QUIET Summary• Probing Inflationary Scalar fields at GUT-scale energies

• Phase I has already demonstrated its technology and methodology (100 detectors)– The most sensitive CMB polarization array yet fielded

• Phase II has been proposed– NSF Reverse site visit in Jan-Feb– FNAL involvement critical to get to Phase II level (1600)

• “HEP” approach more important as experiments grow

• QUIET is unique: (verified) technology, frequencies, year-round access, best able to forecast sensitivity, and alliances with other experiments

•The Cosmic Microwave Background and Particle Physics

M. Kamionkowski, A. Kosowsky, Ann.Rev.Nucl.Part.Sci.49:77-123,1999 •The Cosmic Microwave Background for Pedestrians: A Review for Particle and Nuclear Physicists

D. Samtleben, S. Staggs, B. W., Ann.Rev.Nucl.Part.Sci.57:245-283,2007

11/12/09 FNAL PAC

CaltechJPL

Stanford(KIPAC)

Miami

Chicago (KICP)Fermilab

ColumbiaPrinceton

ManchesterOxford Oslo

MPI-Bonn

KEK

Chajnantor Plateau, Chile

2

11/12/09 FNAL PAC

The Site: Atacama Desert in Chile

• Home for many expts– ALMA, ACT, ASTE, QUIET, POLARBEAR, CLOVER, …

• High and Dry: – 16,700 feet

• Year-round access• Lots of room

11/12/09 FNAL PAC

11/12/09 FNAL PAC

Integrating the W-band Array the Chicago

(5 times as many elements to be integrated at FNAL)

11/12/09 FNAL PAC U

Ex

Eb

Ey

Ea

QUIET L/R Correlator:Simultaneous Q/U measurements

Q

4kHz phase switching

An Unpolarized pixel gives ZERO even with a gain difference between the legs!

11/12/09 FNAL PAC

8 sec of data 100kHz sampling

unswitched

switched

Temperature vs. time, 10 ms bins

11/12/09 FNAL PAC

Map precision on1x1 degree pixel:

Planck: 1 K (100 GHz) QUIET: 10-1 K (90 GHz)

11/12/09 FNAL PAC

Galaxy(Pol., <100 hrs)sytematic efectsnot considered yet

WMAP5 years

Q U

11/12/09 FNAL PAC

QUIET CMB Temperature Map

(1 detector, 1 month vs. 5 years)

11/12/09 FNAL PAC

QUIET ~ 600 hrs WMAP 5 years

QUIET-I Stokes Q map of one patch:Already deeper than Planck forecasts

11/12/09 FNAL PAC

Null Power Spectra

11/12/09 FNAL PAC

Phase I has already shown:

• Platelet, OMT technology works• Module technology works

– Want to improve sensitivity and production

• Crossed Dragone Optics verified– Now the most popular choice

• High speed sampling works and is valuable

• The site works: duty cycle, atmosphere• We can reliable forecast Phase II• Cautious approach has paid off

11/12/09 FNAL PAC

QUIET Phase-I Forecasts

11/12/09 FNAL PAC

Phase II Plan

• 4 Telescopes – (3 CMB & 1 Foreground)

• “Small things”– Electronics improvements– Thermal control– Matching band-passes

• “Big things”– Improving module production– Improving module performance

11/12/09 FNAL PAC

Foregrounds(Planck Sky Model)

• Dust(synchrotron) negligible for QUIET(SPT)

• Broad frequency range important to determine contamination

• 100% overlap with ABS, Polarbear; less w/SPT

r=0.1

QUIET

PolarbearABS, SPT

11/12/09 FNAL PAC

Current* Performance(noise, duty cycle, 1/f) Likely Improvements

0.018r 0.00510 lensing 35 * already better! < 0.3 ev

11/12/09 FNAL PAC

• “While QUIET I has been pursued primarily with non-HEP funding, HEP has unique capabilities to offer the project as it moves to the next step, QUIET II: (a) Fermilab has unique large-scale fabrication capabilities required to mass-produce the detectors; (b) HEP scientists have valuable experience with the high-speed electronics the project will require; (c) the approaches to data analysis and related capabilities that have been developed for particle physics experiments will become increasingly important to CMB science as the scope of CMB experiments, and scale of the collaborations, increases.

• Recommendations: PASAG recommends that QUIET II be supported at the proposed scope under all budget scenarios. Given the central importance of the CMB to our understanding of energy, matter, space, and time and the unique contributions HEP can provide to CMB science, PASAG further recommends that the future upgrade path for QUIET II should be considered for support at the appropriate time.”

Field does support multiple efforts, e.g. Dark Matter searches

11/12/09 FNAL PAC

What Characterizes/Distinguishes

QUIET?• Unique RF technology

– Different systematics, Q & U measured simultaneously– Large dynamic range

• Modulation:– 4 kHz inside modules– From sky rotation: Q to U to -Q every 6 hours– From telescope deck rotation: Q to U every week

• ~6% of the sky mapped 100 times deeper than Planck– Sensitivity to r < 0.02 [based on current performance (noise, duty cycle)]

• Alliance with (bolometric) POLARBEAR and ABS (and SPT)– Identical Patches– frequencies straddle WMAP “sweet spot”

• HEP-like:– 800kHz digitization (FPGA demodulation)– Volume production, quality control– simulations, data reduction, blind analyses, systematics, systematics, …..– Increased appreciation of our field

• Upgrade Path:– Sharing ATACAMA telescopes– MMIC improvements: from 15 QL to 8 QL to 3QL

11/12/09 FNAL PAC

Bruce’s Backup Slides

NSF Site Visit – May 18 - 19, 2009

The National Science Foundation

ATACAMA Experiments

NSF Site Visit – May 18 - 19, 2009

32/

11/12/09 FNAL PAC

Lensing Simulation (W. Hu et al.)

11/12/09 FNAL PAC

Lensing BB Power Spectrum vs. Neutrino Mass

€

mυ∑ ≈10ev ⇒ Ωm = 0.3

11/12/09 FNAL PAC

Current CMB Polarization Status(QUIET has already collected data which will improve these measurements)

11/12/09 FNAL PAC

Telescope• 1.4m primary mirror

• FWHM:– 13 arcmin (W-band)– 28 arcmin (Q-band)

11/12/09 FNAL PAC

Q/U measurement every 250 sMonitors high-frequency

noisePermits Quadrature Samples

– TOD noise with no signal

High Speed Sampling18 bits @ 800 kHz

+Q -Q +Q -Q

0.5ms

11/12/09 FNAL PAC

Moon

Galaxy (TT, <100 hrs)

QUIET

WMAPPRELIMINARY

11/12/09 FNAL PAC

CMB & Collider DM Constraints

EPP2010