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Cosmology with the South Pole Telescope Zak Staniszewski (Case)

Cosmology with the South Pole Telescope Zak Staniszewski (Case). University of Chicago: John Carlstrom (P.I) Steve Padin (Proj. Manager, yr1 winter) Stephan Meyer Clem Pryke Tom Crawford Jeff McMahon Clarence Chang Kathryn Miknaitis Joaquin Vieira Ryan Keisler Lindsey Bleem

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Cosmology with the South Pole Telescope Zak Staniszewski (Case)

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  1. Cosmology with the South Pole TelescopeZak Staniszewski(Case)

  2. University of Chicago: John Carlstrom (P.I) Steve Padin (Proj. Manager, yr1 winter) Stephan Meyer Clem Pryke Tom Crawford Jeff McMahon Clarence Chang Kathryn Miknaitis Joaquin Vieira Ryan Keisler Lindsey Bleem Abigail Crites Year 2 winterovers: Keith Vanderlinde Dana Hrubes University of Chicago: John Carlstrom (P.I) Steve Padin (Proj. Manager, yr1 winter) Stephan Meyer Clem Pryke Tom Crawford Jeff McMahon Clarence Chang Kathryn Miknaitis Joaquin Vieira Ryan Keisler Lindsey Bleem Abigail Crites Year 2 winterovers: Keith Vanderlinde Dana Hrubes Berkeley: William Holzapfel Adrian Lee Helmuth Spieler Sherry Cho Bradford Benson Huan Tran Martin Lueker Jared Mehl Tom Plagge Dan Schwan Erik Shirokoff Berkeley: William Holzapfel Adrian Lee Helmuth Spieler Sherry Cho Bradford Benson Huan Tran Martin Lueker Jared Mehl Tom Plagge Dan Schwan Erik Shirokoff Case: John Ruhl Tom Montroy Zak Staniszewski (Me, yr1 Winterover) Wenyang Lu UIUC: Joe Mohr McGill: Matt Dobbs Gil Holder Trevor Lanting UC Davis: Lloyd Knox Jason Dick Harvard Smithsonian: Antony Stark Colorado: Nils Halverson JPL: Erik Leitch

  3. What is SPT • 10 meter telescope • At South Pole • CMB telescope • 90,150, 220 GHz • WMAP(20-90) • 1 arcminute resolution

  4. SPT optics features • 10 meter off axis Gregorian design • 1 meter cold secondary mirror • Paneled primary mirror • 20-30 micron primary, 40-50 micron secondary (current) • Warm receiver cabin

  5. Science with SPT • Dark Energy • Cluster survey • High ell power spectrum • Cluster science • Tracing Baryons • Point sources • Learn astronomy • Help Planck • Unresolved sources may bias non-Gaussianity result

  6. SPT Primary goalDN/DZ with clusters G. Holder in Ruhl et al 2004

  7. The SunyaevZel’dovich Effect

  8. Measured SZ spectrumof A2163 Design considerations focal plane

  9. SPT observing regions Observed SPT regions in Magenta First year results only from green BCS 5Hr field. *BCS optical data in green First results are only from one small green region

  10. We find clusters! Known cluster from REFLEX survey

  11. First Galaxy clusters discovered with the SZ effect!!! http://arxiv.org/abs/0810.1578 • - First Clusters ever discovered with the SZE • First SPT results paper out just 2 months ago

  12. Three new discoveries • First clusters discovered with an SZ survey!!! • All confirmed by optical follow up • Two near redshift 0.8

  13. Optical confirmation from BCS

  14. You should be excited • We want Dn/Dz • Remember, these are only our slam dunk cluster candidates • Only from 40 square degrees. We currently have 200 square degrees • Second 100 sq degree field is deeper • Better processing and cluster finding • Map processing studies • Utilize 90, 220 GHz for a multi frequency filter • In two years we should have both 90 and 150 to equal the same sensitivity in ~1000 square degrees.

  15. SPT ScienceHigh el CMB Projected SPT ACBAR 2008 Reichardt et al 2008 W. Hu from Ruhl et al 2004

  16. More on power spectrum • Could constrain ns • Lensing, v in the future • Need good calibration Hu (2001)

  17. Absolute calibration MAT5a • HII regions • RCW 38, MAT5a • Integrate RCW38 flux and compare to ACBAR or Boomerang • WMAP • Dedicate ~20 hours to look at 500 sq.

  18. SZ image of Bullet Cluster • SZ emission radial profile • r500 = 1.6 Mpc; q500 = 5.4’; q200 = 8.6’ • Significant signal seen at q > 12’ radius • Model shown is b=.87, qc=1.8 (very well constrained) • z = .297 • 7 hours of observation • ~ 20 mK RMS per 60” pixel

  19. Targeted program • Where are the baryons • How does SZ flux scale with mass • 25 massive clusters observed • Some relaxed clusters

  20. SED of SMG Credit: Blain, Smail, Ivison, Kneib, & Frayer 2002 SPT SCUBA

  21. Point sources

  22. Conclusion • Expect variety of result papers soon. • dn/dz from cluster survey on its way • ACT,APEX,Planckas well • Planck’s beam a bit too big • High ell power spectrum • Ns, neutrinos, lensing • Cluster science, missing baryons • Emerging point source field • Also help Planck • Polarization receiver in 2-3 years • High ell polarization

  23. Thank You

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