1. Systematic Errors in Weak Lensing Measurements Jun Zhang, Eiichiro Komatsu (The University of Texas at Austin) IHEP, Nov 8, 2011 arXiv: 1002.3614; 1002.3615; 0901.4781, Astro-ph/0612146.

2. Outline: Introduction of Weak Lensing Problems in Weak Lensing Measurement ◦ The Form of Cosmic Shear Estimator (general) ◦ The Reduced Shear (general) ◦ The Pixelation Effect (specific) ◦ The Photon Noise (specific) Summary

3. Introduction Credit: NASA / WMAP Science Team

4. Introduction Credit: NASA/WMAP

5. Introduction Credit: Wittman et al., (LSST team)

6. Introduction Image Credit: Hoekstra & Jain (2008) Credit: Clowe et al. (2006)

7. Introduction

8. Introduction y x y’ x’ Lensing

9. Introduction y x y’ x’ Lensing y x y’ x’ Lensing y x y’ x’ Lensing

10. Introduction

11. Introduction DES LSST WFIRST EUCLID HSC KDUST

12. Problems in Weak Lensing Measurements How to accurately measure the cosmic shear? The shear signal: a few percent V.S. Intrinsic variance of the galaxy ellipticity (shape noise): of order one Systematic errors are not tolerable!!!

13. 引力透镜所致形变观测所致图像模糊 光子噪音 有限像素 LensingPSF Pixelation Noise Image Credit: GREAT08 team

14. Problems in Weak Lensing Measurements

15. Credit: Huterer et al. 2006, MNRAS, 366, 101

16. Problems in Weak Lensing Measurements Credit: Huterer et al. 2006, MNRAS, 366, 101

17. Problems in Weak Lensing Measurements Sources of Systematic Errors: Corrections due to the Point Spread Function (PSF); Photon Noise; Pixelation Effect; High Order Terms in Shear/Convergence; Charge Transfer Inefficiency; PSF determination from Star Shapes; Source Selection Bias; Photometric Redshift Errors; Galaxy Intrinsic Alignment.

18. Problems in Weak Lensing Measurements Sources of Systematic Errors: Corrections due to the Point Spread Function (PSF); Photon Noise; Pixelation Effect; High Order Terms in Shear/Convergence; Charge Transfer Inefficiency; PSF determination from Star Shapes; Source Selection Bias; Photometric Redshift Errors; Galaxy Intrinsic Alignment.

19. Problems in Weak Lensing Measurements The Form of Cosmic Shear Estimator (general) The Reduced Shear (general) The Pixelation Effect (specific) The Photon Noise (specific)

20. The Form of Shear Estimator STEP I, STEP II, GREAT 08, GREAT 10 ?

21. The Form of Shear Estimator

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24. Warming Up Exercise The Form of Shear Estimator

25. Warming Up Exercise The Form of Shear Estimator

26. Are there ideal/conventional shear estimators existing in convenient forms? ? The Form of Shear Estimator

27. Coordinate Rotation: The Form of Shear Estimator

31. Indeed, we only need to consider spin-2 shear estimators because of the following: The Form of Shear Estimator

32. On spin-2 shear estimators: The Form of Shear Estimator

33. On spin-2 shear estimators: Scalar Pseudo-Scalar Spin-4 The Form of Shear Estimator

34. On spin-2 shear estimators: The Form of Shear Estimator

35. Consider a special type of galaxies: (, ) The Form of Shear Estimator

36. Consider a special type of galaxies: The Form of Shear Estimator

37. Consider a special type of galaxies: The Form of Shear Estimator

38. Consider a special type of galaxies: The Form of Shear Estimator

39. Consider a special type of galaxies: The Form of Shear Estimator

40. Consider a special type of galaxies: Bartelmann & Schneider 2001, Phys. Rept., 340, 291 The Form of Shear Estimator

41. In the Presence of PSF: ? ✗ The Form of Shear Estimator

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46. Ref: Astro-ph/0612146, arXiv: 0901.4781, arXiv: 1002.3614 The Form of Shear Estimator

47. Ref: Astro-ph/0612146, arXiv: 0901.4781, arXiv: 1002.3614 The Form of Shear Estimator

48.  Correct for the Point Spread Function;  No Assumptions on the Morphologies of the Galaxies or the PSF;  Exact & Simple Math;  Well Defined Treatment of Background Noise;  Accurate to the 2nd Order in Shear/Convergence;  Immune to Misidentification of Sources (faint/small galaxies, stars)  < 10 -2 seconds/Galaxy  S / N per galaxy Increased. The Form of Shear Estimator

49. The Reduced Shear

50. If one plans to calibrate the multiplicative factor “a+b κ ”, one should pay attention to its dependence on “ κ ”, which, though, is not known a priori in observations.

51. The Reduced Shear Theorem:,

52. The Pixelation Effect (specific) Moffat PSFGaussian PSF FWHM of both PSF = 12

53. The Pixelation Effect (specific) FWHM (PSF) = 12

54. The Photon Noise (specific)

57. In fact :

58. A Fun Thing to Share

60. Summary The Form of Shear Estimator (general) The Reduced Shear (general) The Pixelation Effect (specific) The Photon Noise (specific)