The QUIET Experiment. Bruce Winstein The University of Chicago Inflation Probe Systematics Workshop Annapolis, MD July 28-30

Transcription

1 The QUIET Experiment Bruce Winstein The University of Chicago Inflation Probe Systematics Workshop Annapolis, MD July 28-30

2 Chicago (KICP) Collaboratoration ( Manchester Oxford Oslo MPIfR-Bonn Amber Charles Kris Michele Osamu Suzanne Stanford (KIPAC) Caltech JPL KEK Columbia Princeton Miami Atacama Observational Site Chile (CBI site) 5 countries, 12 institutes, ~30 people

3 Outline Introduction Detectors Instrument/Observing/Status Systematic Studies Forecasts Conclusions

4 Caldwell, Kamionkowski, Wadley, astro-ph/

5 Simulated sky with T/S= deg by 10 deg field

6 Simulated sky with T/S= deg by 10 deg field

7 Simulated sky with T/S=0.2 B-modes only 50 Times smaller anisotropy 20 times smaller still for r=0.01

8 Other obviously impossible experiments strain measurements from G. Waves Measuring difference between particle and anti-particle branching ratios to 10-7 Measuring a change/year in m e m p

9 Experiment Details: QUIET Phase I Angular resolution Q:28/W:12 Arcminutes Frequency Coverage 44/90 GHz Sky Coverage 4x400 Square Degrees Multipole Coverage ~ / Polarization Modulation? Phase switching PA sky rotation Dec angle rotation Rapid scanning Types of Detectors MMIC based - Location Atacama Desert Ground Instrument NEQ 70/60 (from lab measurements) - µk s 1/2 Expected limit on r ~0.15 (?) (no foregrounds) Status Phase I Funded (Funded/Proposed/Future)

10 Receiver/Telescope Receivers Q Integration: Columbia W Integration: Chicago Platelet Arrays Miami OMTs Princeton Modules JPL, CIT Electronics Chicago, JPL, Columbia Cryostats Columbia TT MPI Telescope Integration: Stanford Optics Design JPL Construction Stanford Ground Screens Stanford Oxford Manchester Calibration Princeton

11 Detectors

12 Sensitivity of a Radiometer ΔT = T sys Δν t obs T sys Δν ΔT sec Dicke 1600K 16 MHz 400 mk Today s HEMTs 50K 16 GHz 400 µk

13 90 GHz Module Automatic Assembly L R Simultaneous Q/U detections +Q +U -Q -U

14 QUIET L/R Correlator: Simultaneous Q/U measurements E a E y E b E x 50Hz switching 4kHz phase switching Q U

15 Time-Stream Noise Reduction with Differencing -J. Richards

16 High Speed Sampling khz Monitors spurious highfrequency noise Digital blanking of phase transitions Permits Quadrature Samples TOD noise with no signal Q/U measurement every 250 µs 0.5ms +Q -Q +Q -Q

17 Instrument/Observing

18 Q-band Receiver/Telescope Integration ~8 deg FOV

19 Upper Ground Screen Q-band is now at the Site!

20 W-band Receiver Integration W-band should ship in January

21 Tim Thurston Side-Fed Dragonian geometry

22 Calibration/Characterization (lab) Polarized gains Polarization sensitivity I to Q/U leakages

23 QUIET Calibration/Optimization 116 mk (Al)

24 Module Calibration & +Q1 Sensitivity +U1 -U1 Can measure relative Q/U phase to a few degrees in the lab

25 Polarized gain/sensitivity 4 diodes from one module Ti SS Al

26 Observing Strategy

27 QUIET Scan Simulation A. Kusaka

28 Observed Patches Quiet Polarbear Alliance with POLARBEAR Observe from the same location Choose patches in concert Provides 45, 90, 150, 225 GHz Clover

29 Scanning Pattern A. Kusaka

30 Site Affords Excellent Paralactic Angle Coverage

31 A. Kusaka Sky Coverage, Noise Filter CMB Signal Observed Sky After Filtering Detector Noise Huge contamination by detector 1/f noise 1/f noise is removed by high-pass filtering CMB power extraction

32 CMB Power, QUIET A. Kusaka Sensitivity E-mode power Observed Sky Auto Correlation B-mode power QUIET sensitivity (10 months, 50% duty) 2σ B-mode indication for r=0.3 Precise measurement of E-mode r=0.3 assumed

33 Sensitivity

34 Sensitiivity ΔP P 3 ΔT exp ΔT cos (Fractional error on power for a signal with Δl=l, Optimized scanning) ΔT exp ΔT cos ΔP/P Improvement Factor CAPMAP 0.2 µk 6 µk QUIET-I µk 0.14 µk (r=0.1) Detectors Q/U Time Tsys CAPMAP QUIET Factor Conclude: factor of 200 needed, 240 designed.

35 Systematic Studies Cross-polar leakage Polarization Angle EB mixing: geometry/weighting TOD filtering Instrumental I Q/U Gain Fluctuations Pointing Errors (very preliminary) Akito Kusaka

36 QUIET Cross-polar leakage H.K. Eriksen T/S=0.01

37 Polarization Angles We are hopeful to be able to get <1 degree from moon observations BB sin 2 (2θ) EE 4θ 2 EE EB sin(2θ) EE 2θ EE Setting <EB>=0 ok but we would be giving up sensitivity to a non-standard model effect

38 E/B mixing (geometry) A = 1/3

39 TOD Filtering No bias without acceleration Acceleration introduces leakages ~0.001 level (E to B)

40 Instrumental I to Q/U (OMT/Module mis-match) W band Q band

41 Gain Fluctuations Negligible issues with changes: Day by day Hour by hour Horn by horn Q/U gain mismatch:

42 Pointing Errors

43 QUIET Schedule Data till end of 2009 Phase II: ~2010/11

44

45 Issues/Lessons/Concerns For an experiment in development, what are your major concerns? ie, what systematics worry you most? Are we really serious about systematic uncertainty? Need to give numbers

46 Tip on dealing with speakers running over Coltrane to Miles: I can t figure out a way to stop my solos. Why don t you try taking the horn out of your mouth?

47 The End