Cosmological simulations with suppressed small-scale power

Beyond-CDM Simulation Compilation

Warm, fuzzy, interacting and mixed dark matter runs, placed by the mass they simulate and the particle mass that resolves it, next to each model's transfer function T²(k) = PX/PCDM. Hover a marker to see the wavenumbers that run resolves, click to pin it, and press play to watch the field grow.

–papers
–simulations
–transfer functions

TimelineOne square per paper

Drag across the years to filter, or press play.

aResolution of each simulation

Diagonals: particles in the host or box, N = M/mDM

bThe same models as T²(k)

Bold where each run resolves them

Papers

Click a row to highlight its simulations.

Transfer functions

  • Thermal WDM: Viel+05, or Bode+01 and Lovell+14 (ν = 1) where the paper used them.
  • Sterile neutrinos: the thermal relic with the same half-mode wavenumber (approximate). Runs without a compiled T(k) appear in panel a only.
  • FDM: Hu, Barkana & Gruzinov 2000.
  • DM–baryon scattering and ETHOS: Bohr+20 shapes with example parameters, no second peak (approximate).
  • Mixed cold + warm or fuzzy: (1 − f) + f TX (approximate).

Hollow bold segments mark approximate transfer functions. Suites that sample a range of models are drawn as a shaded band, or as the two edge models for oscillating DAO shapes.

Resolved wavenumbers

k(M) = π / RL(M),   M = (4π/3) ρ̄m RL³

Mlim = 10.1 ρ̄m d kpeak−2 is the Wang & White (2007) spurious-halo mass, with d the mean interparticle spacing and kpeak the peak of Δ²(k). The halo-mass axis above each small multiple uses the same k(M).

What is counted

Markers group runs of one suite that share family, run type, simulated mass and particle mass to 0.1 dex. Marker area grows as √N, capped at 300 runs so the largest suites do not bury the rest.