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. 4.

Relative outflow strength (the outflow rate divided by the respective halo mass, $\frac{\dot{M}}{M}$ $\frac{\dot{M}}{M}$ ) as a function of mass. The line colours indicate the different radii the flow strength is measured at.

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