Extended Data Figure 4: Turbulent heating per unit density versus radiative cooling per unit density, and the Ozmidov scale in the Perseus and Virgo clusters. | Nature

Extended Data Figure 4: Turbulent heating per unit density versus radiative cooling per unit density, and the Ozmidov scale in the Perseus and Virgo clusters.

From: Turbulent heating in galaxy clusters brightest in X-rays

Extended Data Figure 4

a, The same as Fig. 3, but with the turbulent heating and cooling rates divided by the mass density of gas in each annulus. b, The same as Fig. 2 with the Ozmidov scale lO = 1/kO = N−3/2ε1/2 shown for each annulus (vertical black lines), estimated using ε = Qcool/ρ0 (assuming that Qturb = Qcool).

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