The kinetic evolution and velocity distribution of gravitational galaxy clustering

Saslaw, William C.; Chitre, S. M.; Itoh, Makoto; Inagaki, Shogo

doi:10.1086/169496

Cited by 44 publications

(67 citation statements)

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“…Thus we may Ðnd it easier to go back to z B 3 from the present relatively less complicated state than to go forward to z B 3 from a much more complicated situation at very high redshift. Third, cosmological many-body clustering has also predicted the peculiar velocity distribution function for galaxies (Saslaw et al 1990), which was subsequently found to agree with observations (Raychaudhury & Saslaw 1996) at low redshifts. This agreement is less certain than for the spatial distribution, and further observations would provide an additional test of the model.…”

Section: Introductionsupporting

confidence: 65%

High‐Redshift Galaxy Clustering and \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} \

Saslaw

Edgar

2000

ApJ

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We develop the properties of cosmological many-body clustering at high redshift and compare the resulting theoretical distributions with recent observations of groups of galaxies around z B 3. Analyses of the observed variance of counts-in-cells and of the probability for forming strongly overdense regions suggest and respectively, for Einstein-Friedmann universes. Since these3, models are essentially analytical, they allow us to examine statistical questions that have analogs in more complicated cold dark matter models based on small numbers of simulations. We show how future observations of the galaxy distribution function can test cosmological many-body clustering and determine more precisely. For these models predict that galaxies start clustering at redshifts

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Section: Introductionsupporting

confidence: 65%

High‐Redshift Galaxy Clustering and \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} \

Saslaw

Edgar

2000

ApJ

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“…We can now use the pressure power spectrum to calculate the SZ angular power spectrum by projecting it along the line of sight following equation (231).…”

Section: Clustering Properties Of Large Scale Structure Pressurementioning

confidence: 99%

Halo models of large scale structure

2002

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We review the formalism and applications of the halo-based description of nonlinear gravitational clustering. In this approach, all mass is associated with virialized dark matter halos; models of the number and spatial distribution of the halos, and the distribution of dark matter within each halo, are used to provide estimates of how the statistical properties of large scale density and velocity fields evolve as a result of nonlinear gravitational clustering. We first describe the model, and demonstrate its accuracy by comparing its predictions with exact results from numerical simulations of nonlinear gravitational clustering. We then present several astrophysical applications of the halo model: these include models of the spatial distribution of galaxies, the nonlinear velocity, momentum and pressure fields, descriptions of weak gravitational lensing, and estimates of secondary contributions to temperature fluctuations in the cosmic microwave background.

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“…This is the same as the previous results (Ahmad et al 2002) which neglected the second-order terms. This approach may be extended to derive higher order velocity distributions (Saslaw et al 1990;Leong & Saslaw 2004) also. Figure 1 illustrates the effects of the sub-virial terms on f (N ) using the full solution (Equation (27)), rather than the loworder expansion (Equation (28)), for point particles, α 1 = 1, α 2 = 2/3, and various values of b .…”

Section: More Exact Distribution Functionsmentioning

confidence: 99%

Gravitational Phase Transitions in the Cosmological Many-Body System

Saslaw

Ahmad

2010

ApJ

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Gravitational many-body clustering of particles (e.g., galaxies) in an expanding universe may be regarded as a form of phase transition. We calculate its properties here and find that it differs in several ways from usual laboratory phase transitions. The cosmological case is never complete since it takes longer to evolve dynamically on larger spatial scales. To examine this, we calculate the effects of higher order corrections on the thermodynamic properties and distribution functions (which are known to agree with observations). The additional higher order terms are subdominant and decrease as the number of particles in the system increases. We also propose an order parameter for this hierarchical phase transition and discuss its relation to the Yang-Lee theory of phase transitions. These results also help to quantify earlier ideas of "continuous clustering."

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The kinetic evolution and velocity distribution of gravitational galaxy clustering

Cited by 44 publications

References 0 publications

Halo models of large scale structure

Gravitational Phase Transitions in the Cosmological Many-Body System

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