Simulation-based priors that depend on cluster morphology allow mock X-ray/SZ cluster samples to recover the input Hubble constant with 4% (100 clusters) and 1.5% (1000 clusters) precision plus a systematic floor of 0.6–0.8 km/s/Mpc.
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DESI kinematics of Coma yield M_200 ≈ 1.04×10^15 M_⊙ under NFW and show colour-dependent orbital anisotropy, with blue galaxies implying a higher virial mass.
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The Three Hundred Project: Validating $H_0$ inference from mock X-ray and millimetre analyses of galaxy clusters
Simulation-based priors that depend on cluster morphology allow mock X-ray/SZ cluster samples to recover the input Hubble constant with 4% (100 clusters) and 1.5% (1000 clusters) precision plus a systematic floor of 0.6–0.8 km/s/Mpc.
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Novel insights into the Coma cluster kinematics with DESI. I. Linking mass profile, orbital anisotropy, and galaxy populations
DESI kinematics of Coma yield M_200 ≈ 1.04×10^15 M_⊙ under NFW and show colour-dependent orbital anisotropy, with blue galaxies implying a higher virial mass.