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Orsay, Sept. 12 th 2005. Polarisation of the CMB An introduction. S. Prunet (IAP). Theoretical perspective. Theoretical introduction Gravitational waves signature in B modes Additional information on cosmological parameters Nature of perturbations: Scalars versus tensors - PowerPoint PPT Presentation
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Polarisation of the CMBAn introduction
S. Prunet (IAP)
Orsay, Sept. 12th 2005
Theoretical perspective
• Theoretical introduction
• Gravitational waves signature in B modes
• Additional information on cosmological parameters
• Nature of perturbations:– Scalars versus tensors– Adiabatic versus isocurvature
Polarisation: Physical origin• Generated by Thomson scattering• Due to quadrupolar anisotropy in the electron rest frame• Linked to velocity field gradients at recombination/reionisation
In the electron rest frame
Boltzmann transport equation describes the evolution of the photon distribution function
Collisional part describes the scattering of the photons with electrons
Gravitational part describes the motion of the photons in the perturbed background
Differential form in Fourier space
Calculation of Theoretical Cl
(e.g. CMBFAST)
Theory: a brief reminder
Scalar perturbations
Rotationally invariant polarisation variablesSummation on Fourier modes
Angle needed to rotate Stokes Parameters from k-dependentBasis to fixed frame on the sky
(Q+iU) is a spin-2 quantity
Decomposition on spin-2 harmonics
Rotationally invariant quantities
E and B modes of polarisation
Scalar quantity
Pseudo-scalar quantity
Scalar perturbations cannot produce B modesB modes are model-independent tracers of tensor perturbations
Computation of the spectrum
Linearized Einstein and Boltzmann equations
• System of coupled ODEs in multipole space (e.g. Bond & Efstathiou)• Closure relation at• Transport, gravity and collision phenomena intricately mixed• Slow codes (up to ½ hour per spectrum)
• “Line of sight” integration (e.g. Seljak & Zaldarriaga)• Closure relation of ODEs at low • Disentangle transport / projection effects from anisotropy sources• Fast codes (a few seconds per spectrum)
• Approximate calculations (e.g. DASH)• Very fast• Useful for parameter estimation with Markov chains (IS)
Polarisation power spectra
Wayne Hu
Effect of reionisation on polarisationEffect of reionisation: rescattering of CMB photons
http://background.uchicago.edu/~whu/
Amplitude – optical depth to LSS degeneracy: polarization does help !
Models with constant C2eà2üC are hard to separate with T only
Zaldarriaga, Spergel, Seljak 97
Impact on optical depth measurement
Impact on other cosmological parametersAdding polarisation: improved parameters measurements as a function of multipole
Case of the Planck mission
Zaldarriaga, Spergel, Seljak 97
Isocurvature perturbations
Introducing isocurvature modes invalidates parameter estimation…
Degeneracies are broken with polarisation measurements
Delicate cancellation in the temperature spectrum (most poorly determined combination in the Fisher matrix)
Bucher, Moodley, Turok 2001
Measuring polarisation improves a lot !
Bucher, Moodley, Turok 2001
Observing the polarisation
• Signal is tiny ! the field is (very) young !
• Multiple methods:– HEMTs vs bolometers– Interferometers versus scanned single dish– In common: huge increase of #detectors
• Data processing, detectors, are still in R&D phase
Polarisation: first measurement
First detection ofE-mode polarisationby DASI (2002)
3 years results:sharpened E detection
Kovac et al. 2002Leitch et al. 2005
PolarisationUpper limits and first measurement by DASI
Polarisation spectra: present observational status
EE power spectrumTE cross-spectrum
B03
DASICBI
CAPMAP
WMAP
Interferometer - HEMTs
HEMTs- differential
Interferometer - HEMTs
Sing. dish - HEMTs
Sing. Dish - Bolometers
Montroy et al. 2005
Piacentini et al. 2005
Cosmological consistency
WMAP TT+TE CBI+B03+DASI EE+TE WMAP TT+TE + CBI+B03+DASI TT+TE+EE
Sievers et al. 2005
Polarisation: on-going
QUAD
BICEP
Polarisation: Planck (>= 2007)
Nice propaganda ! But does not include systematics …
http://background.uchicago.edu/~whu/
Space-borne polarimeter
• Specific design to control instrumental systematics– Thermal stability (tiny signals !)– Instrumental polarisation control– Optimized scanning strategy
• Detectors are ~background limited– Need a lot of them !!– Detector arrays, no horns, big focal planes
Specific needs
Polarisation: the future challenge
• Primordial GW background: no theoretical prior on amplitude…• One-field inflationary models: Tensor amplitude varies as E inf
4
• Lensing-induced B-modes: dominant at least on small scales• Polarized foreground emissions are nearly unknown ...
Cou
rtes
y E
PIC
con
sort
ium
Polarisation from space: requirements
• Large scales: space required• Stable environment: space …• Detectors are background limited
• need lots of them !• detector arrays• large telemetry …
• Stringent systematics control
Courtesy EPIC consortium
Lensing-induced B-mode cleaning
Kesden, Cooray, Kamionkowski (2002)
Substract lensing-induced BB by reconstruction of deflection angle using 4-point minimum variance estimators (Hu & Okamoto 2002)
Exponantial cut-off of CMB anisotropies at small scales limits lensing reconstruction
Lensing “cleaning”: improvement ?
Hirata & Seljak 2003
• Iterative ML method• Gains in the low-noise limitby reducing the CV of the residual
Cut-sky effects: E-B mixing
• Mixing occurs from line integrals on the border• Define STF windows that project out E contribution• This can be achieved by SVD of coupling matrix• For each m, 2 modes are lost
Lewis, Challinor, Turok 2001
• Separation is done at the map level• Block-diagonal structure of coupling allows to gain CPU time for azimuthally symmetric patches• Pixel effects can be important if no quadrature sampling … (e.g. Bunn et al. 2002)
E-B mixing: statistical separation• Use integrals of the Stokes correlations functions over observed angular range to construct pure E and B statistics• Originally derived for lensing (Crittenden et al. 2002)• Generalized to the sphere (Chon et al. 2004) and coupled to fast, edge-corrected estimation of correlation functions
Fast decoupled, edge-corrected estimators of polarized spectra available
• E-B separation only in the mean !• E-mode cosmic variance leaks into B-mode variance• Only valid for sufficiently large surveys (Challinor & Chon 2005)
OR
• Use the coupling kernels of polarised pseudo-Cls (Hansen & Gorski 2003)• Generalise MASTER (or FASTER) method• Regularised (binned) inversion of coupling kernel• This was used in the B03 data processing
The case of interferometers
Visibilities: sample the convolved UV space:
Idem for Q and U Stokes parameters
RL and LR baselines give (Q§iU)
Relationship between (Q,U) and (E,B) in UV (flat) space
Visibilities correlation matrix
UV coverage of a single pointing of CBI (10 freq. bands)( Pearson et al. 2003)
Pixelisation in UV/pixel space• Redundant measurements in UV-space• Possibility to compress the data ~w/o loss
• Hobson and Maisinger 2002• Myers et al. 2003• Park et al. 2003
Least squares solution
For an NGP pointing matrix:
Resultant noise matrix
Use in conjonction with an ML estimator
Newton-like iterative maximisation
Fisher matrix
Covariance derivatives for one visibility
Foregrounds: component separation• Unlike temperature, foregrounds are a big problem
• Bayesian methodology– Maximum A Posteriori maximization– Different priors give different methods
• Relaxing assumptions on foreground properties– Blind & semi-blind methods (spectral matching, ICA)– Spatially varying spectral indices
• Too many parameters Not good !– Astrophysics needed !!– Statistical (proper) characterization on templates for
prior building …
• Tucci et al. 2005• Ponthieu et al. 2005• Giardino et al. 2002• Tucci et al. 2000• Prunet et al. 1998
Bayesian formulation
Assume a linear problem:
Add in some important assumptions:• Azimuthally symmetric beams• Spatial-(E.M.) frequency decoupling• Statistical isotropy• Known mixing matrix
Tegmark &Efstathiou 1997Hobson et al. 1998Bouchet & Gispert 1999
Likelihood (gaussian noise)
Gaussian prior
WIENER FILTER
Wiener filter
• Optimal linear filter (min residual power)• Analytical predictions for errors
• on the maps• on the power spectra
• Easily extended to polarized data• Everything is assumed gaussian…
Fractional error on ClE:
• Dotted: best channel (no forgs)• Dashed: combined channels (no forgs)• Solid: WIENER (CMB+dust+sync.)
Bouchet, Prunet, Sethi 1999
The entropic prior: MEM• Initially designed for positive, uncorrelated distributions• Extended to non-positive distributions• Include correlations via Cholesky decomposition
with u, v, positive
Cross-entropy of the distributions:
• Non-linear maximization problem• Approximate error predictions (Fisher approach)• Recover Wiener in small-fluctuations limit
Hobson et al. 1998
Input processes
CMB
SZ (thermal)
SZ (kinetic)
Dust (thermal)
Free-freeSynchrotron
Hobson et al. 1998
•Planck specs•Assumed known spectra•Assumed known mixing matrix•MEM full ICF
10x10 deg
Hobson et al. 1998
Wiener full ICF
Hobson et al. 1998
Relaxing assumptions …
• Reality is more complex !!!• Keep (E.M) frequency – space factorization (no varying spectral indices)• Unknown Mixing matrix
BLIND METHODS
• Problem is non-linear• Needs good minimisation engine• Arbitrary parametrisation of E.M. behaviour• Direct fit of component power spectra: spectral matching (gaussian priors)
Bilinear model:
MATCH
Delabrouille, Cardoso, Patanchon 2003
Gaussian likelihood:
Parameters to adjust
Relaxing assumptionsCMB + DUST + SZ + NOISEHFI channels (6 frequencies)
EM and BFGS combined algorithmsDelabrouille, Cardoso, Patanchon 2003
• Relaxing (E.M.) frequency – space factorization e.g. Tegmark et al. 2000, Bennett et al. 2003, Eriksen et al. 2005• High S/N limit: maximize non-gaussianity (ICA) e.g. Maino et al. 2003, Stivoli et al. 2005 • Combined MEM/Wavelets: emissions and PS separation e.g. Vielva et al. 2001• Statistical isotropy of CMB/foregrounds e.g. Hajian & Souradeep 2003, de Oliveira-Costa et al. 2004, Prunet et al. 2005 • Etc !
Conclusions
• CMB physics OK
• Data processing: OK, but still in development phase
• Component separation: pfff…– Foregrounds are ugly (yes,yes)– Break about all assumptions you can do– Need to assess robustness of techniques– ASTROPHYSICAL INSIGHT NEEDED
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