Download presentation
Presentation is loading. Please wait.
Published byJanel Sharp Modified over 9 years ago
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 the likelihood is given by C.Gordon, W.Hu, D.Huterer and T.M.Crawford, arXiv:astro-ph/0509301 H.K.Eriksen, A.J.Banday, K.M.Gorski, F.K.Hansen and 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.Hansen and P.B.Lilje, arXiv:0903.1229 P.A.R.Ade et al. [Planck Collaboration], arXiv:1303.5083
8
preferred dipole directions dependence on smoothing scale
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
a superhorizon perturbation A.L.Erickcek, M.Kamionkowski and S.M.Carroll, arXiv:0806.0377 the Sachs-Wolfe effect
12
the diploe modulation of curvature perturbation the asymmetry A is a single modulated mode D.H.Lyth, arXiv:1304.1270 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
semispherical power asymmetry power deficit on large angular scales signals in the TE and EE spectra? scale dependent? A<0.015 (99% CL) outlook
17
Thanks!
Similar presentations
© 2024 SlidePlayer.com Inc.
All rights reserved.