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High Resolution Observations of the CMB with the CBI Interferometer

High Resolution Observations of the CMB with the CBI Interferometer. Carlo Contaldi CITA. XVIII th IAP Colloquium - July 1 2002. T. Readhead (Caltech) T. Pearson (Caltech) S. Myers (NRAO) B. Mason (Caltech/NRAO) J. Sievers (Caltech) J. Cartwright (Caltech) P. Udompraesert (Caltech)

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High Resolution Observations of the CMB with the CBI Interferometer

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  1. High Resolution Observations of the CMB with the CBI Interferometer Carlo Contaldi CITA XVIIIth IAP Colloquium - July 1 2002

  2. T. Readhead (Caltech) • T. Pearson (Caltech) • S. Myers (NRAO) • B. Mason (Caltech/NRAO) • J. Sievers (Caltech) • J. Cartwright (Caltech) • P. Udompraesert (Caltech) • M. Shepherd (Caltech) • Farmer (Caltech) • S. Padin (Caltech) J. R. Bond (CITA) C. Contaldi (CITA) D. Pogosyan (U of Alberta) U.-L. Pen (CITA) M. Ruetalo (CITA/UofT) P. Zhang (CITA/UofT) J. Wadsley (McMaster) S. Prunet (IAP)

  3. The Cosmic Background Imager > 5000m Atacama Plateau Chile • 13 elements • 0.90 m dishes • 45’ FWHM • 78 baselines • 10 frequency channels 26-36 GHz • l~200

  4. mosaic pointings 10-channel single pointing uv-coverage 26-36 GHz single pointing uv-coverage

  5. CBI Power spectrum extraction • Visibilities ‘gridded’ in uv plane [Myers at al. 2002]. • Quadratic estimator solves for the ML band powers • 6x7 field mosaic; ~10 hrs. 16 processor GS320 cluster @ CITA • Foreground templates projected out using known positions

  6. 3 6x7 field mosaics • ~ 145’x165’ each • ~ 40 sq. deg. • [Pearson et al. 2002] “Silk” damping CBI Mosaic Power Spectrum

  7. Mosaic Window Functions

  8. Weak Weak + Flat +LSS Flat + LSS + HST-h [Sievers et al. 2002] CBI+DMR

  9. [Mason et al. 2002] CBI Deep Field Power Spectrum BOOMERanG 2001

  10. CBI High-l Excess Significant power above l=2000. 3.5 inconsistent with zero and 3.1 inconsistent with best-fit model. Amplitude ~ 4.5 higher than expected signal from residual low-flux sources Estimate includes 50% error in residual source flux. Secondary Anisotropies from Sunyaev-Zeldovich Effect?

  11. Raw map

  12. Total Signal

  13. CMB + ?

  14. OVRO & NVSS Source residuals

  15. SZE Angular Power Spectrum [Bond et al. 2002] • Smooth Particle Hydrodynamics (5123) [Wadsley et al. 2002] • Moving Mesh Hydrodynamics (5123) [Pen 1998] • 143 Mpc 8=1.0 • 200 Mpc 8=1.0 • 200 Mpc 8=0.9 • 400 Mpc 8=0.9 Dawson et al. 2002

  16. Simulation of Deep Observations by the CBI Input SZ map Reconstructed Signal

  17. Bandpower Estimation with a SZ Foreground Single Deep Field (08h) simulated observation CBI Pipeline recovers input SZE signal at observed amplitudes Non-Gaussian scatter from the SZ signal is significant in the high-l band given the small areas observed

  18. LSS parameters from CMB and other Cosmological Surveys Priors Flat HST-h

  19. Summary • The CBI observations l<2000 give consistent parameters with those of previous experiments on larger angular scales • Measurement of the damping tail at l>1000 • 6’ scales probing ~1014MO seeds of clusters • High-l excess; Simulations show the Sunyaev-Zeldovich Effect fits the observed power for 8~1.0. This is in the high-end of the range allowed by CMB and LSS surveys • SZE: high-accuracy determination of 8. Break 8-ΩM degeneracy  ΩΛ • Follow-up on excess • Extended mosaic data ~ 80 sq. deg. • Improved hydrodynamical simulations

  20. Polarization Observations 2002/3 • Optimally configured for resolution of peaks • Polarization upgrade nearly complete • Calibration runs in August

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