Development of the 220/270 GHz Receiver of BICEP Array

The BICEP/Keck Collaboration: Y. Nakato (1); P. A. R. Ade (2); Z.; Ahmed (3); M. Amiri (4); D. Barkats (5); R. Basu Thakur (6,8); C. A. Bischoff; (7); D. Beck (1,3); J. J. Bock (6,8); V. Buza (9); B. Cantrall (1); J. R.; Cheshire IV (10); J. Cornelison (5); M. Crumrine (11); A. J. Cukierman (6),; E. Denison (12); M. Dierickx (5); L. Duband (13); M. Eiben (5); B. D. Elwood; (5,16); S. Fatigoni (4,6); J. P. Filippini (14,15); A. Fortes (1); M. Gao; (6); C. Giannakopoulos (7); N. Goeckner-Wald (1); D. C. Goldfinger (3); J. A.; Grayson (1); P. K. Grimes (5); G. Hall (11); G. Halal (1); M. Halpern (4); E.; Hand (7); S. Harrison (4); S. Henderson (3); J. Hubmayr (12); H. Hui (6); K.; D. Irwin (1,3,12); J. Kang (1,6); K. S. Karkare (3); E. Karpel (1); S. Kefeli; (6); J. M. Kovac (5,16); C. L. Kuo (1,3); K. Lau (6); M. Lautzenhiser (7); A.; Lennox (14); T. Liu (1); K. G. Megerian (8); M. Miller (5); L. Minutolo (6),; L. Moncelsi (6); H. T. Nguyen (8); R. O'Brient (6,8); A. Patel (6); M.; Petroff (5); A. R. Polish (5,16); T. Prouve (13); C. Pryke (10,11); C. D.; Reintsema (12); T. Romand (6); M. Salatino (1); A. Schillaci (6); B. L.; Schmitt (5,19); B. Singari (10); A. Soliman (6,8); T. St. Germaine (5,16); A.; Steiger (6); B. Steinbach (6); R. Sudiwala (2); K. L. Thompson (1,3); C.; Tucker (2); A. D. Turner (8); C. Verg\`es (5); A. Wandui (6); A. C. Weber; (8); J. Willmert (11); W. L. K. Wu (3); H. Yang (1); E. Young (1,3); C. Yu; (1); L. Zeng (5); C. Zhang (1,6); S. Zhang (6) ((1) Stanford University; (2); Cardiff University; (3) KIPAC/SLAC; (4) University of British Columbia; (5); Harvard/CfA; (6) Caltech; (7) University of Cincinnati; (8) NASA JPL; (9); University of Chicago; (10) Minnesota Institute for Astrophysics; (11); University of Minnesota; (12) NIST; (13) SBT Grenoble; (14) University of; Illinois Urbana-Champaign; (15) University of Illinois Urbana-Champaign; (16); Harvard University; (17) The University of Tokyo; (18) Aix-Marseille; Universite; (19) University of Pennsylvania)

arXiv:2409.02296·astro-ph.IM·September 5, 2024

Development of the 220/270 GHz Receiver of BICEP Array

The BICEP/Keck Collaboration: Y. Nakato (1), P. A. R. Ade (2), Z., Ahmed (3), M. Amiri (4), D. Barkats (5), R. Basu Thakur (6,8), C. A. Bischoff, (7), D. Beck (1,3), J. J. Bock (6,8), V. Buza (9), B. Cantrall (1), J. R., Cheshire IV (10), J. Cornelison (5), M. Crumrine (11)

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TL;DR

This paper describes the development, integration, and commissioning of the 220/270 GHz receiver for the BICEP Array, aimed at measuring CMB B-mode polarization and characterizing Galactic dust.

Contribution

It introduces the design, integration, and commissioning progress of the high-frequency receiver for the BICEP Array, enhancing multi-frequency CMB observations.

Findings

01

Receiver undergoing commissioning at Stanford

02

Test results demonstrate readiness for deployment

03

Scheduled deployment to the South Pole in 2024-2025

Abstract

Measurements of B-mode polarization in the CMB sourced from primordial gravitational waves would provide information on the energy scale of inflation and its potential form. To achieve these goals, one must carefully characterize the Galactic foregrounds, which can be distinguished from the CMB by conducting measurements at multiple frequencies. BICEP Array is the latest-generation multi-frequency instrument of the BICEP/Keck program, which specifically targets degree-scale primordial B-modes in the CMB. In its final configuration, this telescope will consist of four small-aperture receivers, spanning frequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to characterize Galactic dust is currently undergoing commissioning at Stanford University and is scheduled to deploy to the South Pole during the 2024--2025 austral summer. Here, we will provide an overview of this…

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Taxonomy

TopicsSuperconducting and THz Device Technology · Particle Accelerators and Free-Electron Lasers · Particle accelerators and beam dynamics