  We present a quantitative analysis of the properties of galaxies and
structures evolving in universes dominated by different modified gravitational
models, including two variants of the f(R)-gravity (F) and two of the
Dvali-Gabdadze-Poratti (N) braneworld model, which respectively feature the
chameleon and Vainshtein screening mechanisms. Using the Simulation
HYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamical
full-physics simulations suite, we study the departures in the properties of
galaxies residing in different environments with respect to the standard model
(GR). Using two different criteria to compare, we find that structures formed
within modified gravity tend to show a denser gas density profile than their GR
counterparts. Within the different modified gravity models, N1 and F5 gravity
models show greater departures from the standard model, with gas density
profiles $\rho_{\rm IGM} \geq 30\%$ denser in the outskirts for the N1 model,
and in the inner parts for the F5 model. Additionally, we find that haloes
evolving in MG universes show, in general, larger quenched fractions than GR,
reaching up to $20\%$ larger quenching fractions in F5 regardless of the
stellar mass of the galaxy. With respect to the other models, F6, N1 and N5
show slightly larger quenched fractions, but no strong differences can be
found. These results directly impact the colour distribution of galaxies,
making them in MG models redder and older than their GR counterparts. Like GR,
once the environment starts to play a role, galaxies rapidly get quenched and
the differences between models vanish.
