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STRUCTURE FORMATION
MATTEO VIEL
INAF and
INFN Trieste
SISSA LECTURE nr 6 - 15th March 2011
OUTLINE: LECTURES
1.
Structure formation: tools and the high redshift universe
2.
The dark ages and the universe at 21cm
3.
IGM cosmology at z=2=6
4.
IGM astrophysics at z=2-6
5. Cosmological probes LCDM scenario
6. Review of main concepts
GOING NON-LINEAR
MEAN CORR FUNCTION
WITHIN R
INITIAL
NEW
While non-linear ~ a3
For larger x
UNIVERSAL MASS CONSERVATION MAPPING
OF LINEAR INTO NON-LINEAR
GOING NON-LINEAR-I
COSMIC
EXPANSION
Measuring the cosmic expansion?
This is a fundamental quantity not related at all to the FRW equations! If you want
to do such a thing then…
COsmicDynamicEXperiment
Dz/Dt
(10-10 yr-1)
REDSHIFT
CODEX-I
Ultra-stable spectrograph
CODEX and cosmology -II
Liske et al., 2007, in preparation
CODEX and cosmology-III
CODEX only no priors
cosmological constant
CODEX only assuming flatness
72 ± 2 km/s/Mpc and d Wm = 1%
100 yrs
30 yrs
10 yrs
w = -1
w = w0 + w a ( 1 - a )
NON – LINEAR
EVOLUTION OF
COSMIC STRUCTURE
LECTURE # 1
Neutralino DM
Extrapolating a bit…. !!!
LECTURE # 2
21 cm cosmic structures
How would the universe at z~12 look like - III?
LCDM
DARK ENERGY
Gas overdensity
Neutral hydrogen fraction
SKY AND FREQUENCY INFORMATION
Radio sky much brighter
than CMB
LECTURE # 3
NEUTRINOS and LYMAN-a
Active neutrinos - VIII
Seljak, Slosar, McDonald, 2006, JCAP, 0610, 014
normal
3
1,2
inverted
2
1
3
2s limit
Tight constraints because data
are marginally compatible
mn (eV) < 0.17 (95 %C.L.), < 0.19 eV (Fogli et al. 08)
r < 0.22 (95 % C.L.)
running = -0.015 ± 0.012
Neff = 5.2 (3.2 without Ly a)
CMB + SN + SDSS gal+ SDSS Ly-a
Goobar et al. 06 get upper limits 2-3 times larger……
for forecasting see Gratton, Lewis, Efstathiou 2007
LECTURE # 4
FEEDBACK FROM GALACTIC
WINDS
Springel & Hernquist 2002,2003
LECTURE # 5
BAO
Cosmological parameters from baryonic oscillations
Baryonic acoustic oscillation in SDSS galaxy power spectrum detected in Dec 2004
46748 LRG in 0.72 (Gpc/h)3 at <z>=0.35 - Eisenstein et al., 2005, ApJ, 633,560
- They are a standard ruler and a signature of the photons-baryons interaction in the
the plasma at recombination (z=1100) and provide measurement of H (z) and DA (z)
- These soundwaves could either be seen in the CMB peaks or in the galaxy powerspec.
with the complication of: bias (galaxy-matter) and peculiar velocities
Physical length depends on the sound horizon at recombination
Different Wm h2
DM is angular diameter distance - from CMB
DV = [DM2 cz/H(z)] 1/3 distance - from LRG
dilation scale of the correlation function