Go with the flow: The self-similar and non-linear behaviour of large-scale in- and outflows and the impact of accretion shocks from galaxies to galaxy clusters

Open Access

Fig. 1.

Four fields (density, radial velocity, temperature, and metallicity) interpolated on the spherical shells just outside the virial surface (r = 1.2r_vir) shown for an exemplary cluster from the highest mass bin (10¹⁵ M_⊙). The contours indicate the $\bar{ρ}$ $\bar{\rho}$ , $3 \bar{ρ}$ $3\bar{\rho}$ , and $8 \bar{ρ}$ $8\bar{\rho}$ level, respectively, relative to the mean density of the shell.

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