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Influence of Planck foreground masks in the large angular scale quadrant CMB asymmetry
Santos, L; Cabella, P; Villela, T; Zhao, W; Santos, L (reprint author), Chinese Acad Sci, Univ Sci & Technol China, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China.
2015
发表期刊ASTRONOMY & ASTROPHYSICS
卷号584期号:0页码:A115
文章类型Article
摘要Context. The measured cosmic microwave background (CMB) angular distribution shows high consistency with the Lambda CDM model, which predicts cosmological isotropy as one of its fundamental characteristics. However, isotropy violations were reported in CMB temperature maps of the Wilkinson Microwave Anisotropy Probe (WMAP) and confirmed by Planck satellite data. Aims. Our purpose is to investigate the influence of different sky cuts (masks) employed in the analysis of CMB angular distribution, in particular in the excess of power in the southeastern quadrant (SEQ) and the lack of power in the northeastern quadrant (NEQ), found in both WMAP and Planck data. Methods. We compared the two-point correlation function (TPCF) computed for each quadrant of the CMB foreground-cleaned temperature maps to 1000 Monte Carlo (MC) simulations generated assuming the Lambda CDM best-fit power spectrum using four different masks, from the least to the most severe one: mask-rulerminimal, UT78, U73, and U66. In addition to the quadrants and for a better understanding of these anomalies, we computed the TPCF using the mask-rulerminimal for circular regions in the map where the excess and lack of power are present. We also compared, for completeness, the effect of Galactic cuts (+/-10, 20, 25, and 30 degrees above/below the Galactic plane) in the TPCF calculations as compared to the MC simulations. Results. We found consistent results for three masks, namely mask-rulerminimal, U73, and U66. The results indicate that the excess of power in the SEQ tends to vanish as the portion of the sky covered by the mask increases and the lack of power in the NEQ remains virtually unchanged. A different result arises for the newly released UT78 Planck mask. When this mask is applied, the NEQ is no longer anomalous. On the other hand, the excess of power in the SEQ becomes the most significant one among the masks. Nevertheless, the asymmetry between the SEQ and NEQ is independent of the mask and it disagrees with the isotropic model with at least 95% C.L. Conclusions. We find that UT78 disagrees with the other analyzed masks, especially when considering the SEQ and the NEQ individual analysis. Most important, the use of UT78 washes out the anomaly in the NEQ. Furthermore, we find an excess of kurtosis, compared with simulations, in the NEQ for the regions not masked by UT78 but masked by the other masks, indicating that the previous result could be due to unremoved residual foregrounds by UT78.
关键词Cosmic Background Radiation Cosmology: Observations Methods: Data Analysis Methods: Statistical
学科领域Astronomy & Astrophysics
资助者project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; KIP of CAS ; KIP of CAS ; KIP of CAS ; KIP of CAS ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; KIP of CAS ; KIP of CAS ; KIP of CAS ; KIP of CAS ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8]
DOIhttp://dx.doi.org/10.1051/0004-6361/201526713
关键词[WOS]MICROWAVE-ANISOTROPY-PROBE ; WMAP OBSERVATIONS ; NON-GAUSSIANITY ; COLD SPOT ; SKY MAPS ; ANOMALIES ; CONSTRAINTS ; TEMPERATURE
收录类别SCI
语种英语
资助者project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; KIP of CAS ; KIP of CAS ; KIP of CAS ; KIP of CAS ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; project 973 [2012CB821804] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; NSFC [11173021, 11322324, 11421303] ; KIP of CAS ; KIP of CAS ; KIP of CAS ; KIP of CAS ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8] ; CNPq [308876/2014-8]
WOS类目Astronomy & Astrophysics
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文献类型期刊论文
条目标识符http://ir.itp.ac.cn/handle/311006/20769
专题理论物理所SCI论文
通讯作者Santos, L (reprint author), Chinese Acad Sci, Univ Sci & Technol China, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China.
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Santos, L,Cabella, P,Villela, T,et al. Influence of Planck foreground masks in the large angular scale quadrant CMB asymmetry[J]. ASTRONOMY & ASTROPHYSICS,2015,584(0):A115.
APA Santos, L,Cabella, P,Villela, T,Zhao, W,&Santos, L .(2015).Influence of Planck foreground masks in the large angular scale quadrant CMB asymmetry.ASTRONOMY & ASTROPHYSICS,584(0),A115.
MLA Santos, L,et al."Influence of Planck foreground masks in the large angular scale quadrant CMB asymmetry".ASTRONOMY & ASTROPHYSICS 584.0(2015):A115.
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