2016/12/31 by Georgios Valogiannis, Rachel Bean · 58 citations
Physics and Astronomy · #Astrophysics #Classical mechanics #Computer science #Consistency (knowledge bases) #Cosmology #Cosmology and Gravitation Theories #Dark energy #Galaxies: Formation, Evolution, Phenomena #Gravitation #Halo mass function #Lambda #Matter power spectrum #Physics #Quantum mechanics #Radio Astronomy Observations and Technology #Redshift #Theoretical physics #astro-ph.CO #gr-qc
paper · pdf · doi:10.1103/physrevd.95.103515
published in Physical review. D/Physical review. D. 95(10) (American Physical Society) · 15 pages, 9 figures. Updated to match version published in PRD
arxiv created 2017/04/18 · openalex publication_date 2017/05/26 · arxiv updated 2017/05/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We implement an adaptation of the cola approach, a hybrid scheme that combines Lagrangian perturbation theory with an N-body approach, to model nonlinear collapse in chameleon and symmetron modified gravity models. Gravitational screening is modeled effectively through the attachment of a suppression factor to the linearized Klein-Gordon equations. The adapted cola approach is benchmarked, with respect to an N-body code both for the \mathrm\ensuremathΛ cold dark matter (\mathrm\ensuremathΛCDM) scenario and for the modified gravity theories. It is found to perform well in the estimation of the dark matter power spectra, with consistency of 1% to k\ensuremath∼2.5 h/Mpc. Redshift space distortions are shown to be effectively modeled through a Lorentzian parametrization with a velocity dispersion fit to the data. We find that cola performs less well in predicting the halo mass functions but has consistency, within 1\ensuremathσ uncertainties of our simulations, in the relative changes to the mass function induced by the modified gravity models relative to \mathrm\ensuremathΛCDM. The results demonstrate that cola, proposed to enable accurate and efficient, nonlinear predictions for \mathrm\ensuremathΛCDM, can be effectively applied to a wider set of cosmological scenarios, with intriguing properties, for which clustering behavior needs to be understood for upcoming surveys such as LSST, DESI, Euclid, and WFIRST.