Lensing effect on polarization in microwave background: extracting convergence power spectrum TeX Export

@article{Guzik:2000ju, abstract = {Matter inhomogeneities along the line of sight deflect the cosmic microwave background (CMB) photons originating at the last scattering surface at redshift \$z \sim 1100\$. These distortions modify the pattern of CMB polarization. We identify specific combinations of Stokes \$Q\$ and \$U\$ parameters that correspond to spin 0,\$\pm 2\$ variables and can be used to reconstruct the projected matter density. We compute the expected signal to noise as a function of detector sensitivity and angular resolution. With Planck satellite the detection would be at a few \$\sigma\$ level. Several times better detector sensitivity would be needed to measure the projected dark matter power spectrum over a wider range of scales, which could provide an independent confirmation of the projected matter power spectrum as measured from other methods.}, archivePrefix = {arXiv}, author = {Guzik, Jacek and Seljak, Uros and Zaldarriaga, Matias}, citeulike-article-id = {5427205}, citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/9912505}, citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/9912505}, day = {23}, eprint = {astro-ph/9912505}, keywords = {cmb-lensing, cosmology, reconstruction, weak-lensing}, month = {Dec}, posted-at = {2009-08-12 15:21:26}, priority = {2}, title = {Lensing effect on polarization in microwave background: extracting convergence power spectrum}, url = {http://arxiv.org/abs/astro-ph/9912505}, year = {1999} }

TY - JOUR ID - Guzik:2000ju L3 - citeulike-article-id:5427205 N2 - Matter inhomogeneities along the line of sight deflect the cosmic microwave background (CMB) photons originating at the last scattering surface at redshift $z \sim 1100$. These distortions modify the pattern of CMB polarization. We identify specific combinations of Stokes $Q$ and $U$ parameters that correspond to spin 0,$\pm 2$ variables and can be used to reconstruct the projected matter density. We compute the expected signal to noise as a function of detector sensitivity and angular resolution. With Planck satellite the detection would be at a few $\sigma$ level. Several times better detector sensitivity would be needed to measure the projected dark matter power spectrum over a wider range of scales, which could provide an independent confirmation of the projected matter power spectrum as measured from other methods. TI - Lensing effect on polarization in microwave background: extracting convergence power spectrum KW - cmb-lensing KW - cosmology KW - reconstruction KW - weak-lensing AU - Guzik, Jacek AU - Seljak, Uros AU - Zaldarriaga, Matias PY - 1999/Dec/23/ UR - http://arxiv.org/abs/astro-ph/9912505 ER -