1. QUIET Q/U Imaging ExperimenT

2. QUIET Project Miami Physics Conference 2009 December 16 Raul Monsalve for the QUIET Collaboration University of Miami QUIET Project Miami Physics Conference 2009 December 16 Raul Monsalve for the QUIET Collaboration University of Miami

3. What is QUIET ? Radiotelescope that measures intensity and polarization of the CMB Located in Chile Main science objective is to improve characterization of E- mode polarization and detect the difficult B-mode polarization Two phases are planned. Phase-I is ongoing, started in August 2008. Phase II is planned to start in 2012, in a larger scale, improving the techniques learned during phase-I

4. CALTECH STANFORD FERMILAB U. CHICAGO COLUMBIA U. MIAMI JPL SITE MANCHESTER OSLO MPI-BONN KEK PRINCETON OXFORD QUIET Collaboration

5. Science Goals We can measure the polarisation of the CMB the same way as for light The Stokes parameters quantify the polarization properties of a light ray ▫ I = no filter at all ▫ Q = linear polarizer at 0 and 90° ▫ U = linear polarizer at -45 and 45 ° ▫ V = circular polarizer I is just the temperature Q and U combine to form E- and B-modes No known physical process can generate V- polarized CMB radiation

6. Status and Forecast on the EE and BB characterization Science Goals

7. Site and Instrumentation

8. Site Chajnantor Scientific Reserve in Chile at 5080 m above sea level Among the best places for mm and submm astronomy Access to CBI infrastructure Accessible at all times 1 hour drive from San Pedro de Atacama Good sky coverage For outside work bottled oxygen systems are used Oxygen concentration in control room is increased ~27%

9. Q BandW Band Frequency40 GHz90 GHz N° of HEMT Detectors17/284/6 Resolution28 arcmin (FWHM)12 arcmin (FWHM) Telescope TypeCrossed Dragone Module Sensitivity300 μK s½550 μK s½ Array Sensitivity70 μK s½60 μK s½ Observation PeriodOct 2008 – June 2009June 2009 – Mid 2010 ? Phase-I Summary

10. Mount Inherited from CBI Alt-Az axes Rotation about optical axis (boresight axis) Elevation range limited to 43 deg < el < 87 deg

11. Optics Crossed Dragone design 1.4 m primary and secondary mirrors FWHM: 28 (Q) and 12 (W) arcmin

12. Horn Arrays Conical corrugated feed horn arrays Excellent beam symmetry Low sidelobe response Low cross-polarization Broad frequency band Typical FWHM of ~7 deg Built by UM

13. OMTs Splits incoming radiation into L and R 20% bandwidth Low loss High isolation on the output ports to avoid temperature-to-polarization leakage

14. Detector Modules Heart of the receiver Polarimeter on a chip Automated assembly and operation Measuring of Q and U simultaneously in each pixel Operate at ~20K

15. Module/OMTs Seven element demonstration array

16. Receiver

17. Calibration and Preliminary Data

18. Polarization MOON Once/7 days, Relative Gains, Angles NOISE SOURCE Once/1.5 hours, Relative Gains, Angles TAU A Once/2 days, Absolute Gains, Angles, Beams SKY-DIP Once/1.5 hours, Relative Gains, Stability JUPITER Once/7 days, ∆T Gains, Beam Gain Stability Temperature Calibration Strategy + supplemental measurements

19. Beam Shape using Jupiter Calibration

20. Tau A Gains Moon Polarization Fits Calibration

21. CMB Analysis

22. Observation Regions 4x(15x15)=900 [deg²] Patch Centers Low foreground regions in coordination with ABS, Polarbear (Multifrequency measurements for galactic foreground removal) Distribution to allow continuous scanning

23. Average 68.1% Downtime mainly due to: -Mechanical Problems -Generator problems -Bad weather Telescope Operation during Q-Band Season

24. Phase-I, EE Power-spectra Forecasts Q W

25. Patch 2a Results (PRELIMINARY)

26. Other Interesting Observations Galactic Center Polarization Maps with Q-Band Data (PRELIMINARY)

27. Other Interesting Observations Galactic Center Temperature Map with Q-Band Data (PRELIMINARY) QUIET WMAP

28. Phase-II

29. Phase-II Summary Ka BandQ BandW Band Frequency32 GHz40 GHz90 GHz N° of modules (P/T)16/255/61389/108 Beamsize (FWHM)28 arcmin20 arcmin8.5 arcmin Module Sensitivity165 μK s½178 μK s½364 μK s½ Beginning operations2013 ? N° of telescopes3 Telescope typeCrossed Dragone

30. Phase-II Power-spectra Forecasts Current Performance Likely Improvement (noise, duty cycle, 1/f)

31. Appendix Alternate technique to identify gravitational lensing effects (Zaldarriaga(1999), Hu(2002)) Lens reconstruction: Lensing Deflection Field calculation from cross-correlation of E- and B-modes Stronger constraints on cosmological parameters than using B-mode power spectrum By measuring shape and amplitude of the Deflection power spectrum QUIET Phase-II can place constraints on parameters such as: Neutrino mass (Maltoni, 2004) Dark energy density (Stompor, 1999) Spatial curvature (Stompor, 1999)

32. Summary QUIET Science: Experiment addressing fundamental questions in physics Taking the CMB polarization knowledge to new levels QUIET Status: Largest HEMT-based focal plane array ever deployed, using state of the art MMIC packaging techniques Phase-I observing and proposing Phase-II to start in 2012/2013

34. Systematic Errors o Overall signal size o Overall gain calibration o Beamsize calibration o Pointing error o Fake signal source o Instrumental I->Q/U : caused by OMT, 1% for Q-band. Negligible. o Gain fluctuations : up to 20% negligible for phase I. o E->B mixing source o Polarization angle : calibration better than 5% for phase I. o Optics cross polarization : only affects by order of ∆ө² o Q/U gain mismatch : relative gain between Q and U stable. o Patch geometry : finite patch, patch irregularity, pixelization

35. Systematic Errors E->B, Patch geometry