Detection of a non‐Gaussian spot in WMAP
暂无分享,去创建一个
P. Vielva | L. Cayón | M. Cruz | P. Vielva | E. Martínez-González | L. Cayón | M. Cruz | E. Martínez-González
[1] Testing the cosmological principle of isotropy: Local power spectrum estimates of the WMAP data , 2004, astro-ph/0404206.
[2] Anthony N. Lasenby,et al. Testing the Gaussianity of the COBE DMR data with spherical wavelets , 2000 .
[3] Non-Gaussianity of the Derived Maps from the First-Year Wilkinson Microwave Anisotropy Probe Data , 2003 .
[4] H. K. Eriksen,et al. On Foreground Removal from the Wilkinson Microwave Anisotropy Probe Data by an Internal Linear Combination Method: Limitations and Implications , 2004, astro-ph/0403098.
[5] N. Aghanim,et al. Non-Gaussianity: Comparing wavelet and Fourier based methods , 2003 .
[6] G. A. Ruiz,et al. Analysis of CMB maps with 2D wavelets , 1999 .
[7] Edward J. Wollack,et al. First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters , 2003, astro-ph/0302209.
[8] F. Argueso,et al. The performance of spherical wavelets to detect non‐Gaussianity in the cosmic microwave background sky , 2002 .
[9] Non-Gaussian signatures in the temperature fluctuation observed by the Wilkinson Microwave Anisotropy Probe , 2003, astro-ph/0307469.
[10] Italy,et al. Wavelets applied to cosmic microwave background maps: a multiresolution analysis for denoising , 1999 .
[11] Edward J. Wollack,et al. First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results , 2003, astro-ph/0302207.
[12] Multipole vectors - A New representation of the CMB sky and evidence for statistical anisotropy or non-Gaussianity at 2 <= l <= 8 , 2003, astro-ph/0310511.
[13] Pierre Vandergheynst,et al. Wavelets on the n-sphere and related manifolds , 1998 .
[14] Wayne Hu,et al. Weak lensing of the CMB: A harmonic approach , 2000, astro-ph/0001303.
[15] L. Toffolatti,et al. Combining maximum-entropy and the Mexican hat wavelet to reconstruct the microwave sky , 2001 .
[16] U. Seljak,et al. A Line of sight integration approach to cosmic microwave background anisotropies , 1996, astro-ph/9603033.
[17] F. Hansen,et al. Asymmetries in the Local Curvature of the Wilkinson Microwave Anisotropy Probe Data , 2004 .
[18] V. Acquaviva,et al. Gauge-invariant second-order perturbations and non-Gaussianity from inflation , 2003 .
[19] B. Wandelt,et al. The Hot and Cold Spots in the Wilkinson Microwave Anisotropy Probe Data Are Not Hot and Cold Enough , 2004 .
[20] P. Vielva,et al. Detection of non-Gaussianity in the WMAP 1-year data using spherical wavelets , 2003 .
[21] R. Durrer. Topological defects in cosmology , 1999 .
[22] Edward J. Wollack,et al. First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission , 2003, astro-ph/0302208.
[23] D. Spergel,et al. Global texture and the microwave background. , 1990, Physical review letters.
[24] A. Lasenby,et al. Wavelet analysis and the detection of non-Gaussianity in the cosmic microwave background , 1998 .
[25] Dan McCammon,et al. ROSAT Survey Diffuse X-Ray Background Maps. II. , 1997 .
[26] James E. Taylor,et al. Observing the Sunyaev–Zel'dovich effect closer to home , 2003, astro-ph/0303262.
[27] M. Halpern,et al. First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Tests of Gaussianity , 2003 .
[28] A. J. Banday,et al. Spherical Mexican hat wavelet: an application to detect non-Gaussianity in the COBE-DMR maps , 2001 .
[29] C. H. Lineweaver,et al. Applications of Wavelets to the Analysis of Cosmic Microwave Background Maps , 1999, astro-ph/9903206.
[30] The Effect of Weak Gravitational Lensing on the Cosmic Microwave Background Anisotropy: Flat versus Open Universe Models , 1997, astro-ph/9702231.
[31] P. Vielva,et al. Detection of Non-Gaussianity in the Wilkinson Microwave Anisotropy Probe First-Year Data Using Spherical Wavelets , 2004 .
[32] Yun Wang,et al. Wavelets and Wilkinson Microwave Anisotropy Probe Non-Gaussianity , 2004 .
[33] Microwave background bispectrum. II. A probe of the low redshift universe , 1998, astro-ph/9811251.
[34] J. L. Sanz,et al. CMB anisotropies generated by cosmic voids and great attractors , 1990 .
[35] Jeremiah P. Ostriker,et al. Generation of microwave background fluctuations from nonlinear perturbations at the era of galaxy formation , 1986 .
[36] A. Banday,et al. COBE—DMR constraints on the non-linear coupling parameter: a wavelet based method , 2002, astro-ph/0211399.
[37] L. Toffolatti,et al. Predicted Planck extragalactic point-source catalogue , 2001, astro-ph/0104077.
[38] R. B. Barreiro,et al. Isotropic wavelets: a powerful tool to extract point sources from cosmic microwave background maps , 1999, astro-ph/9912471.
[39] P. Lilje,et al. Asymmetries in the Cosmic Microwave Background Anisotropy Field , 2004 .
[40] Pia Mukherjee,et al. Wavelets and Wilkinson Microwave Anisotropy Probe Non-Gaussianity , 2004, astro-ph/0402602.
[41] L. Toffolatti,et al. Point source detection using the Spherical Mexican Hat Wavelet on simulated all-sky Planck maps , 2002, astro-ph/0212578.
[42] P. Peebles. An Isocurvature Model for Early Galaxy Assembly , 1997 .
[43] David Valls-Gabaud,et al. Evidence for Scale-Scale Correlations in the Cosmic Microwave Background Radiation , 1998 .
[44] R. B. Barreiro,et al. The discriminating power of wavelets to detect non-Gaussianity in the cosmic microwave background , 2001 .
[45] T. Piran,et al. The Signature of a Correlation between Cosmic-Ray Sources above 1019 eV and Large-Scale Structure , 1996, astro-ph/9604005.
[46] Francis Bernardeau,et al. Non-Gaussianity in multifield inflation , 2002 .