The History of the Universe in One Hour. Max Tegmark, MIT
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1 The History of the Universe in One Hour Max Tegmark, MIT
2 QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. Other people associated with MIT who worked on COBE: Chuck Bennett, Ed Cheng, Steve Meyer, Rai Weiss & Ned Wright
3 OUR PLACE IN SPACE Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
4 DSE
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17 SDSS movie from MW
18 OUR PLACE IN TIME Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
19 The sky as a time machine
20 Figure from WMAP team
21 (Figure from Wayne Hu) (Figure from WMAP team)
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23 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/ CMB Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
24 Fluctuation generator Brief History of our Universe Fluctuation amplifier 400 (Graphics from Gary Hinshaw/WMAP team)
25 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 Formation movies
26 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
27 Galaxy surveys Microwave background Supernovae Ia THE COSMIC SMÖRGÅSBORD Gravitational lensing Big Bang nucleosynthesis Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 Galaxy clusters Lyman forest Neutral hydrogen tomography
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29 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/ CMB Our observable universe Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
30 LSS Our observable universe
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32 Springel, Frenk & White 2006, Nature, 440, 11
33 Measuring cosmological parameters
34 What s the matter? 75% 4% 21%
35 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 How flat is space?
36 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 How flat is space?
37 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 How flat is space? Somewhat.
38 How flat is space? tot =1.003 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
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40 Q: Is there more that exists than we can see? Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 Cosmology suggests yes!
41 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 How big is our Universe?
42 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/
43 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
44 PHYSICS OR PHILOSOPHY? Q: Are theories which predict the existence of unobservable parallel universes untestable? A: No, as long as they also make predictions for things we can observe. Example 1: GR predicts black hole interiors? infinite Example 2: Inflation predicts space Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
45 Cosmological data Cosmological Parameters 75% 4% 21%
46 Cosmological data Cosmological Parameters 75% 4% 21% Why these particular values? Fundamental theory? Nature of dark matter? Nature of dark energy? Nature of early Universe? Map our universe!
47 Galaxy surveys Microwave background Supernovae Ia Gravitational lensing What s the next big thing in cosmology? Big Bang nucleosynthesis Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Amateur Astronomer Assoc. NY, October 1, 2010 Galaxy clusters Lyman forest Neutral hydrogen tomography
48 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/ CMB Our observable universe Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
49 LSS Our observable universe
50 The time frontier LSS
51 The Omniscope MT & Matias Zaldarriaga, arxiv: ,
52 How get huge sensitivity at low cost? Sensitivity T (A ) -1/2 Single-dish telescope: cost A 1.35 Interferometer: cost N 2 A 2 FFT telescope idea: cost A, ~2 Telescopes as Fourier transformers
53 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 QuickTime and a decompressor are needed to see this picture.
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55 Where are we now? Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
56 Foreground modeling Foreground removal astro-ph/ , , Optimal mapmaking Automatic calibration Faster correlation , Corner turning Survey design optimization
57 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
58 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
59 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
60 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 Eben Kunz
61 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
62 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
63 Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
64 Where are we going? Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010
65 The sensitivity frontier FFTT Max Tegmark Dept. of Physics, MIT Amateur Astronomer Assoc. NY, October 1, 2010 Tegmark & Zaldarriaga 2008
66 LSS Our observable universe
67 Our observable universe LSS Spatial curvature: WMAP+SDSS: tot = 0.01 Planck: tot = cm: tot = Mao, MT, McQuinn, Zahn & Zaldarriaga 2008
68
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