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BICEP: B ackground I maging of C osmic E xtragalactic P olarization. Jamie Bock Hien Nguyen Caltech/JPL. Andrew Lange Brian Keating Ki Won Yoon Eric Hivon Cynthia Chiang. Bill Holzapfel Yuki Takihashi U.C. Berkeley. Peter Ade U. Cardiff. “The Muscle Behind Curls”. - PowerPoint PPT Presentation
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BICEP: Background Imaging of Cosmic
Extragalactic Polarization
“The Muscle Behind Curls”
Jamie BockHien Nguyen
Caltech/JPL
Andrew LangeBrian KeatingKi Won YoonEric HivonCynthia Chiang
Bill HolzapfelYuki Takihashi
U.C. Berkeley
Peter Ade
U. Cardiff
http://www.astro.caltech.edu/~lgg/bicep_front.htm
The Challenge of CMB Polarimetry
What do we need?• Significant advance system sensitivity• Control systematic errors at < 0.1 K levels• Distinguish CMB from Galactic Foregrounds• Distinguish Gravity-wave Signal from Lensing
BICEPQUEST
BICEP
• A uniquely powerful probe for curl modes – key to understanding the physics of inflation
• ~100 times faster mapping speed than current experiments (e.g. BOOMERANG)
• 8” aperture refractor • Minimal Systematics• Technological Precursor for NASA “Beyond
Einstein” Mission CMBPOL 2003-2020 http://universe.gsfc.nasa.gov/roadmap.html
Instrument
The first pair of PSBs
• ~20 cm primary aperture
• Refractive wide-field optics
• ~20 FOV
• 0.7 (150 GHz) and 1.0 (100 GHz) resolutions
• 48 feeds / 96 polarization-sensitive bolometers at 250 mK
• South Pole site: great atmosphere, low foregrounds & conducive to deep integrations
•BICEP is a large Cryostat.
•Refracting optics cooled to 4K
•Uses both LN2 and LHe with a four day hold time.
Detectors cooled to 250 mK
BICEP is an Experiment- Not a Facility
•BICEP will deploy in December 2004
•BICEP will need to observe for three seasons in order to reach its scientificgoals.
•At the end of this time, the telescope will be removed.
Major Support Requirements
Facilities: Modification of DSL penthouse for BICEP mount
Temporary Summer Laboratory Space
Cryogenics: Liquid Nitrogen 20 liters/day,
Liquid Helium 17 liters/day
Power: ~15 KW
Data Transmission: ~2GB/day
Critical Schedule Dates
Laboratory Space: becomes available 11/22/04
DSL Modifications: complete 12/4/04
Mount installation: 12/7/04
Receiver installation: 12/22/04
Telescope Operations Begin: 1/14/05
Condition occupancy of DSL was not scheduled until 1/1/05.This presented a significant challenge to this “success oriented” schedule. – as of today, problem solved