Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Measuring cosmological parameters.

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Presentation transcript:

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Measuring cosmological parameters

par movies

Cmbgg OmOl 4% 21% 75% Using WMAP3 + SDSS LRGs:

Cmbgg OmOl Standard model parameters: Cosmology Particle physics Required Optional C = h = G = k b = q e = 1 

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl How flat is space? flat closed open Why are we cosmologists so excited?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl How flat is space?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl How flat is space?Somewhat.

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl  tot =1.003  How flat is space?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB+SN Ia CMB+LRG Beth Reid et al, arXiv

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB + LSS Planck + SDSS:  n=0.008,  r=0.012

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 THE FUTURE It's tough to make predictions, especially about the future. Yogi Berra

4% 75% 21% Cosmological data Cosmological Parameters

4% 75% 21% Cosmological data Cosmological Parameters ARE WE DONE?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

4% 75% 21% Cosmological data Fundamental theory ? Cosmological Parameters Nature of dark matter? Nature of dark energy? Nature of early Universe? Why these particular values?

4% 75% 21% Cosmological data Fundamental theory ? Cosmological Parameters Nature of dark matter? Nature of dark energy? Nature of early Universe? Why these particular values? Map our universe!

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Physics with 21 cm tomography

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Courtney Peterson Andy Lutomirski Tongyan Lin Adrian Liu Mike matejek Chris Williams T H E O M N I S C O P E R S

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Courtney Peterson Andy Lutomirski Tongyan Lin Adrian Liu Mike matejek Chris Williams Ed Morgan Joel Villasenor Jackie Hewitt T H E O M N I S C O P E R S

Scott Morrison T H E O M N I S C O P E R S

Scott Morrison Nevada Sanchez Henrique Pond é Oliveira Pinto Joe Lee Angelica de Oliveira-Costa

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Matias Zaldarriaga T H E O M N I S C O P E R S

Foreground modeling Foreground removal astro-ph/ , Optimal mapmaking Automatic calibration Liu et al, in prep Faster correlation , Corner turning Survey design optimization

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 What are we so excited?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/ Our observable universe

LSS Our observable universe

LSS The time frontier

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 The scale frontier

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles GMRT = Giant Metrewave Radio Telescope

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles 21CMA/PaST = Primeval Structure Telescope

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles LOFAR = Low Frequency ARray 2 Km 100 Km 32 sta. 77 sta. v v v v v v v v

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles MWA = Murchison Widefield Array

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles Cas A 3C 392 Cygnus A PAPER = Precision Array to Probe Epoch of Reionization

Physics of the 21 cm Line: # of Antennas(Total) 30 dishes 10,000 8,19216 (4) # of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0) # of Tiles NA20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA Effective Area (m 2 ) ~ Imaging Field of View 2 o 3 o o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year (?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles SKA = Square Kilometer Array

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Image: FORTE satellite MWA PAST/21CMA LOFARGMRTPAPER SKA ? 21 cm tomography experiments:

Participants: MIT, Harvard, Washington, Berkeley, JPL, NRAO PI: Jacqueline Hewitt, MIT LARC: Lunar Array for Radio Cosmology

The Omniscope MT & Matias Zaldarriaga, arXiv [astro-ph]

Single-dish telescope: cost  A 1.35 Sensitivity  T  (A  ) -1/2 Interferometer: cost  N 2  A 2 FFTT telescope idea: cost  A,  ~2  Telescopes as Fourier transformers How get huge sensitivity at low cost?

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010

Max Tegmark Dept. of Physics, MIT Cosmologia en la Playa January 11-15, 2010 Tegmark & Zaldarriaga 2008 The sensitivity frontier Omniscope

LSS Our observable universe

LSS Our observable universe Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Spatial curvature: WMAP+SDSS:  tot = 0.01 Planck:  tot = cm:  tot =0.0002

LSS Our observable universe Spectral index running: Planck:  = cm  =  2 -potential:   4 -potential:  Mao, MT, McQuinn, Zahn & Zaldarriaga 2008

LSS Our observable universe Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Neutrino mass: WMAP+SDSS: m <0.3 eV +Ly  F: m <0.17 eV Oscillations m >0.04 eV Future lensing:  m ~0.03 eV 21cm:  m =0.007 eV