Open AccessGalactic haloes in MONDian cosmological simulations
Author(s) -
Knebe Alexander,
Gibson Brad K.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07182.x
Subject(s) - physics , astrophysics , modified newtonian dynamics , redshift , dark matter , cold dark matter , galaxy , galaxy formation and evolution , cosmology , structure formation , astronomy , galaxy rotation curve
In this paper, a series of high‐resolution N ‐body simulations is presented in which the equations of motion have been changed to account for modified Newtonian dynamics (MOND). It is shown that a low‐Ω 0 MONDian model with an appropriate choice for the normalization σ 8 can lead to clustering properties at redshift z = 0 similar to the commonly accepted (standard) Λ cold dark matter (ΛCDM) model. However, such a model shows no significant structures at high redshift, with only very few objects present beyond z > 3 that can be readily ascribed to the low Ω 0 value adopted. The agreement with ΛCDM at redshift z = 0 is driven by the more rapid structure evolution in MOND. Moreover, galaxy formation appears to be more strongly biased in MONDian cosmologies. Within the current implementation of MOND, density profiles of gravitationally bound objects at z = 0 can still be fitted by the universal Navarro, Frenk & White (NFW) profile, but MOND haloes are less clumpy.