Transcript CMB Polarization A New Tool for Cosmology & Fundamental Physics James G. Bartlett

CMB Polarization
A New Tool for Cosmology &
Fundamental Physics
James G. Bartlett
APC - Université Paris 7
We are approaching the ultimate limit on
CMB temperature measurements with
WMAP and Planck (2007)
The next major step is to measure the
polarization anisotropy: important
fundamental science
This is happening now…
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CMB Polarization – a new tool
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
The CMB and Cosmology
CMB polarization anisotropies
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
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Their use



Origin
Description (E & B modes)
Primordial gravity waves
Lensing (dark energy, neutrino mass)
Observational effort
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The CMB and
Cosmology
V ( )  EI4
GUT?
Perturbations
o density (scalar)
EI 6
matter ~ 3 ~ 105
M plV 
o gravity waves (tensor)
 gw
 EI 

~
M 
 pl 
r
2
T
 0.5
2
S
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m
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Dark Energy
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(douspis)
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State of the Art
(Spergel et al 02)
6 parameters & flat

  {h,  M h 2 ,  b h 2 , , As , ns }
h  0.72  0.05
 B h 2  0.024  0.001
 M h 2  0.14  0.02
As  0.9  0.1
ns  0.99  0.04
  0.166  0.076
r  0.5 (95%)
No running; WMAPext+LSS

WMAPext + LSS
m  0.6 eV (95%)
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The Planck Mission (2007)
(Planck Blue Book)
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CMB Polarization Anisotropies
Thompson scattering in the plasma
Hu & White 97
d
3
2


 T  
d 8
• Linear polarization
• Local quadrupole anisotropy
• Finite optical depth
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Two Kinds of Spatial Patterns
E-modes (even parity)
Density perturbations

k
k
Gravity waves

B-modes (odd parity)

k

k
Gravity waves
Gravitational lensing
Zaldarriaga
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Importance of decomposition


T (intensity), E & B call all be measured
separately
They isolate different physical processes
T spectrum
E spectrum
Cross TE spectrum
TT
l
EE
l
TE
l
C
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B spectrum
C
BB
l
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Gravity Waves
 EI 
T

r  2 
M 
S
 pl 
2
Produced with CAMB
4
r  0.5
E I ~ 3 1016 GeV
r  104
E I ~ 3.6 1015 GeV
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Fiducial WMAP Model
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  0.17
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Lensing
Hu & Okamoto astro-ph/ 0111606
(Zaldarriaga & Seljak 1998
Bernardeau 1997
Blanchard & Schneider 1987)
10 degs
Lensed E field
Unlensed E field
B-mode induced by lensing of E-mode
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Produced with CAMB
Grav. Lensing
Weak
lensing
signal
m
dark energy
Fiducial WMAP Model
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
 0.17 
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Uses of CMB Polarization
 Constraining ICs & tighter
constraints on params
 Gravity waves from
Inflation
 nature of gravity
 test of inflation
 energy scale
 Planck-era physics?
 Lensing reconstruction
 constraints on Dark Energy
 neutrino mass measurement
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Observational Effort
E & TE modes
first detected
by DASI
Oliveira-Costa et al. 02
Kovac et al. 2002
(South Pole Station)
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WMAP
TE cross power spectrum
Kogut et al. 2003
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BOOMERanG 03
MacTavish et al. 0507503
r  0.36 (95%)
CMBall+B03+LSS
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CBI
Sievers et al. 0509203
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Planck Polarization
(Planck Blue Book)
TE cross spectra
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Planck Polarization
(Planck Blue Book)
E spectra
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Planck Polarization
(Planck Blue Book)
Grav. Waves
r  0.1
  0.17
Lensing
B spectra
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Long-term Effort
Bowden et al. 04
~2005
Ground/
balloon
BICEP
QUaD
~2008-2010
ClOVER
Taylor
et al. 04
EBEX
PolarBear
QUIET
SPIDER
Grav. Waves
>2015
Dark Energy
 m  0.03 eV
(Kaplinghat et al. 2003)
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Ganga 04
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CMBpol (NASA
& ESA)
SAMPAN (CNES)
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Neutrino mass
Fogli et al. 2005
Should measure
Something!!
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Conclusions

Exciting Science
 Constraining ICs & tighter
constraints on params
 Gravity waves from
Inflation





Challenges
nature of gravity
test of inflation
energy scale
Planck-era physics?


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 Lensing reconstruction
 constraints on Dark Energy
 neutrino mass measurement

Sensitivity
Systematics
Foregrounds: TE, EE not
so bad, it would seem (on
small well-chosen
patches)… BB??
…
 Currently:
 Several measurements EE, TE
 Boomerang 03 r  0.36 (95%)
 Adiabatic seems good

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Orders of mag.to be
gained
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