Fundamental physics and cosmology CMB polarization and cosmology J.L. Puget Institut d'Astrophysique Spatiale Orsay Berlin, May 18th, 2004 J.L. Puget Standard cosmology : reverse the expansion... 16 -42 10 GeV GUT 10 s Theoretical extrapolations -32 1015 GeV 10 s (high energy) 300 GeV E-W Transition 10-10 s 0.1 MeV Nucleosynthesis 100 s Known Physics 1 eV 104 yrs (low energy) Matter-Radiation equality 0.1 eV 5 Z=1000 10 yrs Z=20 ? Reionization Remarkable achievements : • Light elements abundance Z=10 Galaxies prediction Z=4 Clusters • Existence and correct temperature Z=0 of the CMB 0.2 meV 14 109 yrs Berlin, May 18th, 2004 J.L. Puget Problems... 1. High energy symetry breakings t ≈ 0 A B generate magnetic monopoles, stables, heavy: ~1016 GeV CMB ÒMm ý Òtot Causal Causal Horizon A Horizon B 2. We now measure: Ωtot ≈ 1 à43 à60 jÒtot(10 sec) à 1jô O(10 ) 3. Causal distance in the sky: 1 deg Observer ÉT=T ø 10à5 4. Large scale structures generation in an isotropic and homogeneous universe. Berlin, May 18th, 2004 J.L. Puget The Inflation C GUT Inflation A B 1016GeV -42 GUT 10 s 1015GeV 10-32s 300GeV E-W Transition 10-10s Inflationary causal horizon 0.1MeV Nucleosynthesis 100s 1eV 104 yrs 0.1eV Matter-Radiation equality 5 Z=1000 10 yrs CMB z =1000 Z=20 ? Reionization Observer Z=10 Galaxies 1. Monopoles diluted Z=4 Clusters 2. Ω = 1 predicted Z=0 3. Diverging horizon 0.2meV 14 109yrs 4. Perturbations generation mechanism Berlin, May 18th, 2004 J.L. Puget Basic mechanism Scalar field going down to its minimum The Reheating sets the end of Inflation and the beginning of the standard expansion Main constraints : • Large scale structures • Primordial nucleosynthesis •CMB Kolb & Turner Berlin, May 18th, 2004 J.L. Puget High Energy Physics The gravitino (ψµ) problem Stable Unstable 10 eV 1 keV 1 GeV 100 GeV 1 TeV 10 TeV m3/2 GMSSB mSUGRA T < 1011 GeV n3=2 / TRH RH 16 Inflation ↔ GUT TRH ≈ 10 GeV + polarization Incompatible with a detection of tensor modes except in the Thermal inflation scenario. + constraints on m3/2 with primordial black holes Barrau & NP, 2004, PRD Berlin, May 18th, 2004 J.L. Puget fundamental physics and cosmology • inflation • string theory : extra dimensions, branes, cyclic universe • physics beyond the standard model : supersymetry (dark matter) • dark energy Berlin, May 18th, 2004 J.L. Puget CMB T0 = 2.725 ± 0.002 (95% CL) ÉT P (ò;þ) = almYlm(ò;þ) T0 lm ? h i 0 0 alma 0 0 =Clî ll î mm l m P ê 1 2 Cl = 2l+ 1 m jalmj • Sensitive to cosmological •Degeneracies parameters but • Cosmic Variance • accuracy ~ % Berlin, May 18th, 2004 J.L. Puget WMAP, février 2003 Bennett et al, 2003 WMAP + Ωtot = 1.02 ± 0.02 Ωm = 0.27 ± 0.04 ACBAR + CBI ns = 0.93 ± 0.03 + 2dF + Lyα ΩΛ = 0.73 ± 0.04 Ωb = 0.044 ± 0.004 Confirmation of ‘Standard’ ΛCDM (?) et… τ = 0.17 ± 0.04 Berlin, May 18th, 2004 J.L. Puget CMB polarization Temperature alone leaves degeneracies… T Variation of nT • Break of degeneracies • Window on Inflation • Neutrinos mass • Primordial Universe : light on GUT, SuSy Barrau & NP, 2004, PRD Berlin, May 18th, 2004 J.L. Puget Recombination Thomson scattering : dσ/dΩ ~ |ε.ε’|2 Isotropic radiation (monopole) y’ x’ ε z’ ’ e- y x ε z No polarization Berlin, May 18th, 2004 J.L. Puget Recombination Thomson scattering : dσ/dΩ ~ |ε.ε’|2 Dipole y’ x’ ε z’ ’ e- y x ε z No polarisation Berlin, May 18th, 2004 J.L. Puget Recombination Thomson scattering : dσ/dΩ ~ |ε.ε’|2 Quadrupole y’ x’ ε z’ ’ e- y x ε z Polarization Berlin, May 18th, 2004 J.L. Puget Berlin, May 18th, 2004 J.L. Puget CMB : global description y (QæiU)0(nê) =eç2i (Q+ iU)(nê) y’ x’ Projection ψ x P (QæiU)(nê) = lmaæ2;l mYæ2;l m(nê) Algebra… E < 0 E > 0 P E= aE Y lm lm lm P B < 0 B > 0 B= aB Y lm lm lm Newman & Penrose, (1966), J. Math. Phys., 7, 863 Seljak & Zaldarriaga, (1997), PRD 55, 1830 Berlin, May 18th, 2004 J.L. Puget Simplest inflation predictions • spectral index ns close to 1: ns-1 = -3(1+w)~0.05 • directly related to w=P/ρ ∼ −1: 1+w ~ 0.02 • primordial gravitational waves produce B mode polarization • inflation energy scale ~ GUT • tensor to scalar fluctuations: r~20 to 30 % • In cyclic universe r is very low Berlin, May 18th, 2004 J.L. Puget CMB polarization spectra 3 observables : T, E, B 6 spectra : TT, EE, BB, TE, TB, EB T, E : scalars B : pseudo-scalars TB, EB = 0 1 to 4 orders of magnitude weaker than T… Berlin, May 18th, 2004 J.L. Puget lensing of the CMB • lensing by dark matter structures at low z produces B mode polarization at sub degree scales – depends on the structure – depends on the expansion rate (which in turn affects the structure development) • lensing of CMB is a probe of dark energy complementary to weak lensing on galaxies Berlin, May 18th, 2004 J.L. Puget Neutrinos masses Oscillations experiments are only sensitive to the squared mass difference between the different neutrinos Modification of the mass spectrum Massive neutrinos cluster on large + non gaussian signature in the scale but free-stream on small scale polarization B mode WMAP (TT) + cosmo : mν < 0.23 eV B mode: mν < 0.05 eV Kaplinghat et al, 2002 Berlin, May 18th, 2004 J.L. Puget Experimental results 1 measurement EE (DASI) TE, WMAP Kovac et al, 2002 Reionization Upper limits EE TE de Oliveira Costa et al, 2002 Kogut et al, 2002 Berlin, May 18th, 2004 J.L. Puget Berlin, May 18th, 2004 J.L. Puget Planck can detect the tensor modes if inflation energy scale is the GUT scale (1016GeV) Planck Berlin, May 18th, 2004 J.L. Puget W. Hu Future experiments Dedicated CMB polarization satellite : EPIC Important efforts invested in the quest for CMB polarization Systematics and foregrounds ! Berlin, May 18th, 2004 J.L. Puget Planck mission concept • Planck conceived to be limited by foregrounds for T measurements – instantaneous sensitivity limited by photon noise (cryogenic detectors), total power measurements ` – broad frequency coverage: 30 GHz to 1 THz (2 technologies) – 5 arc minutes resolution for the best CMB channels – polarization measurements in a very broad ` range • For Polarization Planck will be sensitivity limited but the broad frequency coverage (30 GHz-353 GHz) should be very good for foregrounds • half way between WMAP and an inflation probe mission Berlin, May 18th, 2004 J.L. Puget Focal Plane Unit – Focal Plane System is FPU without horns, filters, bolometers – it does include blind bolometers and all thermometers 25 Berlin, May 18th, 2004 J.L. Puget FPS at Air Liquide Berlin, May 18th, 2004 J.L. Puget Planck planned capabilities Berlin, May 18th, 2004 J.L. Puget Planck Polarized planned capabilities (and comparison to WMAP) sensitivity for 20 arcmin pixels, Planck:14 months WMAP: 2 years Berlin, May 18th, 2004 J.L. Puget Measured performances: HFI • bolometers in specs (most time constants close to the goals, a few at the specification level, NEP below or within 10% of the photon noise) • excellent total optical efficiency measured in the ARCHEOPS flight (better than 40%) • read out electronics: no 1/f noise down to 10-2 Hz • many aspect of the Planck HFI concept have been tested with the ARCHEOPS balloon borne experiment Berlin, May 18th, 2004 J.L. Puget spectra on Archeops coverage linear fit with error bars in both coordinates nsidenside== 512 512 fcut(archeops)fcut(archeops) = = 0.1/38 0.1/38 Hz Hz nopondnopond chi2chi2 = = 23.6/24 23.6/24 goodnessgoodness of of fit fit q q = = 0.48 0.48 Berlin, May 18th, 2004 J.L. Puget Foregrounds 143 217 353 545 GHz Bremsstrahlung: Dust: Electrons are deviated by Dust is heated by nearby stars ISM atoms and radiates in the IR and Synchrotron: submm domains Electrons are deviated by the galactic magnetic field Significant contribution wrt the CMB + polarization… Berlin, May 18th, 2004 J.L. Puget Archeops maps Feb 7th 2002 12 hours of night data First submillimetric maps at 15 arcmin resolution, 30% sky 353 GHz 545 GHz 850 µm 550 µm Polarized 217 GHz 143 GHz 1.4 mm 2.1 mm Berlin, May 18th, 2004 J.L. Puget 7 6 3 1 4 9 Taurus Gemini 5 2 10 Cassiopeia 8 P (%) θ (deg) (Stat ,syst) 12.1 ± 1.8 ± 1.8 59 ± 4.7 ±1.0 8.5 ± 0.7 ± 2.6 85 ± 2.8 ± 3.1 22.2 ± 3.4 ± 4.0 78 ± 3.7 ±0.8 Taurus 7.5 ± 0.9 ±1.5 46 ± 3.6 ±2.0 5.3 ± 3.1 ± 1.5 101± 13.6 ± 6.3 23.3 ± 6.7 ±9.7 175 ± 7.5 ±3.2 7.2 ± 2.8 ±4.1 133 ± 11.5 ± 3.8 12.3 ± 2.9 ±2.6 87 ± 6.7 ±2.8 < 3.4 23 ± 16 ± 105 16.3 ± 1.7 ±3.5 89 ± 3.2 ±1.1 Berlin, May 18th, 2004 J.L. Puget Diffuse radiation 5 deg wide bands (except edges) Values scaled to mean intensity over -2 < b < 2) Orientation mainly orthogonal to the galactic plane P ~ 3-5% on average Berlin, May 18th, 2004 J.L. Puget Archeops / Polarization Dust will be the major foreground for CMB temperature measurements at high frequencies Fosalba et al 2002, ApJ, 564, 762 Serkowski et al Heiles Expectation of at least 3% in submm Stein 1966, ApJ, 144, 318 No measurement on large scales available yet Berlin, May 18th, 2004 J.L.