understanding the cosmic acceleration using kdust n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
Understanding the Cosmic Acceleration using KDUST PowerPoint Presentation
Download Presentation
Understanding the Cosmic Acceleration using KDUST

play fullscreen
1 / 84

Understanding the Cosmic Acceleration using KDUST

92 Views Download Presentation
Download Presentation

Understanding the Cosmic Acceleration using KDUST

- - - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript

  1. Understanding the Cosmic Acceleration using KDUST 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)

  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) KDUST workshop, IHEP, Beijing

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

  4. Cosmic Acceleration MG DE KDUST workshop, IHEP, Beijing

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

  6. KDUST is useful for DE KDUST workshop, IHEP, Beijing

  7. KDUST Site Performance credit: Hu Zhan LSST 15000 sq. deg. Ugrizy GBZ, H.Zhan, L. Wang, Z. Fan, X.Zhang, 1005.3810, PASP 11 15000 sq. deg.: n(z) ~ z2exp(-z/0.5) Photo-z rms: sz=0.04(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.003 Residual shear power: 6×10-10 KDUST workshop, IHEP, Beijing

  8. KDUST—LSST Synergy credit: Hu Zhan KDUST JH + LSST ugrizy 5000 sq. deg.: n(z) ~ z2exp(-z/0.6) Photo-z rms: sz=0.03(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.002 Residual shear power: 4×10-10 15000 sq. deg.: n(z) ~ z2exp(-z/0.5) Photo-z rms: sz=0.04(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.003 Residual shear power: 6×10-10 KDUST workshop, IHEP, Beijing

  9. KDUST—LSST Synergy credit: Hu Zhan KDUST JH + LSST ugrizy 10000 sq. deg.: n(z) ~ z2exp(-z/0.6) Photo-z rms: sz=0.03(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.002 Residual shear power: 4×10-10 10000 sq. deg.: n(z) ~ z2exp(-z/0.5) Photo-z rms: sz=0.04(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.003 Residual shear power: 6×10-10 KDUST workshop, IHEP, Beijing

  10. KDUST—LSST Synergy credit: Hu Zhan KDUST JH + LSST ugrizy 5000 sq. deg.: n(z) ~ z2exp(-z/0.6) Photo-z rms: sz=0.03(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.002 Residual shear power: 4×10-10 15000 sq. deg.: n(z) ~ z2exp(-z/0.5) Photo-z rms: sz=0.04(1+z) Photo-z bias prior: sP(dz)=0.2sz Shear calibration error: ±0.003 Residual shear power: 6×10-10 SNe:(z < 1.5) KDUST workshop, IHEP, Beijing

  11. 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! KDUST workshop, IHEP, Beijing

  12. KDUST is useful for MG KDUST workshop, IHEP, Beijing

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

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

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

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

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

  18. CMN data KDUST workshop, IHEP, Beijing

  19. Cosmological applications KDUST workshop, IHEP, Beijing

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

  21. Power of CMN • B0<0.4 (95% CL, CMB+SN) • B0<5x10-5(95% CL, CMB+SN+CMN) 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?? KDUST workshop, IHEP, Beijing

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

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

  25. In GR KDUST workshop, IHEP, Beijing

  26. In f(R) lC KDUST workshop, IHEP, Beijing

  27. In very dense regions lC KDUST workshop, IHEP, Beijing

  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 KDUST workshop, IHEP, Beijing

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

  34. Get some sense… KDUST workshop, IHEP, Beijing

  35. GR KDUST workshop, IHEP, Beijing

  36. f(R) KDUST workshop, IHEP, Beijing

  37. Structure formation in GR KDUST workshop, IHEP, Beijing

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

  39. Dynamical Mass KDUST workshop, IHEP, Beijing

  40. Dynamical Mass KDUST workshop, IHEP, Beijing

  41. Dynamical Mass Spherical symmetry KDUST workshop, IHEP, Beijing

  42. Lensing Mass KDUST workshop, IHEP, Beijing

  43. Lensing Mass KDUST workshop, IHEP, Beijing

  44. Lensing Mass Spherical symmetry KDUST workshop, IHEP, Beijing

  45. Mass Difference KDUST workshop, IHEP, Beijing

  46. KDUST workshop, IHEP, Beijing

  47. In underdense environment KDUST workshop, IHEP, Beijing

  48. In underdense environment KDUST workshop, IHEP, Beijing

  49. KDUST workshop, IHEP, Beijing

  50. In dense environment KDUST workshop, IHEP, Beijing