WMAP3宇宙微波背景图中的轴向和平面镜不均匀性
On Axial and Plane--Mirror Inhomogeneities in the WMAP3 Cosmic Microwave Background Maps
摘要：
本文研究了威尔金森微波各向异性探测器（WMAP）三年巡天所获得的宇宙微波背景（CMB）温度图中漂移集分布的不均匀性。当温度阈值|T| <90 μK时，超过200个像元的漂移集分布集中在两个区域，接近于对极，银河坐标为l= 94^ \circ .7，b= 34^ \circ .4和l= 279^ \circ .8，b=-29 ^\circ .2.这两个区域的中心向赤道漂移时，温度阈值的增加。中心位于接近\ell =3多极的矢量之一。在偏移集的分布中，子结构的两种模式是镜像的，χ^2=0.7-1.5。在WMAP的噪声结构中，这种效应没有明显的起源，也没有证据表明它依赖于银河系的切割。如果这种效应是宇宙学的，它可能是视界大小的密度扰动的一个非常大的分量的指示，独立于空间坐标之一，和/或宇宙的非平凡的板状空间拓扑结构。
英文摘要：
We study inhomogeneities in the distribution of the excursion sets in the Cosmic Microwave Background (CMB) temperature maps obtained by the three years survey of the Wilkinson Microwave Anisotropy Probe (WMAP). At temperature thresholds |T|<90 μK, the distributions of the excursion sets with over 200 pixels are concentrated in two regions, nearly at the antipodes, with galactic coordinates l= 94^\circ.7, b= 34^\circ.4 and l= 279^\circ.8, b= -29^\circ.2. The centers of these two regions drift towards the equator when the temperature threshold is increased. The centers are located close to one of the vectors of \ell =3 multipole. The two patterns of the substructures in the distribution of the excursion sets are mirrored, with χ^2=0.7-1.5. There is no obvious origin of this effect in the noise structure of WMAP, and there is no evidence for a dependence on the galactic cut. Would this effect be cosmological, it could be an indication of an anomalously large component of horizon-size density perturbations, independent of one of the spatial coordinates, and/or of a non-trivial slab-like spatial topology of the Universe.
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