Kavli Affiliate: Chao-Lin Kuo
| First 5 Authors: The BICEP/Keck Collaboration, :, Y. Nakato, P. A. R. Ade, Z. Ahmed
| Summary:
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 high-frequency
receiver and discuss the integration status and test results as it is being
commissioned.
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