Woodcraft, Adam L. and Sudiwala, Rashmi V. and Ade, Peter A. R. and Griffin, Matthew J. and Wakui, Elley and Bhatia, Ravinder S. and Lange, Andrew E. and Bock, James J. and Turner, Anthony D. and Yun, Minhee H. and Beeman, Jeffrey W. (2003) Predicting the response of a submillimeter bolometer to cosmic rays. Applied Optics, 42 (25). pp. 5009-5016. ISSN 0003-6935 http://resolver.caltech.edu/CaltechAUTHORS:WOOao03
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Bolometers designed to detect. submillimeter radiation also respond to cosmic, gamma, and x rays. Because detectors cannot be fully shielded from such energy sources, it is necessary to understand the effect of a photon or cosmic-ray particle being absorbed. The resulting signal (known as a glitch) can then be removed from raw data. We present measurements using an Americium-241 gamma radiation source to irradiate a prototype bolometer for the High Frequency Instrument in the Planck Surveyor satellite. Our measurements showed no variation in response depending on where the radiation was absorbed, demonstrating that the bolometer absorber and thermistor thermalize quickly. The bolometer has previously been fully characterized both electrically and optically. We find that using optically measured time constants underestimates the time taken for the detector to recover from a radiation absorption event. However, a full thermal model for the bolometer, with parameters taken from electrical and optical measurements, provides accurate time constants. Slight deviations from the model were seen at high energies; these can be accounted for by use of an extended model.
|Additional Information:||© 2003 Optical Society of America. Received 16 January 2003; revised manuscript received 9 May 2003.|
|Subject Keywords:||Noise in imaging systems; Photon statistics; Quantum optics : Fluctuations, relaxations, and noise; Astronomy and astrophysics|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Lindsay Cleary|
|Deposited On:||28 Jun 2006|
|Last Modified:||26 Dec 2012 08:55|
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