2. Large-Scale Structure & Surveys Max Tegmark, MIT

3. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Onion Tegmark 2002, Science, 296, 1427-33 Summary of last lecture

4. Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy Summary of last lecture 400

5. SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 Assumes k=0 Vanilla rules OK! 0th order: what we’ve learned about our expansion history Summary of last lecture

6. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/0207047 + updates CMB 1st order: what we’ve learned about cosmic clustering Summary of last lecture

7. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 1st order: what we’ve learned about cosmic clustering Summary of last lecture

8. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 000619 DO ANY OF THESE QUESTIONS CONFUSE YOU? 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? 12. What came before the Big Bang? 13.Should I feel insignificant?

9. The cosmic plan: Survey of cosmology basics Measuring large-scale structure with galaxy surveys Measuring large-scale structure neutral hydrogen L1: L3: L2:

10. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Springel, Frenk & White 2006, Nature, 440, 11

11. Measuring large-scale structure with galaxy surveys: what are the challenges? Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1

12. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LSS de Lapparent, Geller & Huchra 1986

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

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

15. Cmbgg OmOl LSS

16. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

17. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 PSCz 15000 gals: (Data points uncorrelated) (Hamilton, Tegmark & Padmanabhan 2000)

18. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 SDSS 2006: 2dFGRS 250000 gals SDSS DR4 400000 gals, now ~10 6 gals

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

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

21. Cmbgg OmOl

22. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 (Table from Natalie Roe) SOME SURVEYS TO LOOK FORWARD TO:

23. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LAMOST: The Large Sky Area Multi-Object Fibre Spectroscopic Telescope

24. Measuring large-scale structure with galaxy surveys: what are the challenges? Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1

25. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Why are LRGs so useful?

26. 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

27. LSS Our observable universe

28. LSS Our observable universe

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

30. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LSS LRG’s

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

32. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LSS Common gals: too dense Quasars: too sparse LRG’s: just right! Why LRG’s are “Goldilocks galaxies”: 60000 LRG’s have more statistical power than 2 million regular gals

33. Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities Measuring large-scale structure with galaxy surveys: what are the challenges?  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1

34. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Sky coverage of SDSS DR4 redshift survey (Aitoff projection, equatorial coordinates) (Dust map fromSchlegel, Finkbeiner & Davis)

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

36. Measuring large-scale structure with galaxy surveys: what are the challenges? Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1

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

38. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 MT, Hamilton, Strauss, Vogeley & Szalay 1998 SDSS

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

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

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

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

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

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

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

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

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

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 LSS

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

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

55. 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 Sky coverage of SDSS DR4 redshift survey (Aitoff projection, equatorial coordinates) (Dust map fromSchlegel, Finkbeiner & Davis)

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

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

59. Measuring large-scale structure with galaxy surveys: what are the challenges? Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1

60. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 Virgo LCDM simulation CMB

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

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

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

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

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

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

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

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

69. Max Tegmark Dept. of Physics, MIT tegmark@mit.edu Cosmologia en la Playa January 11-15, 2010 LSS Lum funcs & sel funcs by Michael Blanton (NYU)

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

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

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

73. Molly Swanson, MT, Mike Blanton, Idit Zehavi: arXiv: 0702584

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

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

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

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

79. Measuring large-scale structure with galaxy surveys: what are the challenges? Statistical errors - Sample variance: want big V - Shot noise: want large n Systematic errors - Dust extinction (angular selection function) - Radial selection function errors Data analysis - Survey geometry (window functions) - Numerical challenges Linking light to mass: - bias - redshift distortions - nonlinearities  P ~ N -1/2 (P+n -1 ) N ~ V k^3 So aim for as large V as possible with nP~1