An Alabastron by the Sphinx Painter

Weinberg, Saul S.

doi:10.2307/3774171

Cited by 3 publications

(4 citation statements)

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“…To the extent that the assumed and measured power spectra match, and the nal results agree with the original data, one has demonstrated consistency with the input model. Weinberg (1989) applied this technique on a volumelimited subsample of the Pisces-Perseus survey of Giovanelli & Haynes (1988). The power spectrum was consistent with that of standard CDM.…”

Section: Non-linear E Ectsmentioning

confidence: 81%

“…Here we wish to concentrate on methods to take redshift surveys back in time to their initial conditions. Weinberg (1989; adopts the assumption that the initial density distribution function is Gaussian, and notes that the rank order of densities is likely to be preserved even as non-linear e ects skew the distribution function. Thus he applies a technique called Gaussianization, whereby the rank order of the densities at di erent points is conserved, but the densities are reassigned to t a Gaussian form.…”

Section: Non-linear E Ectsmentioning

confidence: 99%

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The density and peculiar velocity fields of nearby galaxies

1995

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We review the quantitative science that can be and has been done with redshift and peculiar velocity surveys of galaxies in the nearby universe. After a brief background setting the cosmological context for this work, the rst part of this review focuses on redshift surveys. The practical issues of how redshift surveys are carried out, and how one turns a distribution of galaxies into a smoothed density eld, are discussed. Then follows a description of major redshift surveys that have been done, and the local cosmography out to 8,000 km s 1 that they have mapped. We then discuss in some detail the various quantitative cosmological tests that can be carried out with redshift data. The second half of this review concentrates on peculiar velocity studies, beginning with a thorough review of existing techniques. After discussing the various biases which plague peculiar velocity work, we survey quantitative analyses done with peculiar velocity surveys alone, and nally with the combination of data from both redshift and peculiar velocity surveys. The data presented rule out the standard Cold Dark Matter model, although several variants of Cold Dark Matter with more power on large scales fare better. All the data are consistent with the hypothesis that the initial density eld had a Gaussian distribution, although one cannot rule out broad classes of non-Gaussian models. Comparison of the peculiar velocity and density elds constrains the Cosmological Density Parameter. The results here are consistent with a at universe with mild biasing of the galaxies relative to dark matter, although open universe models are by no means ruled out.

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Section: Non-linear E Ectsmentioning

confidence: 81%

Section: Non-linear E Ectsmentioning

confidence: 99%

The density and peculiar velocity fields of nearby galaxies

1995

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“…Park 1990;Weinberg & Gunn 1990;Park & Gott 1991). As such models evolve in time, there is a draining of matter by gravity from minor walls onto filaments which produces an even larger network of voids as minor walls become so thinly populated as to effectively disappear (Weinberg 1990). This leaves a distinctive pattern of major and minor walls.…”

Section: Introductionmentioning

confidence: 99%

Topology of Large-Scale Structure by Galaxy Type: Hydrodynamic Simulations

Gott¹,

Cen²,

Ostriker³

1996

ApJ

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The topology of large scale structure is studied as a function of galaxy type using the genus statistic. In hydrodynamical cosmological CDM simulations, galaxies form on caustic surfaces (Zeldovich pancakes) then slowly drain onto filaments and clusters. The earliest forming galaxies in the simulations (defined as "ellipticals") are thus seen at the present epoch preferentially in clusters (tending toward a meatball topology), while the latest forming galaxies (defined as "spirals") are seen currently in a spongelike topology. The topology is measured by the genus (= number of "donut" holes -number of isolated regions) of the smoothed density-contour surfaces. The measured genus curve for all galaxies as a function of density obeys approximately the theoretical curve expected for random-phase initial conditions, but the early forming elliptical galaxies show a shift toward a meatball topology relative to the late forming spirals. Simulations using standard biasing schemes fail to show such an effect. Large observational samples separated by galaxy type could be used to test for this effect.

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“…Earlier attempts to reconstruct observational data include the reconstruction of the Perseus-Pisces redshift survey of Giovanelli & Haynes (1989) by Weinberg (1989) using the Gaussianization technique and the reconstruction of the IRAS 1.2Jy redshift survey by Kolatt et al (1996) using the dynamical scheme of Nusser & Dekel (1992). This dynamical scheme was also used by Nusser, Dekel & Yahil (1995) to recover the PDF of the initial density field from the IRAS 1.2Jy redshift survey.…”

Section: Introductionmentioning

confidence: 99%

Reconstruction Analysis of theIRASPoint Source Catalog Redshift Survey

Narayanan

Weinberg

Branchini

et al. 2001

ASTROPHYS J SUPPL S

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We present the results of reconstruction analysis of the galaxy distribution in a spherical region of radius 50h −1 Mpc centered on the Local Group, as mapped by the IRAS Point Source Catalog Redshift Survey (PSCz). We reconstruct this galaxy distribution using 15 different models for structure formation in the universe, each model consisting of a set of assumptions regarding the value of the cosmological mass density parameter Ω m , and the amplitude and nature of the biasing between IRAS galaxies and the underlying mass. For every model, we also reconstruct ten mock PSCz catalogs derived from the outputs of numerical simulations that have the appropriate values of Ω m and bias. We quantify the accuracy of a reconstruction using a variety of statistics and compare the accuracy of each reconstruction of the PSCz catalog to the accuracy expected based on the mock catalog reconstructions of the corresponding model. We find that gravitational instability of Gaussian primordial mass density fluctuations can account for the galaxy distribution in the PSCz catalog, at least for some plausible assumptions about the value of Ω m and the biasing between IRAS galaxies and mass. However, unbiased models in which IRAS galaxies trace mass fail to reconstruct the PSCz catalog accurately, both for Ω m = 0.4 and for Ω m = 1. Low Ω m models in which IRAS galaxies are antibiased with respect to the mass distribution are the most successful in reconstructing the PSCz catalog. In particular, a model with Ω m = 0.4 and IRAS galaxies related to the mass distribution according to the predictions of a semi-analytic galaxy formation model is very successful in reproducing the properties of the PSCz galaxy distribution.

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An Alabastron by the Sphinx Painter

Cited by 3 publications

References 0 publications

The density and peculiar velocity fields of nearby galaxies

The density and peculiar velocity fields of nearby galaxies

Topology of Large-Scale Structure by Galaxy Type: Hydrodynamic Simulations

Reconstruction Analysis of theIRASPoint Source Catalog Redshift Survey

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