1. PLANCK
L’IMPATTO
SULLA
COSMOLOGIA
ALESSANDRO MELCHIORRI

3. PLANCK@ROMA1 PLANCK@ROMA2 (Analisi Dati e Implicazioni Cosmologiche)
Paolo de Bernardis (Roma1)
Erminia Calabrese (Roma1) (PhD)
Silvia Masi (Roma1)
Alessandro Melchiorri (Roma1)
Luca Pagano (Roma1) (PhD)
Francesco Piacentini
Francesco De Bernardis (PhD)
Silvia Galli (PhD)
Giulia Gubitosi (PhD)
Matteo Martinelli (PhD)
Stefania Pandolfi (PhD)
Marcella Veneziani (ass. ric).
Laureandi Magistrale:
Maria Archidiacono
Paolo Fermani
Elena Giusarma
Andrea Maselli
Eloisa Menegoni
Marco Ruzza
…in collaborazione con
Grazia De Troia
Marina Migliaccio
Paolo Natoli
Nicola Vittorio
Giancarlo de Gasperis
….e altro

6. Current status of CMB observations

7. We can measure cosmological parameters with CMB !
Wtot , Wb , Wc, L, t, h, ns, …
Temperature Angular spectrum varies with

8. How to get a bound on a cosmological parameter
Fiducial cosmological model:
(Ωbh2 , Ωmh2 , h , ns , τ, Σmν )
DATA
PARAMETER
ESTIMATES

9. Dunkley et al., 2008

10. Blu: Dati attuali
Rosso: Planck

11. F. De Bernardis, E. Calabrese, P. de Bernardis, S. Masi, AM 2009

12. Next experiment for measuring neutrino mass: KATRIN
Current limits from laboratory:

13. Constraints on Newton’s constant
Likelihood
G/G0
S. Galli, A. Melchiorri, G. Smoot, O. Zahn, arxiv:

16. CMB Temperature Lensing
unlensed
lensed
When the luminous source is the CMB, the lensing effect essentially
re-maps the temperature field according to :

17. Analysis Method
We 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 lensing
AL=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 constraints
Planck
HFI 143 GHz Channel:
fsky =1
θ=7’
NoiseVar=3,4·10-4 μK2
fiducial model with ACBAR+WMAP3 best fit parameters
Letting the lensing parameter vary, the obtained constraints are:
E. Calabrese, A. Slosar, A. Melchiorri, G. Smoot, O. Zahn, PRD, 2008

19. Calabrese, Martinelli, AM, Pagano, 2009

20. CMB POLARIZATION

25. Fluctuation and GW generator Fluctuation amplifier But GW dissipator…
Hot Dense Smooth
Cool Rarefied Clumpy

27. On this map we see 100000 horizons at z=1000….

29. SCALAR +
TENSOR =
We measure the
sum of the two spectra.
If GW are present this
lowers the amplitude
of the peak.
Degeneracy with other
Parameters.

31. CMB Polarization Polarization is described by Stokes-Q and -U
These are coordinate dependent
The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B).
Grad (or E) modes
Curl (or B) modes
(density fluctuations have no handness, so no contribution
to B-modes). B-Modes=Gravity Waves !!

33. Several inflationary
models predict
a sizable GW background
(r>0.01) if n<1.
Pagano, Cooray, Melchiorri
And Kamionkowsky, JCAP 08.