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BAO,ISW+SZ from AA +SDSS

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

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BAO,ISW+SZ from AA +SDSS

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  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! Galaxy clustering +CMB  total= m=0.1 n=0 Isocurvature perturbations “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. linear no wiggle linear no wiggle SDSS (s) fit SDSS (s) fit 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)

  11. Linear theory SDSS (s) fit “Filtered” w() - final result? • 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 linear no wiggle SDSS (s) fit SDSS (s) fit LRG-WMAP ISW

  14. linear no wiggle linear no wiggle SDSS (s) fit 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. LRG-WMAP W-band ISW? AA now using SDSS Uber-calibration of Padmanabhan et al

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

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

  23. Z~0.1 Z=0.02 Coma cluster 172 Abell Clusters (arcmin) Z~0.2 Z~0.4 235 Abell Clusters 38 OVRO/BIMA Clusters Abell cluster + WMAP  SZ T WMAP SZ at 94GHz SZ effect decreases with z? Bielby + Shanks 2007 astro-ph/ 0703407

  24. 1500deg2 3000deg2 VST ATLAS VST ATLAS, ESO “core” project, ugriz (+VISTA VHS YJK)  “Southern Super Sloan”, 2009-11 16k x 16k OmegaCam  1 deg2 field-of-view 2.6-m VLT Survey Telescope

  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 1.5x106 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

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