摘要
We investigate large-angle scale temperature anisotropy in the Cosmic Microwave Background (CMB) with the Wilkinson Microwave Anisotropy Probe (WMAP) data and model the large-angle anomalies as the effect of the CMB quadrupole anisotropies caused by the local density inhomogeneities. The quadrupole caused by the local density inhomogeneities is different from the special relativity kinematic quadrupole. If the observer inhabits a strong inhomogeneous region, the local quadrupole should not be neglected. We calculate such local quadrupole under the assumption that there is a huge density fluctuation field in the direction (284-, 74-), where the density fluctuation is 10-3 , and its center is ～ 112 h-1 Mpc away from us. After removing such mock signals from WMAP data, the power in the quadrupole, C 2 , increases from the range (200 ～ 260 μK 2 ) to ～ 1000 μK 2 . The quantity S, which is used to estimate the alignment between the quadrupole and the octopole, decreases from (0.7 ～ 0.74) to (0.31 ～ 0.37), while the model predicts that C 2 = 1071.5 μK 2 , and S = 0.412. So our local density inhomogeneity model can, in part, explain the WMAP low-anomalies.
We investigate large-angle scale temperature anisotropy in the Cosmic Microwave Background （CMB） with the Wilkinson Microwave Anisotropy Probe （WMAP） data and model the large-angle anomalies as the effect of the CMB quadrupole anisotropies caused by the local density inhomogeneities. The quadrupole caused by the local density inhomogeneities is different from the special relativity kinematic quadrupole. If the observer inhabits a strong inhomogeneous region, the lo- cal quadrupole should not be neglected. We calculate such local quadrupole under the assumption that there is a huge density fluctuation field in the direction （284°, 74°）, where the density fluctuation is 10-3, and its center is - 112 h-1 Mpc away from us. After removing such mock signals from WMAP data, the power in the quadrupole, C2, increases from the range （200 - 260 μK2） to - 1000 μK2. The quantity S, which is used to estimate the alignment between the quadrupole and the octopole, decreases from （0.7 - 0.74） to （0.31 - 0.37）, while the model predicts that C2 = 1071.5 μK2, and S = 0.412. So our local density inhomogeneity model can, in part, explain the WMAP low-l anomalies.
