PPT-CMB, lensing, and non-

Gaussianities Antony Lewis httpcosmologistinfo Lewis arXiv11075431 Hanson amp Lewis arXiv09080963 Lewis Challinor amp Hanson arXiv11012234 Pearson Lewis amp Regan arXiv12011010. Surveys of large scale structure will probe Dark Energy by measuring the BAO scale vs. redshift. . Planned:. DESI, Euclid, WFIRST, .... 2. Hydrogen Intensity Mapping. To measure BAO scale there is no need to resolve individual galaxies. Map intensity of HI gas using redshifted 21 cm emission along the line of sight.. weak . lensing. science. Rachel . Mandelbaum. , CMU. Cosmology. A homogeneous . and isotropic. universe. Spatially flat . and . expanding (accelerating!). General Relativity:. 2. Function of the metric (defining space-time behavior). Boot Camp. Robert Nemiroff. Michigan Tech . Abstract. What is gravitational lensing, what has it told us about the universe, and what more can it tell us about the universe? Lenses such as black holes, stars, galaxies, clusters of galaxies, and the universe as a whole will be covered. Concepts such as Einstein rings, photon spheres, image pair creation events, and shear will be defined and briefly discussed. The intersection of gravitational lensing with current research frontiers will be reviewed including how microlensing is being used to search for extra-solar planets, how radio telescopes are being used to probe galaxy-center black holes, and how weak lensing is being used to probe galaxy evolution in the early universe. Possible lensing signals in continuing and upcoming missions such as Planck, DES, LSST, Euclid, and WFIRST will be reviewed. Relevant parts of the lecturer's own research will also be briefly mentioned. . and. Quasars . “A man should look for what is, and not what he thinks should be.” – Albert Einstein . Arvind. Haran and David Johnston. What is Gravitational Lensing?. Let’s take a step back to the Einstein days…. Sarah Bridle. University College London. 3d vs 2d (tomography). Non-Gaussian -> higher order statistics. Low redshift -> dark energy. versus. Weak Lensing Tomography. In principle (perfect zs). Antony Lewis. http://cosmologist.info/. Lewis . arXiv:1204.5018. see also . Creminelli. . et al . astro-ph. /0405428, . arXiv:1109.1822, . Bartolo. et al arXiv:1109.2043. Lewis . arXiv:1107.5431. Lewis. ICRR, U Tokyo. Weak lensing of CMB. from. . cosmic (super-)strings. 9/28/2011 JGRG21 @ Tohoku U. w. ith A. . Taruya. (U Tokyo, RESCEU), T. . Namikawa. (U Tokyo), . K. Takahashi (Kumamoto U), Y. . Examples of Lens Systems. about 1 arcminute. about 1 arcsecond. Galaxy Clusters. Galaxies. More examples. Clusters of galaxies as lenses. T. Johnson . (U Michigan). Many examples. are known, but. strong lensing. in Globular Clusters. Margarita . Safonova. . Ancient Greeks knew that light travels in a straight line... Or you wouldn’t be able to cross the road!. Gravitational . Lensing. —. Astronomical Mirages. Towards the first detection using SPT polarisation. ASA 2016 meeting, . Sydney. 04. 07. 2016. Srinivasan. . Raghunathan. School of Physics. University of Melbourne. In a nutshell . …. . South Pole Telescope – Observes CMB (both T, and P).. Kaiki Taro Inoue . (KINDAI U.). Seminar. @Osaka U 22 Feb 2017. Outline. Missing Satellite Problem. Gravitational Lensing . Substructure vs Line-of-sight Halos. ALMA Observations (SDP.81, MG0414+0534). Ue. -Li Pen. Tingting. Lu. Olivier Dore. Cosmological Errors. How do we know errors on measurement and theory?. For Gaussian field, P(k) is 2-PCF, its error (Fisher) is 4-PCF, and the error on Fisher is 8-PCF.. 6. Extragalactic Microlensing. Wambsganss. . 2001. /sharp caustic crossing. /2,3-pt lens. Local Group vs. Extragalactic Microlensing. =k. Local Group Microlensing – . very very low optical depth.