1. Cosmic shear Henk Hoekstra Department of Physics and Astronomy University of Victoria Current status and prospects

2. Large scale structure  CDM OCDM Spot the difference… Different values for cosmological parameters lead to a different distribution of (dark) matter and a different evolution. z=3 z=1 z=0 The clustering properties of matter as a function of scale and redshift can be used as a tool to measure the cosmology!

3. But how to measure it? Always look on at the bright side…

4. The light distribution can tell us some things about the dark side. How to measure it?

5. Simple: use the Force (of gravity) !

6. Gravitational lensing The angle of deflection is a direct measure of mass! As predicted in the early 20 th century, rays of light are deflected by massive objects in the universe.

7. Gravitational lensing The large scale mass distribution causes a distortion in the shapes of background galaxies. This can lead to spectacular lensing examples…

8. Gravitational lensing

9. A measurement of the ellipticity of a galaxy provides an unbiased but noisy measurement of the shear Weak gravitational lensing

10. Cosmic shear is the lensing of distant galaxies by the overall distribution of matter in the universe: it is the most “common” lensing phenomenon. Cosmic shear

11. In the absence of noise we would be able to map the matter distribution in the universe (even “dark” clusters). We can see dark matter! Courtesy B. Jain

12. We can see dark matter! Where expected: in the “Bullet Cluster” Clowe et al. (2006)

13. We can see dark matter! Or where we don’t expect it! Dark matter/X-ray peak, without galaxies?! (Mahdavi et al. 2007) Abell 520

14. Why weak lensing?  Weak lensing provides a direct measurement of the projected (dark) matter distribution, which can be used for cosmological parameter estimation.  The physics is well understood: General Relativity.  The applications are numerous.  statistical properties of the matter (cosmological parameters).  relation between galaxies and dark matter (galaxy biasing).  properties of dark matter halos (test of CDM and law of gravity).

15. Why cosmic shear? Current observational constraints on the properties of dark energy are still crude. Progress depends critically on how well various cosmological probes can be understood: Do we understand what we are doing? DETF comments: “The WL technique is also an emerging technique. Its eventual accuracy will also be limited by systematic errors that are difficult to predict. If the systematic errors are at or below the level asserted by the proponents, it is likely to be the most powerful individual Stage-IV technique and also the most powerful component in a multi-technique program.”

16. Why cosmic shear? Although weak lensing has many interesting applications, cosmic shear is the most demanding and has been driving most “technological” advances in the past decade.  How do we measure this signal?  How do we interpret this signal?

17. Averaged shape: The underlying assumption is that the position angles are random in the absence of lensing. At some level intrinsic alignments will complicate things (can be dealt with using photometric redshifts?). no lensinglensing How to measure the signal?

18. What do we need? The weak lensing signal is small:  We need to measure the shapes of many galaxies.  We need to remove systematic signals at a high level of accuracy. Only recently we have been able to overcome both obstacles, although we still need various improvements to deal with the next generation of surveys

19.  1 square degree field of view  ~350 megapixels Megacam: Build a big camera…

20. Put it on a good telescope… Such as the CFHT or VST, LSST, SNAP, etc

21. … and take a lot of data! That’s when the “fun” starts… CFHTLS RCS2 KIDS

22. Dealing with systematics The induced lensing signal is small and observational distortions are typically larger than the lensing signal. The observed shapes of galaxies need to be corrected for  PSF anisotropyadditive  Circularisation by seeingmultiplicative  Camera shearadditive Various correction techniques have been developed and tested extensively. In particular the Kaiser et al. (1995) approach is widely used. This method works fine for current data sets, but we need improved methods for upcoming large surveys: shapelets?

23. Dealing with systematics: the PSF The first step in the correction for the PSF is to identify a suitable sample of stars and quantify their shape parameters The smaller the PSF the better the result!

24. Dealing with systematics: improvements There are two concerns with PSF correction:  Correct PSF model?  Correct correction? Jarvis & Jain (2004) have shown how to get a (near?) “perfect” PSF model. Much work is devoted to improve the correction itself (shapelets, lensreg, etc.)

25. Dealing with systematics: the PSF Weak lensing is rather unique in the sense that we can study (PSF-related) systematics very well. Several diagnostic tools can be used. However, knowing systematics are present doesn’t mean we know how to deal with them… E-mode (curl-free) B-mode (curl)

26. Dealing with systematics: STEP The Shear TEsting Programme (Heymans et al., 2006; Massey et al., 2007) provides a snapshot of the current accuracy that currently can be reached (~1-2%) using simulated data. Correction for PSF size PSF anisotropy

27. What does the signal mean? The cosmic shear signal is mainly a measurement of the variance in the density fluctuations. Little bit of matter, large fluctuations Lot of matter, small fluctuations Same “lensing” signal To first order lensing measures a combination of the amount of matter  m and the normalisation of the power spectrum   

28. What does the signal mean? The statistical properties of the (dark) matter distribution depend on the cosmology. The power spectrum (the variance as a function of scale) contains a wealth of information.

29. The lensing signal depends on the (non-linear) matter power spectrum; this gives extra sensitivity to the parameter estimation and can break degeneracies We need improved estimates for the power spectrum in the non-linear regime (now use Peacock & Dodds and Smith et al. (2003) recipes). The lensing signal depends on the redshift distribution of the (faint) source galaxies; this allows us to measure how structure grows in the universe We need better estimates for the source redshift distribution, e.g. from photometric redshift surveys. What does the signal mean?

30. Results: a decade ago… This page was left blank intentionally…

31. What have we done so far? Since the first detections reported in spring 2000, many cosmic shear measurements have been published. Status in 2001 Courtesy Y. Mellier

32. Comparison of results Benjamin et al. (2007) compared and carefully combined the results for 4 surveys. The total area is about 100 square degrees.

33. The Canada-France-Hawaii Telescope Legacy Survey is a five year project, with three major components. The Wide Survey’s focus is weak lensing. ~140 square degrees 4 fields 5 filters (u,g,r,i,z’) i<24.5 CFHT Legacy Survey

34. CFHTLS: first results ~20 square degree used in Hoekstra et al. (2006)

35. CFHTLS: first results Hoekstra et al. (2006)

36. We think the observed lensing signal is fairly accurate. But how about the interpretation. Do we know? Were getting there! The early results were based on the HDF photometric redshift distribution. The redshift distribution obtained by Ilbert et al. (2006) based on CFHTLS Deep data suggests a higher mean redshift! Comparison of results

37. CFHTLS-Deep redshifts Knowledge of the source redshifts is currently the dominant limiting factor for cosmic shear surveys. Redshift information will allow for a proper interpretation of the signal, improve accuracy on w and help with intrinsic alignments. A lot of work is needed to improve the current situation!

38. CFHTLS: current status Since the publication of the first results a number of things have improved: Reduced systematics Larger area observed (we can probe larger scales) Improve estimates of cosmological parameters using photo-z’s The latest results, based on the analysis of 57 sq. deg. spread over 3 fields have recently been published in Fu et al. (2008)

39. CFHTLS: the measurement Measurements out to 4 degree scales!

40. Cosmology is “scale independent”: non-linear corrections sufficient so far. CFHTLS: recent results

41. Results agree well with WMAP3 (and WMAP5…)

42. What to do next? Currently ~35 sq. deg. of data have the full ugriz coverage and photometric redshift are being determined. With photometric redshift information for the sources we can study the growth of structure, which significantly improves the sensitivity to cosmological parameters.

43. CFHTLS: first results Wide only Wide+Deep (cheap tomography)

44. Details, details, details… The devil is in the details. The accuracy of first cosmic shear surveys is mostly limited by statistical noise (small areas). For the next generation many subtle effects need to be taken into account. We are discovering these (or correcting these) as we go along…

45. Intrinsic alignments Intrinsic alignments complicate the cosmological interpretation of the lensing signal. CFHTLS and other surveys will allow us to measure the amplitude of the intrinsic alignments. Dealing with intrinsic alignments will benefit greatly from these photometric redshift data and we can eliminate the “classical” alignments. However, Hirata et al. and Heymans et al. have pointed out more subtle effects, namely the alignment between shear (LSS) and intrinsic alignments.

46. Further ahead… The study of dark energy is an important application of cosmic shear. The CFHTLS will provide the first constraints from a ground based survey. But a useful measurement of the dark energy parameters requires much better precision. The several hundred million dollar question is: Can we reach the 1% precision from the ground or should we go to space?

47. Advantages of space SuperNova Acceleration Probe  much smaller PSF  optical + NIR bands  higher source density  higher source redshift  better photo-z’s  large reduction in systematics

48. The CFHTLS lensing project is progressing well and is producing competitive cosmological results, but it is work in progress. To achieve the full potential of the survey a number of remaining hurdles need to be jumped over… …but no show-stopper has been found! Conclusions