Use of High Sensitivity Bolometers for Astronomy: Planck High Frequency Instrument
Creators
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1.
Institut d'Astrophysique Spatiale
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2.
Cardiff University
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3.
Jet Propulsion Lab
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4.
Sapienza University of Rome
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5.
Centre d'Etudes Supérieures de la Renaissance
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6.
California Institute of Technology
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7.
National University of Ireland, Maynooth
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8.
Institut d'Astrophysique de Paris
Contributors
Other:
Abstract
The Planck satellite is dedicated to the measurement of the anisotropy of the Cosmic Microwave Background (CMB) with unprecedented sensitivity and angular resolution. It is a project of the European Space Agency based on a wide international collaboration, including United States and Canadian laboratories. The detectors of its High Frequency Instrument (HFI) are bolometers cooled down to 100 mK. Their sensitivity will be limited by the photon noise of the CMB itself at low frequencies, and of the instrument background at high frequencies. The requirements on the measurement chain are directly related to the strategy of observation used for the satellite. This impacts the bolometer design as well as other elements: The cooling system must present outstanding temperature stability, and the amplification chain must show a flat noise spectrum down to very low frequencies.
Additional Information
© 2002 American Institute of Physics. Issue Date: 5 February 2002.Attached Files
Published - LAMaipcp02a.pdf
Files
LAMaipcp02a.pdf
Additional details
Identifiers
- Eprint ID
- 27556
- Resolver ID
- CaltechAUTHORS:20111101-111656544
Dates
- Created
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2011-11-01Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Physics Department
- Series Name
- AIP Conference Proceedings
- Series Volume or Issue Number
- 605