English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present a quantitative analysis of the properties of galaxies andstructures evolving in universes dominated by different modified gravitationalmodels, including two variants of the f(R)-gravity (F) and two of theDvali-Gabdadze-Poratti (N) braneworld model, which respectively feature thechameleon and Vainshtein screening mechanisms. Using the SimulationHYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamicalfull-physics simulations suite, we study the departures in the properties ofgalaxies residing in different environments with respect to the standard model(GR). Using two different criteria to compare, we find that structures formedwithin modified gravity tend to show a denser gas density profile than their GRcounterparts. Within the different modified gravity models, N1 and F5 gravitymodels show greater departures from the standard model, with gas densityprofiles $\rho_{\rm IGM} \geq 30\%$ denser in the outskirts for the N1 model,and in the inner parts for the F5 model. Additionally, we find that haloesevolving in MG universes show, in general, larger quenched fractions than GR,reaching up to $20\%$ larger quenching fractions in F5 regardless of thestellar mass of the galaxy. With respect to the other models, F6, N1 and N5show slightly larger quenched fractions, but no strong differences can befound. 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 andthe differences between models vanish.

Galaxy evolution in modified gravity simulations: using passive galaxies to constrain gravity with upcoming surveys