Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy

12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference

Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy ΛCDM direct confirmation Doppler peaks structure of the CMB power spectrum hierarchical structure formation via gravitational instability cluster abundances at small redshifts spatial distribution and the number density of galaxies LSS matter power spectrum Lyman-α forest amplitude and spectrum ΛCDM issues on small scale: galaxy rotation curves too much substructure baryon angular momentum problems observed halos have softer cores, lower concentrations, less clumped

Probing Fundamental Physics with Planck: add physical properties to the ΛCDM model components Physics behind the dark components of the Universe - DM is the lightest supersymmetric particle? - DE is cosmological constant or quintescence field? - DM & DE are related by an unknown mechanism? - net contribution of the HDM Physics of inflation - nature of the primordial perturbations? - slope of the primordial perturbations depends of the inflation model? - can inflation be realized in string theory? - are cosmic defects produced at the end of inflation? Answer to these questions requires the control of the behavior of systematic effects and the detailed knowledge of the nature and behavior of the foregrounds 12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference

Control of systematic effects in LFI Systematic effects will produce different responses in the in the two instruments provided Planck with a powerful tool for detection and mitigation of systematic which will ensures that the final maps are limited only by instrument sensitivity and unavoidable astrophysical foregrounds sidelobe pickup of the Galaxy and solar system bodies (Burigana et al. 2001, 2004) distorted beam shapes (Burigana et al. 1998, 2001, Mandolesi et al. 2000) non-idealities in the radiometer (Seiffert et al. 2002) 1/f noise and destriping (Maino et al. 1999) effects induced by temperature instability (Mennella et al. 2002) spacecraft pointing errors and nutation (Bersanelli et al. 1996) LFI goal: systematic contribution less than 3μK

Planck is designed to extract all information available in temperature anisotropies of the CMB WMAP (1, 4 & 8 yrs) vs. Planck (14 months)

EE and TE are noise limited for l >1000 GW BB at l > 150 is swamped by the week lensing EE BB TE 12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference

Planck will achieve a major advance in polarization but will be limited by the knowledge of the polarized foregrounds Typical predicted range for E & B modes compared to the polarized foregrounds contamination

Planck can set significant constraints on primordial B-mode if polarized foregrounds are accurately known and subtracted

4 x 10 8 yrs WMAP 3-Yrs τ es 0.1 z re ~ 12 - affects the subsequent structure formation - direct consequence of the formation of the first structures and luminous souces

WMAP 3Yrs PLANCK x e x e 65% 65% 95% 95% 95% z re Spergel et al.2006 WMAP is not sensitive to the details of the ionization history Planck will distinguish among different ionization histories even when they imply the same value of τ es

Physical model of reionization J ( υ, z z sc c e τ 4π dt ε ( dz eff ( υ0, 0, ) 0) = υ z 0 z z, z) dz Ionizing UV flux dz dt = H + Ω + 3 0 1 z) m(1 z) + Ω ( cosmology V Ωb d * Ωm dt M dn ε( υ, z ) Lυ ( z) τlife f ( Mh, z) M dm min h h dm h source dt τ eff ( υ0, z0, z) = c κ( υ, z) dz dz z z 0 IGM properties

Reionization history with Planck When: z re, x e How long: Δz Once or twice Ionizing flux and feedback: UV/ X-ray POP III /POPII: z tr SFR IMF UV vs. FIR : role of zodiacal light

Uncertainty about the ionization history will provide a limit of 0.005 on how well τ es can be estimated from Planck polarization data

Physical model of recombination dx dz e dt = α dz [ ] C ( T ) x 2 n ( z) I ( z) I ( z) B e b s X i recombination rate ionization rate standard sources ionization rate other mechanisms inverse Compton scattering on CMB radiative decay Energy injection delays the recombination at z 10 3 and distorts the temporal evolution of the ionization fraction at high redshifts (z > z re ).

υ X υ a + e123 + + e γ I X i ( z) = (1 x e ) m E b 0 Ω Ω X b Γ X H ( z)

Knowledge of foregrounds and systematics will set the limit on how well we can constrain the Reionization History with CMB anisotropy measurements.