21 cm tomography - Berkeley Center for Cosmological Physics
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Measuring cosmological parameters Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 par movies Using WMAP3 + SDSS LRGs: Ordinary Matter Dark Energy Cold Dark Matter 75% Hot Dark Matter Photons Budget Deficit Ordinary Matter 4% 5% Cold Dark Matter 23% 21% 386 430 13.8 Cosmology Particle physics Standard model parameters: C = h = G = kb = qe = 1 How flat is space? Why are we cosmologists so excited? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Somewhat. How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 tot=1.003 CMB+SN Ia CMB+LRG Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Beth Reid et al, arXiv 0907.1559 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Planck + SDSS: n=0.008, r=0.012 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 THE FUTURE It's tough to make predictions, especially about the future. Yogi Berra Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Cosmological data 75% Cosmological Parameters 4% 21% Cosmological data 75% Cosmological Parameters 4% 21% ARE WE DONE? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Cosmological data 75% Cosmological Parameters 21% 4% Why these particular values? Nature of dark matter? Fundamental theory ? Nature of dark energy? Nature of early Universe? Cosmological data 75% Cosmological Parameters 21% 4% Why these particular values? Nature of dark matter? Fundamental theory ? Nature of dark energy? Nature of early Universe? Map our universe! Physics with 21 cm tomography Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Courtney Peterson Tongyan Mike Lin matejek Andy Chris Lutomirski Adrian Liu Williams Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 TH E O M NI S C O PER S Courtney Peterson Tongyan Mike Joel Lin matejek Andy Ed Villasenor Adrian Chris Morgan Lutomirski Jackie Liu Williams Hewitt Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 TH E O M NI S C O PER S Scott Morrison TH E O M NI S C O PER S Angelica de Oliveira-Costa Scott Morrison Nevada Sanchez Joe Lee Henrique Pondé Oliveira Pinto Matias Zaldarriaga Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 TH E O M NI S C O PER S • Foreground modeling 0802.1525 • Foreground removal astro-ph/0501081, 0807.3952 0903.4890 • Optimal mapmaking 0909.0001 • Automatic calibration Liu et al, in prep • Faster correlation 0805.4414, 0909.0001 • Corner turning 0910.1351 • Survey design optimization 0802.1710 What are we so excited? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/03 History CMB Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Our observable universe Our observable universe LSS The time frontier LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 The scale frontier Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Physics of the 21 cm Line: GMRT = Giant Metrewave Radio Telescope Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 Physics of the 21 cm Line: 21CMA/PaST = Primeval Structure Telescope Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 Physics of the 21 cm Line: 2 Km 100 Km 77 sta. 32 sta. LOFAR = Low Frequency ARray Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 Physics of the 21 cm Line: MWA = Murchison Widefield Array Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 Physics of the 21 cm Line: Cas A Cygnus A 3C 392 PAPER = Precision Array to Probe Epoch of Reionization Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 Physics of the 21 cm Line: SKA = Square Kilometer Array Experiment GMRT PAST/21CMA # of Antennas(Total) 30 dishes 10,000 # of Antennas(Installed) 30 dishes # of Tiles NA LOFAR 2,000 (4 Tiles) 20 (1 Tile=500 ant) MWA PAPER 8,192 16 (4) 512 (32 Tiles) 96(1 Tile=16 ant) SKA 8 (0) 512 (1 Tile=16 ant) NA 96 V crossed Dipoles Effective Area (m 2) 5.104 Imaging Field of View 7.0.104 1.0.105 ~ 104 1.0.104 2o 3o - 7.5o ~ 5o 30o - 1o < 0.1’ Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200 Australia USA/AUS 15mK/(day)1/2 Mapping Sensitivity Site India China Netherlands Year 2007 2007 2007 2008 2008 AUS(?) 2015(?) 1.0.106 21 cm tomography experiments: PAPER Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LOFAR GMRT PAST/21CMA Image: FORTE satellite SKA ? MWA LARC: Lunar Array for Radio Cosmology Participants: MIT, Harvard, Washington, Berkeley, JPL, NRAO PI: Jacqueline Hewitt, MIT The Omniscope MT & Matias Zaldarriaga, arXiv 0805.4414 [astro-ph] How get huge sensitivity at low cost? Sensitivity T (A)-1/2 Single-dish telescope: cost A1.35 Interferometer: cost N2 A2 FFTT telescope idea: cost A, ~2 Telescopes as Fourier transformers QuickTime™ and a decompressor are needed to see this picture. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 The sensitivity frontier Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Omniscope Tegmark & Zaldarriaga 2008 Our observable universe LSS Our observable universe LSS Spatial curvature: WMAP+SDSS: tot= 0.01 Planck: tot= 0.003 21cm: tot=0.0002 Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Our observable universe LSS Spectral index running: Planck: =0.005 21cm =0.00017 2-potential: 0.0007 4-potential: 0.008 Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Neutrino mass: WMAP+SDSS: m <0.3 eV +LyF: m <0.17 eV Oscillations m>0.04 eV LSS Future lensing: m~0.03 eV 21cm: m=0.007 eV Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Our observable universe
