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We search for detectable signatures of f(R) gravity and its chameleonscreening mechanism in the baryonic and dark matter (DM) properties ofsimulated void galaxies. The enhancement of the gravitational acceleration canhave a meaningful impact on the scaling relations as well as on the halomorphology. The galaxy rotational velocity field (calculated with the velocityof the gas disc and the acceleration fields) deviates from the typical valuesof the Tully-Fisher Relation (TFR) in GR. For a given stellar mass, f(R)gravity tends to produce greater maximum velocities. On the other hand, themass in haloes in f(R) gravity is more concentrated than their counterparts inGR. This trend changes when the concentration is calculated with the dynamicaldensity profile, which takes into account the unscreened outer regions of thehalo. Stellar discs interact with the overall potential well in the centralregions, modifying the morphology of the screening regions and reshaping them.We find a trend for galaxies with a more dominant stellar disc to deviatefurther from round screening regions. We find that small haloes are lesstriaxial and more round in f(R) than their GR counterparts. The differencebetween halo morphology becomes smaller in f(R) haloes whose inner regions arescreened. These results suggest possible observables that could unveil modifiedgravity effects on galaxies in voids in future cosmological tests of gravity.

Fingerprints of modified gravity on galaxies in voids