64 research outputs found
Perturbation Theory for BAO reconstructed fields: one-loop results in real-space matter density field
We compute the power spectrum at one-loop order in standard perturbation
theory for the matter density field to which a standard Lagrangian Baryonic
acoustic oscillation (BAO) reconstruction technique is applied. The BAO
reconstruction method corrects the bulk motion associated with the
gravitational evolution using the inverse Zel'dovich approximation (ZA) for the
smoothed density field. We find that the overall amplitude of one-loop
contributions in the matter power spectrum substantially decrease after
reconstruction. The reconstructed power spectrum thereby approaches the initial
linear spectrum when the smoothed density field is close enough to linear,
i.e., the smoothing scale larger than around 10Mpc. On smaller
,however, the deviation from the linear spectrum becomes significant on
large scales () due to the nonlinearity in the smoothed density
field, and the reconstruction is inaccurate. Compared with N-body simulations,
we show that the reconstructed power spectrum at one loop order agrees with
simulations better than the unreconstructed power spectrum. We also calculate
the tree-level bispectrum in standard perturbation theory to investigate
non-Gaussianity in the reconstructed matter density field. We show that the
amplitude of the bispectrum significantly decreases for small after
reconstruction and that the tree-level bispectrum agrees well with N-body
results in the weakly nonlinear regime.Comment: 18 pages, 7 figures, accepted for publications in PR
Primordial Non-Gaussianity and Analytical Formula for Minkowski Functionals of the Cosmic Microwave Background and Large-scale Structure
We derive analytical formulae for the Minkowski Functions of the cosmic
microwave background (CMB) and large-scale structure (LSS) from primordial
non-Gaussianity. These formulae enable us to estimate a non-linear coupling
parameter, f_NL, directly from the CMB and LSS data without relying on
numerical simulations of non-Gaussian primordial fluctuations. One can use
these formulae to estimate statistical errors on f_NL from Gaussian
realizations, which are much faster to generate than non-Gaussian ones, fully
taking into account the cosmic/sampling variance, beam smearing, survey mask,
etc. We show that the CMB data from the Wilkinson Microwave Anisotropy Probe
should be sensitive to |f_NL|\simeq 40 at the 68% confidence level. The Planck
data should be sensitive to |f_NL|\simeq 20. As for the LSS data, the late-time
non-Gaussianity arising from gravitational instability and galaxy biasing makes
it more challenging to detect primordial non-Gaussianity at low redshifts. The
late-time effects obscure the primordial signals at small spatial scales.
High-redshift galaxy surveys at z>2 covering \sim 10Gpc^3 volume would be
required for the LSS data to detect |f_NL|\simeq 100. Minkowski Functionals are
nicely complementary to the bispectrum because the Minkowski Functionals are
defined in real space and the bispectrum is defined in Fourier space. This
property makes the Minksowski Functionals a useful tool in the presence of
real-world issues such as anisotropic noise, foreground and survey masks. Our
formalism can be extended to scale-dependent f_NL easily.Comment: 16 pages, 5 figures, accepted for publication in ApJ (Vol. 653, 2006
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