Planck 2013 results
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Table 25

Summary of the best-fit power dipole directions on the sky up to max = 600/1500, for each of the four component separation methods, together with the 143 GHz map cleaned using the SEVEM method and denoted SEVEM-143.

Frac.
Method Mask (l,b) [°] [°] max

C-R ........ U73 (231, 2) 86.7 493/500 1500
NILC ........ U73 (214, 4) 85.7 500/500 1500
SEVEM ........ U73 (215, 9) 85.8 500/500 1500
SMICA ........ U73 (220, 4) 86.2 499/500 1500
SEVEM-143 ........ U73 (228, 1) 86.7 496/500 1500
SEVEM-143DB ........ U73 (218, 21) 87.6 487/500 1500
WMAP-9 ........ KQ85 (209, 24) 82.3 9966/10 000 600
C-R ........ U73 (192, 5) 81.7 500/500 600
NILC ........ U73 (194, 3) 80.8 500/500 600
SEVEM ........ U73 (195, 2) 81.2 500/500 600
SMICA ........ U73 (196, 2) 81.9 500/500 600
SEVEM-143 ... U73 (195, 3) 81.6 500/500 600
SEVEM-143DB .. U73 (189, 10) 81.9 500/500 600

Notes. These are determined from maps of the power spectrum estimated on 12 non-overlapping patches in bins of 16 multipoles. The preferred direction is the mean of the separate 16-multipole dipole directions in the range = 2 to max. The angle θmean is the mean separation angle between all possible pair-wise combinations of these 16-multipole dipoles over the same range. The p-value for the power asymmetry is given by the fraction of simulations with a larger mean separation angle, , than the observed data, . SEVEM-143DB corresponds to data corrected for Doppler boosting, while all other results are derived without this correction. In fact, due to the frequency dependence of this effect, deboosting is not important for the WMAP data. For the Planck analysis, 500 FFP6 simulations were analysed, while 10 000 Gaussian simulations were used to study the WMAP data.

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