High resolution foreground cleaned CMB map from WMAP
High resolution foreground cleaned CMB map from WMAP
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DOI：
10.1103/physrevd.68.123523
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发表时间：
2003-02
影响因子：
5
通讯作者：
Max Tegmark;A. D. Oliveira-Costa;A. Hamilton
中科院分区：
文献类型：
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作者：
Max Tegmark;A. D. Oliveira-Costa;A. Hamilton
我们对威尔金森微波各向异性探测器（WMAP）地图进行了独立的前景分析，以产生一个干净的宇宙微波背景（CMB）地图（可在线获得），用于互相关，例如，星系和X射线图我们使用Tegmark-Efstathiou技术的一个变体，该变体假设CMB具有黑体光谱，但在其他方面是完全盲的，不对CMB功率谱、前景、WMAP检测器噪声或外部模板做出任何假设。与WMAP团队制作的前景清洁内部线性组合地图相比，我们的地图具有包含较少的非CMB功率（来自前景和探测器噪声）的优势。这种差异在第一个声学峰值及以下的角度尺度上最为重要，因为我们的清洁地图是在最高的${（12.6}^{\ensuremath\'}}）$而不是最低的${（49.2}^{\ensuremath\'}}）$ WMAP分辨率。我们还制作了一个维纳滤波的CMB地图，代表我们最好的猜测，CMB天空实际上看起来像什么，以及CMB免费地图在五个WMAP频率有用的前景研究。我们认为，我们的CMB地图是足够干净的，最低的多极可以测量没有任何星系切割，并获得四极值，略低于从切割天空WMAP团队分析。这可以从CMB四极图中理解，它显示出它的大部分能量落在银河系切割区域内，似乎是巧合。有趣的是，四极子和八极子都被发现沿沿着一个特定的空间轴具有功率抑制，该轴在两者之间，大致朝向室女座的$（l，B）\ensuremath{\sim}（\ensuremath{-}110\ifmmode^\circ\else\textdegree\fi{}，60\ifmmode^\circ\else\textdegree\fi {}）$。
We perform an independent foreground analysis of the Wilkinson Microwave Anisotropy Probe (WMAP) maps to produce a cleaned cosmic microwave background (CMB) map (available online) useful for cross-correlation with, e.g., galaxy and x-ray maps. We use a variant of the Tegmark-Efstathiou technique that assumes that the CMB has a blackbody spectrum, but is otherwise completely blind, making no assumptions about the CMB power spectrum, the foregrounds, WMAP detector noise or external templates. Compared with the foreground-cleaned internal linear combination map produced by the WMAP team, our map has the advantage of containing less non-CMB power (from foregrounds and detector noise) outside the Galactic plane. The difference is most important on the angular scale of the first acoustic peak and below, since our cleaned map is at the highest ${(12.6}^{\ensuremath{'}})$ rather than lowest ${(49.2}^{\ensuremath{'}})$ WMAP resolution. We also produce a Wiener filtered CMB map, representing our best guess as to what the CMB sky actually looks like, as well as CMB-free maps at the five WMAP frequencies useful for foreground studies. We argue that our CMB map is clean enough that the lowest multipoles can be measured without any galaxy cut, and obtain a quadrupole value that is slightly less low than that from the cut-sky WMAP team analysis. This can be understood from a map of the CMB quadrupole, which shows much of its power falling within the Galaxy cut region, seemingly coincidentally. Intriguingly, both the quadrupole and the octopole are seen to have power suppressed along a particular spatial axis, which lines up between the two, roughly towards $(l,b)\ensuremath{\sim}(\ensuremath{-}110\ifmmode^\circ\else\textdegree\fi{},60\ifmmode^\circ\else\textdegree\fi{})$ in Virgo.