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Alfredo Montana, Msc. Thesis @ INAOE

Simulations of the millimeter sky Alpha meeting @ Durham May 21, 2004 E.Gaztañaga I nstitut d'Estudis Espacials de Catalunya, IEEC/CSIC. INAOE - Barcelona Durham - Barcelona (Alfa, RAS-CSIC, IBM Earth-Simulator).

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Alfredo Montana, Msc. Thesis @ INAOE

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  1. Simulations of the millimeter skyAlpha meeting @ Durham May 21, 2004E.GaztañagaInstitut d'Estudis Espacials de Catalunya, IEEC/CSIC INAOE - Barcelona Durham - Barcelona (Alfa, RAS-CSIC, IBM Earth-Simulator) 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 Alfredo Montana, Msc. Thesis @ INAOE

  2. Alfredo Montana, Msc. Thesis @ INAOE 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

  3. PRIMARY & SECONDARY ANISOTROPIES Sachs-Wolfe (ApJ, 1967) DT/T(n) = [ 1/4 dg (n) + v.n + F (n) ]if Temp. F. = Photon-baryon fluid AP + Doppler + N.Potential (SW) SZ- Inverse Compton Scattering -> Polarization Ff Fi + Integrated Sachs-Wolfe (ISW) & Rees-Sciama (Nature, 1968) non-linear + 2 ∫if dtdF/dt(n) In EdS (linear regime) D(z) = a , and therfore dF/dt = 0 Not in L dominated universe !

  4. SDSS APM

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

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

  7. Pablo Fosalba, EG, F.Castander (astro-ph/0307249) 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) WL = 0.69-0.87 ( 2-sigma)

  8. Conclusions P.Fosalba, EG, F.Castander (astro-ph/ 0305468/0307249) 0.77 < WL < 0.85 ( 2-sigma) WMAP team (Nolta et al., astro-ph/0305467) and Boughm & Crittenden (astro-ph/0305001). Radio Galaxies (NVSS) z=0.8-1.0 SDSS team (Scranton et al 0307335) z=0.3-0.5 2dF (Myers etal 0306180, groups) 2Mass (Afshordi et al 0308260) z=0.1 • bias from gal-gal correlation: • Agree with z-evolution of ISW effect (WL ~ 0.8) • At smaller scales (1 deg) and low-z signal drops, indicating SZ. • No foreground contamination: clean, W and V-bands. • => WL = 0.69-0.87 ( 2-sigma) with SDSS+APM

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

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

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