The Polarbear-2 and the Simons Array Experiments

By A. Suzuki, P. Ade, Y. Akiba, C. Aleman, K. Arnold, C. Baccigalupi, B. Barch, D. Barron, A. Bender, D. Boettger and 80 more. 2015

165 citations recorded by the source corpus.

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 $$\upmu $$μK$$_\mathrm{CMB}\sqrt{s}$$CMBs 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 $$\sigma (r) = 6\times 10^{-3}$$σ(r)=6×10-3 at $$r = 0.1$$r=0.1 and $$\sum m_{\upnu } (\sigma =1)$$∑mν(σ=1) to 40 meV.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e17f70b0b1bdf2fbf5b43f18d6e15dcd4ba011f0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

CMB-S4: Forecasting Constraints on Primordial Gravitational Waves (2020, unknown): “There are currently a number of ground-based experiments measuring the CMB polarization to high precision on a range of scales, and attempting to constrain the tensor-to-scalar ratio, including ACT (Aiola et al. 2020), BICEP/Keck (BICEP2/Keck Array Collabora- tions X 2018), CLASS (Harrington et al. ”
Neutrino Mass Ordering from Oscillations and Beyond: 2018 Status and Future Prospects (2018, background): “The latter list includes ground-based observatories as the ACT (Atacama Cosmology Telescope) (De Bernardis et al., 2016), the SPT-3G (South Pole Telescope-3G) (Benson et al., 2014), the Simons Array (Suzuki et al., 2016), CLASS (EssingerHileman et al., 2014), BICEP3 (Ahmed et al., 2014), and the Sim”
A unified pseudo-Cℓ framework (2018, methodology): “…such as BICEP/Keck (BICEP2 Collaboration et al. 2016), Advanced ACTPol (De Bernardis et al. 2016; Louis et al. 2017) or the Simons Array (Suzuki et al. 2016; POLARBEAR Collaboration et al. 2017), as well as next-generation facilities such as the Simons Observatory (The Simons…”
Measurements of the E -mode polarization and temperature- E -mode correlation of the CMB from SPT-3G 2018 data (2021, background): “Several current and upcoming experiments aim to improve existing power spectrum constraints, including Advanced ACT [18], BICEP3/BICEP Array [19,20], POLARBEAR2/Simons Array [21], the Simons Observatory [22], and SPT-3G [23].”
The Simons Observatory: science goals and forecasts (2018, background): “The rapid progress of ground-based measurements in the last decade has been driven by the development of arrays of superconducting transition-edge sensor (TES) bolometers coupled to multiplexed readout electronics (Henderson et al. 2016; Posada et al. 2016; Suzuki et al. 2016; Hui et al. 2016).”