Weak gravitational lensing of CMB
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1 Weak gravitational lensing of CMB (Recent progress and future prospects) Toshiya Namikawa (YITP) Lunch May 08, 2013
2 Cosmic Microwave Background (CMB) Precise measurements of CMB fluctuations taken from The energy components of Universe is well described by flat ΛCDM model Cosmology can now focus on more advanced and fundamental issues! dark energy mass of neutrinos cosmic strings dark matter primordial gravitational waves primordial non-gaussianity
3 Cosmological probes CMB temperature/ polarizations Type-Ia Super Novae Baryon Acoustic Oscillations Cluster abundance 21cm brightness temperature Weak Lensing Compared to other observables, weak lensing is sensitive to both geometry and density fluctuations free from galaxy bias (Important for accurate cosmology) for CMB lensing, the properties of source (CMB) is well known
4 CMB Lensing CMB Lensing = distortion of spatial pattern of CMB anisotropies (Reviews : Lewis&Challinor 06, Hanson+ 10) Deflection angle d Θ n Θ n + d Θ n Last scattering surface Distance observer Lensed anisotropies Θ(n) = Θ n + d(n) χ s 2 dχ χ s χ ψ(η χχ 0 χ, χn) s 0 Lensing potential φ Gravitational potential
5 Dark Energy/ Massive Neutrinos Evolution of gravitational potential is affected by the properties of dark energy (or modified gravity), massive neutrinos, etc Massive neutrinos At small scales, the density fluctuations of neutrinos do not grow, because of their velocity dispersion Massive neutrinos do not contribute to the gravitational clustering, and the gravitational potential becomes weak k [Amplitude of gravitational potential]^2 m ν = 0.0 ev m ν = 1.0 ev (for details, see, e.g., Lesgourgues & Pastor 13)
6 Other motivations to measure CMB lensing CMB Lensing generates B-mode polarization and secondary non-gaussianity Significant contamination for a detection of primordial GWs / primordial non-gaussianity CMB polarizations y E-mode (even parity) Primordial GWs [B-mode power spectrum] C l BB = Σ m B lm 2 /(2l + 1) B lm = dn Y lm n B (n) x B-mode (odd parity) e.g., Knox+ 02, Kesden+ 02, Smith+ 09
7 Recent detections CMB lensing signals are detected from several CMB experiments 2011: First detection! from Atacama Cosmology Telescope (ACT) + WMAP 2012: Detection from South Pole Telescope (SPT) + WMAP (Das+ 11) (van Engelen+ 12) 2013: Detection with ~25σ!! from Planck (see also Planck 2013 results XVII) Lensing signals significantly improve the constraints on cosmological parameters Lensing still do not have enough sensitivity to constrain e.g. mass of neutrinos
8 Future prospects CMB experiments Planck(Pol), SPTpol, PolarBear, ACTPol, Polar, LiteBird, CMBPol expected 1σ-constraints TN+ 10 ACTPol + CMB lensing + cosmic shear + CMB lensing + cosmic shear Lensing signals would be measured with enough precision to probe, e.g., dark energy and massive neutrinos
9 Summary CMB lensing as a cosmological probe CMB lensing has sensitivity to probe massive neutrinos, dark energy, etc. Measurement of CMB lensing is also important to probe primordial GWs and primordial non-gaussianity Near future Recent CMB lensing detection is from temperature maps, but polarization data from upcoming experiments would significantly improve the current constraints from CMB lensing Practical methods of lensing measurement from polarization are required
10 Short summary of lensing reconstruction History Reconstruction technique - Basic ideas for quadratic estimator (e.g., Seljak 97; Seljak&Zaldarriaga 98; Hu&Okamoto 02; Okamoto & Hu 03; Lewis+ 11) - Maximum-likelihood estimator (Hirata&Seljak 03a,b; Hanson+ 09) - Curl mode estimator (Cooray+ 05; TN+ 12) Estimating lensing power spectrum, C l xx (e.g., Kesden&Cooray 03; Cooray&Kesden 04; Hanson+ 10; TN+ 13) Method in practical cases (masking, inhomogeneous noise, etc.) (e.g., Carvalho&Tereno 11; Hanson+ 11; TN+ 13) Future Method in practical cases for polarization Importance of higher-order statistics
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