- Page 1 and 2: arXiv:astro-ph/0112551v1 27 Dec 200
- Page 3: 4.1.1 Emergence of Non-Gaussianity
- Page 7 and 8: 1 Introduction and Notation Underst
- Page 9 and 10: with N-point functions, whereas Cha
- Page 11 and 12: Table 3 Notation for the Cosmic Fie
- Page 13 and 14: 2 Dynamics of Gravitational Instabi
- Page 15 and 16: In the following we will only use c
- Page 17 and 18: ∂u(x, τ) + H(τ) u(x, τ) = −
- Page 19 and 20: Eq. (17) we can write the vorticity
- Page 21 and 22: θn(k) = d 3 q1 . . . d 3 qn δD(k
- Page 23 and 24: 2.4.3 Cosmology Dependence of Non-L
- Page 25 and 26: approximation f(Ωm, ΩΛ) = Ω3
- Page 27 and 28: The somewhat complicated expression
- Page 29 and 30: where Φ denotes the gravitational
- Page 31 and 32: or more precisely D2(τ) ≈ − 3
- Page 33 and 34: ever turning around, washing out st
- Page 35 and 36: 2.9.2 Direct Summation Also known a
- Page 37 and 38: (e.g., [314,532]). Finally, it is w
- Page 39 and 40: such initial conditions are likely
- Page 41 and 42: 3.2.1 Statistical Homogeneity and I
- Page 43 and 44: δ 1 δ δ 2 3 c = δ1 c = 00000 11
- Page 45 and 46: 3.2.5 Probabilities and Correlation
- Page 47 and 48: 3.3.3 Generating Functions It is co
- Page 49 and 50: values of y are then also of the or
- Page 51 and 52: 4 From Dynamics to Statistics: N-Po
- Page 53 and 54: Figures 5 and 6 show the tree diagr
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e approximated by a fitting functio
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Fig. 10. The tree-level three-point
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4 2 0 0.2 0.4 0.6 0.8 0.2 0.4 0.6 0
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n P13/(πA 2 a 4 ) P22/(πA 2 a 4 )
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Fig. 13. The power spectrum for n =
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where: B222 ≡ 8 d 3 qPL(q, τ)F
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Fig. 16. The left panel shows the o
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them in Sect. 5.6. It is worth emph
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Fig. 17. The reduced bispectrum ˜
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(1) There are no characteristic tim
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velocity exactly cancels the Hubble
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A simple generalization of this arg
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growth factor has been written as D
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function in the stable clustering l
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S sat 4 (n) = 16 Qsat 4 (n) = 8 54
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For the reasons discussed in Sect.
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δ δ Evolution of an initially und
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obtained by expansion about Ωm =
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y the orthogonality relation betwee
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σ = 2 ; ν σ = ; 4 2 ν σ = 6 3
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(that plays a role similar to the v
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Fig. 26. The predicted Sp parameter
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Table 6 Tree-level and one-loop cor
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expressed in terms of the linear de
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give to non-Gaussian initial condit
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+ −4 + 8 3 SG 3 − 1 S 6 G 2 3
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the initial conditions. In Sect. 2.
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Fig. 30. The ratio of the tree-leve
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5.8 The Density PDF Up to now, we h
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Fig. 32. Comparison between predict
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9 5 p(δ) = 3/2 4π Ns(1 + δ) 3 σ
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Table 10 Parameters of the singular
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5.10.2 The Shape of the PDF The abo
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Fig. 35. Example of a joint PDF of
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Table 11 The coefficients a1,... ,a
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originally in previous work in the
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Table 12 Parameters used in fit (35
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6 From Theory to Observations: Esti
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the size of the catalog and optimiz
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The cosmic error is most useful whe
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expectation number ¯ N = ¯ngv, P
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1 〈δn(k1)δn(k2)δn(k3)〉 = N2
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catalog, the latter being equivalen
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size. In this regime, where ξ(r) i
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The expressions (395) and (400) can
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The techniques developed to measure
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At smaller scales, in the regime k
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Fig. 38. The top panel shows the me
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If ¯ng is determined with arbitrar
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Factorial moments thus verify Fk =
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To second order the cosmic bias [Eq
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The finite-volume error comes from
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6.7.5 Cosmic Error and Cosmic Bias
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factorial moment correlators [620]
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The generalization of Eq. (422) rea
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in [152]. Similarly to Eq. (472), t
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constrain theories with observation
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From this simple result, we see tha
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Fig. 41. The cosmic distribution fu
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of functions of the data ˆx. The p
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6.11.2 Quadratic Estimators In real
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is positive and compact in Fourier
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6.12 Measurements in N-Body Simulat
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7 Applications to Observations 7.1
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properties of the matter distributi
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deterministic bias results hold for
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effects due to the gravitational dy
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0000 1111 0000 1111 ϕ (y)= 0000 11
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where the volume V = 4πR3 /3 is re
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in Sect. 7.1.3, Eq. (555), plus Eqs
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In the following we first review th
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if the 3D correlation function is
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Table 13 Projection factors for dif
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Note that the rp coefficients are v
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Fig. 47. Tree-level PT predictions
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7.3 Weak Gravitational Lensing The
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elation (598) is then entirely dime
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7.4 Redshift Distortions In order t
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where [δD]n ≡ δD(k − k1 −
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proximation. In fact, Eq. (616) is
- Page 215 and 216:
Fig. 48. The left panel shows the b
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They obtained analogous results to
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that for wide surveys such as 2dFGR
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Machine, [374]) and COSMOS [421] mi
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Table 14 Angular Catalogs. The firs
- Page 225 and 226:
The DeepRange Catalog ([530] 1998)
- Page 227 and 228:
Fig. 50. The two-point angular corr
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Fig. 51. The APM 3D power spectrum
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linearization first done in [289] a
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most of the measurements only probe
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and Rb = 4.3 ± 1.2 [226]. These re
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3 2 1 3 2 1 0 -1 10 5 0 -5 -10 0 90
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Table 16 The reduced skewness and k
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estimations are split in its 6 × 6
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the near future. An early applicati
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The Stromlo-APM redshift survey ([4
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A recent linear analysis of the LCR
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at the non-linear scale, and no sig
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Fig. 57. The redshift-space reduced
- Page 253 and 254:
Table 19 Some measurements of S3 an
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Fig. 60. The redshift-space skewnes
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such as the abundance of massive cl
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the weakly non-linear regime is qui
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the mock catalogs. The resulting 3D
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few technical issues that need more
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A The Spherical Collapse Dynamics T
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More specifically we define ϕ(y) a
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∞ (−τ1) τ2 =ξ y1 νp p=1 p
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This result writes as a kind of com
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E PDF Construction from Cumulant Ge
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E.3 Approximate Forms for P(ρ) whe
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A simple change of variable, t 1−
- Page 279 and 280:
It is then easy to calculate cross-
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References [1] S.J. Aarseth, E.L. T
- Page 283 and 284:
[54] F. Bernardeau, R. Van De Weyga
- Page 285 and 286:
[100] A. Buchalter, M. Kamionkowski
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[150] S. Colombi, F.R. Bouchet, L.
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[196] G. Efstathiou, in Cosmology a
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[245] A. Gangui, Phys. Rev. D, 62,
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[299] A.J.S. Hamilton, M. Tegmark,
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[352] R. Jeannerot, Phys. Rev. D, 5
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[399] A.R. Liddle, D.H. Lyth, Phys.
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[448] P. McDonald, J. Miralda-Escud
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[497] J.A. Peacock, S. Cole, P. Nor
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[547] R.F. Sanford, 1917, Lick Obse
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[597] M. Snethlage, Metrica, 49, (1
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[644] A.N. Taylor, P.I.R. Watts, MN
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[692] M.B. Wise, in The Early Unive