large scale structure (galaxy correlations)...large scale structure (lss) structures larger than...
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Large Scale Structure(Galaxy Correlations)
Bob Nichol (ICG,Portsmouth)Bob Nichol (ICG,Portsmouth)
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Overview
• Redshift Surveys• Theoretical expectations• Statistical measurements of LSS• Observations of galaxy clustering• Baryon Acoustic Oscillations (BAO)• ISW effect
I will borrow heavily from two recent reviews:1.Percival et al. 2006, astro-ph/06015382.Nichol et al. 2007 (see my webpage)
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Redshift SurveysRich history from Hubble, through CfA, to SDSS
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Random galaxyz =
λobs
λemitted
−1
cz ≈ H0d(locally)
Z=0.182
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Redshift Surveys IINow on an industrial scale
Random galaxy
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SDSS (DR6 ~800k galaxies)SDSS (DR6 ~800k galaxies)QuickTime™ and a
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Apache Point
Fermilab
UWashington
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Large Scale Structure (LSS)
Structures larger than clusters, typically > 10Mpc(larger than a galaxy could have moved in a Hubble time)
Observational Definition
1.37 billion lyrs - 420 Mpcs
SDSS
2dfGRSCfA2
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CMBOnly gain insight from the combination of LSS & CMB
0.6<h<0.8
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Definitions
We define a dimensionless overdensity as
where δ<<1 on large scales. Then, the autocorrelation function is
where <> denote the average over an ensemble of points or densities. Assuming homogeneity and isotropy, then
In practical terms, the correlation function is given by
δ(x) =ρ(x)− ρ
ρ
ξ(x1, x2 ) = δ(x1)δ(x2 )
ξ(x1, x2 ) = ξ( x1 −x2 ) = ξ(r)
P12 = n2 (1+ξ(r))dV 2
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Definitions IIThe equivalent in Fourier space is the power spectrum
we have suppressed the volume term on the P(k) and therefore it has units of Mpc3
The correlation function and power spectrum are related
P(k) = ξ(r)e∫ ik .rd 3r
P(k) =1
(2π )3 δ(k1)δ(k2 ) = δdirac(k1 − k2 )P(k)
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Inflation
We do not consider inflation here. We just assume an adiabatic scale-invariant power spectrum of fluctuation created by quantum processes deep in the Inflationary era,
P(k) = kn (n ≈ 1)
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Jeans LengthAfter inflation, the evolution of density fluctuations in the
matter depend on scale and the composition of that matter (CDM, baryons, neutrinos, etc.)
An important scale is the Jeans Length which is the scale of fluctuation where pressure support equals gravitational collapse,
where cs is the sound speed of the matter, and ρ is the density of matter.
λJ =cs
Gρ
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Transfer FunctionThe ratio of the time-integrated growth on a particular
scale compared to scales much larger than the Jeans Length is known as the Transfer Function:
where δ(k,z) are density perturbations at k and z. By definition, T(k) goes to 1 on large scales. Therefore,
Eisenstein & Hu, 1998, 496, 605
Eisenstein & Hu, 1999, 511, 5
P(k) ≈ δ(k) 2 ≈ T (k)2
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Matter-radiation equality
For λ > λJ, the fluctuations grow at the same rate independent of scale and therefore, the primordial power spectrum is maintained
For λ < λJ, the fluctuations can not grow in the radiation era because of pressure support (or velocities for collisionless particles). In matter dominated era, pressure disappears and thus all scales can grow.
Therefore, in a Universe with CDM and radiation the Jeans length of the system grows to the particle horizon at matter-radiation equality and then falls to zero. Critical scale of λeq or keq
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Matter-radiation equality IIThe redshift of equality is
The particle horizon therefore is
which is imprinted on the power spectrum as fluctuations smaller than this scale are suppressed in the radiation era compared to scales on larger scales
The existence of dark energy and curvature today is insignificant. Ωm is the density of CDM and baryons
zeq ≈ 25000Ωmh
keq ≈ 0.075Ωmh2
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P(k) models[U
nits
of V
olum
e]
Primordial P(k) on large scales
T(k)~1
keq
keq
Full boltzmann codes now exist or fitting formulae
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Baryons
Although they make-up a small fraction of the density(which is dominated by CDM), they dominate the pressure term. Baryons have two effects on the T(k):
1. Suppression of the growth rates on scales smaller than the Jeans length
2. Baryon Acoustic Oscillations (BAO), which are sound waves in the primordial plasma
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Baryon Acoustic Oscillations
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baryons photons
Initial fluctuation in DM. Sound wave driven out by intense pressure at 0.57c.
Courtesy of Martin White
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Baryon Acoustic Oscillations
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baryons photons
After 105 years, we reach recombination and photons stream away leaving the baryons behind
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Baryon Acoustic Oscillations
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baryons photons
Photons free stream, while baryons remain still as pressure is gone
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Baryon Acoustic Oscillations
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baryons photons
Photons almost fully uniform, baryons are attracted back by the central DM fluctuation
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Courtesy of Martin White
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Baryon Acoustic Oscillations
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baryons photons
Today. Baryons and DM in equilibrium. The final configuration is the original peak at the center and an
echo (the sound horizon) ~150Mpc in radius
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Fourier transform gives sinusoidal
function
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Baryon Acoustic Oscillations
Daniel Eisenstein
Many superimposed waves. See them statistically
Sound horizon can be predicted once (physical) matter and baryon density known
≈ Ωmh2
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P(k) models II[U
nits
of V
olum
e]
Suppression of power
Stronger BAO
Lack of strong BAO means low baryon
fraction
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Neutrinos
The existence of massive neutrinos can also introduce a suppression of T(k) on small scales relative to their Jeans length. Degenerate with the suppression caused by baryons
Δ�k����π�P(k)
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Non-linear scales
We have discussed linear perturbations, but on small scales we must consider non-linear effects.
These can be modeled or numerically solved using N-body simulations etc.
k ~ 0.2 (~10 Mpc)
Coma
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Measuring ξ(r) or P(k)
Data
Random
r
Simple estimator:ξ(r) = DD(r)/RR(r) - 1
Advanced estimator:ξ(r) = (DD-RR)2/RR-1
The latter does a better job with edge effects, which cause a bias to the mean density of points
Usually 10x as many random points over SAME area / volume
Same techniques for P(k) - take Fourier transform of density field relative to a random catalog over same volume. Several techniques for this - see Tegmark et al.
and Pope et al. Also “weighted” and mark correlations
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Measuring ξ(r) IIEssential the random catalog looks like the real data!
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ξ(r) for LRGs
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Errors on ξ(r)
On small scales, the errors are Poisson
On large scales, errors correlated and typically larger than Poisson
• Use mocks catalogs• PROS: True measure of cosmic variance• CONS: Hard to include all observational
effects and model clustering• Use jack-knifes (JK)
• PROS: Uses the data directly• CONS: Noisy and unstable matrices
Hardest part of estimating these statistics
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Jack-knife Errors
5 64
2 3
Real Data • Split data into N equal subregions• Remove each subregion in turn and compute ξ(r )• Measure variance between regions as function of scale
5 64
1 3
N=6
σ 2 =(N −1)
N(
i=1
N
∑ ξi −ξ)2
Note the (N-1) factor because there or N-1 estimates of mean
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Latest P(k) from SDSS
keq ≈ 0.075Ωmh2
Ωm=0.22±0.04
Ωm=0.32±0.01
No turn-over yet seen in data!
2σ difference
Depart from “linear”predictions at much lower k than expected
Strongest evidence yet for Ωm << 1 and therefore, DE
Errors from mocks(correlated)
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Hindrances
There are two “hindrances” to the full interpretation of the P(k) or ξ(r)
• Redshift distortions
• Galaxy biasing
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Redshift distortions
Therefore we usually quote ξ(s) as the “redshift-space” correlation function, and ξ(r) as the “real-space”correlation function.
We can compute the 2D correlation function ξ(π,rp), then
“Fingers of God”
Infall around clusters
Expected
We only measure redshifts not distances
w(rp ) = 2 ξ(rp0
π max∫ ,π )dπ
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Biasing
Maximal ignorance
However, we know it depends on color & L
Is there also a scale dependence?
We see galaxies not dark matter
δgal = bδdm
P(k)gal = b2P(k)dm
bb*
= 0.85 + 0.15 LL*
+ 0.04(M* − M 0.1r)
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Biasing II
All galaxies reside in a DM halo
Elegant model to decompose intra-halophysics (biasing) from inter-halo physics (DM clustering)
Halo model
2-haloterm
1-haloterm
P(k) = P1−halo + P2−halo
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Biasing III
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Hindrances (cont.)
There are two “hindrances” to the full interpretation of the P(k) or ξ(r)
• Redshift distortions
• Galaxy biasing
How will we solve these problems?
Higher-order statistics can help greatly