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COSMIC POLARIZATION ROTATION & COSMOLOGICAL MODELS AND Detectability of Primordial G-Waves

COSMIC POLARIZATION ROTATION & COSMOLOGICAL MODELS AND Detectability of Primordial G-Waves. Wei-Tou Ni

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COSMIC POLARIZATION ROTATION & COSMOLOGICAL MODELS AND Detectability of Primordial G-Waves

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  1. COSMIC POLARIZATION ROTATION & COSMOLOGICAL MODELS AND Detectability of Primordial G-Waves Wei-Tou Ni Center for Gravitation and Cosmology, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, CHINANational Astronomical Observatories, Chinese Academy of Sciences, Beijing, CHINA

  2. CMB Polarization Observation • In 2002, DASI microwave interferometer observed the polarization of the cosmic background. • With the pseudoscalar-photon interaction , the polarization anisotropy is shifted relative to the temperature anisotropy. • In 2003, WMAP found that the polarization and temperature are correlated to 10σ. This gives a constraint of 10-1 rad or 6 degrees of the cosmic polarization rotation angleΔφ. Cosmic polarization rotation, cosmological models & Primordial GW

  3. CMB Polarization Observation • In 2005, the DASI results were extended (Leitch et al.) and observed by CBI (Readhead et al.) and CAPMAP (Barkats et al.) • In 2006, BOOMERANG CMB Polarization • DASI, CBI, and BOOMERANG detections of Temperature-polarization cross correllation • Planck Surveyor will be launched next year with better polarization-temperature measurement and will give a sensitivity to cosmic polarization rotation Δφ of 10-2-10-3. Cosmic polarization rotation, cosmological models & Primordial GW

  4. WMAP 3 year Polarization Maps TT TT TE foreground EE BB(lensing) BB(r=0.3) Cosmic polarization rotation, cosmological models & Primordial GW

  5. Pseudo-scalars: Pseudoscalar-Photon Coupling Cosmic polarization rotation, cosmological models & Primordial GW

  6. ≈ ξφ,μAνF~μν≈ ξ(1/2)φFμνF~μν(Mod Divergence) Cosmic polarization rotation, cosmological models & Primordial GW

  7. Change of Polarization due to Cosmic Propagation • The effect ofφin (2) is to change the phase of two different circular polarizations of electromagnetic-wave propagation in gravitation field and gives polarization rotation for linearly polarized light.[6-8] • Polarization observations of radio galaxies put a limit ofΔφ≤1 over cosmological distance.[9-14] • Further observations to test and measureΔφ to 10-6 is promising. • The natural coupling strength φ is of order 1. However, the isotropy of our observable universe to 10-5 may leads to a change (ξ)Δφ of φ over cosmological distance scale 10-5 smaller. Hence, observations to test and measureΔφ to 10-6are needed. Cosmic polarization rotation, cosmological models & Primordial GW

  8. Pseudoscalar-Photon Interaction andAxion • W.-T. Ni, A Nonmetric Theory of Gravity, preprint, Montana State University, Bozeman, Montana, USA (1973), http://gravity5.phys.nthu.edu.tw. • W.-T. Ni, Bull. Am. Phys. Soc., 19, 655 (1974). • W.-T. Ni, Phys. Rev. Lett. 38, 301 (1977). • S. Weinberg, {\sl Phys. Rev. Lett}. 40, 233 (1978). • F. Wilczek, {\sl Phys. Rev. Lett}. 40, 279 (1978). • M. Dine {\sl et al.}, {\sl Phys. Lett}. 104B, 1999 (1981). • M. Shifman {\sl et al.}, {\sl Nucl. Phys}. B166, 493 (1980). • J. Kim, {\sl Phys. Rev. Lett}. 43, 103 (1979). • S. L. Cheng, C. Q. Geng and W.-T. Ni, {\sl Phys. Rev.} D52 3132 (1995) and references therein. Cosmic polarization rotation, cosmological models & Primordial GW

  9. Electomagnetic Wave Propagation and Polarization EP • W.-T. Ni, "Equivalence Principles and Precision Experiments" pp.~647-651, in Precision Measurement and Fundamental Constants II, ed. by B. N. Taylor and W. D. Phillips, Natl. Bur. Stand. (U.S.), Spec. Publ.~{\bf 617} (1984). • W.-T. Ni, "Timing Observations of the Pulsar Propagations in the Galactic Gravitational Field as Precision Tests of the Einstein Equivalence Principle", pp.~441-448 in Proceedings of the Second Asian-Pacific Regional Meeting of the International Astronomical Union, ed. by B. Hidayat and M. W. Feast (Published by Tira Pustaka, Jakarta, Indonesia, 1984). • W.-T. Ni, "Equivalence Principles, Their Empirical Foundations, and the Role of Precision Experiments to Test Them", pp.~491-517 in Proceedings of the 1983 International School and Symposium on Precision Measurement and Gravity Experiment, Taipei, Republic of China, January 24-February 2, 1983, ed. by W.-T. Ni (Published by National Tsing Hua University, Hsinchu, Taiwan, Republic of China, June, 1983). • M. P. Haugan and T. F. Kauffmann, {\sl Phys. Rev}. D {\bf 52}, 3168 (1995). • T. P. Krisher, {\sl Phys. Rev}. D {\bf 44}, R2211 (1991). Cosmic polarization rotation, cosmological models & Primordial GW

  10. Pseudoscalar-Photon Interaction and Astrophysical/Cosmic Polarization Rotation Δθ (=Δφ) of Electromagnetic Wave Propagation • W.-T. Ni, A Nonmetric Theory of Gravity, preprint, Montana State University, Bozeman, Montana, USA (1973), http://gravity5.phys.nthu.edu.tw. • S. M. Carroll, G. B. Field, R. Jackiw, {\sl Phys. Rev}. D {\bf 41}, 1231 (1990). • S. M. Carroll and G. B. Field, {\sl Phys. Rev}. D {\bf 43}, 3789 (1991). • B. Nodland and J. P. Ralston, {\sl Phys. Rev. Lett}. {\bf 78}, 3043 (1997). • J. F. C. Wardle, R. A. Perley, and M. H. Cohen, {\sl Phys. Rev. Lett.} {\bf 79}, 1801 (1997). • D. J. Eisenstein and E. F. Bunn, {\sl Phys. Rev. Lett.} {\bf 79}, 1957 (1997). • S. M. Carroll and G. B. Field, {\sl Phys. Rev. Lett.} {\bf 79}, 2394 (1997). • T. J. Loredo, E. A. Flanagan, and I. M. Wasserman, {\sl Phys, Rev.} {\bf D 56}, 7507 (1997). • S. M. Carroll, {\sl Phys. Rev. Lett.} {\bf 81}, 3067 (1998). • A. Lue, L. Wang, and M. Kamionkowski, Phys. Rev. Lett. {\bf 83}, 1506 (1999). Cosmic polarization rotation, cosmological models & Primordial GW

  11. Nomenclature in Optics • Birefringence: velocity dependent on polarization  linear-polarization to elliptical-polarization • Dichroism: absorption varies with polarization • Faraday rotation (dependent on wavelength) • Cosmic polarization Rotation – not like QED vacuum birefringence (no V [Stokes parameter] produced) Cosmic polarization rotation, cosmological models & Primordial GW

  12. Space contribution to the local polarization rotation angle -- [μΣ13φ,μΔxμ] = |▽φ| cos θΔx0. The time contribution is φ,0Δx0. The total contribution is (|▽φ| cos θ + φ,0) Δx0. (Δx0 > 0) Intergrated: φ(2) - φ(1) 1: a point at the decoupling epoch 2: observation point Cosmic polarization rotation, cosmological models & Primordial GW

  13. Variations and Fluctuations • rotationφ(2) - φ(1) • δφ(2) - δφ(1): δφ(2) variations and fluctuations at the last scattering surface of the decoupling epoch; δφ(1), at present observation point, fixed • <[δφ(2) - δφ(1)]^2> variance of fluctuation ~ [couplingξ × 10^(-5)]^2 • The coupling depends on various cosmological models Cosmic polarization rotation, cosmological models & Primordial GW

  14. Constraints on cosmic polarization rotation from CMB All consistent with null detection and with one another at 2 σ level Cosmic polarization rotation, cosmological models & Primordial GW

  15. FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP1) OBSERVATIONS:COSMOLOGICAL INTERPRETATION, Komatsu et al., arXiv:0803.0547v2 [astro-ph] 17 Oct 2008 • The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than −5.9◦ < α < 2.4◦ (95% CL) between the decoupling and the present epoch. I.e. -30 ± 73 mrad (2σ) Cosmic polarization rotation, cosmological models & Primordial GW

  16. References Cosmic polarization rotation, cosmological models & Primordial GW

  17. COSMOLOGICAL MODELS • PSEUDO-SCALAR COSMOLOGY, e.g., Brans-Dicke theory with pseudoscalar-photon coupling • NEUTRINO NUMBER ASYMMETRY • BARYON ASYMMETRY • SOME other kind of CURRENT • LORENTZ INVARIANCE VIOLATION • CPT VIOLATION • DARK ENERGY (PSEUDO)SCALAR COUPLING • OTHER MODELS Cosmic polarization rotation, cosmological models & Primordial GW

  18. Cosmic polarization rotation, cosmological models & Primordial GW

  19. Pseudoscalar Quintessence Cosmic polarization rotation, cosmological models & Primordial GW

  20. JCAP Cosmic polarization rotation, cosmological models & Primordial GW

  21. Neutrino number asymmetry • Neutrino number asymmetry is function of electron-neutrino degeneracy parameterξν e with ξν e = μν e (chemical potential) / Tνe • μν ecould be ± 0.001 Cosmic polarization rotation, cosmological models & Primordial GW

  22. Significance and Outlook • Pseudoscalar-photon interaction is proportional to the gradient of the pseudoscalar field. From phenomenological point of view, this gradient could be neutrino number asymmetry, other density current, or a constant vector. In these situations, Lorentz invariance or CPT may effectively be violated. • Probing neutrino number asymmetry • Better accuracy in CMB polarization observation is expected from PLANCK mission to be launched this year. A dedicated CMB polarization observer in the future would probe this fundamental issue more deeply. Cosmic polarization rotation, cosmological models & Primordial GW

  23. Detectability of Primordial G-Waves Cosmic polarization rotation, cosmological models & Primordial GW

  24. The Gravitational Wave Background from Cosmological Compact BinariesAlison J. Farmer and E. S. Phinney (Mon. Not. RAS [2003]) Optimistic (upper dotted), fiducial (Model A, lower solid line) and pessimistic (lower dotted) extragalactic backgrounds plotted against the LISA (dashed) single-arm Michelson combination sensitivity curve. The‘unresolved’ Galactic close WD–WD spectrum from Nelemans et al. (2001c) is plotted (with signals from binaries resolved by LISA removed), as well as an extrapolated total, in which resolved binaries are restored, as well as an approximation to the Galactic MS–MS signal at low frequencies. Super-ASTROD Region DECIGO BBO Region Cosmic polarization rotation, cosmological models & Primordial GW

  25. LISA LISA consists of a fleet of 3 spacecraft 20º behind earth in solar orbit keeping a triangular configuration of nearly equal sides (5 × 106 km). Mapping the space-time outside super-massive black holes by measuring the capture of compact objects set the LISA requirement sensitivity between 10-2-10-3 Hz. To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz. (2017) Cosmic polarization rotation, cosmological models & Primordial GW

  26. ASTROD configuration (baseline ASTROD after 700 days from launch) Cosmic polarization rotation, cosmological models & Primordial GW

  27. Super-ASTROD (1st TAMA Meeting1996)W.-T. Ni, “ASTROD and gravitational waves” in Gravitational Wave Detection, edited by K. Tsubono, M.-K. Fujimoto and K. Kuroda (Universal Academy Press, Tokyo, Japan, 1997), pp. 117-129. • With the advance of laser technology and the development of space interferometry, one can envisage a 15 W (or more) compact laser power and 2-3 fold increase in pointing ability. • With these developments, one can increase the distance from 2 AU for ASTROD to 10 AU (2×5 AU) and the spacecraft would be in orbits similar to Jupiter's. Four spacecraft would be ideal for a dedicated gravitational-wave mission (Super-ASTROD). Cosmic polarization rotation, cosmological models & Primordial GW

  28. Primordial GW and Super-ASTROD • For detection of primordial GWs in space. One may go to frequencies lower or higher than LISA/ASTROD bandwidth where there are potentially less foreground astrophysical sources to mask detection. • DECIGO and Big Bang Observer look for gravitational waves in the higher range • Super-ASTROD look for gravitational waves in the lower range. • Super-ASTROD (ASTROD III) : 3-5 spacecraft with 5 AU orbits together with an Earth-Sun L1/L2 spacecraft and ground optical stations to probe primordial gravitational-waves with frequencies 0.1 μHz - 1 mHz and to map the outer solar system. Cosmic polarization rotation, cosmological models & Primordial GW

  29. Primordial Gravitational Waves[strain sensitivity  (ω^2) energy sensitivity] Cosmic polarization rotation, cosmological models & Primordial GW

  30. Sensitivity to Primordial GW • The minimum detectable intensity of a stochastic GW background is proportional to detector noise spectral power density S_n(f) times frequency to the third power • with the same strain sensitivity, lower frequency detectors have an f ^(-3)-advantage over the higher frequency detectors. • compared to LISA, ASTROD has 27,000 times (30^3) better sensitivity due to this reason, while Super-ASTROD has an additional 125 (5^3) times better sensitivity. Cosmic polarization rotation, cosmological models & Primordial GW

  31. Primordial Gravitational Waves[strain sensitivity  (ω^2) energy sensitivity] Cosmic polarization rotation, cosmological models & Primordial GW

  32. Polarization as a tool to test cosmological models and to look into (gravitational) axion and possible dark energy pseudoscalar, CPT, Neutrino Asymmetry, etc. • Primordial gravitational waves may possibly be detected by ASTROD/Super-ASTROD and DECIGO/Big Bang Observer Cosmic polarization rotation, cosmological models & Primordial GW

  33. Thank you ! Cosmic polarization rotation, cosmological models & Primordial GW

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