16 CMB Temperature Lensing unlensedlensedWhen the luminous source is the CMB, the lensing effect essentiallyre-maps the temperature field according to :
17 Analysis MethodWe phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the lensing potential such as :AL=0 corresponds to a theory ignoring lensingAL=1 corresponds to the standard weak lensing scenario.AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks. In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0, 1, 3, 6, 9).
18 Letting the lensing parameter vary, the obtained constraints are: Future constraintsPlanckHFI 143 GHz Channel:fsky =1θ=7’NoiseVar=3,4·10-4 μK2fiducial model with ACBAR+WMAP3 best fit parametersLetting the lensing parameter vary, the obtained constraints are:E. Calabrese, A. Slosar, A. Melchiorri, G. Smoot, O. Zahn, PRD, 2008
31 CMB Polarization Polarization is described by Stokes-Q and -U These are coordinate dependentThe two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B).Grad (or E) modesCurl (or B) modes(density fluctuations have no handness, so no contributionto B-modes). B-Modes=Gravity Waves !!