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

3. par movies

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

5. 430 386 13.8

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

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

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

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

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

11. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Cmbgg OmOl CMB+SN Ia CMB+LRG Beth Reid et al, arXiv 0907.1559

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

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

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

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

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

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

18. 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

19. 4% 75% 21% Cosmological data Cosmological Parameters

20. 4% 75% 21% Cosmological data Cosmological Parameters ARE WE DONE?

21. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

22. 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?

23. 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!

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

25. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu 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

26. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu 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

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

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

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

30. 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

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

32. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496 Our observable universe

33. LSS Our observable universe

34. LSS The time frontier

35. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

36. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

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

38. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles GMRT = Giant Metrewave Radio Telescope

39. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles 21CMA/PaST = Primeval Structure Telescope

40. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) 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

41. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles MWA = Murchison Widefield Array

42. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles Cas A 3C 392 Cygnus A PAPER = Precision Array to Probe Epoch of Reionization

43. 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 ) 5.10 4 7.0.10 4 1.0.10 5 ~ 10 4 1.0.10 4 1.0.10 6 Imaging Field of View 2 o 3 o - 7.5 o ~ 5 o 30 o - 1 o Angular Resolution 3.8 o - 0.4 o 3’ 25” - 3.5” ~ 15’< 0.1’ Frequency Range (MHz) 50 - 142050 - 200 10 - 240 80 - 300110 - 200 Mapping Sensitivity 15mK/(day) 1/2 Site IndiaChina Netherlands AustraliaUSA/AUSAUS(?) Year 20072007 2007 200820082015(?) Experiment GMRTPAST/21CMA LOFAR MWAPAPERSKA 96 V crossed Dipoles SKA = Square Kilometer Array

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

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

46. The Omniscope MT & Matias Zaldarriaga, arXiv 0805.4414 [astro-ph]

47. 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?

48. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

49. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

50. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

51. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

52. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

53. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010

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

57. LSS Our observable universe

58. LSS Our observable universe Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 Spatial curvature: WMAP+SDSS:  tot = 0.01 Planck:  tot = 0.003 21cm:  tot =0.0002

59. LSS Our observable universe Spectral index running: Planck:  =0.005 21cm  =0.00017  2 -potential:  0.0007  4 -potential:  0.008 Mao, MT, McQuinn, Zahn & Zaldarriaga 2008

60. 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