The POLARBEAR CMB polarization experiment

Arnold, K.; Ade, Peter A. R.; Anthony, A. E.; Aubin, F.; Boettger, D.; Borrill, J.; Cantalupo, C. M.; Dobbs, M.; Errard, Josquin; Flanigan, D.; Ghribi, A.; Halverson, N. W.; Hazumi, M.; Holzapfel, W. L.; Howard, J.; Hyland, P.; Jaffe, A. H.; Keating, Brian; Kisner, T. S.; Kermish, Z.; Lee, A. T.; Linder, Eric V.; Lungu, Marius; Matsumura, Tomotake; Miller, Nathan J.; Meng, Xiaofan; Myers, Michael J.; Nishino, Hitoshi; O’Brient, R.; O'Dea, D.; Paar, H. P.; Reichardt, Christian; Schanning, I.; Shimizu, A.; Shimmin, C. O.; Shimon, Meir; Spieler, H.; Steinbach, B.; Stompor, R.; Suzuki, Aritoki; Tomaru, T.; Tran, Hung V.; Tucker, C.; Quealy, E.; Richards, P. L.; Zahn, O.

doi:10.1117/12.858314

Cited by 36 publications

(31 citation statements)

References 23 publications

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“…The focal plane and readout are assembled from several modular components enabling scaling to larger arrays. These components have been used in SPT, which started observations in 2007 with 960 detectors, and POLARBEAR, 19 an upcoming Berkeley CMB polarization experiment with over 1200 detectors. The analog multiplexed SQUID readout developed for APEX-SZ has evolved into a next-generation digital multiplexed readout system described in Ref.…”

Section: Opticsmentioning

confidence: 99%

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Invited Article: Millimeter-wave bolometer array receiver for the Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument

Schwan

Basu

Bender

et al. 2011

Review of Scientific Instruments

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The Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument is a millimeter-wave cryogenic receiver designed to observe galaxy clusters via the Sunyaev-Zel'dovich effect from the 12 m APEX telescope on the Atacama plateau in Chile. The receiver contains a focal plane of 280 superconducting transition-edge sensor (TES) bolometers instrumented with a frequency-domain multiplexed readout system. The bolometers are cooled to 280 mK via a three-stage helium sorption refrigerator and a mechanical pulse-tube cooler. Three warm mirrors, two 4 K lenses, and a horn array couple the TES bolometers to the telescope. APEX-SZ observes in a single frequency band at 150 GHz with 1' angular resolution and a 22' field-of-view, all well suited for cluster mapping. The APEX-SZ receiver has played a key role in the introduction of several new technologies including TES bolometers, the frequency-domain multiplexed readout, and the use of a pulse-tube cooler with bolometers. As a result of these new technologies, the instrument has a higher instantaneous sensitivity and covers a larger field-of-view than earlier generations of Sunyaev-Zel'dovich instruments. The TES bolometers have a median sensitivity of 890 μK(CMB)√s (NEy of 3.5 × 10(-4) √s). We have also demonstrated upgraded detectors with improved sensitivity of 530 μK(CMB)√s (NEy of 2.2 × 10(-4) √s). Since its commissioning in April 2007, APEX-SZ has been used to map 48 clusters. We describe the design of the receiver and its performance when installed on the APEX telescope.

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Section: Opticsmentioning

confidence: 99%

“…19. (Color online) Measured power spectral density (PSD) for a type-1 bolometer channel during a single scan made in weather typical of the August 2007 observing run.…”

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confidence: 99%

Invited Article: Millimeter-wave bolometer array receiver for the Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument

Schwan

Basu

Bender

et al. 2011

Review of Scientific Instruments

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“…These goals are already aimed at by an entire slew of current, forthcoming, and planned CMB observations, e.g., [1][2][3][4][5]. Probably most importantly, CMB B-mode measurements could open up a window, as direct as likely ever possible, onto the physics of the very early Universe, giving us unique insights on the physical laws governing at the highest energies.…”

Section: Introductionmentioning

confidence: 99%

Framework for performance forecasting and optimization of CMBB-mode observations in the presence of astrophysical foregrounds

2011

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We present a formalism for performance forecasting and optimization of future cosmic microwave background (CMB) experiments. We implement it in the context of nearly full sky, multifrequency, B-mode polarization observations, incorporating statistical uncertainties due to the CMB sky statistics, instrumental noise, as well as the presence of the foreground signals. We model the effects of a subtraction of these using a parametric maximum likelihood technique and optimize the instrumental configuration with predefined or arbitrary observational frequency channels, constraining either a total number of detectors or a focal plane area. We showcase the proposed formalism by applying it to two cases of experimental setups based on the CMBpol and COrE mission concepts looked at as dedicated B-mode experiments. We find that, if the models of the foregrounds available at the time of the optimization are sufficiently precise, the procedure can help to either improve the potential scientific outcome of the experiment by a factor of a few, while allowing one to avoid excessive hardware complexity, or simplify the instrument design without compromising its science goals. However, our analysis also shows that even if the available foreground models are not considered to be sufficiently reliable, the proposed procedure can guide a design of more robust experimental setups. While better suited to cope with a plausible, greater complexity of the foregrounds than that foreseen by the models, these setups could ensure science results close to the best achievable, should the models be found to be correct.

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“…With the improvement in sensitivity expected in future experiments [14][15][16], it is becoming increasingly more important to take into consideration corrections to the observed power spectra, which have until now been negligible. One such effect comes from the fact that on scales smaller than the diffusion length, the density anisotropies are smoothed out due to photon diffusion damping.…”

Section: Introductionmentioning

confidence: 99%

Small-scale modification to the lensing kernel

2018

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Calculations of the Cosmic Microwave Background lensing power implemented into the standard cosmological codes such as CAMB and CLASS usually treat the surface of last scatter as an infinitely thin screen. However, since the CMB anisotropies are smoothed out on scales smaller than the diffusion length due to the effect of Silk damping, the photons which carry information about the small-scale density distribution come from slightly earlier times than the standard recombination time. The dominant effect is the scale dependence of the mean redshift associated with the fluctuations during recombination. We find that fluctuations at k = 0.01 Mpc −1 come from a characteristic redshift of z ≈ 1090, while fluctuations at k = 0.3 Mpc −1 come from a characteristic redshift of z ≈ 1130. We then estimate the corrections to the lensing kernel and the related power spectra due to this effect. We conclude that neglecting it would result in a deviation from the true value of the lensing kernel at the half percent level at small CMB scales. For an all-sky, noise-free experiment, this corresponds to a ∼ 0.1σ shift in the observed temperature power spectrum on small scales (2500 l 4000).

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The POLARBEAR CMB polarization experiment

Cited by 36 publications

References 23 publications

Invited Article: Millimeter-wave bolometer array receiver for the Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument

Invited Article: Millimeter-wave bolometer array receiver for the Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument

Framework for performance forecasting and optimization of CMBB-mode observations in the presence of astrophysical foregrounds

Small-scale modification to the lensing kernel

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