1. Gong-Bo Zhao ICG, Portsmouth 1106.3327 (PRL submitted) 1105.0922 (PRL 11) 1011.1257(PRD 11) 1005.3810 (PASP 11) 0905.1326 (PRL 09) Understanding the Cosmic Acceleration using KDUST

2. My main collaborators Robert Crittenden (Portsmouth), Zuhui Fan (PKU) Aireza Hojjati (SFU), Kazuya Koyama (Portsmouth) Baojiu Li (Durham, Cambridge),Yinzhe Ma (UBC, Cambridge)Jeremiah Ostriker (Princeton, Cambridge), Levon Pogosian (SFU) Alessandra Silvestri (MIT), Lifan Wang (TAMU), Hu Zhan (NAOC) Xinmin Zhang (IHEP) Nov 9, 2011 KDUST workshop, IHEP, Beijing

3. Nov 9, 2011 KDUST workshop, IHEP, Beijing Nobel Prize, 2011

4. Cosmic Acceleration Nov 9, 2011 KDUST workshop, IHEP, Beijing DE MG

5. Nov 9, 2011 KDUST workshop, IHEP, Beijing Weak Lensing Galaxy Counts ISW KDUST

6. KDUST is useful for DE Nov 9, 2011 KDUST workshop, IHEP, Beijing

7. Nov 9, 2011 KDUST workshop, IHEP, Beijing LSST 15000 sq. deg. Ugrizy GBZ, H.Zhan, L. Wang, Z. Fan, X.Zhang, 1005.3810, PASP 11 15000 sq. deg.: n(z) ~ z 2 exp(-z/0.5) Photo-z rms:  z =0.04(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.003 Residual shear power: 6×10 -10

8. Nov 9, 2011 KDUST workshop, IHEP, Beijing 5000 sq. deg.: n(z) ~ z 2 exp(-z/0.6) Photo-z rms:  z =0.03(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.002 Residual shear power: 4×10 -10 15000 sq. deg.: n(z) ~ z 2 exp(-z/0.5) Photo-z rms:  z =0.04(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.003 Residual shear power: 6×10 -10 KDUST JH + LSST ugrizy

9. Nov 9, 2011 KDUST workshop, IHEP, Beijing 10000 sq. deg.: n(z) ~ z 2 exp(-z/0.6) Photo-z rms:  z =0.03(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.002 Residual shear power: 4×10 -10 10000 sq. deg.: n(z) ~ z 2 exp(-z/0.5) Photo-z rms:  z =0.04(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.003 Residual shear power: 6×10 -10 KDUST JH + LSST ugrizy

10. Nov 9, 2011 KDUST workshop, IHEP, Beijing 5000 sq. deg.: n(z) ~ z 2 exp(-z/0.6) Photo-z rms:  z =0.03(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.002 Residual shear power: 4×10 -10 15000 sq. deg.: n(z) ~ z 2 exp(-z/0.5) Photo-z rms:  z =0.04(1+z) Photo-z bias prior:  P (  z)=0.2  z Shear calibration error: ±0.003 Residual shear power: 6×10 -10 KDUST JH + LSST ugrizy SNe: (z < 1.5) KDUST—LSST Synergy credit: Hu Zhan

11. Nov 9, 2011 KDUST workshop, IHEP, Beijing Reconstructing w(a) precisely R.Crittenden, GBZ, L.Pogosian, L.Samushia, X.Zhang To appear soon see Levon’s talk Straightforward to apply to KDUST data!

12. KDUST is useful for MG Nov 9, 2011 KDUST workshop, IHEP, Beijing

13. On linear scale PCA (see Levon’s talk) Cosmic Mach Number Nov 9, 2011 KDUST workshop, IHEP, Beijing

14. arXiv: 1106.3327 with Yinzhe Ma (UBC, Cambridge) Jeremiah Ostriker (Princeton and Cambridge) Cosmic Mach Number: A robust tool to test Einstein Gravity

15. What is Mach Number?? Nov 9, 2011 KDUST workshop, IHEP, Beijing

16. Cosmic Mach Number (CMN) Ostriker & Suto 1990 Nov 9, 2011 KDUST workshop, IHEP, Beijing

17. Nov 9, 2011 KDUST workshop, IHEP, Beijing The shape of velocity power spectrum can be reconstructed from CMN

18. Nov 9, 2011 KDUST workshop, IHEP, Beijing CMN data

19. Cosmological applications Nov 9, 2011 KDUST workshop, IHEP, Beijing

20. Nov 9, 2011 KDUST workshop, IHEP, Beijing WMAP7 + UNION2 +CMN (6dF)

21. Power of CMN B 0 <0.4 (95% CL, CMB+SN) B 0 <5x10 -5 (95% CL, CMB+SN+CMN) Nov 9, 2011 KDUST workshop, IHEP, Beijing

22. CMN is a promising tool Immune to galaxy bias, overall amplitude, nonlinearities Highly sensitive to the scale-dependence of the growth, thus an ideal tool to constrain MG parameters and neutrino mass Complimentary to weak lensing Measure CMN from KDUST?? Nov 9, 2011 KDUST workshop, IHEP, Beijing

23. On Non-linear scale Environmental dependence of dark matter halos Nov 9, 2011 KDUST workshop, IHEP, Beijing

24. f(R) Gravity Nov 9, 2011 KDUST workshop, IHEP, Beijing Mimic GR at high z; Accelerate the expansion at low z; Recover GR locally to pass solar system test.

25. In GR Nov 9, 2011 KDUST workshop, IHEP, Beijing

26. In f(R) Nov 9, 2011 KDUST workshop, IHEP, Beijing lClC

27. In very dense regions Nov 9, 2011 KDUST workshop, IHEP, Beijing lClC

28. 12 billion years ago

29. 10 billion years ago

30. 8 billion years ago

31. Now

32. Numerical Simulations 1011.1257 GBZ, B.Li, K.Koyama, PRD 11 Code: Modified MLAPM f(R) model: Model parameters: Cosmological parameters: WMAP7 Nov 9, 2011 KDUST workshop, IHEP, Beijing

33. Equations to solve in the code Nov 9, 2011 KDUST workshop, IHEP, Beijing

34. Nov 9, 2011 KDUST workshop, IHEP, Beijing Get some sense…

35. Nov 9, 2011 KDUST workshop, IHEP, Beijing GR

36. Nov 9, 2011 KDUST workshop, IHEP, Beijing f(R)

37. Structure formation in GR KDUST workshop, IHEP, Beijing Nov 9, 2011

38. Structure formation in f(R) KDUST workshop, IHEP, Beijing Nov 9, 2011

39. Dynamical Mass KDUST workshop, IHEP, Beijing Nov 9, 2011

40. Dynamical Mass KDUST workshop, IHEP, Beijing Nov 9, 2011

41. Dynamical Mass KDUST workshop, IHEP, Beijing Spherical symmetry Nov 9, 2011

42. Lensing Mass KDUST workshop, IHEP, Beijing Nov 9, 2011

43. Lensing Mass KDUST workshop, IHEP, Beijing Nov 9, 2011

44. Lensing Mass KDUST workshop, IHEP, Beijing Spherical symmetry Nov 9, 2011

45. KDUST workshop, IHEP, Beijing Mass Difference Nov 9, 2011

46. KDUST workshop, IHEP, Beijing Nov 9, 2011

47. KDUST workshop, IHEP, Beijing In underdense environment Nov 9, 2011

48. KDUST workshop, IHEP, Beijing In underdense environment Nov 9, 2011

49. KDUST workshop, IHEP, Beijing Nov 9, 2011

50. KDUST workshop, IHEP, Beijing In dense environment Nov 9, 2011

51. KDUST workshop, IHEP, Beijing In dense environment The halos are screened so that they cannot feel the enhancement of gravity! Nov 9, 2011

52. How to define “Environment”? Number of neighbours in spheres of radius R Mass or density in spheres of radius R Matter density in spherical shells Average mass density of surrounding halos Distance to nearest halo with minimum mass Projected galaxy number density out to the Nth nearest neighbour with a maximum radial velocity … KDUST workshop, IHEP, Beijing Nov 9, 2011

53. KDUST workshop, IHEP, Beijing Haas et al., 1103. 0547 All these quantities strongly correlate with halo mass! Nov 9, 2011

54. To see the pure environmental effect, we need a new environment indicator which is uncorrelated with halo mass KDUST workshop, IHEP, Beijing The three-dimensional distance to the Nth nearest neighbour with a viral mass that is at least f times that of the halo under consideration, divided by the virial radius of the Nth nearest neighbour: Haas et al., 1103. 0547 Nov 9, 2011

55. KDUST workshop, IHEP, Beijing Small D Affected by the local environment Nov 9, 2011

56. KDUST workshop, IHEP, Beijing Small D Affected by the local environment Large D Affecting the local environment Nov 9, 2011

57. KDUST workshop, IHEP, Beijing GR analysis, Haas et al., 1103. 0547 D is a clean indicator for the local environment! Nov 9, 2011

58. KDUST workshop, IHEP, Beijing f(R) analysis, 1105.0922 GBZ, Baojiu Li, Kazuya Koyama (PRL 2011) Nov 9, 2011

59. KDUST workshop, IHEP, Beijing Nov 9, 2011

60. KDUST workshop, IHEP, Beijing Similar pattern!! Nov 9, 2011

61. KDUST workshop, IHEP, Beijing Similar pattern!! The screening is only determined by the halo mass for the isolated halos! Nov 9, 2011

62. KDUST workshop, IHEP, Beijing Different pattern Nov 9, 2011

63. KDUST workshop, IHEP, Beijing Different pattern The screening of the clustered halos is not determined by the halo mass only! Nov 9, 2011

64. KDUST workshop, IHEP, Beijing Different pattern Environmental Effect!! Nov 9, 2011

65. KDUST workshop, IHEP, Beijing Nov 9, 2011

66. KDUST workshop, IHEP, Beijing Clean mass dependence! Nov 9, 2011

67. KDUST workshop, IHEP, Beijing Nov 9, 2011

68. KDUST workshop, IHEP, Beijing Large scatter shows the environmental effect!! Nov 9, 2011

69. KDUST workshop, IHEP, Beijing Nov 9, 2011

70. KDUST workshop, IHEP, Beijing Apparent environmental dependence!! Nov 9, 2011

71. KDUST workshop, IHEP, Beijing Nov 9, 2011

72. KDUST workshop, IHEP, Beijing No screening at all!! Nov 9, 2011

73. KDUST workshop, IHEP, Beijing Nov 9, 2011

74. KDUST workshop, IHEP, Beijing No screening! Nov 9, 2011

75. KDUST workshop, IHEP, Beijing Nov 9, 2011

76. KDUST workshop, IHEP, Beijing Maximum screening Core is better screened Nov 9, 2011

77. KDUST workshop, IHEP, Beijing Nov 9, 2011

78. KDUST workshop, IHEP, Beijing Screened purely by environment Nov 9, 2011

79. KDUST workshop, IHEP, Beijing Nov 9, 2011

80. KDUST workshop, IHEP, Beijing Screening on the edge shows environmental dependence! Nov 9, 2011

81. Observationally… KDUST workshop, IHEP, Beijing Lensing MassDynamical Mass Nov 9, 2011

82. Measure lensing and dynamical mass for each halo; Divide the sample using D; Compare! KDUST workshop, IHEP, Beijing Nov 9, 2011

83. Measure lensing and dynamical mass for each halo; Divide the sample using D; Compare! KDUST workshop, IHEP, Beijing Apply to KDUST data?! Nov 9, 2011

84. Summary and Outlook KDUST is powerful to constrain DE and MG by measuring SN, WL, BAO; KDUST is powerful to constrain MG by measuring CMN, lensing and dynamical mass of galaxies; KDUST can do more science, RSD, ISW, etc Nov 9, 2011 KDUST workshop, IHEP, Beijing