Gravitational clustering of galaxies: Comparison between thermodynamic theory and N-body simulations. IV - The effects of continuous mass spectra

Itoh, Makoto; Inagaki, Shogo; Saslaw, William C.

doi:10.1086/172219

Cited by 50 publications

(53 citation statements)

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“…This provides a very good description of observed galaxy clustering in the Zwicky catalog (Crane & Saslaw 1986, Saslaw & Crane 1991, in the UGC and ESO catalogs (Lahav & Saslaw 1992), the Abell cluster catalog (Coleman & Saslaw 1990), the IRAS catalog (Sheth, Mo and Saslaw, 1994) and the Southern Sky Redshift Catalog (Fang & Zou, 1994). It also agrees very well with computer N-body simulations of galaxy clustering (Sheth and Saslaw 1995;Itoh, Inagaki & Saslaw 1993, and earlier references therein). This approach predicts a velocity distribution function f(v) dv whose integral over the transverse velocities gives Equation (2) for f(v r ) dv r (Inagaki et al 1992).…”

Section: Discussionsupporting

confidence: 83%

“…Partly as a result of sparse sampling and other selection procedures, the spatial pattern value of b ' 0:6 for large cells in the ESO may be reduced from its value of about 0.75 in the Zwicky catalog (Saslaw & Crane 1991). The numerical simulations of Figure 10 also give a spatial pattern value of b 0:75 for large cells (Itoh et al 1993). This spatial value is about 80% of b velocity ' 0:9 in Figure 2a, where the Dressler et al subtraction is used.…”

Section: Discussionmentioning

confidence: 89%

“…Numerical simulations for a range of more realistic mass spectra than the single mass simulation in Figure 10 also generally show b velocity > b pattern , depending on the details of the mass spectrum and the value of 0 . (Itoh et al 1993). A partial reason for this di erence is that in the simulations and in the observations the ts of the velocity distributions involve all the galaxies present (and all the dark matter in the observations), whereas the ts of the spatial distributions generally involve less representative subsamples.…”

Section: Discussionmentioning

confidence: 92%

“…This indicates that the velocities are very nearly isotropic. For the data in The distribution of radial peculiar velocities for the 10,000 galaxies in the simulation (model S) of Itoh et al (1993), where all galaxies are of equal mass. The simulations start from Poisson initial conditions, and are observed at an expansion factor of 8.…”

Section: Discussionmentioning

confidence: 99%

“…To compare our observed distribution function with the N-body simulations of Itoh et al (1993), we have to scale their velocities to the observed sample. The simulations use \natural units" with G=m=R=1.…”

Section: Discussionmentioning

confidence: 99%

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The Observed Distribution Function of Peculiar Velocities of Galaxies

Raychaudhury

Saslaw

1996

ApJ

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We give the rst determination of the observed peculiar velocity distribution function for a representative sample of galaxies which includes a wide range of clustering properties. We explore in detail the e ects of uncertainties in sampling and in distance measures on the estimated distribution function. The observed distribution function is consistent with an earlier prediction of gravitational clustering, over the entire range of peculiar velocities, from eld galaxies to rich clusters, on scales up to 50h 1 100 Mpc. In the simplest consistent model, most of the inhomogeneous mass of the Universe is in galaxies or their halos.We estimate the \Mach Number" for the bulk ow within 50h 1 100 Mpc from us to be M = v r =hv 2 r i 1 2 = 599=717 ' 0:8, which includes the e ect of high-dispersion galaxies in clusters. The observed velocity distribution function agrees quantitatively with N-body simulations with 0 = 1. Further comparisons of the observed distribution with N-body simulations will provide a new technique for measuring H 0 and 0 . These results provide new tests for all models of galaxy clustering.

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Section: Discussionsupporting

confidence: 83%

Section: Discussionmentioning

confidence: 89%

Section: Discussionmentioning

confidence: 92%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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The Observed Distribution Function of Peculiar Velocities of Galaxies

Raychaudhury

Saslaw

1996

ApJ

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Generalized Poisson Distributions

Famoye

Lee

2020

Wiley StatsRef: Statistics Reference Online

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The generalized Poisson distribution (GPD) is a two‐parameter discrete distribution. One of the parameters measures the location and the other measures the dispersion. The distribution is unimodal, and it can be skewed to the right or the left. It approaches the normal distribution when the location parameter gets very large. In this article, we present the definition and derive several important properties of the GPD. We review statistical inference and state some characterizations of the distribution. This article is expected to serve as a reference and stimulate further research work on the GPD.

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Fractal Dimensions and Scaling Laws in the Interstellar Medium and Galaxy Distributions: A New Field Theory Approach

Vega

Sánchez

Combes

1998

Current Topics in Astrofundamental Physics: Primordial Cosmology

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We develop a field theoretical approach to the cold interstellar medium (ISM) and large structure of the universe. We show that a non-relativistic self-gravitating gas in thermal equilibrium with variable number of atoms or fragments is exactly equivalent to a field theory of a single scalar field φ( x) with exponential self-interaction. We analyze this field theory perturbatively and non-perturbatively through the renormalization group approach. We show scaling behaviour (critical) for a continuous range of the temperature and of the other physical parameters. We derive in this framework the scaling relation M (R) ∼ R d H for the mass on a region of size R, and ∆v ∼ R q for the velocity dispersion where q = 1 2 (d H − 1). For the density-density correlations we find a power-law behaviour for large distances ∼ | r 1 − r 2 | 2d H −6 . The fractal dimension d H turns to be related with the critical exponent ν of the correlation length by d H = 1/ν. The renormalization group approach for a single component scalar field in three dimensions states that the long-distance critical behaviour may be governed by the (nonperturbative) Ising fixed point. The Ising values of the scaling exponents are ν = 0.631..., d H = 1.585... and q = 0.293.... Mean field theory yields for the scaling exponents ν = 1/2, d H = 2 and q = 1/2. Both the Ising and the mean field values are compatible with the present ISM observational data: 1.4 ≤ d H ≤ 2, 0.3 ≤ q ≤ 0.6 . As typical in critical phenomena, the scaling behaviour and critical exponents of the ISM can be obtained without dwelling into the dynamical (time-dependent) behaviour. We develop a field theoretical approach to the galaxy distribution. We consider a gas of selfgravitating masses on the FRW background, in quasi-thermal equilibrium. We show that it exhibits scaling behaviour by renormalization group methods. The galaxy correlations are first computed assuming homogeneity for very large scales and then without assuming homogeneity. In the first case we find ξ(r) ≡< ρ( r 0 )ρ( r 0 + r) > / < ρ > 2 −1 ∼ r −γ , with γ = 2. In the second case we find D(r) =< ρ( r 0 )ρ( r 0 + r) > ∼ r −Γ with Γ = 1. While the universe

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Gravitational clustering of galaxies: Comparison between thermodynamic theory and N-body simulations. IV - The effects of continuous mass spectra

Cited by 50 publications

References 0 publications

The Observed Distribution Function of Peculiar Velocities of Galaxies

The Observed Distribution Function of Peculiar Velocities of Galaxies

Generalized Poisson Distributions

Fractal Dimensions and Scaling Laws in the Interstellar Medium and Galaxy Distributions: A New Field Theory Approach

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