26 research outputs found
The dynamical state of dark matter haloes in cosmological simulations - I. Correlations with mass assembly history
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2011 RAS © 2011 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.Using a statistical sample of dark matter haloes drawn from a suite of cosmological N-body simulations of the cold dark matter (CDM) model, we quantify the impact of a simulated halo's mass accretion and merging history on two commonly used measures of its dynamical state, the virial ratio η and the centre of mass offset Δr. Quantifying this relationship is important because the degree to which a halo is dynamically equilibrated will influence the reliability with which we can measure characteristic equilibrium properties of the structure and kinematics of a population of haloes. We begin by verifying that a halo's formation redshift zform correlates with its virial mass Mvir and we show that the fraction of its recently accreted mass and the likelihood of it having experienced a recent major merger increase with increasing Mvir and decreasing Zform. We then show that both η and Δr increase with increasing Mvir and decreasing zform, which implies that massive recently formed haloes are more likely to be dynamically unrelaxed than their less massive and older counterparts. Our analysis shows that both η and Δr are good indicators of a halo's dynamical state, showing strong positive correlations with recent mass accretion and merging activity, but we argue that Δr provides a more robust and better defined measure of dynamical state for use in cosmological N-body simulations at z≃ 0. We find that Δr≲ 0.04 is sufficient to pick out dynamically relaxed haloes at z= 0. Finally, we assess our results in the context of previous studies, and consider their observational implicationsAK is supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramon y Cajal programme as well as the grants AYA 2009-13875-C03-02, AYA2009-12792-C03-03, CSD2009- 00064 and CAMS2009/ESP-1496. He acknowledges support by the MICINN under the Consolider-Ingenio, SyeC project CSD- 2007-0005
Dark Matter Halo Profiles in Scale-Free Cosmologies
We explore the dependence of the central logarithmic slope of dark matter
halo density profiles on the spectral index of the linear matter
power spectrum using cosmological -body simulations of scale-free
models (i.e. ). For each of our simulations we identify
samples of well resolved haloes in dynamical equilibrium and we analyse their
mass profiles. By parameterising the mass profile using a ``generalised''
Navarro, Frenk & White profile in which the central logarithmic slope
is allowed to vary while preserving the asymptotic form at large
radii, we obtain preferred central slopes for haloes in each of our models.
There is a strong correlation between and , such that
becomes shallower as becomes steeper. However, if we normalise our mass
profiles by , the radius at which the logarithmic slope of the density
profile is -2, we find that these differences are no longer present. We
conclude that there is no evidence for convergence to a unique central
asymptotic slope, at least on the scales that we can resolve.Comment: 9 pages, 4 figures. Accepted for publication in MNRA
The luminosities of backsplash galaxies in constrained simulations of the Local Group
We study the differences and similarities in the luminosities of bound,
infalling and the so-called backsplash (Gill et al. 2005) galaxies of the Milky
Way and M31 using a hydrodynamical simulation performed within the Constrained
Local UniversE Simulation (CLUES) project. The simulation models the formation
of the Local Group within a self-consistent cosmological framework. We find
that even though backsplash galaxies passed through the virial radius of their
host halo and hence may have lost a (significant) fraction of their mass, their
stellar populations are hardly affected. This leaves us with comparable
luminosity functions for infalling and backsplash galaxies and hence little
hope to decipher their past (and different) formation and evolutionary
histories by luminosity measurements alone. Nevertheless, due to the tidal
stripping of dark matter we find that the mass-to-light ratios have changed
when comparing the various populations against each other: they are highest for
the infalling galaxies and lowest for the bound satellites with the backsplash
galaxies in-between.Comment: 9 pages, 10 figures, 1 table, accepted for publication in MNRA
On the starting redshift for cosmological simulations: Focusing on halo properties
We systematically study the effects of varying the starting redshift z_i for
cosmological simulations in the highly non-linear regime. Our primary focus
lies with the (individual) properties of dark matter halos -- namely the mass,
spin, triaxiality, and concentration -- where we find that even substantial
variations in z_i leave only a small imprint, at least for the probed mass
range M \in [10^{10}, 10^{13}] Msun/h and when investigated at redshift z=0. We
further compare simulations started by using the standard Zel'dovich
approximation to runs based upon initial conditions produced with second order
Lagrangian perturbation theory. Here we observe the same phenomenon, i.e. that
differences in the studied (internal) properties of dark matter haloes are
practically undetectable. These findings are (for the probed mass range) in
agreement with other work in the literature. We therefore conclude that the
commonly used technique for setting up cosmological simulations leads to stable
results at redshift z=0 for the mass, the spin parameter, the triaxiality, and
the concentration of dark matter haloes.Comment: 10 pages, 9 figures, accepted for publication in Ap
The impact of baryonic physics on the shape and radial alignment of substructures in cosmological dark matter haloes
We use two simulations performed within the Constrained Local UniversE
Simulation (CLUES) project to study both the shape and radial alignment of (the
dark matter component of) subhaloes; one of the simulations is a dark matter
only model while the other run includes all the relevant gas physics and star
formation recipes. We find that the involvement of gas physics does not have a
statistically significant effect on either property -- at least not for the
most massive subhaloes considered in this study. However, we observe in both
simulations including and excluding gasdynamics a (pronounced) evolution of the
dark matter shapes of subhaloes as well as of the radial alignment signal since
infall time. Further, this evolution is different when positioned in the
central and outer regions of the host halo today; while subhaloes tend to
become more aspherical in the central 50% of their host's virial radius, the
radial alignment weakens in the central regime while strengthening in the outer
parts. We confirm that this is due to tidal torquing and the fact that
subhaloes at pericentre move too fast for the alignment signal to respond.Comment: 10 pages, 8 figures, 2 tables, accepted for publication in MNRAS,
replaced with proof-corrected version (minor typos
Constrained simulations of the Local Group: on the radial distribution of substructures
We examine the properties of satellites found in high resolution simulations
of the local group. We use constrained simulations designed to reproduce the
main dynamical features that characterize the local neighborhood, i.e. within
tens of Mpc around the Local Group (LG). Specifically, a LG-like object is
found located within the 'correct' dynamical environment and consisting of
three main objects which are associated with the Milky Way, M31 and M33. By
running two simulations of this LG from identical initial conditions - one with
and one without baryons modeled hydrodynamically - we can quantify the effect
of gas physics on the population of subhaloes in an environment similar
to our own. We find that above a certain mass cut, subhaloes in hydrodynamic simulations are more
radially concentrated than those in simulations with out gas. This is caused by
the collapse of baryons into stars that typically sit in the central regions of
subhaloes, making them denser. The increased central density of such a subhalo,
results in less mass loss due to tidal stripping than the same subhalo
simulated with only dark matter. The increased mass in hydrodynamic subhaloes
with respect to dark matter ones, causes dynamical friction to be more
effective, dragging the subhalo towards the centre of the host. This results in
these subhaloes being effectively more radially concentrated then their dark
matter counterparts.Comment: 12 pages, 9 figure
Cosmic variance of the local Hubble flow in large-scale cosmological simulations
The increasing precision in the determination of the Hubble parameter has reached a per cent level at which large-scale cosmic flows induced by inhomogeneities of the matter distribution become non-negligible. Here, we use large-scale cosmological N-body simulations to study statistical properties of the local Hubble parameter as measured by local observers. We show that the distribution of the local Hubble parameter depends not only on the scale of inhomogeneities, but also on how one defines the positions of observers in the cosmic web and what reference frame is used. Observers located in random dark matter haloes measure on average lower expansion rates than those at random positions in space or in the centres of cosmic voids, and this effect is stronger from the halo rest frames compared to the cosmic microwave background (CMB) rest frame. We compare the predictions for the local Hubble parameter with observational constraints based on Type Ia supernova (SNIa) and CMB observations. Due to cosmic variance, for observers located in random haloes we show that the Hubble constant determined from nearby SNIa may differ from that measured from the CMB by ±0.8 per cent at 1σ statistical significance. This scatter is too small to significantly alleviate a recently claimed discrepancy between current measurements assuming a flat Λ cold dark matter (ΛCDM) model. However, for observers located in the centres of the largest voids permitted by the standard ΛCDM model, we find that Hubble constant measurements from SNIa would be biased high by 5 per cent, rendering this tension non-existent in this extreme case
Ahf: Amiga's Halo Finder
Cosmological simulations are the key tool for investigating the different
processes involved in the formation of the universe from small initial density
perturbations to galaxies and clusters of galaxies observed today. The
identification and analysis of bound objects, halos, is one of the most
important steps in drawing useful physical information from simulations. In the
advent of larger and larger simulations, a reliable and parallel halo finder,
able to cope with the ever-increasing data files, is a must. In this work we
present the freely available MPI parallel halo finder AHF. We provide a
description of the algorithm and the strategy followed to handle large
simulation data. We also describe the parameters a user may choose in order to
influence the process of halo finding, as well as pointing out which parameters
are crucial to ensure untainted results from the parallel approach.
Furthermore, we demonstrate the ability of AHF to scale to high resolution
simulations.Comment: 18 pages, 18 figures. Accepted for publication in ApJ