Diapositiva 1

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PLANCK
LIMPATTO SULLA COSMOLOGIA
ALESSANDROMELCHIORRI
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PLANCK_at_ROMA1
(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

in collaborazione con
PLANCK_at_ROMA2
Grazia De Troia Marina Migliaccio Paolo
Natoli Nicola Vittorio Giancarlo de Gasperis .e
altro
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Current status of CMB observations
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We can measure cosmological parameters with CMB !
Wtot , Wb , Wc, L, t, h, ns,
Temperature Angular spectrum varies with
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How to get a bound on a cosmological parameter
Fiducial cosmological model (Obh2 , Omh2 , h ,
ns , t, Sm? )
PARAMETER ESTIMATES
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Dunkley et al., 2008
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Blu Dati attuali Rosso Planck
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F. De Bernardis, E. Calabrese, P. de Bernardis,
S. Masi, AM 2009
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Next experiment for measuring neutrino mass
KATRIN
Current limits from laboratory
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Constraints on Newtons constant
Likelihood
G/G0
S. Galli, A. Melchiorri, G. Smoot, O. Zahn,
arxiv0905.1808
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CMB Temperature Lensing
When the luminous source is the CMB, the lensing
effect essentially re-maps the temperature
field according to
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Analysis Method

• We phenomenologically uncoupled weak lensing from
  primary anisotropies by introducing a new
  parameter AL that scales the lensing potential
  such as
• AL0 corresponds to a theory ignoring lensing
• AL1 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).
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Future constraints
Planck

• HFI 143 GHz Channel
• fsky 1
• ?7
• NoiseVar3,4?10-4 µK2
• fiducial model with ACBARWMAP3 best fit
  parameters

Letting the lensing parameter vary, the obtained
constraints are
E. Calabrese, A. Slosar, A. Melchiorri, G. Smoot,
O. Zahn, PRD, 2008
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Calabrese, Martinelli, AM, Pagano, 2009
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CMB POLARIZATION

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Fluctuation and GW generator
Fluctuation amplifier But GW dissipator
Hot Dense Smooth
Cool Rarefied Clumpy
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On this map we see 100000 horizons at z1000.
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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.
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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-ModesGravity Waves !!
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Several inflationary models predict a sizable GW
background (rgt0.01) if nlt1. Pagano, Cooray,
Melchiorri And Kamionkowsky, JCAP 08.
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