Max Tegmark
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SDSS slideshow Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 COSMOLOGY BASICS Max Tegmark, MIT Midsummer holiday, Leksand, Sweden Max Tegmark Where I was born and raised University of Pennsylvania Who are you? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 The cosmic plan: L1: • Overview of cosmology theory & observation - 0th order: cosmic expansion history Sarah Church - 1st order: cosmic clustering history - Observational tools: supernovae, CMB, galaxy clustering, . clusters, lensing, Ly forest, etc L2: - Cosmological parameters Sean Carroll, Phil Marshall • Revolutions on the horizon: QuickTime™ and a decompressor are needed to see this picture. - Nature of dark energy How will the Universe end? Will it? Neal Weiner - Nature of dark matter What is the Universe made of? - Nature of our early universe Sean Carroll How did the Universe begin? Did it? - String theory? Multiverse? - 21 cm tomography Galaxy surveys Microwave background Supernovae Ia THE COSMIC SMÖRGÅSBORD Gravitational lensing Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Big Bang nucleosynthesis Galaxy clusters Lyman forest Neutral hydrogen tomography What have we learned? OUR PLACE IN SPACE Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 DSE SDSS movie OUR PLACE IN TIME Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 The sky as a time machine Dark matter creation? Antimatter annihilation Creation of atomic nuclei Brief History of our Universe Dark energy evidence 400 (Graphics from Gary Hinshaw/WMAP team) Formation movies Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Fluctuation generator To 0th order: Fluctuation amplifier 386 400 (Graphics from Gary Hinshaw/WMAP team) Fluctuation generator To 1st order: Fluctuation amplifier 386 400 (Graphics from Gary Hinshaw/WMAP team) (Figure courtesy of COBE team) Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 0th order: a(t) 1st order: g(z,k) 400 Higher order: gastrophysics 13.7 0th order: Measuring Expansion: a(t) <=> H(z) (More on this in the lectures of Sean Carroll & Phil Marshall) Figure from WMAP team Distant light is -dimmed -redshifted Redshift Distant light is -dimmed -redshifted Dimming Redshift Distant light is -dimmed -redshifted Dimming Standard candles, rulers or clocks Standardizable candles (From Saul Perlmutter’s web site) QuickTime™ and a YUV420 codec decompressor are needed to see this picture. Using CMB blobs as a standardizable ruler: Open universe Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Guth & Kaiser 2005 (Science) + WMAP3 Inflation with Inflation without Cosmic strings Using galaxy correlations as a standardizable ruler: (Eisenstein, Hu & MT 1998; Eisenstein et al 2005; Cole et al 2005) Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Easiest to understand in real space (Bashinsky & Bertschinger, PRL, 87, 1301, 2001; PRD 123008, 2002) (Eisenstein et al 2005, for the SDSS collaboration astro-ph/050112) We’ve measured distance to z=0.35 to 5% accuracy Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Updates in Reid et al 0907.1659, Percival et al 0907.1660, Kazin et al 2009 in prep George Gamow 1904-1968 Big Bang nucleosynthesis as a standardizable clock: QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Kirkman et al 2003, astro-ph/0302006 George Gamow 1904-1968 Big Bang nucleosynthesis as a standardizable clock: H = dlna/dt, H2 Assumes k=0 SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 a = 1/(1+z) Inflationary gravitational waves as a standardizable clock: Qt ~ H/mplanck What we’ve learned about H(z) from SN Ia, CMB, BAO, BBN, etc: Assumes k=0 SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 Vanilla rules OK! What we’ve learned about H(z) from SN Ia Riess et al, astro-ph/0611572 • curvature: consistent with vanilla (k = 0) • topology: consistent with vanilla 1st order: measuring clustering Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496 CMB z = 1000 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 z=0 CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley) Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS (More from Sarah Church) Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 (Figure from Wayne Hu) (Figure from WMAP team) Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/030 CMB Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Why are there any CMB fluctuations at all? Why the wiggles? What’s their scale? Open universe Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Guth & Kaiser 2005 (Science) + WMAP3 Inflation with Inflation without Cosmic strings 3 CMB Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Lyman Alpha Forest Simulation: Cen et al 2001 LyF Quasar You Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 GRAVITATIONAL LENSING: A1689 imaged by Hubble ACS, Broadhurst et al 2004 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Lensing Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley) Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 But the best is yet to come… Precision, 21cm tomography, … Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Our observable universe LSS DO ANY OF THESE QUESTIONS CONFUSE YOU? QuickTime™ and a decompressor are needed to see this picture. 1. What is the Universe expanding into? 2. How can stuff be more than 14 billion light years away when the Universe is only 14 billion light years old? 3. Where in space did the Big Bang explosion happen? 4. Did the Big Bang happen at a single point? 5. How could a the Big Bang create an infinite space in a finite time? 6. How could space not be infinite? 7. If the Universe is only 10 billion years old, how can we see objects that are now 30 billion light years away? 8. Don’t galaxies receeding faster than c violate relativity theory? 9. Are galaxies really moving away from us, or is space just expanding? 10. Is the Milky Way expanding? 11. Do we have evidence for a Big Bang singularity? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 12. What came before the Big Bang? 13. Should I feel insignificant? END OF LECTURE I Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Tegmark 2002, Science, 296, 1427-33 Onion Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Summary of last lecture Fluctuation generator Summary of last lecture Fluctuation amplifier 400 (Graphics from Gary Hinshaw/WMAP team) 0th order: what we’ve learned about our expansion history Summary of last lecture Assumes k=0 SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 Vanilla rules OK! 1st order: what we’ve learned about cosmic clustering CMB Summary of last lecture Clusters LSS Lensing Ly Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Tegmark & Zaldarriaga, astro-ph/0207047 + updates 1st order: what we’ve learned about cosmic clustering Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Summary of last lecture DO ANY OF THESE QUESTIONS CONFUSE YOU? QuickTime™ and a decompressor are needed to see this picture. 1. What is the Universe expanding into? 2. How can stuff be more than 14 billion light years away when the Universe is only 14 billion light years old? 3. Where in space did the Big Bang explosion happen? 4. Did the Big Bang happen at a single point? 5. How could a the Big Bang create an infinite space in a finite time? 6. How could space not be infinite? 7. If the Universe is only 10 billion years old, how can we see objects that are now 30 billion light years away? 8. Don’t galaxies receeding faster than c violate relativity theory? 9. Are galaxies really moving away from us, or is space just expanding? 10. Is the Milky Way expanding? 11. Do we have evidence for a Big Bang singularity? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 12. What came before the Big Bang? 13. Should I feel insignificant? Measuring cosmological parameters Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 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 SLAC Summer Institute August 3-4, 2009 How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Somewhat. How flat is space? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 tot=1.003 CMB+SN Ia CMB+LRG Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Reid et al, arXiv 0907.1559 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Planck + SDSS: n=0.008, r=0.012 CMB + LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 THE FUTURE It's tough to make predictions, especially about the future. Yogi Berra Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 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 SLAC Summer Institute August 3-4, 2009 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? What’s dark energy? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 DARK ENERGY SUMMARY: Observation: • Still no observed departures from “vanilla” • #1 goal is searching for any non-vanilla behavior (density changing with time, clustering) (never mind w’ etc) Theory: • Zillions of papers and models, wide open: - cosmological constant + ground state density? - evolving scalar field? - modified gravity? • Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 The least unsuccessful solution to the coincidence problem is probably anthropic - but this depends on the inflationary measure problem, which remains unsolved What’s dark matter? Bullet Cluster, Clowe et al 2006, ApJ, 648, L109 100dpi Four roads to dark matter: catch it, infer it, make it, weigh it Direct: Indirect: Production: LHC restarts in ‘09 Gravitational: Fermi (né GLAST) launched 6/11-08, Pamela Planck launched May 2009 21 cm tomography coming DARK MATTER SUMMARY: Observation: • Make it: LHC may discover SUSY • Catch it: Direct detection experiments may succeed soon • Weigh it: Still no observed departures from “vanilla” observing this would be sensational (non-vanilla fluctuation growth, evidence of interaction) • Infer it: Indirect detection possible from annihilation Theory: • Zillions of papers and models, wide open: - WIMP? - axion? - multiple dark matters? - modified gravity? • Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Why is its density comparable to that for baryons? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Measured value=4eV Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 WHAT DO WE WANT TO MEASURE? 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 SLAC Summer Institute August 3-4, 2009 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/030 History CMB Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Our observable universe Our observable universe LSS The time frontier LSS Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 The scale frontier Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 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 SLAC Summer Institute August 3-4, 2009 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 SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 The sensitivity frontier Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 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 DO ANY OF THESE QUESTIONS CONFUSE YOU? QuickTime™ and a decompressor are needed to see this picture. 1. What is the Universe expanding into? 2. How can stuff be more than 14 billion light years away when the Universe is only 14 billion light years old? 3. Where in space did the Big Bang explosion happen? 4. Did the Big Bang happen at a single point? 5. How could a the Big Bang create an infinite space in a finite time? 6. How could space not be infinite? 7. If the Universe is only 10 billion years old, how can we see objects that are now 30 billion light years away? 8. Don’t galaxies receeding faster than c violate relativity theory? 9. Are galaxies really moving away from us, or is space just expanding? 10. Is the Milky Way expanding? 11. Do we have evidence for a Big Bang singularity? Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009 12. What came before the Big Bang? 13. Should I feel insignificant? Got to here Max Tegmark Dept. of Physics, MIT tegmark@mit.edu SLAC Summer Institute August 3-4, 2009
