PLANCK'S VIEW OF THE UNIVERSE IN FRONT OF THE MICROWAVE BACKGROUND

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1 PLANCK'S VIEW OF THE UNIVERSE IN FRONT OF THE MICROWAVE BACKGROUND Gravitational lensing and Sunyaev-Zeldovich signals The Planck Consortium (presented by Simon White) Paris 21/03/2013

2 PLANCK'S FIRST IMAGE OF THE WHOLE SKY Planck's multi-frequency imaging allows different emission components to be separated and mapped Here emission from our own Milky Way is emphasised, particularly infrared emission from interstellar dust warmed by star-light Planck foregrounds S.White Paris Planck press conf. Pag. 2

3 PLANCK S MAP OF THE MICROWAVE BACKGROUND Planck's multi-frequency imaging allows different emission components to be separated and mapped Here emission from our own Milky Way is removed, together with light from other galaxies, leaving an image of the young Universe (t~380,000 yrs) Planck foregrounds S.White Paris Planck press conf. Pag. 3

4 GRAVITATIONAL LENSING DISTORTS IMAGES The gravitational effects of intervening matter bend the path of CMB light on its way from the early universe to the Planck telescope. This gravitational lensing distorts our image of the CMB UPlanck foregrounds S.White Paris Planck press conf. Pag. 4

5 GRAVITATIONAL LENSING OF THE CMB A simulated patch of CMB sky before lensing 10º Planck foregrounds S.White Paris Planck press conf. Pag. 5

6 GRAVITATIONAL LENSING OF THE CMB A simulated patch of CMB sky after lensing 10º Planck foregrounds S.White Paris Planck press conf Pag. 6

7 PLANCK MAPS THE DARK MATTER DISTRIBUTION Planck images of the mass distribution throughout (almost) the entire visible Universe. This is 85% Dark Matter, 15% ordinary matter... Planck foregrounds S.White Paris Planck press conf. Pag. 7...but these maps are noisy!

8 THE EFFECT OF NOISE ON THE MASS MAPS Simulated Planck mass image without noise Planck foregrounds S.White Paris Planck press conf Pag. 8

9 THE EFFECT OF NOISE ON THE MASS MAPS Simulated Planck mass image with realistic noise Planck foregrounds S.White Paris Planck press conf Pag. 9

10 THE CLUMPINESS OF THE PLANCK CMB MAP Fluctuations in the Planck CMB map as a function of angular scale. This is clumpiness in the early universe at an age of 380,000 years Planck foregrounds S.White Paris Planck press conf Pag. 10

11 THE CLUMPINESS OF THE PLANCK MASS MAP Fluctuations in the Planck mass map as a function of angular scale. This is clumpiness in the modern universe, measured though gravitational lensing. 2º 0.2º prediction based on the primary CMB fluctuations and the standard model Planck foregrounds S.White Paris Planck press conf Pag. 11

12 GALAXIES MIRROR THE PLANCK MASS MAP The mass distribution seen in the Planck map follows the distributions of galaxies, galaxy clusters and quasars found by other telescopes Quasars redshift ~ 1 Galaxy clusters redshift ~ 0.2 Galaxies redshift ~ 0.5 Galaxies redshift ~ 0.1 Planck foregrounds S.White Paris Planck press conf Pag. 12

13 THE COSMIC INFRARED BACKGROUND Planck image of part of the sky with little Milky Way dust emission. What there is has been removed using Galactic hydrogen maps made by other telescopes. This map primarily shows the Cosmic Infrared Background, emission from warm dust in distant star-forming galaxies at redshifts between 1 and 3 Planck foregrounds S.White Paris Planck press conf Pag. 13

14 CIB PEAKS CORRESPOND TO MASS PEAKS Stacking the Planck mass maps at the positions of peaks and troughs of Cosmic Infrared Background leads to a strong detection of the mass associated with these distant star forming galaxies. This is mostly Dark Matter, 1º Planck foregrounds S.White Paris Planck press conf Pag. 14

15 THE MASS AND CIB MAPS CORRESPOND CLOSELY The Planck mass map correlates very strongly with the CIB maps. This is a direct detection of the total mass associated with galaxies at the time they were making most of their stars. During this epoch, the Universe went from 20% to 50% of its present age. Planck foregrounds S.White Paris Planck press conf Pag. 15

16 PLANCK MAP OF THE BARYON DISTRIBUTION Planck can also image the gas (baryon) distribution in the low-redshift Universe using scattering of CMB photons off the electrons. This SZ (Sunyaev-Zeldovich) effect causes a change in the shape of the CMB spectrum Planck foregrounds S.White Paris Planck press conf Pag. 16

17 PLANCK MAP OF THE BARYON DISTRIBUTION Planck can also image the gas (baryon) distribution in the low-redshift Universe using scattering of CMB photons off the electrons. This SZ (Sunyaev-Zeldovich) effect causes a change in the shape of the CMB spectrum Planck foregrounds S.White Paris Planck press conf Pag. 17

18 PLANCK S CATALOGUE OF BIG GALAXY CLUSTERS The SZ effect allows Planck to find massive galaxy clusters over the whole sky. The most massive object in the observable universe is probably among them cluster candidates including 861 confirmed clusters Planck foregrounds S.White Paris Planck press conf Pag. 18

19 PLANCK IMAGE OF THE COMA GALAXY CLUSTER The nearest very massive cluster of galaxies. Planck detects the cluster atmosphere much farther from the centre than was previously possible Planck not only allows us to explore the early universe by mapping the clouds at t~380,000 years which hide it from us, but also maps the ordinary and Dark Matter distributions throughout the visible universe in front of those clouds. This brings us closer to understanding how today s universe emerged from the Big Bang Planck foregrounds S.White Paris Planck press conf Pag. 19

20 THANK YOU Simon White, for the Planck Consortium Director, Max Planck Institute for Astrophysics

Malcolm S. Longair. Galaxy Formation. With 141 Figures and 12 Tables. Springer

Malcolm S. Longair. Galaxy Formation. With 141 Figures and 12 Tables. Springer Malcolm S. Longair Galaxy Formation With 141 Figures and 12 Tables Springer Contents Part I Preliminaries 1. Introduction, History and Outline 3 1.1 Prehistory 3 1.2 The Theory of the Expanding Universe