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. Puget Importance of foregrounds for very sensitive polarization measurements:
• the synchrotron spectral index is variable • The dust polarization is high • the dust emission long wavelenths spectrum is somewhat flatter than expected
Berlin, May 18th, 2004 J.L. Puget Berlin, May 18th, 2004 J.L. Puget Berlin, May 18th, 2004 J.L. Puget noise power spectrum of the electronic detection chain QM (REU + PAU + J-FET) nominal noise 7nV/Hz1/2
Berlin, May 18th, 2004 J.L. Puget Blind bolometer on the Qualification model of the FPS cooled to 98mK
Berlin, May 18th, 2004 J.L. Puget ARCHEOPS as a Planck HFI demonstrator
• ARCHEOPS is a balloon borne experiment with a Planck HFI type focal plane – same bolometers, horns, filters, dilution cooler, total power readout electronics – Planck telescope, about 10 arc minutes resolution – He cryostat – scanning strategy similar to Planck spinning at 2 RPM – capability to cover 1/3 of the sky in one flight
Berlin, May 18th, 2004 J.L. Puget RESULTS I (353 GHz)
Cygnus Gemini
Cassiopeia Taurus
mKRJ 17% of sky, Galactic anticenter Smoothed, 1deg
Berlin, May 18th, 2004 J.L. Puget Signal to noise 2 2 2 2 (Q + U )/(σQ + σU )
1σ 1.1 2σ 3.1 3σ 5.8 Smoothed, 1deg
Berlin, May 18th, 2004 J.L. Puget Berlin, May 18th, 2004 J.L. Puget Mode B tensor spectral index nT ΛCDM : nT = -0.3, -0.2, -0.1, 0, 0.1, 0.2
T TE
Variance cosmique E B
Berlin, May 18th, 2004 J.L. Puget