O VII and O VIII in the CGM of simulated Milky Way mass galaxies

Median quenching timescales of passive galaxies at z = 0, separating those that were central (blue) and satellite (red) galaxies around the time they left the star-forming

Despite the differences in model parameters between eagle and hydrangea, we combine the two models because.. Comparison of simulated and observational data in the size-mass diagram.

This is different to the result presented in Figure 10, where the star formation rate surface density in ring galaxies is higher in the outer radii (r > 20 kpc) in comparison

Figure 4 shows left the fraction of the baryonic mass (in the form of stars and gas) in the simulation that is inside dark matter haloes with m > m min = 3.1 × 10 8 M  as a

In this paper, we present the projected red giant branch (RGB) star density profiles out to projected radii ∼40–75 kpc along the disc’s minor and major axis profiles out to

We conclude that, in order to develop strong bars, discs must be locally and globally dominant; in other words, they must contribute a large fraction of the inner mass budget to

(ii) The similarity of the Ref-L025N0752 and Recal-L025N0752 H I CDDFs indicates that numerical resolution influences column densities more than the recalibration of the

Thus, the trends with environment seen for the sSFR of satellite galaxies are not driven by differences in stellar mass but are a reflection of the effect of environment (host