Fig. 8
Timescale of the different energy loss mechanisms (in years) as a function of redshift, adopting a star formation surface density of 10 M⊙ kpc-2 yr-1 and a cosmic ray energy of 1 GeV. Inverse Compton losses become dominant from z ∼ 2, while synchrotron losses dominate at lower redshift. We assume here no evolution of the B − ΣSFR-relation with redshift, i.e. ξ = α / 6 = 0.
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