The Bicep/Keck Array experiment is a series of small-Aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial B-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high-fidelity, in-situ measurements of the beam response to estimate the temperature-To-polarization (T → P) leakage in our latest data including observations from 2016 through 2018. This includes three years of Bicep3 observing at 95 GHz, and multifrequency data from Keck Array. Here we present band-Averaged far-field beam maps, differential beam mismatch, and residual beam power (after filtering out the leading difference modes via deprojection) for these receivers. We show preliminary results of beam map simulations which use these beam maps to observe a simulated temperature (no Q/U) sky to estimate T → P leakage in our real data.
|Original language||English (US)|
|Title of host publication||Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X|
|Editors||Jonas Zmuidzinas, Jian-Rong Gao|
|State||Published - 2020|
|Event||Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 2020 - Virtual, Online, United States|
Duration: Dec 14 2020 → Dec 22 2020
|Name||Proceedings of SPIE - The International Society for Optical Engineering|
|Conference||Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X 2020|
|Period||12/14/20 → 12/22/20|
Bibliographical noteFunding Information:
The BICEP/Keck project (including BICEP2, BICEP3 and BICEP Array) 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, 1313010, 1313062, 1313158, 1313287, 0960243, 1836010, 1056465, & 1255358 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, & 18-SAT18-0017. 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 was partially supported by the Department of Energy, Contract DE-AC02-76SF00515. 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.
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- Cosmic microwave background
- Gravitational waves
- Keck Array