Cluster Overviews
Deep projections of the most massive galaxy clusters in the PICO-Cluster sample
Fig. 1. Halo 4 (M200 = 2.7×1015 M☉) at Z24 resolution. Deep 15 Mpc projections of gas density, temperature, vorticity, and magnetic field strength at z = 0, with a mock HST stellar image inset and a zoom on a spiral galaxy outside the cluster. View full size → Similar images for all 24 clusters are available via the cluster sample table.
Cluster sample — Gas density
Volume-weighted gas density projections of all 24 clusters at z=0, depth 10 Mpc/h. Circles mark R200. The sample spans M200 from 0.75 to 3.3 × 1015 M☉.
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Cluster sample — Vorticity
Mass-weighted root-mean-square vorticity projections of all 24 clusters at z=0, depth 10 Mpc/h. Turbulent wakes of galaxies moving through the ICM and accretion shocks are clearly visible. Circles mark R200.
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Cluster sample — Magnetic field
Volume-weighted root-mean-square magnetic field strength projections of all 24 clusters at z=0, depth 10 Mpc/h. Strong B-field regions correlate with high density and high vorticity, reflecting the small-scale dynamo driven by ICM turbulence. Circles mark R200.
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Cluster sample — Temperature
Mass-weighted temperature projections of all 24 clusters at z=0, depth 10 Mpc/h. Hot accretion shocks and merger-heated regions are visible around and within the clusters. Circles mark R200.
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Cluster sample — Pressure
Volume-weighted thermal pressure projections of all 24 clusters at z=0, depth 10 Mpc/h. Merger-driven shocks and sloshing features are visible in disturbed clusters. Circles mark R200.
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Cluster sample — Metallicity
Mass-weighted gas metallicity projections of all 24 clusters at z=0, depth 10 Mpc/h. Metals are distributed throughout the ICM by galactic winds and AGN feedback, with the metallicity broadly following structures. However, the highest metallicity is found in voids surrounding clusters, which AGN and stellar feedback have polluted with metals. Circles mark R200.
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Cluster sample — Shock heating rate
Shock dissipation heating rate per volume for all 24 clusters at z=0, depth 10 Mpc/h. Highlights merger and accretion shocks at the cluster outskirts as well as weaker internal shocks. Circles mark R500.
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Cluster sample — Mock optical images
Synthetic SDSS gri composite images of the stellar particles for all 24 clusters at z=0, depth 10 Mpc/h. Shows the BCG, member galaxies, and the diffuse intracluster light (ICL). Circles mark R500.
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Parent box & zoom-in technique
The 1 h−1Gpc parent simulation (left), a cluster string (lower right), and the Z24 zoom-in of halo 4 (upper right) illustrating how the zoom-in technique concentrates resolution.
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Resolution Convergence
Fig. 2. Convergence study of halo 4 at Z4, Z8, Z12, and Z24. Rows: gas density, vorticity, magnetic field, mock optical images. Higher resolutions reveal additional low-mass subhalos and finer turbulent structures behind infalling galaxies. View full size →
Contamination radius
Minimum contamination radius (in units of R200) vs. cluster mass (left) and density distributions of high- and low-resolution particles (right). All clusters are clean within >2.74 R200 at all times.
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Cluster Physics
Cluster scaling relations
Six mass–observable scaling relations (richness, SZ signal, X-ray luminosity, K-band luminosity, BCG luminosity, gas fraction) compared to MTNG and LoCuSS observations at z = 0.25.
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Space–time diagram (Z24 simulation)
Time evolution of radial profiles of gas density, vorticity, and magnetic field strength. Galaxy merger tracks, AGN feedback events, and the growing magnetized region are visible. The B-field saturates early and expands outward with the growing cluster.
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Plasma physics slices (Z24)
Slices through the central cluster region: ion mean-free-path (top left), Voronoi cell sizes (top middle), their ratio (top right), pressure anisotropy (bottom left), inverse plasma β (bottom middle), and instability parameter βΔp/p (bottom right). The Z24 simulation resolves λmfp in 98% of the slice.
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