The topology of large-scale structure. III - Analysis of observations

Gott, J. Richard; Miller, John B.; Thuan, T. X.; Schneider, S. E.; Weinberg, David H.; Gammie, Charles F.; Polk, Keith; Vogeley, Michael S.; Jeffrey, S.; Bhavsar, S. P.; Melott, Adrian L.; Giovanelli, Riccardo; Hayes, Michael; Tully, R. Brent; Hamilton, A.

doi:10.1086/167425

Cited by 105 publications

(119 citation statements)

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“…Many possible scenarios are combined and each resulting model predicts its particular topology. For example, good agreement is reached with the conclusion of Gott et al (1989) who state that the large-scale structure of the Universe is spongy rather than bubbly. This supports the comfortable idea that both galaxies and large-scale structures formed from gravitational instability in an inflationary stage of the early evolution of the Universe.…”

Section: Introductionsupporting

confidence: 54%

Detection of structures on multiple scales around the South Galactic Pole

Escalera

MacGillivray

1996

Astron. Astrophys. Suppl. Ser.

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Abstract. -We report the results of a 2D analysis of distributions of galaxies in a search for structures on a wide range of scales, from clusters up to superclusters and beyond, including the identification of voids. The structures are identified in data from the COSMOS/UKST Southern Sky Galaxy Catalogue (CUSSGC). The subsample used in this first investigation contains some 1.4 10 6 galaxies in an area of ∼ 69 × 44 degrees around the South Galactic Pole. From our analysis, we find 25 very large-scale structures (of 10 degrees or more in extent), about 60 structures of intermediate scales (superclusters and/or elongated features), and more than 220 cluster-sized objects. All these features are significant, having high confidence levels for detection. Some extended voids are also detected in this area, likewise with high significance. This work is based on the use of the wavelet transform, the method of which has already been extensively described in a previous paper in which we demonstrated the principle of the technique. The wavelet analysis gives the position of the structures detected, together with significance levels and some parametrisation of their properties (extent, population, elongation, etc). Ultimately, our aim is the construction of a large and homogeneous database of structures on all scales in this important part of the southern sky.

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Section: Introductionsupporting

confidence: 54%

Detection of structures on multiple scales around the South Galactic Pole

Escalera

MacGillivray

1996

Astron. Astrophys. Suppl. Ser.

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“…As an example of this approach, the genus of different iso-density contour surfaces [13][14][15][16][17] has recently been measured in the Sloan Digital Sky Survey (SDSS). The genus curve-i.e.…”

Section: Introductionmentioning

confidence: 99%

Probing cosmology with weak lensing Minkowski functionals

et al. 2012

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In this paper, we show that Minkowski Functionals (MFs) of weak gravitational lensing (WL) convergence maps contain significant non-Gaussian, cosmology-dependent information. To do this, we run a large suite of cosmological ray-tracing N-body simulations to create mock weak WL convergence maps, and study the cosmological information content of MFs derived from these maps. Our suite consists of 80 independent 512 3 N-body runs, covering seven different cosmologies, varying three cosmological parameters Ωm, w, and σ8 one at a time, around a fiducial ΛCDM model. In each cosmology, we use ray-tracing to create a thousand pseudo-independent 12 deg 2 convergence maps, and use these in a Monte Carlo procedure to estimate the joint confidence contours on the above three parameters. We include redshift tomography at three different source redshifts zs = 1, 1.5, 2, explore five different smoothing scales θG = 1, 2, 3, 5, 10 arcmin, and explicitly compare and combine the MFs with the WL power spectrum. We find that the MFs capture a substantial amount of information from non-Gaussian features of convergence maps, i.e. beyond the power spectrum. The MFs are particularly well suited to break degeneracies and to constrain the dark energy equation of state parameter w (by a factor of ≈ three better than from the power spectrum alone). The non-Gaussian information derives partly from the one-point function of the convergence (through V0, the "area" MF), and partly through non-linear spatial information (through combining different smoothing scales for V0, and through V1 and V2, the boundary length and genus MFs, respectively). In contrast to the power spectrum, the best constraints from the MFs are obtained only when multiple smoothing scales are combined.

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“…The genus statistic was used to characterize the topology (Gott et al , 1987(Gott et al , 1989Hamilton et al 1986;Vogeley et al 1994;Park et al 2005aPark et al , 2005b. Measuring the genus as a function of density (Gott et al , 1987 allows us to compare the topology observed with that expected for Gaussian random phase initial conditions, as predicted in a standard big bang inflationary model (Guth 1981;Linde 1983) where structure originates from random quantum fluctuations in the early universe.…”

Section: Introductionmentioning

confidence: 99%

Three-Dimensional Genus Topology of Luminous Red Galaxies

Gott

Choi

Park

et al. 2009

ApJ

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We measure the three-dimensional genus topology of large-scale structure using luminous red galaxies (LRGs) in the Sloan Digital Sky Survey and find it consistent with the Gaussian random phase initial conditions expected from the simplest scenarios of inflation. This studies three-dimensional topology on the largest scales ever obtained. The topology is spongelike. We measure topology in two volume-limited samples: a dense shallow sample studied with smoothing length of 21 h −1 Mpc, and a sparse deep sample studied with a smoothing length of 34 h −1 Mpc. The amplitude of the genus curve is measured with 4% uncertainty. Small distortions in the genus curve expected from nonlinear biasing and gravitational effects are well explained (to about 1σ accuracy) by N-body simulations using a subhalo-finding technique to locate LRGs. This suggests that the formation of LRGs is a clean problem that can be modeled well without any free-fitting parameters. This bodes well for using LRGs to measure the characteristic scales such as the baryon oscillation scale in future deep redshift surveys.

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The topology of large-scale structure. III - Analysis of observations

Cited by 105 publications

References 0 publications

Detection of structures on multiple scales around the South Galactic Pole

Detection of structures on multiple scales around the South Galactic Pole

Probing cosmology with weak lensing Minkowski functionals

Three-Dimensional Genus Topology of Luminous Red Galaxies

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