probing dark energy birefringence by cmb polarization
DESCRIPTION
Probing Dark Energy Birefringence by CMB polarization. Kin-Wang Ng ( 吳建宏 ) Institute of Physics & Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan IOP Mar 27, 2013. Collaborators: Guo-Chin Liu (TKU) Seokcheon Lee (KIAS) - PowerPoint PPT PresentationTRANSCRIPT
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Probing Dark Energy Birefringence
by CMB polarization
Kin-Wang Ng (吳建宏 )
Institute of Physics & Institute of Astronomy and Astrophysics,
Academia Sinica, Taiwan
IOP Mar 27, 2013
Collaborators: Guo-Chin Liu (TKU) Seokcheon Lee (KIAS) Da-Shin Lee (NDHU) Wolung Lee (NTNU)
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The Hot Big Bang Model
What is CDM?Weakly interacting but can gravitationally clump into halos
What is DE??Inert, smooth, anti-gravity!!
Dark Energy
70%
Cold Dark Matter25%
Baryonic Matter
5%
Cosmic Budget
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Do We Really Need Dark Energy
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CMB /SNe /LSS Constraints on Physical State of Dark Energy
SNAPsatellite
SabaruLSSTJDEMEUCLID
Equation of Statew = pDE / ρDE
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CMB Anisotropy and Polarization
• On large angular scales, matter imhomogeneities generate gravitational redshifts
• On small angular scales, acoustic oscillations in plasma on last scattering surface generate Doppler shifts
• Thomson scatterings with electrons generate polarization
Quadrupoleanisotropy
e
Linearly polarized
Thomsonscattering
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Point the telescope to the sky Measure CMB Stokes parameters: T = TCMB− Tmean, Q = TEW – TNS, U = TSE-NW – TSW-NE
Scan the sky and make a sky map Sky map contains CMB signal,
system noise, and foreground contamination including polarized galactic and extra-galactic emissions
Remove foreground contamination by multi-frequency subtraction scheme
Obtain the CMB sky map
RAW DATE
MULTI-FREQUENCY MAPS
MEASUREMENT
MAPMAKING
SKY
FOREGROUNDREMOVAL
CMBSKY MAP
CMB Measurements
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CMB Anisotropy and Polarization Angular Power Spectra
Decompose the CMB sky into a sum of spherical harmonics:
(Q − iU) (θ,φ) =Σlm a2,lm 2Ylm (θ,φ)
T(θ,φ) =Σlm alm Ylm (θ,φ)
(Q + iU) (θ,φ) =Σlm a-2,lm -2Ylm (θ,φ)
CBl =Σm (a*2,lm a2,lm − a*2,lm a-2,lm) B-polarization power spectrum
CTl =Σm (a*lm alm) anisotropy power spectrum
CEl =Σm (a*2,lm a2,lm+ a*2,lm a-2,lm ) E-polarization power spectrum
CTEl = − Σm (a*lm a2,lm) TE correlation power spectrum
(Q,U)
electric-type magnetic-type
l = 180 degrees/
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Theoretical Predictions for CMB Power Spectra
• Solving the radiative transfer equation for photons with electron scatterings
• Tracing the photons from the early ionized Universe through the last scattering surface to the present time
• Anisotropy induced by metric perturbations
• Polarization generated by photon-electron scatterings
• Power spectra dependent on the cosmic evolution governed by cosmological parameters such as matter content, density fluctuations, gravitational waves, ionization history, Hubble constant, and etc.
T
E
B
TE
Boxes are predicted errors in future Planck mission
[l(1
+1)
Cl/2
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CMB Anisotropy CTl 2013
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CMB Polarization Power Spectra 2013
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Best-fit 6-parameter ΛCDM model 2013
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Tensor/Scalar Ratio and Spectral Index 2013ns=0.9675 and r < 0.11 (95% CL)
r=Tensor/Scalar =Ph(k)/PR(k) at k0=0.05 Mpc-1
Beyond ΛCDM model
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Constant w w=w0+wa z/(1+z)
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Observational Constraints on Dark Energy
• Smooth, anti-gravitating, only clustering on very large scales in some models
• SNIa (z≤2): consistent with a CDM model
• CMB (z≈1100): DE=0.70, constant w=−1.7+0.5/−0.3 (Planck 13+WMAP)
• Combined all: DE=0.69, constant w=−1.13+0.13/−0.14 (Planck 13+WMAP+SNe)
• A cosmological constant? Not Yet! Very weak constraint on dynamical DE with a time-varying w
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What is Dark Energy
• DE physical state is measured indirectly through its gravitational effects on cosmological evolution, but what is the nature of DE?
• It is hard to imagine a realistic laboratory search for DE
• Is DE coupled to matter (cold dark matter or ordinary matter)? If so, then what would be the consequences?
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DE as a Scalar Field
S= ∫d4x [f(φ) ∂μφ∂μφ/2 −V(φ)] EOS w= p/ρ= ( K-V)/(K+V)Assume a spatially homogeneous scalar field φ(t) f(φ)=1 → K=φ2/2 → -1 < w < 1 quintessence any f(φ)→ negative K→ w < -1 phantom
kinetic energy K potential energy
.
V(φ)
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• Weak equivalent principle (plus polarized body) =>Einstein gravity =>φFF (Ni 77)
• Spontaneous breaking of a U(1) symmetry, like axion (Frieman et al. 95, Carroll 98)
• DE coupled to cold dark matter to alleviate coincidence problem (Uzan 99, Amendola 00,..)
• etc
A Coupling Dark Energy?
~
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Time-varying Equation of State w(z) (Lee, Ng PRD 03)
=0.7
=0.3
Time-averaged <w>= -0.78
SNIa
Affect the locations of CMB acoustic peaks Increase <w>
RedshiftLast scattering surface
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DE Coupling to Electromagnetism
This leads to photon dispersion relation
± left/right handed η conformal time
then, a rotational speed of polarization plane
Carroll, Field,Jackiw 90
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DE induced vacuum birefringence – Faraday rotation of CMB polarization
Liu,Lee,Ng PRL 06
electric-type magnetic-type
TE spectrum
φγ
β
CMB photon
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Parity violating EB,TB cross power spectra
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Radiative transfer equationμ=n·k, η: conformal timea: scale factorne: e densityσT: Thomson cross section
Source term forpolarization
Rotation angle
Faraday rotation
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g(η): radiative transfer functionST: source term for anisotropySP=SP
(0) r=η0 -η
Powerspectra
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Constraining β by CMB polarization data
2003 Flight of BOOMERANG
<TB>
Likelihood analysis assuming reasonable quintessence models
c.l.
M reduced Planck mass
More stringent limits from WMAP team and QUaD team ‘09
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Gravitational-wave B mode mimicked by late-time quintessence evoution (z<10)
Lensing B mode mimicked by early quintessence evolution
Future search for B mode
CAUTION! Must check with TB and EB cross spectra
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Including Dark Energy PerturbationDark energyperturbation
time and space dependent rotation
Perturbation induced polarization power spectra in previous quintessence models are small Interestingly, in nearly ΛCDM models (no time evolution of the mean field), birefringence generates <BB> while <TB>=<EB>=0
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Dark energy perturbation with w=-1 Lee,Liu,Ng 13
Birefringence generates <BB> while <TB>=<EB>=0
B mode
B mode
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Summary
• Future observations such as SNe, lensing, galaxy survey, CMB, etc. to measure w(z) at high-z or test Einstein gravity
• However, it is also important to probe the nature of DE
• DE coupled to cold dark matter => effects on CMB and matter power spectra, BAO
• DE coupled to photon => time variation of the fine structure constant and creation of large-scale magnetic fields at z ~ 6
• Using CMB B-mode polarization to search for DE induced vacuum birefringence
- Mean field time evolution → <BB>, <TB>, <EB> - Include DE perturbation → <BB>, <TB>=<EB>=0 - This may confuse the searching for genuine B modes
induced by gravitational lensing or primordial gravitational waves, so de-rotation is needed to remove vacuum birefringence effects Kamionkowski 09, Ng 10