Hemispherical Power Asymmetry 郭宗宽

1. Hemispherical Power Asymmetry郭宗宽 昆明 2013.11.2

2. anomalies in CMB map • the quadrupole-octopole alignment • power deficit at low-l • hemispherical asymmetry • parity asymmetry • the cold spot • ……

5. data analysis the CMB temperature sky maps is modeled as C.Gordon, W.Hu, D.Hutererand T.M.Crawford, arXiv:astro-ph/0509301 the likelihood is given by H.K.Eriksen, A.J.Banday, K.M.Gorski, F.K.Hansenand P.B.Lilje, arXiv:astro-ph/0701089

6. the full covariance matrix is • WMAP3: (l, b) = (225◦,−27◦), A=0.114

7. WMAP5(l<64, 4.5◦): (l, b) = (224◦,−22◦), A=0.0720.022 • Planck: J.Hoftuft, H.K.Eriksen, A.J.Banday, K.M.Gorski, F.K.Hansenand P.B.Lilje, arXiv:0903.1229 P.A.R.Ade et al. [Planck Collaboration], arXiv:1303.5083

8. dependence on smoothing scale preferred dipole directions

9. Comment: the dipole anisotropy induced by our velocity the temperature and direction in the observed frame the inferred temperature fluctuations (l, b) = (264◦,48◦)

10. models • a parameterization [astro-ph/0509301] • our peculiar motion [arXiv:1304.3506] • a gauge field [arXiv:1302.7304] • anisotropic metric [arXiv:1303.6058] • a modulation of a cosmological parameter [arXiv:1303.6949] • a superhorizon perturbation [arXiv:0806.0377] • …… [arXiv:yymm.xxxx]

11. asuperhorizon perturbation the Sachs-Wolfe effect A.L.Erickcek, M.Kamionkowski and S.M.Carroll, arXiv:0806.0377

12. the diploe modulation of curvature perturbation D.H.Lyth, arXiv:1304.1270 the asymmetry A is a single modulated mode Z.G.Liu, Z.K.Guo and Y.S.Piao, arXiv:1304.6527

13. the CMB angular power spectrum the GZ effect (the Sachs-Wolfe approximation) observational constraint

14. a single-field slow-roll inflation • a curvaton-type field • a bounce inflation A.L.Erickcek, M.Kamionkowski and S.M.Carroll, arXiv:0806.0377 D.H.Lyth, arXiv:1304.1270 Z.G.Liu, Z.K.Guo and Y.S.Piao, arXiv:1304.6527

15. primordial power spectrum of curvature perturbations

16. outlook • semispherical power asymmetry • power deficit on large angular scales • signals in the TEand EE spectra? • scale dependent? A<0.015 (99% CL)

17. Thanks!