Hierarchical clustering in chameleon $f(R)$ gravity

Hellwing, Wojciech A.; Li, Baojiu; Frenk, Carlos S.; Cole, Shaun

doi:10.1093/mnras/stt1430

Hierarchical clustering in chameleon $f(R)$ gravity

May 31, 2013

17 pages

Published in:

Mon.Not.Roy.Astron.Soc. 435 (2013) 2806

e-Print:

1305.7486 [astro-ph.CO]

DOI:

10.1093/mnras/stt1430

View in:

ADS Abstract Service

pdf

reference search45 citations

Citations per year

Abstract: (arXiv)

We use a suite of high resolution state-of-the-art N-body Dark Matter simulations of chameleon

f(R)

gravity to study the higher order volume averaged correlation functions

\bar{\xi_n}

together with the hierarchical

n

-th order correlation amplitudes

S_n=\bar{\xi}_n/\bar{\xi}_2^{n-1}

and density distribution functions (PDF). We show that under the non-linear modifications of gravity the hierarchical scaling of the reduced cumulants is preserved. This is however characterised by significant changes of both the

\bar{\xi_n}

and

S_n

's values and their scale dependence with respect to General Relativity gravity (GR). In addition, we measure a significant increase of the non linear

\sigma_8

parameter reaching

14, 5

and 0.5% in excess of the GR value for the three flavours of our

f(R)

models. We further note that the values of the reduced cumulants up to order

n=9

are significantly increased in

f(R)

gravity for all our models at small scales R\simlt 30\hmpc. In contrast the values of the hierarchical amplitudes,

S_n

's, are smaller in

f(R)

indicating that the modified gravity density distribution functions are deviating from the GR case. Furthermore we find that the redshift evolution of relative deviations of the

f(R)

hierarchical correlation amplitudes is fastest at high and moderate redshifts

1\leq z \leq4

. The growth of these deviations significantly slows down in the low redshift universe. We also compute the PDFs and show that for scales below \sim 20\hmpc they are significantly shifted in

f(R)

gravity towards the low densities. Finally we discuss the implications of our theoretical predictions for measurements of the hierarchical clustering in galaxy redshifts surveys, including the important problems of the galaxy biasing and redshifts space distortions.

Note:

17 pages, 11 figures, submitted to MNRAS

CDM
hierarchical structure formation
density field
modified gravity
gravitation: model
gravitation: density
galaxy: redshift
redshift: low
density: low
flavor: 3

References(0)

Figures(12)

Loading ...

Hierarchical clustering in chameleon f(R)f(R)f(R) gravity

Citations per year

Hierarchical clustering in chameleon $f(R)$ gravity