We present an overview of the design and status of the Polarbear-2 and the Simons Array experiments. Polarbear-2 is a cosmic microwave background polarimetry experiment which aims to characterize the arc-minute angular scale B-mode signal from weak gravitational lensing and search for the degree angular scale B-mode signal from inflationary gravitational waves. The receiver has a 365 mm diameter focal plane cooled to 270 mK. The focal plane is filled with 7588 dichroic lenslet–antenna-coupled polarization sensitive transition edge sensor (TES) bolometric pixels that are sensitive to 95 and 150 GHz bands simultaneously. The TES bolometers are read-out by SQUIDs with 40 channel frequency domain multiplexing. Refractive optical elements are made with high-purity alumina to achieve high optical throughput. The receiver is designed to achieve noise equivalent temperature of 5.8 μ KCMBs in each frequency band. Polarbear-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three Polarbear-2 type receivers. The Simons Array will cover 95, 150, and 220 GHz frequency bands for foreground control. The Simons Array will be able to constrain tensor-to-scalar ratio and sum of neutrino masses to σ(r) = 6 × 10 - 3 at r= 0.1 and ∑ mν(σ= 1) to 40 meV. © 2016, Springer Science+Business Media New York.
The Polarbear-2 and the Simons Array Experiments / Suzuki, A.; Ade, P.; Akiba, Y.; Aleman, C.; Arnold, K.; Baccigalupi, C.; Barch, B.; Barron, D.; Bender, A.; Boettger, D.; Borrill, J.; Chapman, S.; Chinone, Y.; Cukierman, A.; Dobbs, M.; Ducout, A.; Dunner, R.; Elleflot, T.; Errard, J.; Fabbian, G.; Feeney, S.; Feng, C.; Fujino, T.; Fuller, G.; Gilbert, A.; Goeckner-Wald, N.; Groh, J.; Haan, T. D.; Hall, G.; Halverson, N.; Hamada, T.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Hill, C.; Holzapfel, W.; Hori, Y.; Howe, L.; Inoue, Y.; Irie, F.; Jaehnig, G.; Jaffe, A.; Jeong, O.; Katayama, N.; Kaufman, J.; Kazemzadeh, K.; Keating, B.; Kermish, Z.; Keskitalo, R.; Kisner, T.; Kusaka, A.; Jeune, M. L.; Lee, A.; Leon, D.; Linder, E.; Lowry, L.; Matsuda, F.; Matsumura, T.; Miller, N.; Mizukami, K.; Montgomery, J.; Navaroli, M.; Nishino, H.; Peloton, J.; Poletti, D.; Puglisi, G.; Rebeiz, G.; Raum, C.; Reichardt, C.; Richards, P.; Ross, C.; Rotermund, K.; Segawa, Y.; Sherwin, B.; Shirley, I.; Siritanasak, P.; Stebor, N.; Stompor, R.; Suzuki, J.; Tajima, O.; Takada, S.; Takakura, S.; Takatori, S.; Tikhomirov, A.; Tomaru, T.; Westbrook, B.; Whitehorn, N.; Yamashita, T.; Zahn, A.; Zahn, O.. - In: JOURNAL OF LOW TEMPERATURE PHYSICS. - ISSN 0022-2291. - 184:3-4(2016), pp. 805-810. [10.1007/s10909-015-1425-4]
The Polarbear-2 and the Simons Array Experiments
Arnold, K.;Baccigalupi, C.;Borrill, J.;Fabbian, G.;Jaffe, A.;Keating, B.;Poletti, D.;Puglisi, G.;Stompor, R.;Tikhomirov, A.;Yamashita, T.;
2016-01-01
Abstract
We present an overview of the design and status of the Polarbear-2 and the Simons Array experiments. Polarbear-2 is a cosmic microwave background polarimetry experiment which aims to characterize the arc-minute angular scale B-mode signal from weak gravitational lensing and search for the degree angular scale B-mode signal from inflationary gravitational waves. The receiver has a 365 mm diameter focal plane cooled to 270 mK. The focal plane is filled with 7588 dichroic lenslet–antenna-coupled polarization sensitive transition edge sensor (TES) bolometric pixels that are sensitive to 95 and 150 GHz bands simultaneously. The TES bolometers are read-out by SQUIDs with 40 channel frequency domain multiplexing. Refractive optical elements are made with high-purity alumina to achieve high optical throughput. The receiver is designed to achieve noise equivalent temperature of 5.8 μ KCMBs in each frequency band. Polarbear-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three Polarbear-2 type receivers. The Simons Array will cover 95, 150, and 220 GHz frequency bands for foreground control. The Simons Array will be able to constrain tensor-to-scalar ratio and sum of neutrino masses to σ(r) = 6 × 10 - 3 at r= 0.1 and ∑ mν(σ= 1) to 40 meV. © 2016, Springer Science+Business Media New York.| File | Dimensione | Formato | |
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