1. 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, 2004 E.Gaztañaga I nstitut d'Estudis Espacials de Catalunya, IEEC/CSIC Alfredo Montana, Msc. Thesis @ INAOE INAOE - Barcelona Durham - Barcelona (Alfa, RAS-CSIC, IBM Earth-Simulator)

2. 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

3. PRIMARY & SECONDARY ANISOTROPIES Sachs-Wolfe (ApJ, 1967)  T/T(n) = [ 1/4  (n) + v.n +  (n) ] i f Temp. F. = Photon-baryon fluid AP + Doppler + N.Potential (SW) ii ff In EdS (linear regime) D(z) = a, and therfore d  d   Not in  dominated universe ! SZ- Inverse Compton Scattering -> Polarization + Integrated Sachs-Wolfe (ISW) & Rees-Sciama (Nature, 1968) non-linear + 2 ∫ i f d  d  d  (n)

4. APM SDSS

5. APM WMAP  APM APM WMAP WMAP  APM WMAP 0.7 deg FWHM 5.0 deg FWHM

6. 0.7 deg FWHM 5.0 deg FWHM WMAP SDSS WMAP  SDSS

7. 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)

8. Conclusions P.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)

9. 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 WHY? - Non-linear effects. - Projection effects. -SZ, lensing, sub-mm /dust in galaxies

10. Simulating mm sky DM HV sim Grav Pot. CMB sim Galxies. Delta T. bias Daniel Rosa-Gonzalez Z=1.0 +/- 0.2 5x5 deg^2 proyection dust cross