Optimization and sensitivity of the Keck Array
The Keck Array (SPUD) began observing the cosmic microwave background's polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments Bicep and Bicep2, 1 using five on-axis refracting telescopes. These have a combined imaging array of 25...
| Published in: | SPIE Proceedings, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI |
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| Main Authors: | , , , , , |
| Format: | Conference Object |
| Language: | English |
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Society of Photo-Optical Instrumentation Engineers (SPIE)
2012
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| Subjects: | |
| Online Access: | http://hdl.handle.net/2429/46171 https://doi.org/10.1117/12.926934 |
| Summary: | The Keck Array (SPUD) began observing the cosmic microwave background's polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments Bicep and Bicep2, 1 using five on-axis refracting telescopes. These have a combined imaging array of 2500 antenna-coupled TES bolometers read with a SQUID-based time domain multiplexing system. We will discuss the detector noise and the optimization of the readout. The achieved sensitivity of the Keck Array is 11.5 μK CMB √s in the 2012 configuration. 2012 SPIE. Copyright 2012 Society of Photo-Optical Instrumentation Engineers. One print or electronic copy may be made for personal use only. Systematic reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited. Science, Faculty of Physics and Astronomy, Department of Reviewed Faculty |
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