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On cosmological scales, observations of the cluster abundance currently placethe strongest constraints on f(R) gravity. These constraints lie in thelarge-field limit, where the modifications of general relativity can correctlybe modeled by setting the Compton wavelength of the scalar field to itsbackground value. These bounds are, however, at the verge of penetrating into aregime, where the modifications become nonlinearly suppressed due to thechameleon mechanism and cannot be described by this linearized approximation.For future constraints based on observations subjected to cluster abundance, itis therefore essential to consistently model the chameleon effect. We analyzedescriptions of the halo mass function in chameleon f(R) gravity using a mass-and environment-dependent spherical collapse model in combination withexcursion set theory and phenomenological fits to N-body simulations in theLCDM and f(R) gravity scenarios. Our halo mass functions consistentlyincorporate the chameleon suppression and cosmological parameter dependencies,improving upon previous formalisms and providing an important extension toN-body simulations for the application in consistent tests of gravity withobservables sensitive to the abundance of clusters.

Modeling halo mass functions in chameleon f(R) gravity