Cosmological simulations of self-interacting dark matter
Every cosmological SIDM simulation in the compilation, placed by its Yukawa cross-section parameters (w, σ0/m) and by the halo it resolves. Hover a marker for the papers behind it, click to pin it, and drag across the timeline to see the field grow.
Drag across the years to filter, or press play.
Bold where each host halo probes them
Diagonals: Nhost = Mhost/mDM
Diagonals: N³ DM particles (Ωm = 0.31, h = 0.68)
Click a row to highlight its simulations.
Constant cross sections correspond to w → ∞ and sit in the shaded strip; within each strip row, markers are packed by host mass, so horizontal position there carries no other meaning. Hollow markers use an approximate (σ0, w) mapping of the paper's own parametrisation (a fit or a Rutherford-like form).
σT(v) = 2σ0(w/v)4 [ln(1 + v²/w²) − (v²/w²)/(1 + v²/w²)]
which tends to σ0 for v ≪ w. Bold segments span 0.5–2 Vmax of each zoom-in host, with Vmax = 37 km s−1 (Mhost/1010 M⊙)1/3. The coloured ruler above both plots uses the same relation: it marks the host whose Vmax equals w (or v), so a marker sitting left of its own colour is a model whose cross section is strongly velocity-suppressed in that host.
Each marker groups runs that share (σ0, w), the colour attribute (host-mass bin, code or year) and the run type; marker area grows as √N. Re-analyses of existing runs, convergence re-runs and CDM twins are not counted. Faded markers come mostly from low-confidence table entries.