![Page 1: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/1.jpg)
Wei-Tou NiNational Tsing Hua U., Hsinchu
Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901
[2] W.-T. Ni, Dilaton field and cosmic wave propagation, PLA 378 (2014) 3413
[3] S. di Serego Alighieri, W.-T. Ni and W.-P. Pan, Astrophys. J. 792, 35 (2014).
[4] W.-T. Ni, Spacetime structure …, PLA 379(2015)1297–1303
[5] H.-H. Mei, W.-T. Ni, W.-P. Pan, L. Xu, S. di SA, ApJ (2015); arXiv:1412.8569
New Constraints onCosmic Polarization Rotation (CPR)
fromthe ACTPol, BICEP2 and POLARBEAR
CMB B-Mode Observations
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 1
![Page 2: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/2.jpg)
Outline Introduction – 3 processes to produce B-mode Equivalence Principles, Electromagnetism, & the
Cosmic Connection – Axion, Dilaton and Skewon Photon sector Nonbirefingence axion, dilaton, skewon variation of fundamental constants? Observational constraints on CPR Summary Related talk: XinminZhang Tomorrow
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 2
![Page 3: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/3.jpg)
Let there be light!
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 3
Light abundant at 100 ps (100
Gev): gamma rays
CMBproduced
![Page 4: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/4.jpg)
B-mode production: 3 processes +dust
(i) gravitational lensing from E-mode (iv) dust polarization (Zaldarriaga & Seljak 1997),
alignment (ii) local quadrupole anisotropies in the CMB within the last scattering region by large scale GWs (Polnarev
1985) (iii) cosmic polarization rotation (CPR) due to pseudoscalar-photon interaction (Ni 1973; for a review, see Ni 2010).Propagation effect due to changing Pseudoscalar:the gradient gives a vectorChern-Simons theoryWith an extra field as external field, the cosmoscan have P, CPT and Lorentz asymmetrry(The CPR has also been called Cosmological Birefringence)2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 4
![Page 5: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/5.jpg)
Light, WEP I, WEP II
& EEP
Light is abundant since 100ps (Electroweak phase trans.) or earlier after Big
Bang Galileo EP (WEP I) for photon: the light trajectory
is dependent only on the initial direction – no splitting & no retardation/no advancement, independent of polarization and frequency
WEP II, no polarization rotation EEP, no amplification/no attenuation, no spectral
distortion 2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 5
![Page 6: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/6.jpg)
The ISSUE(Why Minkowski Metric? from
gravity point of view) How to derive spacetime structrure/the lightcone
from classical, local and linear electrodynamics (i) the closure condition (ii) The Galileo weak equivalence principle (iii) The non-birefringence (vanishing double refraction) and “no amplification/dissipation” condition of astrophysical/cosmological electromagnetic wave propagation from observations
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 6
![Page 7: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/7.jpg)
Premetric formulation of electromagnetism
In the historical development, special relativity arose from the invariance of Maxwell equations under Lorentz transformation.
In 1908, Minkowski [1] further put it into 4-dimensional geometric form with a metric invariant under Lorentz transformation.
The use of metric as dynamical gravitational potential [2] and the employment of Einstein Equivalence Principle for coupling gravity to matter [3] are two important cornerstones to build general relativity
In putting Maxwell equations into a form compatible with general relativity, Einstein noticed that the equations can be formulated in a form independent of the metric gravitational potential in 1916 [5,6].
Weyl [7], Murnaghan [8], Kottler [9] and Cartan [10] & Schrödinger further developed and clarified this resourceful approach.
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 7
![Page 8: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/8.jpg)
Metric-Free and Connection-Free
Maxwell equations for macroscopic/spacetime electrodynamics in terms of independently measurable field strength Fkl (E, B) and excitation (density with weight +1) Hij (D, H) do not need metric as primitive concept (See, e. g., Hehl and Obukhov [11]):
Hij,j = − 4π Ji, eijklFjk,l = 0, (1)
with Jk the charge 4-current density and eijkl the completely anti-symmetric tensor density of weight +1 with e0123 = 1. We use units with the light velocity c equal to 1.To complete this set of equations, a constitutive relation is needed between the excitation and the field:
Hij = χijkl Fkl. (2)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 8
![Page 9: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/9.jpg)
Constitutive relation : Hij = χijkl Fkl.
Since both Hij and Fkl are antisymmetric, χijkl must be antisymmetric in i and j, and k and l. Hence
χijkl has 36 independent components.
Principal part: 20 degrees of freedom Axion part: 1 degree of freedom (Ni 1973,1974,1977; Hehl et al. 2008 Cr2O3) Skewon part: 15 degrees of freedom (Hehl-Ohbukhov-Rubilar skewon 2002)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 9
![Page 10: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/10.jpg)
Related formulation in the photon sector: SME & SMS
The photon sector of the SME Lagrangian is given by Lphotontotal =
− (1/4) Fμν Fμν − (1/4) (kF)κλμνFκλ Fμν + (1/2) (kAF)κεκλμνAλFμν (equation (31) of [7]). The CPT-even part (−(1/4) (kF)κλμνFκλ Fμν) has constant components (kF)κλμν which correspond one-to-one to our χ’s when specialized to constant values minus the special relativistic χ with the constant axion piece dropped, i.e. (kF)κλμν = χκλμν – (1/2) (ηκμ ηλν − ηκν ηλμ). The CPT-odd part (kAF)κ also has constant components which correspond to the derivatives of axion φ,κ when specilized to constant values.
SMS in the photon sector due to Bo-Qiang Ma is different from both SME and χκλμν-framework.
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 10
![Page 11: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/11.jpg)
The ISSUE(Why Minkowski Metric? from
gravity point of view) How to derive spacetime structrure/the lightcone
from classical, local and linear electrodynamics (i) the closure condition (ii) The Galileo weak equivalence principle (iii) The non-birefringence (vanishing double refraction) and “no amplification/dissipation” condition of astrophysical/cosmological electromagnetic wave propagation from observations
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 11
![Page 12: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/12.jpg)
Skewonless case: EM wave propagation
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 12
![Page 13: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/13.jpg)
Dispersion relation and Nonbirefringence condition
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 13
![Page 14: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/14.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 14
![Page 15: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/15.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 15
![Page 16: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/16.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 16
![Page 17: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/17.jpg)
Three approaches to Axions/Pseudoscalar-photon
interactions
Top down approach – string theory Bottom up approach – QCD axion Phenomenological approach -- gravitation
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 17
![Page 18: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/18.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 18
≈ ξφ,μ AνF~μν ≈ ξ (1/2)φ FμνF~μν
(Mod Divergence)
φ: Pseudoscalar field or pseudoscalar function of gravitational or relevant fields
![Page 19: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/19.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 19
Galileo EP Electromagnetism:
Charged particles and photons
)()()16
1( 2/1
II
IIk
kklijijkl
I xxdt
dsmgjAFFL
]21
21
[)( 2/1 ijklkjiljlikijkl ggggg ψ
Special Relativity
g framework
Galileo EP constrains to :
)()()16
1( 2/1
II
IIk
kklijjlikjl
I xxdt
dsmgjAFFL
ηη
(Pseudo)scalar-Photon Interaction
![Page 20: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/20.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 20
![Page 21: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/21.jpg)
The birefringence condition in Table I – historical
background
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 21
![Page 22: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/22.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 22
![Page 23: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/23.jpg)
Empirical Nonbirefringence Constraint
to 10−38, i.e., less than 10−34 = O(Mw/Mplanck)2 a significant constraint on quantum gravity
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 23
![Page 24: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/24.jpg)
Empirical foundations of the closure relation for the skewonless case
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 24
The (generalized) closure relation is satisfied
From table I, this is verified to 10×10−38
Less than 100 operations
![Page 25: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/25.jpg)
The Cosmic MW Background Spectrum:
2.7255 ± 0.0006 KD. J. Fixsen, Astrophys. J. 707 (2009) 916
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 25
No amplification/No attenuation(No dilaton)
No distortion(No Type I Skewon
Redshifted(AccelerationEquivalent)
![Page 26: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/26.jpg)
Present & Past
6.0K <T(2.33771) < 14K Prediction: 9.1 K(2000) The measurement is based on the excitation of the
two first hyperfine levels of carbon (C and C+ induced by collisions and by the tail of the CMB photon distributions. Nature 2000
(inconsistency : H2 and HD abundance measurement) (2001) The cosmic microwave background radiation
temperature at z = 3.025 toward QSO0347-3819, P Molaro et al Astronomy & Astrophysics 2002 Measurement of effective temperature at different redshift
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 26
![Page 27: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/27.jpg)
A & A 2014
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 27
![Page 28: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/28.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 28
![Page 29: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/29.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 29
![Page 30: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/30.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 30
![Page 31: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/31.jpg)
Results
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 31
Constraint from CMB spectrum
![Page 32: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/32.jpg)
Dilaton and variation of constants
Fritzsch et al, variation of the fine structure constant (some astophysical observations)
Shu Zhang & Bo-Qiang Ma, (Possible) Lorentz violation from gamma-ray bursts (10 Gev)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 32
![Page 33: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/33.jpg)
CMB observations7 orders or more improvement in
amplitude, 15 orders improvement in power since 1965
1948 Gamow – hot big bang theory; Alpher & Hermann – about 5 K CMB
Dicke -- oscillating (recycling) universe: entropy CMB 1965 Penzias-Wilson excess antenna temperature at 4.08
GHz 3.5±1 K 2.5 4.5 (CMB temperature measurement ) Precision to 10-(3-4) dipolar (earth) velocity
measurement to 10-(5-6) 1992 COBE anisotropy meas. acoustic osc. 2002 Polarization measurement (DASI) 2013 Lensing B-mode polarization (SPTpol) 2014 POLARBEAR, BICEP2 and PLANCK (lensing & dust B-
mode)2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 33
![Page 34: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/34.jpg)
Three processes can produce CMB
B-mode polarization observed
(i) gravitational lensing from E-mode polarization (Zaldarriaga & Seljak 1997), (ii) local quadrupole anisotropies in the CMB within the last scattering region by large scale GWs (Polnarev
1985) (iii) cosmic polarization rotation (CPR) due to pseudoscalar-photon interaction (Ni 1973; for a review, see Ni 2010). (The CPR has also been called Cosmological Birefringence) (iv) Dust alignment
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 34
![Page 35: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/35.jpg)
Cosmic Polarization Rotation
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 35
![Page 36: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/36.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 36
The current combined evidence so far is consistent with a null CPR and upper limits are of the order of 1 degree with fluctuations and
mean is constrained to about 1 degrees.
![Page 37: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/37.jpg)
BB power spectrum from SPTpol, ACTpol, BICEP2/Keck, and POLARBEAR. The solid gray line shows the expected lensed BB spectrum from the Planck+lensing+WP+highL best-fit model. The dotted line shows the nominal 150 GHz BB power spectrum of Galactic dust emission derived from an analysis of polarized dust emission in the BICEP2/Keck field using Planck data. The dash-dotted line shows the sum of the lensed BB power and dust BB power.
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 37
![Page 38: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/38.jpg)
Emode:1502.01589(fig.3)(PLANCK)
DataLensing- ‐B:1502.01591v1(fig.4)(PLANCK)Gravity- ‐Bmode:1403.3985v2(fig.14)(BICEP2)SPT:1503.02315v1; POLARBEAR:1403.2369v1ACTPol:1405.5524v2; dust:1409.5738(fig.9)(PLANCK)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 38
Collaborators:Baccigalupi, Pan, Xia, Xu, NiDi Serego Alighieri,
![Page 39: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/39.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 39
![Page 40: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/40.jpg)
r - 0.050.1 100500 mrad2
Fluctuation amplitude bound: 17 mrad (1 degree)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 40
![Page 41: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/41.jpg)
Summary Pseudoscalar-photon (axion) interactions arisen from
the study of EP, QCD, string theory and pre-metric EM CPR is a way to probe pseudoscalar-photon
interaction and a possible way to probe inflation dynamics,
New CPR constraints from B-mode are summarized Good calibration is a must for measuring mean CPR CPR is a means to test EEP or to find new physics From the empirical route to construct spacetime
structure, axion, dilaton and type II skewon are possibilities which could be explored further
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 41
![Page 42: Wei-Tou Ni National Tsing Hua U., Hsinchu Ref.: [1] W.-T. Ni, PLA 378 (2014) 1217-1223; RoPP 73 (2010) 056901 [2] W.-T. Ni, Dilaton field and cosmic wave](https://reader031.vdocuments.net/reader031/viewer/2022013011/56649f2e5503460f94c47ff7/html5/thumbnails/42.jpg)
2015.05.07 Galileo-Xu 2015 CPR and ACTPol_BICEP2-POLARBEAR Ni 42
Thank you
http://www.arcetri.astro.it/cpr/