tokens: al. ( 2015 ). We do not expect our L62 results to match the obervational data, since the TNG model was tuned for the TNG-L25N512 test simulations using the galaxy properties mentioned above (as well as the BH mass–stellar mass relation and the galaxy size at redshift z = 0; Pillepich et al. 2018a ) and it has been demonstrated that the stellar properties of galaxies depend on the simulation resolution in the TNG model (see appendix A of Pillepich et al. 2018a , b , for details). Figure 8. Stellar and gaseous galaxy properties at z = 0 (unless otherwise stated). Upper left: Stellar-to-halo mass ratio as a function of halo mass. The stellar mass is measured within 30 kpc from the halo centre. Upper right: Galaxy stellar mass function measured within 30 kpc from the centre of the halo. Bottom left: The halo gas fraction within r 500 c as a function of the total halo mass. Bottom right: Star formation rate density as a function of redshift. Different colours represent different gravity models as specified in the legend. The solid colour lines show results from our L25 simulations, while the dashed coloured lines are from our L62 boxes. All lower subpanels show the relative differences between the galaxy properties of nDGP and GR models. In all panels, we compare our results with the IllustrisTNG results at three different resolutions (Pillepich et al. 2018a ): TNG-L25N512 (the solid grey curves), TNG-L25N256 (the grey-dashed curves), and TNG-L25N128 (the grey-dotted curves). The blue solid line in the upper panels shows the results from the TNG100 simulation (Pillepich et al. 2018b ). The light grey symbols represent observational measurements from Behroozi, Wechsler Conroy ( 2013 ), Baldry et al. ( 2012 ), Bernardi et al. ( 2013 ), D’Souza, Vegetti Kauffmann ( 2015 ), Giodini et al. ( 2009 ), and Lovisari, Reiprich Schellenberger ( 2015 ). The upper left-hand panel of Fig. 8 shows the stellar-to-halo mass ratio multiplied by the inverse of the baryon fraction (Ω b /Ω m ), as a function of the total host halo mass ( M 200 c ) for our six full-physics simulations at z = 0. The stellar mass was measured within 30 kpc from the halo centre. First, we note that the L62 simulations (the dashed coloured lines) are in good agreement with the TNG-L25N128 (the grey-dotted line) run at the high-mass end, but is lower than the TNG-L25N256 (the grey-dashed line) and TNG-L25N512 (the grey solid line) results, which is as expected given the resolutions of these runs. Our L25 runs (the solid coloured lines) predict higher stellar mass fractions than the TNG-L25N512 (the grey solid line), despite the fact that these simulations have the same resolution. The differences are due to the combination of the different initial condition realizations we used to run our simulations (i.e. cosmic variance) and the small number of high-mass objects in the small boxes. Note that the final TNG100 run (the blue solid line; Pillepich et al. 2018b ) also has disagreements with the
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