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

• AAOmega photo-z LRG + ACO SZ results

• Sawangwit et al 2007, Bielby et al 2007

1977 Precision Cosmology!

total= m=0.1

n=0

Isocurvature perturbations

Galaxy clustering +CMB

“Cosmologists - frequently in error but never in doubt!”

2SLAQ LRG Wedge Plot

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)

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

Small-scale LRG clustering

SDSSz=0.35

2SLAQz=0.55

AAz=0.7

Large-scale LRG clustering

Are these BAO peaks or just some systematics?

This is the scale where we expect to see BAO peak

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 wiggleSDSS (s) fit

linear no wiggleSDSS (s) fit

“Filtered” w() - final result?

Linear theorySDSS (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

2dFGRS BAO?

• So photo-z route to BAO is hard…

• But so is spectro-z route!

2dFGRS

linear no wiggleSDSS (s) fit

linear no wiggleSDSS (s) fit

LRG-WMAP ISW

linear no wiggleSDSS (s) fit

linear no wiggleSDSS (s) fit

LRG-WMAP ISW

LRG-WMAP Ka-band ISW?

LRG-WMAP K-band ISW?

LRG-WMAP Q-band ISW?

LRG-WMAP V-band ISW?

LRG-WMAP W-band ISW?

LRG-WMAP W-band ISW?

AA now using SDSS Uber-calibration of Padmanabhan et al

LRG-WMAP ILC ISW?

ILCSDSS 2SLAQ AA

AA LRG clusters +WMAP WSZ?

• 10x the negative amplitude seen in ISW-LRG plot

• Possible SZ detection at z~0.7?

Abell cluster + WMAP SZ

WMAP SZat 94GHz

Bielby + Shanks 2007astro-ph/ 0703407

Z=0.02 Z~0.1

Z~0.2 Z~0.4

172 Abell Clusters

235 Abell Clusters 38 OVRO/BIMAClusters

Coma cluster

(arcmin)

T

SZ effect decreases with z?

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

1500deg2

3000deg2

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