BICEP Array cryostat and mount design

Bicep Array is a cosmic microwave background (CMB) polarization experiment that will begin observing at the South Pole in early 2019. This experiment replaces the five Bicep2 style receivers that compose the Keck Array with four larger Bicep3 style receivers observing at six frequencies from 30 to 2...

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Bibliographic Details
Published in:Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX
Main Authors: Crumrine, Michael, Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bishchoff, C. A., Bock, J. J., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Filescher, S., Grayson, J. A., Hall, G., Halpern, M., Harrison, S. A., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J. H., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kemasovskiy, S. A., Kovac, J. M., Kuo, C. L., Larsen, N. A., Lau, K., Leitch, E. M., Lueker, M. V., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn IV, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., St. Germaine, T., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C. E., Turner, A. D., Umilta, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., WIllmert, J., Wong, C. L., Wu, W. L. K., Yang, E., Yoon, K. W., Zhang, C.
Format: Conference Object
Language:unknown
Published: SPIE 2018
Subjects:
South Pole
South pole
Online Access:https://orca.cardiff.ac.uk/id/eprint/156731/
https://doi.org/10.1117/12.2312829
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Summary:Bicep Array is a cosmic microwave background (CMB) polarization experiment that will begin observing at the South Pole in early 2019. This experiment replaces the five Bicep2 style receivers that compose the Keck Array with four larger Bicep3 style receivers observing at six frequencies from 30 to 270GHz. The 95GHz and 150GHz receivers will continue to push the already deep Bicep/Keck CMB maps while the 30/40GHz and 220/270GHz receivers will constrain the synchrotron and galactic dust foregrounds respectively. Here we report on the design and performance of the Bicep Array instruments focusing on the mount and cryostat systems.

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