CaltechAUTHORS
Published December 15, 2020 | Version Published + Presentation
Book Section - Chapter Open

Analysis of Temperature-to-Polarization Leakage in BICEP3 and Keck CMB Data from 2016 to 2018

Creators

Abstract

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.

Additional Information

© 2020 Society of Photo-Optical Instrumentation Engineers (SPIE). 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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Additional details

Identifiers

Eprint ID
107161
Resolver ID
CaltechAUTHORS:20201217-130800252

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
NSF
OPP-1313010
NSF
OPP-1313062
NSF
OPP-1313158
NSF
OPP-1313287
NSF
OPP-0960243
NSF
AST-1836010
NSF
AST-1056465
NSF
AST-1255358
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
NASA
18-SAT18-0017
Gordon and Betty Moore Foundation
Canada Foundation for Innovation
Harvard University
Department of Energy (DOE)
DE-AC02-76SF00515

Dates

Created
2020-12-17
Created from EPrint's datestamp field
Updated
2022-02-08
Created 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
11453