate formula, still gives an unbiased approximation to the true collision physics even when the mean free path becomes much shorter than the gravitational scale height and many particles scatter repeatedly inside one time step.

What would settle it

Evolve the same isolated NFW halo deep into core collapse with both this module and an independent high-resolution Boltzmann or calibrated fluid solver; a statistically significant mismatch in core-density evolution or energy conservation once the Knudsen number falls well below unity would falsify the claim that the scheme remains accurate in the short-mean-free-path regime.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Isolated and cosmological SIDM runs that reach the late core-collapse phase become practical at resolutions previously limited by time-step cost.
  • Full-physics cosmological boxes that include both SIDM and baryons can reuse the hierarchical gravity solver without the order-of-magnitude slowdown of the older gravity-tree neighbour search.
  • Velocity-dependent and inelastic SIDM models can be added by writing only four user functions, without re-engineering the parallel layer.
  • Performance overhead relative to pure CDM stays modest outside deep collapse, making large-volume SIDM survey suites cheaper than before.

Where Pith is reading between the lines

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

  • Because the neighbour tree is already dynamic and shared-memory aware, the same infrastructure can later host other short-range non-gravitational DM interactions (e.g., drag or effective-force schemes) with little extra engineering.
  • The per-pair time-step criterion may allow controlled exploration of the short-mean-free-path regime at mass resolutions still affordable for zoom-in galaxy simulations, tightening empirical calibration of fluid conductivity parameters.
  • Once core-collapse densities become routinely reachable, the module supplies a ready numerical laboratory for testing whether dense SIDM subhaloes can explain the concentrated perturbers inferred from stellar streams and strong lenses.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 5 minor

Summary. The paper presents a new Monte-Carlo SIDM module for AREPO-2. Its main design choices are a dedicated DM-only neighbour tree that decouples scattering from gravity (preserving hierarchical time integration), a pairwise MPI protocol that updates particle states after every accepted scatter so multiple events per step conserve momentum and energy by construction, and a per-pair timestep criterion (C_SIDM=0.1) that is far less restrictive than the total-probability limit used in AREPO-1. The module supports velocity-dependent and inelastic cross-sections through a four-function interface. Validation covers isotropic elastic scattering: beam deflection on a lattice, Maxwellian thermalization (including a Yukawa-type VDCS) against an independent Boltzmann solver, isolated NFW core collapse against a calibrated gravothermal fluid model and against AREPO-1, MW-mass zoom-ins, and 25 cMpc boxes at three resolutions with and without baryons. Performance tests show modest overhead relative to CDM outside late core collapse and substantially lower cost than the legacy AREPO-1 SIDM implementation, especially once baryons force a deep timestep hierarchy.

Significance. If the results hold, this is a solid, practically important methods contribution for the SIDM community. Late-time gravothermal core collapse is currently of high observational interest (dense substructures in lenses and streams; possible DM-seeded black holes), and existing Monte-Carlo implementations become prohibitively expensive precisely in that regime. The multi-scatter MPI scheme, per-pair timestep, and gravity-decoupled neighbour tree make that regime tractable while remaining compatible with modern AREPO-2 gravity and full-physics galaxy formation. The public Boltzmann solver and SoftIsoICs generator, the explicit conservation properties, and the clear extensibility interface are concrete strengths that raise the bar for subsequent SIDM modules.

major comments (1)
  1. The continuum validity of the one-sided cubic-spline estimator (Eq. 14, N_ngb=32±5) deep in the SMFP core-collapse regime (Kn≪1) remains the softest load-bearing point of the “deep-collapse tractability” claim. Table 1 footnote a and §2.3.1 already state that unbiasedness then requires prohibitively fine resolution; the N-body–fluid comparison (Figs. 8, B1) uses a fluid model whose LMFP conductivity is itself calibrated to N-body (C_κ=0.8, §B2). Agreement past Kn=1 is therefore only a partial, non-independent check of the SMFP asymptote. This is a known limitation of the Monte-Carlo class, not a coding error, but the manuscript should state more explicitly in the abstract/conclusions which density range of the collapse phase is considered reliable at the resolutions used, and what additional resolution or alternative estimator (e.g. the overlap kernel of App. A, or the drag-force scheme
minor comments (5)
  1. Fig. 13 (bottom) and the associated text in §6.1 make the wall-clock advantage during runaway collapse clear; a short quantitative statement of the density ratio reached at equal cost (already visible in the figure) would help readers who only skim the text.
  2. The four-function user interface (§4.6) is a genuine strength; a one-line example of how an anisotropic or inelastic model would be registered would make the extensibility claim more concrete for potential users.
  3. In §4.4, the comparison of the new per-pair criterion with the AREPO-1 total-probability limit (Eqs. 18–22) is useful; stating the numerical factor Δt_old/Δt_new ~ 10^{-2} already in the main text (rather than only in the derivation) would help non-specialist readers.
  4. Typos / notation: “arepo-2” / “AREPO-2” capitalization is inconsistent across abstract and body; “gravothermal” vs “gravothermal-fluid” is fine but the fluid-model reference (Outmezguine et al. 2023; Gad-Nasr et al. 2024) should be cited at first mention in §5.3 as well as in App. B.
  5. Table 2: the baryonic full-physics run is only at 2×256^{3}; a brief caveat that the order-of-magnitude speed-up relative to AREPO-1 may change at higher resolution (deeper hierarchy) would be prudent.

Circularity Check

1 steps flagged

Methods paper with external analytic/Boltzmann/fluid benchmarks and free-parameter variation; only minor self-referential calibration of the fluid conductivity used as a check, not a forced prediction.

specific steps
  1. fitted input called prediction [Appendix B2 / Fig. B1 / Eq. (B16)]
    "We find that C_κ = 0.8 gives the best agreement with the N-body benchmark in both collapse time and late-time behaviour (Figure B1); the corresponding core-density evolution is also shown in Figure 8. ... In the LMFP regime ... the fluid approximation requires a calibration parameter C_κ, fitted so that the heat flux matches that measured in N-body simulations"

    The fluid model’s LMFP conductivity is explicitly fitted (C_κ = 0.8) to N-body heat flux before the same fluid solution is plotted as a reference for the N-body core-collapse runs. The late-time visual agreement is therefore partly by construction for the LMFP segment; the paper acknowledges the need for calibration and does not claim a parameter-free first-principles match. This is a minor, field-standard check rather than a load-bearing circular prediction.

full rationale

This is a numerical-methods contribution whose correctness claims rest on (i) analytic beam-deflection and isotropic angular distributions, (ii) an independent kinetic Boltzmann solver for thermalization (publicly released), (iii) energy/momentum conservation to machine precision by construction of the pairwise update, (iv) direct comparison to the legacy AREPO-1 SIDM module on identical ICs, and (v) performance scaling against pure CDM. Free numerical parameters (C_SIDM, N_ngb, η, kernel choice) are varied and shown not to alter the macroscopic outcome within the tested range. The sole mild self-reference is the conventional calibration of the gravothermal-fluid conductivity parameter C_κ against N-body data before using the fluid solution as a visual benchmark for core collapse; the paper itself states that such calibration is required and does not present the fluid agreement as an independent first-principles derivation. No uniqueness theorem, ansatz smuggled via self-citation, or fitted parameter re-used as a prediction appears. Score 1 reflects only that minor calibration step; the central implementation claims remain externally falsifiable.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central claim is algorithmic correctness and efficiency of a Monte-Carlo SIDM solver. It rests on standard kinetic-theory and N-body assumptions plus a handful of numerical control parameters whose values are stated and varied. No new physical entities are postulated; the free parameters are pure numerical knobs.

free parameters (4)
  • C_SIDM = 0.1
    Dimensionless safety factor in the per-pair timestep criterion (Eq. 18); fiducial value 0.1 chosen so that pairwise scatter probability remains ≪1. Varied up to 5 in thermalization tests.
  • N_ngb = 32±5
    Target neighbour number for adaptive smoothing length; fiducial 32±5. Varied 16–64 in validation.
  • C_κ = 0.8
    Calibration constant in the LMFP heat conductivity of the reference gravothermal fluid model; set to 0.8 to match N-body collapse time.
  • η (gravity timestep) = 0.005
    Accuracy parameter in gravitational timestep criterion; set to 0.005 after convergence tests for the short collapse timescale used.
axioms (4)
  • domain assumption The Monte-Carlo pairwise scatter rate with one-sided or overlap kernel converges to the continuum Boltzmann collision operator for large particle number and small smoothing length.
    Stated in §2.2–2.3 and §4.2; standard in the SIDM N-body literature but known to require fine resolution in the SMFP regime.
  • domain assumption Elastic isotropic scattering with the total cross-section σ (rather than σ_T or σ_V) is an adequate description for the validation suite.
    Used throughout §5; velocity-dependent and inelastic channels are supported but not exercised in the main tests.
  • domain assumption Hierarchical operator-splitting time integration of Springel et al. (2021) remains symplectic and accurate when SIDM kicks are inserted after the second half-kick.
    Assumed in §3.2 and §4; compatibility is a design goal of the dedicated tree.
  • standard math Standard mathematical properties of the cubic-spline kernel and of MPI collective/pairwise communication.
    Used for rate estimation and parallel consistency proofs.

pith-pipeline@v1.1.0-grok45 · 44004 in / 2881 out tokens · 29140 ms · 2026-07-11T06:36:40.922970+00:00 · methodology

0 comments
read the original abstract

Self-interacting dark matter (SIDM) influences halo structure through collisional heat transport and may solve several small-scale puzzles in structure formation. SIDM creates thermalized cores in low-mass haloes, which may account for the observed cored dwarf galaxies. During late-time gravothermal core collapse, SIDM can produce dense low-mass DM haloes and substructures detected through perturbations to cold stellar streams and strong gravitational lenses. In this work, we present a new Monte-Carlo SIDM implementation in the moving-mesh code AREPO-2, designed for efficiency, scalability, and extensibility. The central feature of the implementation is a dedicated DM-only neighbour-search tree that decouples the scattering solver from gravity. This preserves compatibility with the hierarchical time integration used by AREPO-2 while leaving the optimized gravity solver unconstrained. A pairwise communication scheme between MPI tasks allows tracking multiple scattering events in a single timestep while conserving momentum and energy and maintaining parallel consistency by construction. This is complemented by a per-pair timestep criterion that significantly reduces unnecessary timestep restrictions. The implementation natively supports velocity-dependent cross-sections and inelastic interactions, while a compact interface is designed for additional SIDM physics to be implemented without knowledge of the parallelization layer. We validate the implementation for isotropic, elastic scattering using a suite of idealized and cosmological tests. We assess performance and scalability in isolated core-collapse simulations and in cosmological boxes, both DM-only and with baryons. Except during the late stages of gravothermal collapse, SIDM simulations incur only modest overhead relative to the corresponding CDM runs and are substantially faster than the previous SIDM implementation in AREPO-1.

Figures

Figures reproduced from arXiv: 2607.05504 by Mark Vogelsberger, Martin Rosenlyst, Oliver Zier, Rongrong Liu, Vinh Tran, Xuejian Shen.

Figure 1
Figure 1. Figure 1: Control flow of the per-timestep SIDM scattering operation in arepo-2, read left to right. It traces the steps the module performs each timestep for the dark-matter particles that are active, starting just after the gravity solver’s second half-step kick. In the legend (top), rounded boxes are local computations, green diamonds are decisions, parallelograms are exchanges between parallel processes, and blu… view at source ↗
Figure 2
Figure 2. Figure 2: Scattering operation for a pair of DM particles in the Monte-Carlo scheme in arepo-2. We assume a target neighbour number 𝑁ngb = 8 and a system of equal-mass particles in this illustration. For an accepted pair of particles (𝑖, 𝑗), the scattering deflection angle 𝜃 in the centre-of-momentum frame is drawn randomly according to the differential cross-section. The outgoing centre-of-momentum-frame relative s… view at source ↗
Figure 3
Figure 3. Figure 3: The two approaches to estimate the scattering rate for a candidate pair (𝑖, 𝑗) in arepo-2, illustrated assuming a target neighbour number 𝑁ngb = 8. Left: The fiducial method based on the one-sided kernel (Equation (14)), for which Γˆ (𝑖| 𝑗) depends only on the smoothing length ℎ𝑖 of particle 𝑖 and the partner 𝑗 is weighted by the kernel of 𝑖 alone. Right: The kernel-overlap approach (Equation (15)), for wh… view at source ↗
Figure 4
Figure 4. Figure 4: The consistent pairwise SIDM parallelization adopted in this work. MPI tasks are paired over a sequence of communication sub-steps sorted by their communication costs (left). We highlight four MPI tasks (A–D) that are next to each other in the domain decomposition. For a given pair of tasks (A,B) that share a domain boundary, the boundary particles of A that can “see” particles on B are first sent to B (st… view at source ↗
Figure 6
Figure 6. Figure 6: Top: speed distribution in the thermalization test with 𝑁part = 104 particles, evolved with 𝑁ngb = 16, 32, 64 (dotted, solid, and dashed). Snap￾shots at 𝑇 = 1𝜏col, 2𝜏col, 5𝜏col are shown in purple, cyan, and red. The shaded region shows the fully thermalized MB distribution of Equation (23). Bottom: evolution of the squared speed dispersion for these runs (red), to￾gether with higher- (green) and lower-res… view at source ↗
Figure 7
Figure 7. Figure 7: Similar to the bottom panel of [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Core-density evolution of an isolated halo with mass 𝑀200 = 1010 M⊙ and concentration 𝑐 = 13.08. The core density 𝜌c is normalized to the NFW scale density 𝜌s , while the physical time 𝑇 is normalized to the collapse timescale 𝜏grav of Equation (29). 𝑁200 indicates the number of particles within the virial radius 𝑟200 for each run. The top panel compares the new and old codes with both adaptive individual … view at source ↗
Figure 9
Figure 9. Figure 9: Density profiles of a Milky Way-mass halo at 𝑧 = 6 (top) and 𝑧 = 0 (bottom), for zoom-in simulations in CDM (black) and SIDM (orange: arepo￾1; blue: arepo-2). Shaded bands show the 1𝜎 uncertainties and the dashed vertical line marks the virial radius 𝑟200. The two SIDM implementations are consistent at both redshifts. 0 50 100 150 200 r [kpc] 10 0 10 1 10 2 Ns u b ( < r ) 10 8 10 9 10 10 Msub [M ] 10 0 10 … view at source ↗
Figure 10
Figure 10. Figure 10: Top: cumulative number of subhaloes with 𝑀sub > 107 M⊙ within radius 𝑟 at 𝑧 = 0 for CDM (black) and SIDM (orange: arepo-1; blue: arepo￾2). Bottom: cumulative subhalo mass function (number with mass greater than 𝑀) at 𝑧 = 0 for the same runs. Shaded bands show the 1𝜎 Poisson uncertainties. As expected, the subhalo spatial distribution and mass function agree between the old and new SIDM implementations, wi… view at source ↗
Figure 11
Figure 11. Figure 11: The two SIDM cross-section models used for our cosmological DM-only simulations (Section 5.5): the constant, velocity-independent cross￾section 𝜎/𝑚 = 1 cm2 g −1 and the velocity-dependent AIDA-TNG model (Correa 2021; Despali et al. 2025a), supplied to the module as a tabulated function of the pair relative velocity. Vertical bands mark the characteristic velocities for haloes of mass 1010 , 1012, and 1014… view at source ↗
Figure 12
Figure 12. Figure 12: Median DM density profiles at 𝑧 = 0 in five virial-mass bins of half-width Δ log (𝑀vir/M⊙ ) = 0.5 (left to right), from the DM-only runs with 10243 particles. Each bin is labelled with the numbers of haloes in the CDM and in the arepo-1 (SIDM) and arepo-2 (SIDM) runs. We compare the density profiles in CDM (black), the arepo-1 SIDM implementation (orange), and the arepo-2 SIDM implementation (blue). The u… view at source ↗
Figure 14
Figure 14. Figure 14: Upper panel: total wall-clock time of the DM-only runs (evolved from 𝑧 = 49 to 𝑧 = 0 in a 25 cMpc box) at three resolutions, for CDM (black), the old SIDM implementation in arepo-1 (orange), and the new SIDM implementation in arepo-2 (blue). The dashed grey line indicates lin￾ear growth with the particle number per dimension as a guide to the eye. The measured runtimes rise somewhat faster (∝ 𝑁1.5 1D ), o… view at source ↗

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

172 extracted references · 128 linked inside Pith

  1. [1]

    Minimizing the force error

    Towards optimal softening in three-dimensional N-body codes - I. Minimizing the force error. , keywords =. doi:10.1046/j.1365-8711.2001.04237.x , archivePrefix =. astro-ph/0011568 , primaryClass =

    doi:10.1046/j.1365-8711.2001.04237.x 2001

  2. [2]

    Computer simulation using particles

  3. [3]

    , keywords =

    Hidden sector hydrogen as dark matter: Small-scale structure formation predictions and the importance of hyperfine interactions. , keywords =. doi:10.1103/PhysRevD.94.123017 , archivePrefix =. 1609.03592 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.94.123017

  4. [4]

    , keywords =

    Colliding clusters and dark matter self-interactions. , keywords =. doi:10.1093/mnras/stt2097 , archivePrefix =. 1308.3419 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stt2097

  5. [5]

    , keywords =

    Halo-Shape and Relic-Density Exclusions of Sommerfeld-Enhanced Dark Matter Explanations of Cosmic Ray Excesses. , keywords =. doi:10.1103/PhysRevLett.104.151301 , archivePrefix =. 0911.0422 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.104.151301

  6. [6]

    arXiv e-prints , keywords =

    SHH method for SIDM: An SIDM-hydro hybrid method for simulating self-interacting dark matter. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.10278 , archivePrefix =. 2508.10278 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2508.10278

  7. [7]

    , keywords =

    Universal gravothermal evolution of isolated self-interacting dark matter halos for velocity-dependent cross-sections. , keywords =. doi:10.1093/mnras/stad1705 , archivePrefix =. 2204.06568 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stad1705

  8. [8]

    , keywords =

    Numerical Evolution of Self-Gravitating Halos of Self-Interacting Dark Matter. , keywords =. doi:10.1103/qht7-5tz3 , archivePrefix =. 2506.04334 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/qht7-5tz3

  9. [9]

    , keywords =

    A semi-analytic study of self-interacting dark-matter haloes with baryons. , keywords =. doi:10.1093/mnras/stad705 , archivePrefix =. 2206.12425 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stad705

  10. [10]

    , keywords =

    The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles. , keywords =. doi:10.1093/mnras/staa3954 , archivePrefix =. 2009.07844 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/staa3954 2009

  11. [11]

    arXiv e-prints , keywords =

    First-Principles Formalism for Simulating Self-Interacting Dark Matter. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.17998 , archivePrefix =. 2512.17998 , primaryClass =

    doi:10.48550/arxiv.2512.17998

  12. [12]

    , keywords =

    Subhaloes in self-interacting galactic dark matter haloes. , keywords =. doi:10.1111/j.1365-2966.2012.21182.x , archivePrefix =. 1201.5892 , primaryClass =

    doi:10.1111/j.1365-2966.2012.21182.x 2012

  13. [13]

    , keywords =

    Improving the convergence properties of the moving-mesh code AREPO. , keywords =. doi:10.1093/mnras/stv2380 , archivePrefix =. 1503.00562 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv2380

  14. [14]

    , keywords =

    E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh. , keywords =. doi:10.1111/j.1365-2966.2009.15715.x , archivePrefix =. 0901.4107 , primaryClass =

    doi:10.1111/j.1365-2966.2009.15715.x 2009

  15. [15]

    , keywords =

    The AREPO Public Code Release. , keywords =. doi:10.3847/1538-4365/ab908c , archivePrefix =. 1909.04667 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4365/ab908c 1909

  16. [16]

    , keywords =

    The MillenniumTNG Project: the hydrodynamical full physics simulation and a first look at its galaxy clusters. , keywords =. doi:10.1093/mnras/stac3620 , archivePrefix =. 2210.10060 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stac3620

  17. [17]

    , keywords =

    Moving mesh cosmology: numerical techniques and global statistics. , keywords =. doi:10.1111/j.1365-2966.2012.21590.x , archivePrefix =. 1109.1281 , primaryClass =

    doi:10.1111/j.1365-2966.2012.21590.x 2012

  18. [18]

    , keywords =

    A hierarchical O(N log N) force-calculation algorithm. , keywords =. doi:10.1038/324446a0 , adsurl =

    doi:10.1038/324446a0

  19. [19]

    Journal of Astrophysics and Astronomy , keywords =

    TreePM: A Code for Cosmological N-Body Simulations. Journal of Astrophysics and Astronomy , keywords =. doi:10.1007/BF02702282 , archivePrefix =. astro-ph/9911025 , primaryClass =

    Pith/arXiv arXiv doi:10.1007/bf02702282

  20. [20]

    , keywords =

    Performance characteristics of TreePM codes. , keywords =. doi:10.1016/S1384-1076(03)00056-3 , archivePrefix =. astro-ph/0212129 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/s1384-1076(03)00056-3

  21. [21]

    , keywords =

    Evaporating the Milky Way halo and its satellites with inelastic self-interacting dark matter. , keywords =. doi:10.1093/mnras/stz340 , archivePrefix =. 1805.03203 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stz340

  22. [22]

    , keywords =

    Simulating galactic dust grain evolution on a moving mesh. , keywords =. doi:10.1093/mnras/sty1248 , archivePrefix =. 1805.04521 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty1248

  23. [23]

    , keywords =

    Simulating galaxy formation with black hole driven thermal and kinetic feedback. , keywords =. doi:10.1093/mnras/stw2944 , archivePrefix =. 1607.03486 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw2944

  24. [24]

    , keywords =

    Supermassive black holes and their feedback effects in the IllustrisTNG simulation. , keywords =. doi:10.1093/mnras/sty1733 , archivePrefix =. 1710.04659 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty1733

  25. [25]

    , keywords =

    Simulating cosmic structure formation with the GADGET-4 code. , keywords =. doi:10.1093/mnras/stab1855 , archivePrefix =. 2010.03567 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stab1855 2010

  26. [26]

    , year = 1994, month = aug, volume =

    Evidence against dissipation-less dark matter from observations of galaxy haloes. , year = 1994, month = aug, volume =. doi:10.1038/370629a0 , adsurl =

    doi:10.1038/370629a0 1994

  27. [27]

    , keywords =

    Where Are the Missing Galactic Satellites?. , keywords =. doi:10.1086/307643 , archivePrefix =. astro-ph/9901240 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/307643

  28. [28]

    , keywords =

    The GD-1 Stellar Stream Perturber as a Core-collapsed Self-interacting Dark Matter Halo. , keywords =. doi:10.3847/2041-8213/ada02b , archivePrefix =. 2409.19493 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ada02b 2041

  29. [29]

    , keywords =

    Universal structure of dark matter haloes over a mass range of 20 orders of magnitude. , keywords =. doi:10.1038/s41586-020-2642-9 , archivePrefix =. 1911.09720 , primaryClass =

    doi:10.1038/s41586-020-2642-9 1911

  30. [30]

    , keywords =

    The abundance of dark matter haloes down to Earth mass. , keywords =. doi:10.1093/mnras/stae289 , archivePrefix =. 2310.16093 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stae289

  31. [31]

    , keywords =

    A Universal Density Profile from Hierarchical Clustering. , keywords =. doi:10.1086/304888 , archivePrefix =. astro-ph/9611107 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/304888

  32. [32]

    Planck 2018 results. VI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  33. [33]

    Reviews of Modern Physics , keywords =

    History of dark matter. Reviews of Modern Physics , keywords =. doi:10.1103/RevModPhys.90.045002 , archivePrefix =. 1605.04909 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/revmodphys.90.045002

  34. [34]

    , keywords =

    The Aquarius Project: the subhaloes of galactic haloes. , keywords =. doi:10.1111/j.1365-2966.2008.14066.x , archivePrefix =. 0809.0898 , primaryClass =

    doi:10.1111/j.1365-2966.2008.14066.x 2008

  35. [35]

    , keywords =

    Clumps and streams in the local dark matter distribution. , keywords =. doi:10.1038/nature07153 , archivePrefix =. 0805.1244 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/nature07153

  36. [36]

    , keywords =

    Earth-mass dark-matter haloes as the first structures in the early Universe. , keywords =. doi:10.1038/nature03270 , archivePrefix =. astro-ph/0501589 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/nature03270

  37. [37]

    , keywords =

    Too big to fail? The puzzling darkness of massive Milky Way subhaloes. , keywords =. doi:10.1111/j.1745-3933.2011.01074.x , archivePrefix =. 1103.0007 , primaryClass =

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

  38. [38]

    , keywords =

    The unexpected diversity of dwarf galaxy rotation curves. , keywords =. doi:10.1093/mnras/stv1504 , archivePrefix =. 1504.01437 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv1504

  39. [39]

    , keywords =

    Small-Scale Challenges to the CDM Paradigm. , keywords =. doi:10.1146/annurev-astro-091916-055313 , archivePrefix =. 1707.04256 , primaryClass =

    Pith/arXiv arXiv doi:10.1146/annurev-astro-091916-055313

  40. [40]

    , keywords =

    The APOSTLE simulations: solutions to the Local Group's cosmic puzzles. , keywords =. doi:10.1093/mnras/stw145 , archivePrefix =. 1511.01098 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw145

  41. [41]

    , keywords =

    Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows. , keywords =. doi:10.1038/nature08640 , archivePrefix =. 0911.2237 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/nature08640

  42. [42]

    , keywords =

    How supernova feedback turns dark matter cusps into cores. , keywords =. doi:10.1111/j.1365-2966.2012.20571.x , archivePrefix =. 1106.0499 , primaryClass =

    doi:10.1111/j.1365-2966.2012.20571.x 2012

  43. [43]

    , keywords =

    Observational Evidence for Self-Interacting Cold Dark Matter. , keywords =. doi:10.1103/PhysRevLett.84.3760 , archivePrefix =. astro-ph/9909386 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.84.3760

  44. [44]

    , keywords =

    Halo Properties in Cosmological Simulations of Self-interacting Cold Dark Matter. , keywords =. doi:10.1086/318417 , archivePrefix =. astro-ph/0006218 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/318417

  45. [45]

    , keywords =

    Core formation in dwarf haloes with self-interacting dark matter: no fine-tuning necessary. , keywords =. doi:10.1093/mnras/stv1470 , archivePrefix =. 1412.1477 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv1470

  46. [46]

    , keywords =

    Dark matter self-interactions and small scale structure. , keywords =. doi:10.1016/j.physrep.2017.11.004 , archivePrefix =. 1705.02358 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/j.physrep.2017.11.004 2017

  47. [47]

    , keywords =

    Dark Matter Halos as Particle Colliders: Unified Solution to Small-Scale Structure Puzzles from Dwarfs to Clusters. , keywords =. doi:10.1103/PhysRevLett.116.041302 , archivePrefix =. 1508.03339 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.116.041302

  48. [48]

    , keywords =

    A Test of the Collisional Dark Matter Hypothesis from Cluster Lensing. , keywords =. doi:10.1086/324138 , archivePrefix =. astro-ph/0002050 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/324138

  49. [49]

    Halo shapes versus observations

    Cosmological simulations with self-interacting dark matter - II. Halo shapes versus observations. , keywords =. doi:10.1093/mnras/sts535 , archivePrefix =. 1208.3026 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sts535

  50. [50]

    , keywords =

    Constraints on the Self-Interaction Cross Section of Dark Matter from Numerical Simulations of the Merging Galaxy Cluster 1E 0657-56. , keywords =. doi:10.1086/587859 , archivePrefix =. 0704.0261 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/587859

  51. [51]

    Science , keywords =

    The nongravitational interactions of dark matter in colliding galaxy clusters. Science , keywords =. doi:10.1126/science.1261381 , archivePrefix =. 1503.07675 , primaryClass =

    Pith/arXiv arXiv doi:10.1126/science.1261381

  52. [52]

    , keywords =

    Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential. , keywords =. doi:10.1103/PhysRevLett.106.171302 , archivePrefix =. 1011.6374 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.106.171302

  53. [53]

    , keywords =

    Dark matter self-interactions and light force carriers. , keywords =. doi:10.1103/PhysRevD.81.083522 , archivePrefix =. 0911.3898 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.81.083522

  54. [54]

    , keywords =

    Beyond collisionless dark matter: Particle physics dynamics for dark matter halo structure. , keywords =. doi:10.1103/PhysRevD.87.115007 , archivePrefix =. 1302.3898 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevd.87.115007

  55. [55]

    , keywords =

    Off the Beaten Path: Gaia Reveals GD-1 Stars outside of the Main Stream. , keywords =. doi:10.3847/2041-8213/aad7b5 , archivePrefix =. 1805.00425 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/aad7b5 2041

  56. [56]

    , keywords =

    Gravothermal collapse of isolated self-interacting dark matter haloes: N-body simulation versus the fluid model. , keywords =. doi:10.1111/j.1365-2966.2011.18684.x , archivePrefix =. 1101.3097 , primaryClass =

    doi:10.1111/j.1365-2966.2011.18684.x 2011

  57. [57]

    , keywords =

    What does the Bullet Cluster tell us about self-interacting dark matter?. , keywords =. doi:10.1093/mnras/stw2670 , archivePrefix =. 1605.04307 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw2670

  58. [58]

    , keywords =

    Weakly Self-interacting Dark Matter and the Structure of Dark Halos. , keywords =. doi:10.1086/317306 , archivePrefix =. astro-ph/0006134 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/317306

  59. [59]

    , keywords =

    The Structure and Evolution of Weakly Self-interacting Cold Dark Matter Halos. , keywords =. doi:10.1086/312674 , archivePrefix =. astro-ph/0002409 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/312674

  60. [60]

    , keywords =

    The cosmological simulation code GADGET-2. , keywords =. doi:10.1111/j.1365-2966.2005.09655.x , archivePrefix =. astro-ph/0505010 , primaryClass =

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

  61. [61]

    , keywords =

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx2656

  62. [62]

    , keywords =

    The interplay of self-interacting dark matter and baryons in shaping the halo evolution. , keywords =. doi:10.1093/mnras/stz273 , archivePrefix =. 1811.02569 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stz273

  63. [63]

    , keywords =

    Observable tests of self-interacting dark matter in galaxy clusters: cosmological simulations with SIDM and baryons. , keywords =. doi:10.1093/mnras/stz1815 , archivePrefix =. 1810.05649 , primaryClass =

    doi:10.1093/mnras/stz1815

  64. [64]

    , keywords =

    Introducing the AIDA-TNG project: Galaxy formation in alternative dark matter models. , keywords =. doi:10.1051/0004-6361/202553836 , archivePrefix =. 2501.12439 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202553836

  65. [65]

    , keywords =

    Eight New Milky Way Companions Discovered in First-year Dark Energy Survey Data. , keywords =. doi:10.1088/0004-637X/807/1/50 , archivePrefix =. 1503.02584 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/807/1/50

  66. [66]

    , keywords =

    Eight Ultra-faint Galaxy Candidates Discovered in Year Two of the Dark Energy Survey. , keywords =. doi:10.1088/0004-637X/813/2/109 , archivePrefix =. 1508.03622 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/813/2/109

  67. [67]

    , keywords =

    Missing Satellites Problem: Completeness Corrections to the Number of Satellite Galaxies in the Milky Way are Consistent with Cold Dark Matter Predictions. , keywords =. doi:10.1103/PhysRevLett.121.211302 , archivePrefix =. 1711.06267 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.121.211302

  68. [68]

    , keywords =

    An unexpected high concentration for the dark substructure in the gravitational lens SDSSJ0946+1006. , keywords =. doi:10.1093/mnras/stab2247 , archivePrefix =. 2011.10627 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stab2247 2011

  69. [69]

    , keywords =

    A Robust Mass Estimator for Dark Matter Subhalo Perturbations in Strong Gravitational Lenses. , keywords =. doi:10.3847/1538-4357/aa7fee , archivePrefix =. 1612.05250 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aa7fee

  70. [70]

    , keywords =

    Gravitational imaging through a triple source plane lens: revisiting the CDM-defying dark subhalo in SDSSJ0946+1006. , keywords =. doi:10.1093/mnras/stae514 , archivePrefix =. 2309.04535 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stae514

  71. [71]

    Constraints on the density profiles of two detected subhaloes

    Detecting low-mass haloes with strong gravitational lensing: II. Constraints on the density profiles of two detected subhaloes. , keywords =. doi:10.1051/0004-6361/202451546 , archivePrefix =. 2407.12910 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202451546

  72. [72]

    , keywords =

    The overconcentrated dark halo in the strong lens SDSS J0946 + 1006 is a subhalo: evidence for self-interacting dark matter?. , keywords =. doi:10.1093/mnras/staf697 , archivePrefix =. 2411.08565 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/staf697

  73. [73]

    Science , keywords =

    An excess of small-scale gravitational lenses observed in galaxy clusters. Science , keywords =. doi:10.1126/science.aax5164 , archivePrefix =. 2009.04471 , primaryClass =

    Pith/arXiv arXiv doi:10.1126/science.aax5164 2009

  74. [74]

    , keywords =

    Galaxies in the central regions of simulated galaxy clusters. , keywords =. doi:10.1051/0004-6361/202243651 , archivePrefix =. 2204.09067 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202243651

  75. [75]

    , keywords =

    A persistent excess of galaxy-galaxy strong lensing observed in galaxy clusters. , keywords =. doi:10.1051/0004-6361/202346975 , archivePrefix =. 2309.05799 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202346975

  76. [76]

    , keywords =

    New Cold Dark Matter Crisis Revealed by Multiscale Cluster Lensing. , keywords =. doi:10.3847/2041-8213/ae53ea , archivePrefix =. 2601.07909 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/2041-8213/ae53ea 2041

  77. [77]

    , year = 1968, month = jan, volume =

    The gravo-thermal catastrophe in isothermal spheres and the onset of red-giant structure for stellar systems. , year = 1968, month = jan, volume =. doi:10.1093/mnras/138.4.495 , adsurl =

    doi:10.1093/mnras/138.4.495 1968

  78. [78]

    , keywords =

    The onset of gravothermal core collapse in velocity-dependent self-interacting dark matter subhaloes. , keywords =. doi:10.1093/mnras/stab1725 , archivePrefix =. 2010.02924 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stab1725 2010

  79. [79]

    , keywords =

    The diverse density profiles of galaxy clusters with self-interacting dark matter plus baryons. , keywords =. doi:10.1093/mnrasl/sly024 , archivePrefix =. 1711.09096 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnrasl/sly024

  80. [80]

    , keywords =

    Galactic satellite systems in CDM, WDM and SIDM. , keywords =. doi:10.1093/mnras/stac3062 , archivePrefix =. 2208.07376 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stac3062

Showing first 80 references.