42 research outputs found
Hydrodynamical Simulations of the IGM at High Mach Numbers
We present a new approach to doing Eulerian computational fluid dynamics that
is designed to work at high Mach numbers encountered in hydrodynamical
simulations of the IGM. In conventional Eulerian CFD, the thermal energy is
poorly tracked in supersonic bulk flows where local fluid variables cannot be
accurately separated from the much larger bulk flow components. We described a
method in which local fluid quantities can be directly tracked and the Eulerian
fluid equations solved in a local frame moving with the flow. The new algorithm
has been used to run large hydrodynamical simulations on a 1024^3 grid to study
the kinetic SZ effect. The KSZ power spectrum is broadly peaked at l~10^4 with
temperature fluctuations on micro Kelvin levels.Comment: 6 pages, to appear in the Proc. from the IGM/Galaxy Connection
conferenc
The Impact of Non-Gaussian Errors on Weak Lensing Surveys
The weak lensing power spectrum carries cosmological information via its
dependence on the growth of structure and on geometric factors. Since much of
the cosmological information comes from scales affected by nonlinear
clustering, measurements of the lensing power spectrum can be degraded by
non-Gaussian covariances. Recently there have been conflicting studies about
the level of this degradation. We use the halo model to estimate it and include
new contributions related to the finite size of lensing surveys, following
Rimes and Hamilton's study of 3D simulations. We find that non-Gaussian
correlations between different multipoles can degrade the cumulative
signal-to-noise for the power spectrum amplitude by up to a factor of 2 (or 5
for a worst-case model that exceeds current N-body simulation predictions).
However, using an eight-parameter Fisher analysis we find that the marginalized
errors on individual parameters are degraded by less than 10% (or 20% for the
worst-case model). The smaller degradation in parameter accuracy is primarily
because: individual parameters in a high-dimensional parameter space are
degraded much less than the volume of the full Fisher ellipsoid; lensing
involves projections along the line of sight, which reduce the non-Gaussian
effect; some of the cosmological information comes from geometric factors which
are not degraded at all. We contrast our findings with those of Lee & Pen
(2008) who suggested a much larger degradation in information content. Finally,
our results give a useful guide for exploring survey design by giving the
cosmological information returns for varying survey area, depth and the level
of some systematic errors.Comment: To appear in MNRAS, 22 pages, 12 figures. Minor modifications made
according to the referee comment
Effects of halo substructure on the power spectrum and bispectrum
We study the effects of halo substructure and a distribution in the
concentration parameter of haloes on large-scale structure statistics. The
effects on the power spectrum and bispectrum are studied on the smallest scales
accessible from future surveys. We compare halo-model predictions with results
based on N-body simulations, but also extend our predictions to 10-kpc scales
which will be probed by future simulations. We find that weak-lensing surveys
proposed for the coming decade can probe the power spectrum on small enough
scales to detect substructure in massive haloes. We discuss the prospects of
constraining the mass fraction in substructure in view of partial degeneracies
with parameters such as the tilt and running of the primordial power spectrum.Comment: 9 pages, 10 figures; replaced with version published in MNRAS;
removed grey-scale versions of figures which were being included at the end
by the serve
Masses of high-z galaxy hosting haloes from angular clustering and their evolution in the CDM model
We examine masses of hosting haloes of two photometrically-selected high-z
galaxy samples: the old passively-evolving galaxies (OPEGs) and Lyman Break
Galaxies (LBGs) both taken from the Subaru/XMM-Newton Deep Survey (SXDS). The
large survey area of the SXDS (1sq deg) allows us to measure the angular
two-point correlation functions to a wide separation of >10 arcmin with a good
statistical quality. We utilize the halo model prescription for estimating
characteristic masses of hosting haloes from the measured large-scale
clustering amplitudes. It is found that the hosting halo mass positively
correlates with the luminosity of galaxies. Then, adopting the extended
Press-Schechter model (EPS), we compute the predictions for the mass evolution
of the hosting haloes in the framework of the cold dark matter (CDM) cosmology
in order to make an evolutionary link between the two galaxy samples at
different redshifts and to identify their present-day descendants by letting
their haloes evolve forward in time. It is found that, in the view of the mass
evolution of hosting haloes in the CDM model, bright LBGs are consistent with
being the progenitor of the OPEGs, whereas it is less likely that the LBG
population, as a whole, have evolved into the OPEG population. It is also found
that the present-day descendants of both the bright LBGs and OPEGs are likely
to be located in massive systems such as groups of galaxies or clusters of
galaxies. Finally, we estimate the hosting halo mass of local early-type galaxy
samples from the 2dF and SDSS based on the halo model and it turns out that
their expected characteristic mass of hosting haloes is in good agreement with
the EPS predictions for the descendant's mass of both the bright LBGs and
OPEGs.Comment: 10 pages, 10 figures, submitted to MNRAS. Fortran programs used to
compute the model predictions in this paper are available at
http://optik2.mtk.nao.ac.jp/~hamanatk/OPENPRO/index.htm
From Weak Lensing to non-Gaussianity via Minkowski Functionals
We present a new harmonic-domain approach for extracting morphological
information, in the form of Minkowski Functionals (MFs), from weak lensing (WL)
convergence maps. Using a perturbative expansion of the MFs, which is expected
to be valid for the range of angular scales probed by most current weak-lensing
surveys, we show that the study of three generalized skewness parameters is
equivalent to the study of the three MFs defined in two dimensions. We then
extend these skewness parameters to three associated skew-spectra which carry
more information about the convergence bispectrum than their one-point
counterparts. We discuss various issues such as noise and incomplete sky
coverage in the context of estimation of these skew-spectra from realistic
data. Our technique provides an alternative to the pixel-space approaches
typically used in the estimation of MFs, and it can be particularly useful in
the presence of masks with non-trivial topology. Analytical modeling of weak
lensing statistics relies on an accurate modeling of the statistics of
underlying density distribution. We apply three different formalisms to model
the underlying dark-matter bispectrum: the hierarchical ansatz, halo model and
a fitting function based on numerical simulations; MFs resulting from each of
these formalisms are computed and compared. We investigate the extent to witch
late-time gravity-induced non-Gaussianity (to which weak lensing is primarily
sensitive) can be separated from primordial non-Gaussianity and how this
separation depends on source redshift and angular scale.Comment: 22 Pages, 12 Figures. Submitting To MNRA
Baryon Oscillations and Dark-Energy Constraints from Imaging Surveys
Baryonic oscillations in the galaxy power spectrum have been studied as a way
of probing dark-energy models. While most studies have focused on spectroscopic
surveys at high redshift, large multi-color imaging surveys have already been
planned for the near future. In view of this, we study the prospects for
measuring baryonic oscillations from angular statistics of galaxies binned
using photometric redshifts. We use the galaxy bispectrum in addition to the
power spectrum; this allows us to measure and marginalize over possibly complex
galaxy bias mechanisms to get robust cosmological constraints. In our parameter
estimation we allow for a weakly nonlinear biasing scheme that may evolve with
redshift by two bias parameters in each of ten redshift bins. We find that a
multi-color imaging survey that probes redshifts beyond one can give
interesting constraints on dark-energy parameters. In addition, the shape of
the primordial power spectrum can be measured to better accuracy than with the
CMB alone. We explore the impact of survey depth, area, and calibration errors
in the photometric redshifts on dark-energy constraints.Comment: 17 pages, 12 figure
A Strategy to Measure the Dark Energy Equation of State using the HII galaxy Hubble Relation & X-ray AGN Clustering: Preliminary Results
We explore the possibility of setting stringent constraints to the Dark
Energy equation of state using alternative cosmic tracers like: (a) the Hubble
relation using HII galaxies, which can be observed at much higher redshifts
(z~3.5) than those currently traced by SNIa samples, and (b) the large-scale
structure using the clustering of X-ray selected AGN,which have a redshift
distribution peaking at z~1.
We use extensive Monte-Carlo simulations to define the optimal strategy for
the recovery of the dark-energy equation of state using the high redshift (z~2)
Hubble relation, but accounting also for the effects of gravitational lensing,
which for such high redshifts can significantly affect the derived cosmological
constraints. Based on a "Figure of Merit" analysis, we provide estimates for
the number of 2<z<3.5 tracers needed to reduce the cosmological solution space,
presently provided by the Constitution SNIa set, by a desired factor. We find
that it is much more efficient to increase the number of tracers than to reduce
their individual uncertainties.
Finally, we propose a framework to put constraints on the dark energy
equation of state by using the joint likelihood of the X-ray AGN clustering and
of the Hubble relation cosmological analyses. A preliminary joint analysis
using the X-ray AGN clustering of the 2XMM survey and the Hubble relation of
the Constitution SNIa set provide: Omega_m= 0.31+-0.01 and w=-1.06+-0.05. We
also find that the joint SNIa-2XMM analysis provides significantly more
stringent cosmological constraints, increasing the Figure of Merit by a factor
~2, with respect to that of the joint SNIa-BAO analysis.Comment: MNRAS in press, 12 colour figure
Cosmological Tests of Gravity
Modifications of general relativity provide an alternative explanation to
dark energy for the observed acceleration of the universe. We review recent
developments in modified gravity theories, focusing on higher dimensional
approaches and chameleon/f(R) theories. We classify these models in terms of
the screening mechanisms that enable such theories to approach general
relativity on small scales (and thus satisfy solar system constraints). We
describe general features of the modified Friedman equation in such theories.
The second half of this review describes experimental tests of gravity in
light of the new theoretical approaches. We summarize the high precision tests
of gravity on laboratory and solar system scales. We describe in some detail
tests on astrophysical scales ranging from ~kpc (galaxy scales) to ~Gpc
(large-scale structure). These tests rely on the growth and inter-relationship
of perturbations in the metric potentials, density and velocity fields which
can be measured using gravitational lensing, galaxy cluster abundances, galaxy
clustering and the Integrated Sachs-Wolfe effect. A robust way to interpret
observations is by constraining effective parameters, such as the ratio of the
two metric potentials. Currently tests of gravity on astrophysical scales are
in the early stages --- we summarize these tests and discuss the interesting
prospects for new tests in the coming decade.Comment: Invited review for Annals of Physics; 58 pages, 8 figures
Forecasting Cosmic Doomsday from CMB/LSS Cross-Correlations
A broad class of dark energy models, which have been proposed in attempts at
solving the cosmological constant problems, predict a late time variation of
the equation of state with redshift. The variation occurs as a scalar field
picks up speed on its way to negative values of the potential. The negative
potential energy eventually turns the expansion into contraction and the local
universe undergoes a big crunch. In this paper we show that cross-correlations
of the CMB anisotropy and matter distribution, in combination with other
cosmological data, can be used to forecast the imminence of such cosmic
doomsday.Comment: 12 pages, 12 figure