161 research outputs found
Numerical Simulations of the Dark Universe: State of the Art and the Next Decade
We present a review of the current state of the art of cosmological dark
matter simulations, with particular emphasis on the implications for dark
matter detection efforts and studies of dark energy. This review is intended
both for particle physicists, who may find the cosmological simulation
literature opaque or confusing, and for astro-physicists, who may not be
familiar with the role of simulations for observational and experimental probes
of dark matter and dark energy. Our work is complementary to the contribution
by M. Baldi in this issue, which focuses on the treatment of dark energy and
cosmic acceleration in dedicated N-body simulations. Truly massive dark
matter-only simulations are being conducted on national supercomputing centers,
employing from several billion to over half a trillion particles to simulate
the formation and evolution of cosmologically representative volumes (cosmic
scale) or to zoom in on individual halos (cluster and galactic scale). These
simulations cost millions of core-hours, require tens to hundreds of terabytes
of memory, and use up to petabytes of disk storage. The field is quite
internationally diverse, with top simulations having been run in China, France,
Germany, Korea, Spain, and the USA. Predictions from such simulations touch on
almost every aspect of dark matter and dark energy studies, and we give a
comprehensive overview of this connection. We also discuss the limitations of
the cold and collisionless DM-only approach, and describe in some detail
efforts to include different particle physics as well as baryonic physics in
cosmological galaxy formation simulations, including a discussion of recent
results highlighting how the distribution of dark matter in halos may be
altered. We end with an outlook for the next decade, presenting our view of how
the field can be expected to progress. (abridged)Comment: 54 pages, 4 figures, 3 tables; invited contribution to the special
issue "The next decade in Dark Matter and Dark Energy" of the new Open Access
journal "Physics of the Dark Universe". Replaced with accepted versio
How closely do baryons follow dark matter on large scales?
We investigate the large-scale clustering and gravitational interaction of
baryons and dark matter (DM) over cosmic time using a set of collisionless
N-body simulations. Both components, baryons and DM, are evolved from distinct
primordial density and velocity power spectra as predicted by early-universe
physics. We first demonstrate that such two-component simulations require an
unconventional match between force and mass resolution (i.e. force softening on
at least the mean particle separation scale). Otherwise, the growth on any
scale is not correctly recovered because of a spurious coupling between the two
species at the smallest scales. With these simulations, we then demonstrate how
the primordial differences in the clustering of baryons and DM are
progressively diminished over time. In particular, we explicitly show how the
BAO signature is damped in the spatial distribution of baryons and imprinted in
that of DM. This is a rapid process, yet it is still not fully completed at low
redshifts. On large scales, the overall shape of the correlation function of
baryons and DM differs by 2% at z = 9 and by 0.2% at z = 0. The differences in
the amplitude of the BAO peak are approximately a factor of 5 larger: 10% at z
= 9 and 1% at z = 0. These discrepancies are, however, smaller than effects
expected to be introduced by galaxy formation physics in both the shape of the
power spectrum and in the BAO peak, and are thus unlikely to be detected given
the precision of the next generation of galaxy surveys. Hence, our results
validate the standard practice of modelling the observed galaxy distribution
using predictions for the total mass clustering in the Universe.Comment: 9 pages, 6 figures. Replaced with version published in MNRA
On the Statistics of Biased Tracers in the Effective Field Theory of Large Scale Structures
With the completion of the Planck mission, in order to continue to gather
cosmological information it has become crucial to understand the Large Scale
Structures (LSS) of the universe to percent accuracy. The Effective Field
Theory of LSS (EFTofLSS) is a novel theoretical framework that aims to develop
an analytic understanding of LSS at long distances, where inhomogeneities are
small. We further develop the description of biased tracers in the EFTofLSS to
account for the effect of baryonic physics and primordial non-Gaussianities,
finding that new bias coefficients are required. Then, restricting to dark
matter with Gaussian initial conditions, we describe the prediction of the
EFTofLSS for the one-loop halo-halo and halo-matter two-point functions, and
for the tree-level halo-halo-halo, matter-halo-halo and matter-matter-halo
three-point functions. Several new bias coefficients are needed in the
EFTofLSS, even though their contribution at a given order can be degenerate and
the same parameters contribute to multiple observables. We develop a method to
reduce the number of biases to an irreducible basis, and find that, at the
order at which we work, seven bias parameters are enough to describe this
extremely rich set of statistics. We then compare with the output of -body
simulations. For the lowest mass bin, we find percent level agreement up to
for the one-loop two-point functions, and up
to for the tree-level three-point functions,
with the -reach decreasing with higher mass bins. This is consistent with
the theoretical estimates, and suggests that the cosmological information in
LSS amenable to analytical control is much more than previously believed.Comment: 54 pages, 16 figures, v2: added references and explanations,
corrected typo
The One-Loop Matter Bispectrum in the Effective Field Theory of Large Scale Structures
Given the importance of future large scale structure surveys for delivering
new cosmological information, it is crucial to reliably predict their
observables. The Effective Field Theory of Large Scale Structures (EFTofLSS)
provides a manifestly convergent perturbative scheme to compute the clustering
of dark matter in the weakly nonlinear regime in an expansion in , where is the wavenumber of interest and is the
wavenumber associated to the nonlinear scale. It has been recently shown that
the EFTofLSS matches to level the dark matter power spectrum at redshift
zero up to Mpc and Mpc at one
and two loops respectively, using only one counterterm that is fit to data.
Similar results have been obtained for the momentum power spectrum at one loop.
This is a remarkable improvement with respect to former analytical techniques.
Here we study the prediction for the equal-time dark matter bispectrum at one
loop. We find that at this order it is sufficient to consider the same
counterterm that was measured in the power spectrum. Without any remaining free
parameter, and in a cosmology for which is smaller than in the
previously considered cases (), we find that the prediction from
the EFTofLSS agrees very well with -body simulations up to Mpc, given the accuracy of the measurements, which is of order a few
percent at the highest 's of interest. While the fit is very good on average
up to Mpc, the fit performs slightly worse on
equilateral configurations, in agreement with expectations that for a given
maximum , equilateral triangles are the most nonlinear.Comment: 39 pages, 12 figures; v2: JCAP published version, improved numerical
data, added explanation and clarification
Noiseless Gravitational Lensing Simulations
The microphysical properties of the DM particle can, in principle, be
constrained by the properties and abundance of substructures in DM halos, as
measured through strong gravitational lensing. Unfortunately, there is a lack
of accurate theoretical predictions for the lensing signal of substructures,
mainly because of the discreteness noise inherent to N-body simulations. Here
we present Recursive-TCM, a method that is able to provide lensing predictions
with an arbitrarily low discreteness noise, without any free parameters or
smoothing scale. This solution is based on a novel way of interpreting the
results of N-body simulations, where particles simply trace the evolution and
distortion of Lagrangian phase-space volume elements. We discuss the advantages
of this method over the widely used cloud-in-cells and adaptive-kernel
smoothing density estimators. Applying the new method to a cluster-sized DM
halo simulated in warm and cold DM scenarios, we show how the expected
differences in their substructure population translate into differences in the
convergence and magnification maps. We anticipate that our method will provide
the high-precision theoretical predictions required to interpret and fully
exploit strong gravitational lensing observations.Comment: 13 pages, 13 figures. Updated fig 12, references adde
Precision modelling of the matter power spectrum in a Planck-like Universe
We use a suite of high-resolution N-body simulations and state-of-the-art perturbation theory to improve the code halofit, which predicts the nonlinear matter power spectrum. We restrict attention to parameters in the vicinity of the Planck Collaboration’s best fit. On large-scales (k≲ 0.07 h Mpc−1), our model evaluates the 2-loop calculation from the Multi-point Propagator Theory of Bernardeau et al. (2012). On smaller scales (k≳ 0.7 h Mpc−1), we transition to a smoothing-spline-fit model, that characterises the differences between the Takahashi et al. (2012) recalibration of halofit2012 and our simulations. We use an additional suite of simulations to explore the response of the power spectrum to variations in the cosmological parameters. In particular, we examine: the time evolution of the dark energy equation of state (w0, wa); the matter density Ωm; the physical densities of CDM and baryons (ωc, ωb); and the primordial power spectrum amplitude As, spectral index ns, and its running α. We construct correction functions, which improve halofit’s dependence on cosmological parameters. Our newly calibrated model reproduces all of our data with ≲ 1% precision. Including various systematic errors, such as choice of N-body code, resolution, and through inspection of the scaled second order derivatives, we estimate the accuracy to be ≲ 3% over the hyper-cube: w0 ∈ { − 1.05, −0.95}, wa ∈ { − 0.4, 0.4}, Ωm, 0 ∈ {0.21, 0.4}, ωc ∈ {0.1, 0.13}, ωb ∈ {2.0, 2.4}, ns ∈ {0.85, 1.05}, As ∈ {1.72 × 10−9, 2.58 × 10−9}, α ∈ { − 0.2, 0.2} up to k = 9.0 h Mpc−1 and out to z = 3. Outside of this range the model reverts to halofit2012. We release all power spectra data with the C-code NGenHalofit at: https://[email protected]/ngenhalofitteam/ngenhalofitpublic.git
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