**Part 4**

**Cosmology and CMB Physics** 

10 Will-be-set-by-IN-TECH

112 Space Science

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3: 10–14.

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279: 767–770.

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**7**

*China*

Hao Liu<sup>1</sup> and Ti-Pei Li2

*Chinese Academy of Sciences*

**Systematics in WMAP and Other CMB Missions**

<sup>2</sup>*Department of Physics and Center for Astrophysics, Tsinghua University, Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences*

When the WMAP team released their unprecedentedly precise CMB anisotropy maps in the year of 2003 (Fig. 1, Bennett et al. (2003)), everyone were celebrating the finally arrival of experimental foundation of precision cosmology. It did worth all praises, because the measured CMB power spectrum was so beautifully consistent with the theoretical expectation, and a clear scene of the birth and growth of a flat and ordered Universe seems to be right within the reach of our hands, as well as the first precision percentage estimation of its contents. Many people begin to believe that, we no longer need to be bored by one new cosmic model per day, and the Big Bang scene and ΛCDM model will be good enough to give

It's not strange that there still remains some small disharmonious flaws, like an unexpectedly low quadrupole power (Bennett et al., 2003; Hinshaw et al., 2003b), alignment issues and NS asymmetry (Bielewicz et al., 2004; Copi et al., 2007; Eriksen et al., 2005; 2007; Hansen et al., 2004; 2006; Wiaux et al., 2006), non-Gaussianity including cold/hot spots (Copi et al., 2004; Cruz et al., 2005; 2007; Komatsu et al., 2003; Liu & Zhang, 2005; McEwen et al., 2006; Vielva et al., 2004; 2007), etc. Among all these flaws, the loss of the quadrupole power is the

Fig. 1. The CMB anisotropy map and power spectrum obtained by WMAP (Bennett et al.,

**1. Introduction**

2003).

**1.1 The success of WMAP**

us satisfactory explanation to anything we want to know.

<sup>1</sup>*Key Laboratory of Particle Astrophysics, Institute of High Energy Physics,*
