Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array
Creators
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Zhang, C.
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Ade, P. A. R.
- Ahmed, Z.
- Amiri, M.
- Barkats, D.
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Basu Thakur, R.
- Bischoff, C. A.
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Bock, J. J.
- Boenish, H.
- Bullock, E.
- Buza, V.
- Cheshire, J.
- Connors, J.
- Cornelison, J.
- Crumrine, M.
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Cukierman, A.
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Dierickx, M.
- Duband, L.
- Fatigoni, S.
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Filippini, J. P.
- Hall, G.
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Halpern, M.
- Harrison, S.
- Henderson, S.
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Hildebrandt, S.R.
- Hilton, G. C.
- Hui, H.
- Irwin, K. D.
- Kang, J.
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Karkare, K. S.
- Karpel, E.
- Kefeli, S.
- Kovac, J. M.
- Kuo, C. L.
- Lau, K.
- Megerian, K. G.
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Moncelsi, L.
- Namikawa, T.
- Nguyen, H. T.
- O'Brient, R.
- Palladino, S.
- Precup, N.
- Prouvé, T.
- Pryke, C.
- Racine, B.
- Reintsema, C. D.
- Richter, S.
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Schillaci, A.
- Schmitt, B.
- Schwarz, R.
- Sheehy, C. D.
- Soliman, A.
- St. Germaine, T.
- Steinbach, B.
- Sudiwala, R. V.
- Thompson, K. L.
- Tucker, C.
- Turner, A. D.
- Umiltà, C.
- Vieregg, A. G.
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Wandui, A.
- Weber, A. C.
- Wiebe, D. V.
- Willmert, J.
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Wu, W. L. K.
- Yang, E.
- Yoon, K. W.
- Young, E.
- Yu, C.
Abstract
The BICEP/Keck (BK) experiment aims to detect the imprint of primordial gravitational waves in the cosmic microwave background polarization, which would be direct evidence of the inflation theory. While the tensor-to-scalar ratio has been constrained to be r_(0.05) < 0.06 at 95% c.l., further improvements on this upper limit are hindered by polarized galactic foreground emissions and removal of gravitational lensing polarization. The 30/40 GHz receiver of the BICEP Array (BA) will deploy at the end of 2019 and will constrain the synchrotron foreground with unprecedented accuracy within the BK sky patch. We will show the design of the 30/40 GHz detectors and test results summarizing its performance. The low optical and atmospheric loading at these frequencies requires our TES detectors to have low saturation power in order to be photon noise dominated. To realize the low thermal conductivity required from a 250 mK base temperature, we developed new bolometer leg designs. We will present the relevant measured detector parameters: G, T_c, R_n, P_(sat), and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07×10⁻¹⁷ W/√Hz, including an anticipated photon noise level 1.54×10⁻¹⁷W/√Hz.
Additional Information
© 2020 Springer Nature Switzerland AG. Received 01 September 2019; Accepted 10 February 2020; Published 24 February 2020. The BICEP/Keck project 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, and 1726917 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 and 16-SAT16-0002. 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 is partially supported by the U.S. DoE Office of Science. 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.Attached Files
Accepted Version - 2002.05219.pdf
Files
2002.05219.pdf
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Additional details
Identifiers
- Eprint ID
- 101522
- DOI
- 10.1007/s10909-020-02411-8
- Resolver ID
- CaltechAUTHORS:20200225-082326440
Related works
- Describes
- 10.1007/s10909-020-02411-8 (DOI)
- https://arxiv.org/abs/2002.05219 (URL)
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
- 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
- Gordon and Betty Moore Foundation
- Canada Foundation for Innovation
- Harvard University
- Department of Energy (DOE)
Dates
- Created
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2020-02-25Created from EPrint's datestamp field
- Updated
-
2023-03-16Created from EPrint's last_modified field