Systematics in WMAP and Other CMB Missions

String Theory Explanation of Large-Scale Anisotropy and Anomalous Alignment

“…[24][25][26][27][28][29][30][31][32][33][34][35] In the analysis on the behavior of the temperature anisotropy power spectrum, the temperature°uctuation is expanded in spherical harmonics. The¯rst three lowest multipoles include dipole (l ¼ 1), quadrupole (l ¼ 2), and octupole (l ¼ 3).…”

A Polytropic Solution of the Expanding Universe – Constraining Relativistic and Non-Relativistic Matter Densities Using Astronomical Results

“…For instance, if Ω m is really around 0.27, as used here, the effects of relativistic matter might be observed in SNe Ia signals. Li and Liu Li & Liu (2009). Our results are reported in Table 5 as functions of Ω m and x, where x is the ratio of Ω r /Ω m , with the sum of relativistic and non-relativistic matter being Ω m .…”

“…Better constraints on these cosmological values can be made using larger SNe Ia (and SDSS) data sets, hopefully with smaller errors, which should be available in the near future after systematic errors have been corrected (Kelly et al, 2009). Likewise estimates of H 0 should await reconciliation between groups analyzing the CMB data (Li & Liu, 2009;Liu & Li, 2010a). The overall aim of all this mental anguish will hopefully lead to a much better understanding of the dynamics and parameters of our expanding Universe and hence our origin and eventual fate.…”

CMB observation and early universe

“…按 照 WMAP 组数据处理的流程 [12] , 我们建立了自己的 分析系统. 利用自己的程序从 WMAP 的 TOD 数据 计算 CMB 温度图和角功率谱, 得到的结果同 WMAP 组有重大差异: CMB 的四极矩成分几乎消失(见图 2), 宇宙学参数的值也显著改变 [13] .…”

“…伪偶极信号对高阶矩(小尺度)区域功率谱的影 响也不可忽视. 在 l=200~675 区间新功率谱的平均 功率比 WMAP 发布值小约 13%, 两个声学峰更符合 BOOMERANG 的观测结果, 从而引起 WMAP 宇宙 学参数拟合值的显著变化 [13] 热斑 [24,25] 、环状结构等 [26,27] , 无论其统计显著性如何, 在作宇宙学的解读时都需要非常谨慎: 在对 CMB 实 验系统误差有更深入的认识和适当的修正之前, 就 宣称发现"宇宙空洞" [25] 或"大爆炸前的宇宙" [27] 都言 之过早.…”