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Figure 1:
Evolution of the cosmic scale factor as a function of ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 2:
Linear growth rate of density fluctuations. |
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Figure 3:
One-point PDFs in CDM models with Gaussian (left panels) and top-hat (right panels) smoothing windows: ![]() ![]() ![]() ![]() |
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Figure 4:
Isodensity surfaces of dark matter distribution from ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 5:
Top-view of distribution of objects at ![]() ![]() ![]() ![]() |
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Figure 6:
Same as Figure 5, but at ![]() |
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Figure 7:
Auto- and cross-correlation functions of dark matter and peaks in SCDM (left panels), LCDM (middle panels), and OCDM (right panels) for (a) ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 8:
Same as Figure 7, but for a halo model, again for (a) ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 9:
Distribution of gas particles (upper right panel), dark matter particles (upper left panel), galaxies (lower right panel), and dark halos (lower left panel) in the volume of a ![]() ![]() |
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Figure 10:
Snapshots of the most massive cluster ( ![]() ![]() ![]() |
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Figure 11:
Joint probability distributions of overdensity fields for dark halos and galaxies with dark matter overdensity smoothed over ![]() ![]() ![]() ![]() ![]() |
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Figure 12:
Two-point correlation functions of dark matter, galaxies, and dark halos from cosmological hydrodynamical simulations. (Figure taken from [103].) |
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Figure 13:
Two-point correlation functions for the old and young populations of galaxies at ![]() ![]() |
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Figure 14:
Mass two-point correlation functions on the light-cone for particles with redshift-dependent selection functions in the SCDM model, for ![]() ![]() ![]() |
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Figure 15:
Same as Figure 14 but for the ![]() |
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Figure 16:
Two-dimensional power spectra in cosmological redshift space at ![]() |
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Figure 17:
The confidence contours on the ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 18:
Light-cone and cosmological redshift-space distortion effects on angle-averaged power spectra. (Figure taken from [84].) |
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Figure 19:
Same as Figure 18 on angle-averaged two-point correlation functions. (Figure taken from [84].) |
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Figure 20:
The 2dFGRS fields (small circles) superimposed on the APM catalogue area (dotted outlines of Sky Survey plates). |
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Figure 21:
The distribution of 63,000 2dFGRS galaxies in the NGP (left panel) and SGP (right panel) strips. |
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Figure 22:
3D redshift-space map centered on us, and its projection on the celestial sphere of SDSS galaxy subset, including the three main regions. (Figure taken from [32].) |
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Figure 23:
Redshift slices of SDSS galaxy data around the equatorial plane. The redshift limits and the thickness of the planes are ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 24:
The power spectrum of the 2dFGRS. The points with error bars show the measured 2dFGRS power spectrum measurements in redshift space, convolved with the window function. Also plotted are linear CDM models with neutrino contribution of ![]() ![]() ![]() ![]() |
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Figure 25:
The variation of the galaxy biasing parameter with luminosity, relative to an ![]() |
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Figure 26:
The two point correlation function ![]() |
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Figure 27:
The correlation function for early and late spectral types. The solid lines show best-fitting models, whereas the dashes lines are extrapolations of these lines. (Figure taken from [45].) |
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Figure 28:
The SDSS (EDR) projected correlation function for blue (squares), red (triangles) and the full sample, with best-fitting models over the range ![]() |
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Figure 29:
Dimensionless amplitude of the three-point correlation functions of SDSS galaxies in redshift space. The galaxies are classified according to their colors; all galaxies in open circles, red galaxies in solid triangles, and blue galaxies in crosses. (Figure taken from [39].) |
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Figure 30:
Same as Figure 29, but for the inverse of the biasing parameter defined through the two-point correlation functions. (Figure taken from [39].) |
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Figure 31:
MFs as a function of ![]() ![]() ![]() ![]() ![]() ![]() |
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