Paper PC13102-11
Paper PC13102-11
Development of the 220/270 GHz BICEP Array CMB receiver
On demand | Presented live 18 June 2024 
Abstract
Measurements of B-mode polarization in the cosmic microwave background (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 (BA) 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, BA will consist of four small-aperture receivers, spanning six different frequency bands. The BA4 receiver is designed to characterize Galactic dust at 220/270 GHz. This receiver is currently undergoing commissioning at Stanford 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, discussing the integration status and test results as it is being commissioned.
BICEP Array (BA) 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, BA will consist of four small-aperture receivers, spanning six different frequency bands. The BA4 receiver is designed to characterize Galactic dust at 220/270 GHz. This receiver is currently undergoing commissioning at Stanford 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, discussing the integration status and test results as it is being commissioned.
Presenter
Yuka Nakato
Stanford Univ. (United States)
Yuka Nakato is a fourth year PhD candidate in Physics at Stanford University and KIPAC. She got her bachelor’s degrees in Physics and Mathematics at the University of Minnesota - Twin Cities, where she did research in cosmology as part of the BICEP/Keck collaboration. At Stanford, she is continuing to work in BICEP, commissioning the 220/270 GHz receiver for the BICEP Array CMB telescope. She is now also a member of the South Pole Telescope collaboration, developing the global minimum variance (GMV) quadratic estimator pipeline for use in a future lensing reconstruction analysis.