Hemispherical Power Asymmetry 郭宗宽 昆明

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

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

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

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

preferred dipole directions dependence on smoothing scale

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

models a parameterization[astro-ph/ ] our peculiar motion[arXiv: ] a gauge field[arXiv: ] anisotropic metric[arXiv: ] a modulation of a cosmological parameter [arXiv: ] a superhorizon perturbation [arXiv: ] …… [arXiv:yymm.xxxx]

a superhorizon perturbation A.L.Erickcek, M.Kamionkowski and S.M.Carroll, arXiv: the Sachs-Wolfe effect

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

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

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

primordial power spectrum of curvature perturbations

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

Thanks!