1. BAO,ISW+SZ from AA  +SDSS R.M. Bielby, U. Sawangwit, T. Shanks, Durham University + 2SLAQ + AAOmega teams

2. Summary SDSS, 2SLAQ + AAOmega LRG z surveys AAOmega photo-z LRG small scale clustering results AAOmega photo-z LRG BAO results AAOmega photo-z LRG ISW results AAOmega photo-z LRG + ACO SZ results Sawangwit et al 2007, Bielby et al 2007

3. 1977 Precision Cosmology!  total =  m =0.1 n=0 Isocurvature perturbations Galaxy clustering +CMB  “Cosmologists - frequently in error but never in doubt!”

4. 2SLAQ LRG Wedge Plot

5. AAOmega AAOmega is the new spectrograph for AAT 2dF (Sharp et al 2006) 392 fibres Blue and Red Arm AAOmega pilot in March 2006 to survey riz selected LRGs to z~0.9 (Ross et al 2007)

6. 1.5 million SDSS LRGs SDSS, 2SLAQ LRGs use gri colour-cuts AAOmega LRGs use riz colour-cuts Simply use w(θ) on colour-cut LRGs rather than photo-z w(θ) for three z bins: 100000 z~0.35 LRGs 600000 z~0.55 LRGs 800000 z~0.7 LRGs

7. Small-scale LRG clustering SDSS z=0.35 2SLAQ z=0.55 AA  z=0.7

8. Large-scale LRG clustering Are these BAO peaks or just some systematics?

9. This is the scale where we expect to see BAO peak

10. Combined w(  ) results 3-D SDSS correlation function,  (s) from 45000 LRGs (Eisenstein et al 2005) 2-D correlation function from 1.5 million DR5 LRGs (this work) linear no wiggle SDSS  (s) fit linear no wiggle SDSS  (s) fit

11. “Filtered” w(  ) - final result? Linear theory SDSS  (s) fit But constant offset at large scales Systematics? Subtract 0.0015 from w(  ) to “filter” Now agrees with linear theory But poorer agreement with SDSS  (s) of Eisenstein et al

12. 2dFGRS BAO? So photo-z route to BAO is hard… But so is spectro-z route! 2dFGRS

13. linear no wiggle SDSS  (s) fit linear no wiggle SDSS  (s) fit LRG-WMAP ISW

14. linear no wiggle SDSS  (s) fit linear no wiggle SDSS  (s) fit LRG-WMAP ISW

15. LRG-WMAP Ka-band ISW?

16. LRG-WMAP K-band ISW?

17. LRG-WMAP Q-band ISW?

18. LRG-WMAP V-band ISW?

19. LRG-WMAP W-band ISW?

20. AA  now using SDSS Uber-calibration of Padmanabhan et al

21. LRG-WMAP ILC ISW? ILC SDSS 2SLAQ AA 

22. AA  LRG clusters +WMAP W  SZ? 10x the negative amplitude seen in ISW- LRG plot Possible SZ detection at z~0.7?

23. Abell cluster + WMAP  SZ WMAP SZ at 94GHz Bielby + Shanks 2007 astro-ph/ 0703407 Z=0.02 Z~0.1 Z~0.2Z~0.4 172 Abell Clusters 235 Abell Clusters38 OVRO/BIMA Clusters Coma cluster  (arcmin)  TT SZ effect decreases with z?

24. VST ATLAS VST ATLAS, ESO “core” project, ugriz (+VISTA VHS YJK)  “Southern Super Sloan”, 2009-11 16k x 16k OmegaCam  1 deg 2 field-of-view 2.6-m VLT Survey Telescope 1500deg 2 3000deg 2

25. Conclusions SDSS colour cut LRGs at z~0.35 (SDSS), z~0.55 (2SLAQ) and z~0.7 (AAOmega) Small-scale (~1Mpc) feature confirmed in w(  ) - important for HOD models and LRG evolution w(  ) of 1.5x10 6 SDSS LRGs close to detecting BAO Possible ISW detections at z~0.35 and z~0.55 but only anti-correlation detected at z~0.7 SZ detection at small-scales at z~0.7? More LRGs to come from VST ATLAS