Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array

C. Zhang; P. A.R. Ade; Z. Ahmed; M. Amiri; D. Barkats; R. Basu Thakur; C. A. Bischoff; J. J. Bock; H. Boenish; E. Bullock; V. Buza; J. Cheshire; J. Connors; J. Cornelison; M. Crumrine; A. Cukierman; M. Dierickx; L. Duband; S. Fatigoni; J. P. Filippini; G. Hall; M. Halpern; S. Harrison; S. Henderson; S. R. Hildebrandt; G. C. Hilton; H. Hui; K. D. Irwin; J. Kang; K. S. Karkare; E. Karpel; S. Kefeli; J. M. Kovac; C. L. Kuo; K. Lau; K. G. Megerian; L. Moncelsi; T. Namikawa; H. T. Nguyen; R. O’Brient; S. Palladino; N. Precup; T. Prouvé; C. Pryke; B. Racine; C. D. Reintsema; S. Richter; A. Schillaci; B. Schmitt; R. Schwarz; C. D. Sheehy; A. Soliman; T. St Germaine; B. Steinbach; R. V. Sudiwala; K. L. Thompson; C. Tucker; A. D. Turner; C. Umiltà; A. G. Vieregg; A. Wandui; A. C. Weber; D. V. Wiebe; J. Willmert; W. L.K. Wu; E. Yang; K. W. Yoon; E. Young; C. Yu

doi:10.1007/s10909-020-02411-8

Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array

C. Zhang, P. A.R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. Cheshire, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, M. Dierickx, L. Duband, S. Fatigoni, J. P. FilippiniG. Hall, M. Halpern, S. Harrison, S. Henderson, S. R. Hildebrandt, G. C. Hilton, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, S. Kefeli, J. M. Kovac, C. L. Kuo, K. Lau, K. G. Megerian, L. Moncelsi, T. Namikawa, H. T. Nguyen, R. O’Brient, S. Palladino, N. Precup, T. Prouvé, C. Pryke, B. Racine, C. D. Reintsema, S. Richter, A. Schillaci, B. Schmitt, R. Schwarz, C. D. Sheehy, A. Soliman, T. St Germaine, B. Steinbach, R. V. Sudiwala, K. L. Thompson, C. Tucker, A. D. Turner, C. Umiltà, A. G. Vieregg, A. Wandui, A. C. Weber, D. V. Wiebe, J. Willmert, W. L.K. Wu, E. Yang, K. W. Yoon, E. Young, C. Yu

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

7 Scopus citations

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 2.07×10-17W/Hz, including an anticipated photon noise level 1.54×10-17W/Hz.

Original language	English (US)
Pages (from-to)	968-975
Number of pages	8
Journal	Journal of Low Temperature Physics
Volume	199
Issue number	3-4
DOIs	https://doi.org/10.1007/s10909-020-02411-8
State	Published - May 1 2020

Bibliographical note

Publisher Copyright:
© 2020, Springer Science+Business Media, LLC, part of Springer Nature.

Keywords

B-Mode polarization
CMB
Cosmology
Inflation
TES

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10.1007/s10909-020-02411-8

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Zhang, C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. B., Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Dierickx, M., Duband, L., Fatigoni, S., ... Yu, C. (2020). Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array. Journal of Low Temperature Physics, 199(3-4), 968-975. https://doi.org/10.1007/s10909-020-02411-8

Zhang, C, Ade, PAR, Ahmed, Z, Amiri, M, Barkats, D, Thakur, RB, Bischoff, CA, Bock, JJ, Boenish, H, Bullock, E, Buza, V, Cheshire, J, Connors, J, Cornelison, J, Crumrine, M, Cukierman, A, Dierickx, M, Duband, L, Fatigoni, S, Filippini, JP, Hall, G, Halpern, M, Harrison, S, Henderson, S, Hildebrandt, SR, Hilton, GC, Hui, H, Irwin, KD, Kang, J, Karkare, KS, Karpel, E, Kefeli, S, Kovac, JM, Kuo, CL, Lau, K, Megerian, KG, Moncelsi, L, Namikawa, T, Nguyen, HT, O’Brient, R, Palladino, S, Precup, N, Prouvé, T, Pryke, C, Racine, B, Reintsema, CD, Richter, S, Schillaci, A, Schmitt, B, Schwarz, R, Sheehy, CD, Soliman, A, Germaine, TS, Steinbach, B, Sudiwala, RV, Thompson, KL, Tucker, C, Turner, AD, Umiltà, C, Vieregg, AG, Wandui, A, Weber, AC, Wiebe, DV, Willmert, J, Wu, WLK, Yang, E, Yoon, KW, Young, E & Yu, C 2020, 'Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array', Journal of Low Temperature Physics, vol. 199, no. 3-4, pp. 968-975. https://doi.org/10.1007/s10909-020-02411-8

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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 r0.05< 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, Tc, Rn, Psat, and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07×10-17W/Hz, including an anticipated photon noise level 1.54×10-17W/Hz.",

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author = "C. Zhang and Ade, {P. A.R.} and Z. Ahmed and M. Amiri and D. Barkats and Thakur, {R. Basu} and Bischoff, {C. A.} and Bock, {J. J.} and H. Boenish and E. Bullock and V. Buza and J. Cheshire and J. Connors and J. Cornelison and M. Crumrine and A. Cukierman and M. Dierickx and L. Duband and S. Fatigoni and Filippini, {J. P.} and G. Hall and M. Halpern and S. Harrison and S. Henderson and Hildebrandt, {S. R.} and Hilton, {G. C.} and H. Hui and Irwin, {K. D.} and J. Kang and Karkare, {K. S.} and E. Karpel and S. Kefeli and Kovac, {J. M.} and Kuo, {C. L.} and K. Lau and Megerian, {K. G.} and L. Moncelsi and T. Namikawa and Nguyen, {H. T.} and R. O{\textquoteright}Brient and S. Palladino and N. Precup and T. Prouv{\'e} and C. Pryke and B. Racine and Reintsema, {C. D.} and S. Richter and A. Schillaci and B. Schmitt and R. Schwarz and Sheehy, {C. D.} and A. Soliman and Germaine, {T. St} and B. Steinbach and Sudiwala, {R. V.} and Thompson, {K. L.} and C. Tucker and Turner, {A. D.} and C. Umilt{\`a} and Vieregg, {A. G.} and A. Wandui and Weber, {A. C.} and Wiebe, {D. V.} and J. Willmert and Wu, {W. L.K.} and E. Yang and Yoon, {K. W.} and E. Young and C. Yu",

note = "Publisher Copyright: {\textcopyright} 2020, Springer Science+Business Media, LLC, part of Springer Nature.",

year = "2020",

month = may,

day = "1",

doi = "10.1007/s10909-020-02411-8",

language = "English (US)",

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AU - Zhang, C.

AU - Ade, P. A.R.

AU - Ahmed, Z.

AU - Amiri, M.

AU - Barkats, D.

AU - Thakur, R. Basu

AU - Bischoff, C. A.

AU - Bock, J. J.

AU - Boenish, H.

AU - Bullock, E.

AU - Buza, V.

AU - Cheshire, J.

AU - Connors, J.

AU - Cornelison, J.

AU - Crumrine, M.

AU - Cukierman, A.

AU - Dierickx, M.

AU - Duband, L.

AU - Fatigoni, S.

AU - Filippini, J. P.

AU - Hall, G.

AU - Halpern, M.

AU - Harrison, S.

AU - Henderson, S.

AU - Hildebrandt, S. R.

AU - Hilton, G. C.

AU - Hui, H.

AU - Irwin, K. D.

AU - Kang, J.

AU - Karkare, K. S.

AU - Karpel, E.

AU - Kefeli, S.

AU - Kovac, J. M.

AU - Kuo, C. L.

AU - Lau, K.

AU - Megerian, K. G.

AU - Moncelsi, L.

AU - Namikawa, T.

AU - Nguyen, H. T.

AU - O’Brient, R.

AU - Palladino, S.

AU - Precup, N.

AU - Prouvé, T.

AU - Pryke, C.

AU - Racine, B.

AU - Reintsema, C. D.

AU - Richter, S.

AU - Schillaci, A.

AU - Schmitt, B.

AU - Schwarz, R.

AU - Sheehy, C. D.

AU - Soliman, A.

AU - Germaine, T. St

AU - Steinbach, B.

AU - Sudiwala, R. V.

AU - Thompson, K. L.

AU - Tucker, C.

AU - Turner, A. D.

AU - Umiltà, C.

AU - Vieregg, A. G.

AU - Wandui, A.

AU - Weber, A. C.

AU - Wiebe, D. V.

AU - Willmert, J.

AU - Wu, W. L.K.

AU - Yang, E.

AU - Yoon, K. W.

AU - Young, E.

AU - Yu, C.

PY - 2020/5/1

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N2 - 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 r0.05< 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, Tc, Rn, Psat, and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07×10-17W/Hz, including an anticipated photon noise level 1.54×10-17W/Hz.

AB - 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 r0.05< 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, Tc, Rn, Psat, and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07×10-17W/Hz, including an anticipated photon noise level 1.54×10-17W/Hz.

KW - B-Mode polarization

KW - CMB

KW - Cosmology

KW - Inflation

KW - TES

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VL - 199

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JO - Journal of Low Temperature Physics

JF - Journal of Low Temperature Physics

IS - 3-4

ER -

Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array

Abstract

Bibliographical note

Keywords

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