Table 1: Cosmological simulations of structure formation analysed in this study.
Name Physics L Resolution $m_{\rm DM}$ $m_{\rm gas}$ $\epsilon_{\rm grav}$
    [ $h^{-1}~{\rm Mpc}$]   [ $h^{-1}~{M}_\odot$] [ $h^{-1}~{M}_\odot$] [ $h^{-1}~{\rm kpc}$]
S1 non-radiative, no star formation (SF) 100 $2\times 256^3$ $4.30\times 10^9$ $6.62\times 10^8$ 15.0
S2 CR-injection at shocks with $\zeta _{\rm inj}=0.5$, $\alpha_{\rm inj}=2.5$, no star formation 100 $2\times 256^3$ $4.30\times 10^9$ $6.62\times 10^8$ 15.0
S3 Mach-number dependent CR injection at shocks, no star formation 100 $2\times 256^3$ $4.30\times 10^9$ $6.62\times 10^8$ 15.0
D1 radiative cooling, star formation (SF), no cosmic rays 10 $2\times 256^3$ $4.30\times 10^6$ $6.62\times 10^5$ 1.3
D2 radiative cooling, SF, CRs from supernovae (SNe) 10 $2\times 256^3$ $4.30\times 10^6$ $6.62\times 10^5$ 1.3
D3 radiative cooling, SF, CRs from SNe and shocks (according to Mach-number) 10 $2\times 256^3$ $4.30\times 10^6$ $6.62\times 10^5$ 1.3

Source LaTeX | All tables | In the text