BICEP3 performance overview and planned Keck Array upgrade

• Published in: SPIE Proceedings, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII
• Main Authors: Grayson, J. A., Bock, J. J., Filippini, J. P., Hristov, V. V., Hui, H., Kefeli, S., Lueker, M., O'Brient, R., Staniszewski, Z. K., Steinbach, B., Teply, G. P.
• Other Authors: Holland, Wayne S., Zmuidzinas, Jonas
• Format: Book Part
• Language: unknown
• Published: Society of Photo-Optical Instrumentation Engineers (SPIE) 2016
• Subjects: Cosmic Microwave Background; Inflation; Gravitational Waves; Polarization; BICEP; Keck Array; British Columbia; Canada; South Pole; South pole
• Online Access: https://doi.org/10.1117/12.2233894

Bicep3 is a 520mm aperture, compact two-lens refractor designed to observe the polarization of the cosmic microwave background (CMB) at 95 GHz. Its focal plane consists of modularized tiles of antenna-coupled transition edge sensors (TESs), similar to those used in Bicep2 and the Keck Array. The increased per-receiver optical throughput compared to Bicep2/Keck Array, due to both its faster f=1:7 optics and the larger aperture, more than doubles the combined mapping speed of the Bicep/Keck program. The Bicep3 receiver was recently upgraded to a full complement of 20 tiles of detectors (2560 TESs) and is now beginning its second year of observation (and first science season) at the South Pole. We report on its current performance and observing plans. Given its high per-receiver throughput while maintaining the advantages of a compact design, Bicep3- class receivers are ideally suited as building blocks for a 3rd-generation CMB experiment, consisting of multiple receivers spanning 35 GHz to 270 GHz with total detector count in the tens of thousands. We present plans for such an array, the new "BICEP Array" that will replace the Keck Array at the South Pole, including design optimization, frequency coverage, and deployment/observing strategies. © 2016 Society of Photo-Optical Instrumentation Engineers (SPIE). This work is supported by the National Science Foundation (grant nos. 1313158, 1313010, 1313062, 1313287, 1056465, 0960243), the SLAC Laboratory Directed Research and Development Fund, the Canada Foundation for Innovation, Science and Technology Facilities Council Consolidated Grant (ST/K000926/1), and the British Columbia Development Fund. The development of detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040, 10-SAT10-0017, and 12-SAT12-0031 from the NASA APRA and SAT programs. The development and testing of detector modules was supported by the Gordon and Betty Moore Foundation. Published - 99140S.pdf Submitted - 1607.04668v1.pdf