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On scales larger than few arcminutes, the millimeter sky is dominated by CMB
temperature fluctuations.
A significant fraction of these CMB photons encode a wealth of information about its
interaction with the local matter distribution (eg lensing, SZ, ISW or Rees-Sciama
effects).
On smaller scales, the millimeter sky is dominated by high redshift star forming
galaxies (see talk by D.H.Hughes). All this provides a complementary tool to
optical/IR view of the universe
Simulations of the millimeter sky
Alpha meeting @ Durham May 21, 2004E.Gaztañaga
Institut d'Estudis Espacials de Catalunya, IEEC/CSIC
Alfredo Montana, Msc. Thesis @ INAOE
INAOE - Barcelona
Durham - Barcelona
(Alfa, RAS-CSIC, IBM Earth-Simulator)
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How to get Dark Energy from the millimeter
sky:
- Modeling cosmological parameters with the acoustic peaks GTM?.
- Normalization of CMB fluctuations from recombination to today (sigma_8).
- Volume dV/dz: eg optical/spect follow-up (GTC) of SZ Cluster Surveys (GTM).
- CMB lensing/polarization surveys.
- Star formation history of the universe (GTM).
- Cross-correlating optical/IR objects with CMB fluctuations.
Miguel Aragon, Msc. Thesis @ INAOE
Alfredo Montana, Msc. Thesis @ INAOE
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PRIMARY & SECONDARY ANISOTROPIES
Sachs-Wolfe (ApJ, 1967)
T/T(n) = [ 1/4 (n) + v.n + (n) ]if
Temp. F. = Photon-baryon fluid AP + Doppler + N.Potential (SW)
i
f
In EdS (linear regime) D(z) = a , and therfore dd
Not in dominated universe !
SZ- Inverse Compton Scattering -> Polarization
+ Integrated Sachs-Wolfe (ISW) & Rees-Sciama (Nature, 1968) non-linear
+ 2 ∫if d dd(n)
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APM
SDSS
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APM
WMAPAPM
APM
WMAP
WMAPAPM
WMAP
0.7 deg FWHM
0.7 deg FWHM
5.0 deg FWHM
5.0 deg FWHM
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0.7 deg FWHM
0.7 deg FWHM
5.0 deg FWHM
5.0 deg FWHM
WMAPWMAP
SDSS SDSS
WMAPSDSS
WMAPSDSS
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Significance (null detection):
SDSS high-z:
P= 0.3% for < 10 deg.
(P=1.4% for 4-10 deg)
SDSS all: P= 4.8%
Combined: P=0.1 - 0.03%
(3.3 - 3.6 sigma)
Pablo Fosalba, EG, F.Castander
(astro-ph/0307249)
= 0.69-0.87 ( 2-sigma)
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ConclusionsP.Fosalba, EG, F.Castander (astro-ph/ 0305468/0307249)
1. WMAP team (Nolta et al., astro-ph/0305467) and Boughm & Crittenden (astro-ph/0305001). Radio Galaxies (NVSS) z=0.8-1.0
2. SDSS team (Scranton et al 0307335) z=0.3-0.5
3. 2dF (Myers etal 0306180, groups)
4. 2Mass (Afshordi et al 0308260) z=0.1
• bias from gal-gal correlation:
• Agree with z-evolution of ISW effect ( ~ 0.8)
• At smaller scales (1 deg) and low-z signal drops, indicating SZ.
• No foreground contamination: clean, W and V-bands.
• => = 0.69-0.87 ( 2-sigma) with SDSS+APM
0.77 < < 0.85 ( 2-sigma)
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Simulating the mm sky
HOW?-Large area (>1000 sqr.deg.’s)
-Large scales (>1 Mpc)
- Back to high redshifts (z=1 => L=1000’s Mpc)
=> Hubble Volume Simulations
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WHY?- Non-linear effects.
- Projection effects.
-SZ, lensing, sub-mm /dust in galaxies
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Simulating mm sky
DM HV sim
Grav Pot.
CMB sim
Galxies.
Delta T.
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bias
Daniel Rosa-Gonzalez
Z=1.0 +/- 0.2
5x5 deg^2 proyection
dust cross