Nonlinear evolution of f ( R ) cosmologies. III. Halo statistics

By F. Schmidt, Marcos Lima, H. Oyaizu, Wayne Hu. 2008

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The statistical properties of dark matter halos, the building blocks of cosmological observables associated with structure in the Universe, offer many opportunities to test models for cosmic acceleration, especially those that seek to modify gravitational forces. We study the abundance, bias, and profiles of halos in cosmological simulations for one such model: the modified action f(R) theory. The effects of f(R) modified gravity can be separated into a large- and small-field limit. In the large-field limit, which is accessible to current observations, enhanced gravitational forces raise the abundance of rare massive halos and decrease their bias but leave their (lensing) mass profiles largely unchanged. This regime is well described by scaling relations based on a modification of spherical collapse calculations. In the small-field limit, the enhancement of the gravitational force is suppressed inside halos and the effects on halo properties are substantially reduced for the most massive halos. Nonetheless, the scaling relations still retain limited applicability for the purpose of establishing conservative upper limits on the modification to gravity.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c629de95d83d7d52d26b0ac4ef5474914bdc057b

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Citations in the corpus

Approaches to understanding cosmic acceleration (2009, background): “Hence, while it is certain that |fR| must be small, any specific bound on its value today will be unreliable until galaxy formation in f(R) is studied in N-body numerical simulations - work that has only recently begun [167, 168].”
Modified Gravity and Cosmology (2011, background): “The formation of non-linear structure has also been considered in [630, 1006, 1007, 1114, 1303].”
Modified Gravity-GADGET: A new code for cosmological hydrodynamical simulations of modified gravity models (2013, background): “…in the statistical and structural properties of collapsed CDM halos, as their impact on e.g. the matter power spectrum (see e.g. Oyaizu 2008; Schmidt et al. 2009; Li et al. 2012b), redshift-space distortions (Jennings et al. 2012), geometrical and dynamical properties of virialized halos…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “These include the self-accelerated branch (Chan & Scoccimarro 2009; Schmidt 2009b) and normal branch (Schmidt 2009a) of DGP gravity, and an f(R) model (Schmidt et al. 2009).”
ECOSMOG: an Efficient COde for Simulating MOdified Gravity (2011, methodology): “There are two such codes known to us to date: one is that of Oyaizu [15], which has been applied to f(R) gravity [16, 17] and the DGP model [18]; the other is a modified MLAPM code [19] written by one of the authors [20] and which has been applied to chameleon theories [21], f(R) gravity [22], coupl”
Cosmological tests of modified gravity (2015, background): “There have been significant progress in developing N-body simulations [275, 276, 277, 278, 279, 280, 281, 282, 283, 283, 284, 285, 286, 287, 288, 289, 290, 291, 292, 293, 294, 295, 296, 297, 298].”
Accurate halo-model matter power spectra with dark energy, massive neutrinos and modified gravitational forces (2016, result): “(38) For Geff/G = 4/3 these results are equivalent to those in Schmidt et al. (2009) for the deviation from a ΛCDM model.”
Formation of Galaxy Clusters (2012, methodology): “…obtained so far suggest that halo mass function and bias can still be described by the universal functions of peak height, in which the threshold for collapse and the linear growth rate are modified appropriately from their standard model values(Schmidt, Hu & Lima 2010; Schmidt et al. 2009).”