Design and performance of wide-band corrugated walls for the BICEP Array detector modules at 30/40 GHz
Abstract
BICEP Array is a degree-scale Cosmic Microwave Background (CMB) experiment that will search for primordial B-mode polarization while constraining Galactic foregrounds. BICEP Array will be comprised of four receivers to cover a broad frequency range with channels at 30/40, 95, 150 and 220/270 GHz. The first low-frequency receiver will map synchrotron emission at 30 and 40 GHz and will deploy to the South Pole at the end of 2019. In this paper, we give an overview of the BICEP Array science and instrument, with a focus on the detector module. We designed corrugations in the metal frame of the module to suppress unwanted interactions with the antenna-coupled detectors that would otherwise deform the beams of edge pixels. This design reduces the residual beam systematics and temperature-to-polarization leakage due to beam steering and shape mismatch between polarized beam pairs. We report on the simulated performance of single- and wide-band corrugations designed to minimize these effects. Our optimized design alleviates beam differential ellipticity caused by the metal frame to about 7% over 57% bandwidth (25 to 45 GHz), which is close to the level due the bare antenna itself without a metal frame. Initial laboratory measurements are also presented.
Additional Information
© 2018 Society of Photo-optical Instrumentation Engineers (SPIE). The Bicep/Keck Array project have been made possible through a series of grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, & 1726917 and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA Grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009 & 16-SAT16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DoE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Tireless administrative support was provided by Kathy Deniston, Sheri Stoll, Irene Coyle, Donna Hernandez, and Dana Volponi. We are grateful our BICEP/Keck Array collaboration colleagues for useful discussions and technical feedback.Attached Files
Published - 107082G.pdf
Submitted - 1808.00571.pdf
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107082G.pdf
Additional details
Identifiers
- Eprint ID
- 92135
- Resolver ID
- CaltechAUTHORS:20190108-104453619
Related works
- Describes
- https://arxiv.org/abs/1808.00571 (URL)
Funding
- NSF
- OPP-0742818
- NSF
- OPP-0742592
- NSF
- OPP-1044978
- NSF
- PLR-1110087
- NSF
- OPP-1145172
- NSF
- OPP-1145143
- NSF
- OPP-1145248
- NSF
- OPP-1639040
- NSF
- OPP-1638957
- NSF
- OPP-1638978
- NSF
- OPP-1638970
- NSF
- OPP-1726917
- W. M. Keck Foundation
- JPL Research and Technology Development Fund
- NASA
- 06-ARPA206-0040
- NASA
- 10-SAT10-0017
- NASA
- 12-SAT12-0031
- NASA
- 14-SAT14-0009
- NASA
- 16-SAT16-0002
- Gordon and Betty Moore Foundation
- Canada Foundation for Innovation
- Harvard University
- Department of Energy (DOE)
Dates
- Created
-
2019-01-08Created from EPrint's datestamp field
- Updated
-
2021-11-16Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Astronomy Department , Physics Department
- Series Name
- Proceedings of SPIE
- Series Volume or Issue Number
- 10708