Probing cosmic structure formation in the wavelet representation Li-Zhi Fang University of Arizona...
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Transcript of Probing cosmic structure formation in the wavelet representation Li-Zhi Fang University of Arizona...
Probing cosmic structure formation in the wavelet representation
Li-Zhi FangUniversity of Arizona
IPAM, November 10, 2004IPAM, November 10, 2004
outline
• introduction
• phenomenological hierarchical clustering models and scale-scale correlation
• intermittency and small scale problem of LCDM model
• quasi-local evolution
• summary
cosmic random fields
• density distribution• velocity field • temperature • entropy • …
),(
),(
),(
),(
tS
tT
t
t
x
x
xv
x
density distribution of hydrogen gas in the LCDM model ),( tx
Feng,Shu, Zhang (2004)
Information of structures: position, scaledark matter baryon gas
representations• x-representation f(x,t)
• k(p)-representation f(k,t), f(p,t),
• Wigner distribution function (WDF), Wigner representation W(x,k,t), W(x,p,t),
phase-space behavior (position and scale) coherent structure phase-sensitive effects
WDF is density matrix, not a linear transform of f(x,t).
2 kx
j=1
j=2
j=3
j=4
mode (j, l)
)12...0( jl
space-scale decompositionby discrete wavelet mode
)()(~),(
)(),()(~
0
12
1
0
xttxf
dxxtxft
jlj l
jl
L
jljl
j
WFCs (wavelet functioncoefficients) of mode (j, l) represents fluctuations on a length scale L/2j
jl~
dynamical models of cosmic structure formation cosmological parameters, initial perturbations
simulation sample
observational samples
predictions
N-body simulationhydrodynamic simulationpseudo-hydro simulationlognormal model
1-D, 2-D, 3-Dbackground radiationIGM, galaxies
wavelet
wavelet
wavelet
hierarchical clustering
scale
j
j+1
j+2
small halos
massive halo
block model
Cole, Kaiser (1988)
2j
branching model
Pando, Lipa, Greiner, Fang (1998)
The first and second orders statistical properties of the block model and branching model are the same if
Pando, Lipa, Greiner, Fang (1998)
scale-scale correlation
1, ppjC
j
j
jC 22
422,2
)1(
)61(
block model
12
0
12
0' ',,
12
0 2,1,1
,1 ~~
~~2j j
j
l l
plj
plj
l
plj
plj
jpp
jC
branching model
Pando, Lipa, Greiner, Fang (1998)
Pando, Lipa, Greiner, Fang (1998)
Lu, Wolfe, Turnshek, sample of Ly-alpha absorption
branching model
Feng, Fang 2000
lognormal model
Feng, Deng, Fang 2000
APM-BGC galaxy sample
mock samples
problem of the LCDM model small scale powers
reducing the power on small scales relative to the `standard' LCDM model is favored by the analysis of WMAP plus galaxy and Lyman-alpha forest data. It can also solve the halo concentration and substructure problems.
Warm dark matter (WDM) models leads to exponential damping of linear power spectrum, and results in better agreement with observations
intermittencyThe lognormal model of IGM (baryon
gas)
(x,t)Jeans is a Gaussian random field derived from the density contrast
DM of dark matter filtered on the Jeans scale.
]2
),([
0
2
),(
JeansJeans t
IGM et
xx
Bi, Davidsen 1997
lognormal model at small scales
Feng, Fang 2000
lognormal field is intermittent
)()]()([
)]()([
][)(
2
2
2
2 nL
r
xrx
xrx
S
Sn
n
nr
nr
)1()( nnn
structure function
intermittent exponent
A field is intermittent if
Lognormal Field:
0)( n
structure function with DWT
][)(
ln1
)1()(
|~|2
1
2
2
2
212
0,
2
nj
nj
n
lljj
nj
S
S
jn
Sj
structure functions of Ly-alpha samples
Samples: 28 Keck HIRES QSO spectra. redshift z from 2.19 – 4.11
km/s24
s/km24.013
11
j
jk
Pando, Feng, Fang 2002
Structure Functions of Ly-alpha transmission
Pando, Feng,Jamkhedkar,Fang, 2002
LCDM
WDM
mw =1000ev
mw =800ev
mw =600ev
mw =300ev
pseudo hydro simulation
Feng, Pando, Fang 2003
simulation box 6 Mpc/h 12 Mpc/h
Fit Keck Data to
Pando, Feng, Jamkhedkar, Fang, 2002
j=11, 12 h-1 kpcj=10, 24 h-1 kpc
)1(log nnSF
Fit LCDM Data to
j=11, 12 h-1 kpcj=10, 24 h-1 kpc
)1(log nnSF
Pando, Feng, Jamkhedkar, Fang, 2002
Fit WDM 300 eV Data to
j=11, 12 h-1 kpcj=10, 24 h-1 kpc
)1(log nnSF
Pando, Feng, Jamkhedkar, Fang, 2002
quasi-local evolution of cosmic clustering
in the wavelet representation
Gaussian field in the DWT representation
''''~~
lljjljjl
j
l
2 kx
strongweak
quasi-locality (second order)
0l if ,0)(
~~
~~)(
',
2/12''
2/12
''',
l
l
jj
ljjl
ljjljj
different physical position
quasi-locality (higher order)
1)0(
~~
~~)(
,',
',',
',',,',
lC
lC
qpjj
qlj
plj
qlj
pljqp
jj
quasi-locality of mass field inZeld’ovich approximation
(weak linear regime)
If the initial perturbations are Gaussian, the cosmic gravitation clustering in weakly nonlinear regime given by the Zeldovich approximation is quasi-localized in the DWT representation.
Pando, Feng, Fang 2001
Mpch 2/189 1jPando, Feng, Fang 2001
second order quasi-locality : Ly-alpha data
Pando, Feng, Fang 2001Mpch 2/189 1j
second order quasi-locality : Ly-alpha data
Mpch 2/189 1j
Pando, Feng, Fang 2001
Ly-alpha data: second order
Pando, Feng, Fang 2001Mpch 2/189 1j
4th order locality: Ly-alpha data
halo model(highly nonlinear regime)
),()()( iii
iii
i mum xxxxx
mrm
rrrmru
sc
s
c
,
)(),(
Feng,Shu, Zhang (2004)
halo model
Xu, Fang, Wu 2000
quasi-locality of mass field in halo model
If the initial perturbations is Gaussian (no correlation between modes at different physical positions), the evolved field will also spatially weakly correlated. The nonlinear evolution of gravitational clustering has memory of the initial spatial correlations.
Feng, Fang 2004
Box size
(Mpc/h)
mp
(M_sun/h)
Lmin
(L_sun/h2)
Realizations
LCDM 100 6.5 x 108 2 x 108 4
LCDM 300 1.8 x 1010 3 x 109 4
N-body simulation samples
Jing, Suto (2000), Jing (2001)
Feng, Fang 2004
N-body simulation sample (Jing, Suto 2002)
One-point distribution of WFCs
Mpch 2/50 -1j
Feng, Fang 2004
two-point correlation functions: N-body simulation sample (Jing, Suto 2002)
Feng, Fang 2004
Scale-scale correlation: N-body simulation sample (Jing, Suto 2002)
Mpch 2/50 -1j
Feng, Fang 2004
DWT mode-mode correlations: N-body simulation sample (Jing, Suto 2002)
Feng, Fang 2004
Feng, Fang 2004
galaxy sample: 2MASS XSC (Jarrett et al. 2000)987,125 galaxies
Guo, Chu, Fang 2004
angular correlation functions: 2MASS data
Guo, Chu, Fang 2004
one-point distribution of WFCs: 2MASS data
Guo, Chu, Fang 2004degreeangular 2/28 j
mode-mode correlations of WFCs: 2MASS data
Guo, Chu, Fang 2004degreeangular 2/28 j
4th order correlations of WFCs: 2MASS data
degreeangular 2/28 j
Guo, Chu, Fang 2004
scale-scale angular correlation functions: 2MASS data
non-local scale-scale angular correlation functions: 2MASS data
Guo, Chu, Fang 2004
Initial perturbations probably are Gaussian on scales > 0.1 Mpc/h
other topics
• scaling of velocity field
• halos and the difference between the Fourier and DWT power spectrum
• redshift distortion and DWT power spectrum of non-diagonal modes
• the statistical decoupling of baryon gas from dark matter
summary• cosmic gravitational clustering essentially is
hierarchical and self-similar. A phase space description of clustering dynamics is necessary.
• The DWT with the features of similarity, admissibility, invertibility, orthogonal and locality in phase space provides an effective representation to describe the nonlinear evolution of the cosmic fields