The large scale structure of the universe.

http://staff.ustc.edu.cn/~wzhao7/c_index_files/main.files/lss.pdf

Large scale structure of the universe and cosmological perturbation theory

Stochastic inflation can be viewed as a sequence of two-step processes In the first step a stochastic impulse from short-distance quantum fluctuations acts on long waves---the interaction In the second step the long waves evolve semiclassically---the propagation Both steps must be developed to address whether fluctuations for cosmic structure formation may be non-Gaussian We describe a formalism for following the nonlinear propagation of long-wavelength metric and scalar-field fluctuations We perform an expansion in spatial gradients of the Arnowitt-Deser-Misner equations and we retain only terms up to first order At each point the fields obey evolution equations like those in a homogeneous universe, but now described by a local scale factor ${e}^{\ensuremath{\alpha}}$ and Hubble expansion rate $H$ However, the different points are joined together through the momentum constraint equation The gradient expansion is appropriate for inflation if the long-wave fields are smoothed over scales below ${e}^{\ensuremath{-}\ensuremath{\alpha}}{H}^{\ensuremath{-}1}$ Our equations are naturally described in the Einstein-Hamilton-Jacobi framework, which governs an ensemble of inhomogeneous universes, and which may be interpreted as a semiclassical approximation to the quantum theory We find that the Hubble parameter, which is a function of the local values of the scalar field, obeys a separated Hamilton-Jacobi equation that also governs the semiclassical phase of the wave functional In our approximation, time hypersurface changes leave the equations invariant However, the stochastic impulses that change the field initial conditions are most simply given on uniform expansion factor hypersurfaces whereas propagation is most easily solved on uniform Hubble hypersurfaces, in terms of $\ensuremath{\alpha}({x}^{j},H)$, the nonlinear analog of $\ensuremath{\zeta}$ of linear perturbation theory; we therefore pay special attention to hypersurface shifting In particular, we describe the transformation process for the fluctuation probability functional Exact general solutions are found for the case of a single scalar field interacting through an exponential potential For example, we show that quantum corrections to long-wavelength evolution of the metric are characteristically small using exact Green's-function solutions of the Wheeler-DeWitt equation for this potential Approximate analytic solutions to our classical system for slowly evolving multiple scalar fields are also easy to obtain in this formalism, contrasting with previous numerical approaches

/pdf/nonlinear-evolution-of-long-wavelength-metric-fluctuations-cccqcsxg6y.pdf

Nonlinear evolution of long-wavelength metric fluctuations in inflationary models

Light Pseudoscalars, Particle Physics and Cosmology

The transformations that take place in late‐type galaxies in the environment of rich clusters of galaxies at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $z=0$ \end{document} are reviewed. From the handful of late‐type galaxies that inhabit local clusters, whether they were formed in situ and survived as such, avoiding transformation or even destruction, or if they are newcomers that have recently fallen in from outside, we can learn an important lesson on the latest stages of galaxy evolution. We start by reviewing t...

https://iopscience.iop.org/article/10.1086/500691/pdf

Environmental Effects on Late-Type Galaxies in Nearby Clusters

A preliminary discussion is presented of recent results obtained as part of the extension of the Center of Astrophysics redshift survey. Several features of the results are striking. The distribution of galaxies in the sample, which contains 1100 galaxies in a 6 deg x 117 deg strip going through the Coma cluster, looks like a slice through the suds in the kitchen sink. It appears that the galaxies are on the surfaces of bubble-like structures with diameters of 25-50/h-Mpc. The largest bubble in the survey has a diameter comparable with the most recent estimates of the diameter of the void in Bootes. This topology poses serious challenges for current models for the formation of large-scale structure. The best available model for generating these structures is the explosive galaxy formation theory of Ostriker and Cowie (1981).

A Slice of the Universe

The CFA Redshift Survey

It is shown that the 2.5 degree-break in the galaxy correlation function derived from the Shane-Wirtanen star counts is indistinguishable from an artifact introduced by residual systematic variations in the effective magnitude limit from plate to plate. In order to avoid the introduction of a break, the maximum error from plate to plate must be no more than about 0.05 mag. Other large scale features in the data which are also affected by the systematic variations are discussed.

The Shane-Wirtanen counts

Voids of galaxies delineated by sharp one- or two-dimensional structures are the main features of the large-scale clustering of galaxies. In order to objectively identify the significant structures in the first slice of the Center for Astrophysics redshift survey, we perform a space-scale analysis of this galaxy catalog by means of the wavelet transform. The wavelet coefficients allow us to detect on all scales within reach both over- and underdense structures. The confidence level of the detection is computed under the assumption that galaxies are distributed according to a Poissonian process with a nonuniform law

Objective Detection of Voids and High-Density Structures in the First CfA Redshift Survey Slice

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A Slice of the Universe

The CFA Redshift Survey

A Slice of the Universe

The Shane-Wirtanen counts

Objective Detection of Voids and High-Density Structures in the First CfA Redshift Survey Slice