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1. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author

Westbrook, B., Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bender, A. N., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Coppi, G., Crowley, K., Cukierman, A., de, T., Dünner, R., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fuller, G., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Holzapfel, W., Howe, L., Inoue, Y., Jaehnig, G., Jaffe, A., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Le, M., Lee, A. T., Leon, D., Linder, E., Lowry, L., Madurowicz, A., Mak, D., Matsuda, F., May, A., Miller, N. J., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Peloton, J., Pham, A., Piccirillo, L., Plambeck, D., Poletti, D., Puglisi, G., Raum, C., Rebeiz, G., Reichardt, C. L., Richards, P. L., Roberts, H., Ross, C., Rotermund, K. M., Segawa, Y., Sherwin, B., Silva-Feaver, M., Siritanasak, P., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Tat, R., Teply, G. P., Tikhomirov, A., Tomaru, T., Tsai, C., Whitehorn, N., and Zahn, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present on the status of POLARBEAR-2 A (PB2-A) focal plane fabrication. The PB2-A is the first of three telescopes in the Simon Array (SA), which is an array of three cosmic microwave background (CMB) polarization sensitive telescopes located at the POLARBEAR (PB) site in Northern Chile. As the successor to the PB experiment, each telescope and receiver combination is named as PB2-A, PB2-B, and PB2-C. PB2-A and -B will have nearly identical receivers operating at 90 and 150 GHz while PB2-C will house a receiver operating at 220 and 270 GHz. Each receiver contains a focal plane consisting of seven close-hex packed lenslet coupled sinuous antenna transition edge sensor bolometer arrays. Each array contains 271 di-chroic optical pixels each of which have four TES bolometers for a total of 7588 detectors per receiver. We have produced a set of two types of candidate arrays for PB2-A. The first we call Version 11 (V11) and uses a silicon oxide (SiOx) for the transmission lines and cross-over process for orthogonal polarizations. The second we call Version 13 (V13) and uses silicon nitride (SiNx) for the transmission lines and cross-under process for orthogonal polarizations. We have produced enough of each type of array to fully populate the focal plane of the PB2-A receiver. The average wirebond yield for V11 and V13 arrays is 93.2% and 95.6% respectively. The V11 arrays had a superconducting transition temperature (Tc) of 452 +/- 15 mK, a normal resistance (Rn) of 1.25 +/- 0.20 Ohms, and saturations powers of 5.2 +/- 1.0 pW and 13 +/- 1.2 pW for the 90 and 150 GHz bands respectively. The V13 arrays had a superconducting transition temperature (Tc) of 456 +/-6 mK, a normal resistance (Rn) of 1.1 +/- 0.2 Ohms, and saturations powers of 10.8 +/- 1.8 pW and 22.9 +/- 2.6 pW for the 90 and 150 GHz bands respectively.

Published
2022
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2. A Measurement of the Degree Scale CMB B-mode Angular Power Spectrum with POLARBEAR

Author

Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background (CMB) using taken from July 2014 to December 2016 with the POLARBEAR experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of $\mathrm{NET}_\mathrm{array}=23\, \mu \mathrm{K} \sqrt{\mathrm{s}}$ on a 670 square degree patch of sky centered at (RA, Dec)=($+0^\mathrm{h}12^\mathrm{m}0^\mathrm{s},-59^\circ18^\prime$). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ effective polarization map noise with a knee in sensitivity of $\ell = 90$, where the inflationary gravitational wave signal is expected to peak. The measured $B$-mode power spectrum is consistent with a $\Lambda$CDM lensing and single dust component foreground model over a range of multipoles $50 \leq \ell \leq 600$. The data disfavor zero $C_\ell^{BB}$ at $2.2\sigma$ using this $\ell$ range of POLARBEAR data alone. We cross-correlate our data with Planck high frequency maps and find the low-$\ell$ $B$-mode power in the combined dataset to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio $r < 0.90$ at 95% confidence level after marginalizing over foregrounds.

Published
2019
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3. Cross-correlation of POLARBEAR CMB Polarization Lensing with High-$z$ Sub-mm Herschel-ATLAS galaxies

Author

Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., and Verges, C.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We report a 4.8$\sigma$ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the POLARBEAR experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of $b = 5.76 \pm 1.25$, corresponding to a host halo mass of $\log_{10}(M_h/M_\odot) =13.5^{+0.2}_{-0.3}$ at an effective redshift of $z \sim 2$ from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the sub-mm galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extra-galactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments., Comment: 14 pages, 6 figures, updated to match published version on ApJ

Published
2019
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4. A Measurement of the Degree-scale CMB B-mode Angular Power Spectrum with Polarbear

Author

Adachi, S, Aguilar Faúndez, MAO, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Bouhargani, HE, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tsai, C, Verges, C, Westbrook, B, and Zhou, Y

Subjects
Cosmic microwave background radiation, Cosmic inflation, Cosmology, Observational cosmology, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We present a measurement of the B-mode polarization power spectrum of the cosmic microwave background (CMB) using data taken from 2014 July to 2016 December with the Polarbear experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of NETarray=23μ K√s on a 670 square degree patch of sky centered at (R.A., decl.) = (+0h12m0s, -59°18′). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve 32 μK arcmin effective polarization map noise with a knee in sensitivity of ℓ = 90, where the inflationary gravitational-wave signal is expected to peak. The measured B-mode power spectrum is consistent with a ΛCDM lensing and single dust component foreground model over a range of multipoles 50 ≤ ℓ ≤ 600. The data disfavor zero CℓBB at 2.2σ using this ℓ range of Polarbear data alone. We cross-correlate our data with Planck full mission 143, 217, and 353 GHz frequency maps and find the low-ℓ B-mode power in the combined data set to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio r < 0.90 at the 95% confidence level after marginalizing over foregrounds.

Published
2020

5. Cross-correlation of CMB Polarization Lensing with High-z Submillimeter Herschel-ATLAS Galaxies

Author

Faúndez, M Aguilar, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Cheung, K, Chinone, Y, Bouhargani, H El, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Hasegawa, M, Hazumi, M, Howe, L, Kaneko, D, Katayama, N, Keating, B, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Teply, GP, Tsai, C, and Vergès, C

Subjects
Particle and High Energy Physics, Physical Sciences, astro-ph.CO, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We report a 4.8σ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the Polarbear experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of b=5.76\pm 1.25, corresponding to a host halo mass log10(Mh M⊙. =13.5+0.2-0.3 of at an effective redshift of z ∼ 2 from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the submillimeter galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extragalactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments.

Published
2019

6. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

Author

Namikawa, T, Chinone, Y, Miyatake, H, Oguri, M, Takahashi, R, Kusaka, A, Katayama, N, Adachi, S, Aguilar, M, Aihara, H, Ali, A, Armstrong, R, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Corbett, L, Crowley, KT, Bouhargani, H El, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Groh, J, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Jeong, O, Kaneko, D, Keating, B, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Miyazaki, S, Murayama, H, Navaroli, M, Nishino, H, Nishizawa, AJ, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Speagle, JS, Stompor, R, Suzuki, A, Tait, PJ, Tajima, O, Takada, M, Takakura, S, Takatori, S, Tanabe, D, Tanaka, M, Teply, GP, Tsai, C, Vergés, C, Westbrook, B, and Zhou, Y

Subjects
Particle and High Energy Physics, Physical Sciences, cosmic background radiation, cosmology: observations, gravitational lensing: weak, polarization, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We present the first measurement of cross-correlation between the lensing potential, reconstructed from cosmic microwave background (CMB) polarization data, and the cosmic shear field from galaxy shapes. This measurement is made using data from the Polarbear CMB experiment and the Subaru Hyper Suprime-Cam (HSC) survey. By analyzing an 11 deg2 overlapping region, we reject the null hypothesis at 3.5σ and constrain the amplitude of the cross-spectrum to , where is the amplitude normalized with respect to the Planck 2018 prediction, based on the flat Λ cold dark matter cosmology. The first measurement of this cross-spectrum without relying on CMB temperature measurements is possible owing to the deep Polarbear map with a noise level of ∼6 μK arcmin, as well as the deep HSC data with a high galaxy number density of . We present a detailed study of the systematics budget to show that residual systematics in our results are negligibly small, which demonstrates the future potential of this cross-correlation technique.

Published
2019

7. The Simons Observatory: Science goals and forecasts

Author

Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, MA, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, JA, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, JR, Borrill, J, Brown, ML, Bruno, SM, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, HMS, Choi, S, Coppi, G, Cothard, NF, Coughlin, K, Crichton, D, Crowley, KD, Crowley, KT, Cukierman, A, D'Ewart, JM, Dünner, R, De Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, CJ, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, JC, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, PA, Ghersi, JTG, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, JE, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, SW, Hervias-Caimapo, C, and Hill, CA

Subjects
CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

Published
2019

8. Measurements of Tropospheric Ice Clouds with a Ground-based CMB Polarization Experiment, POLARBEAR

Author

Takakura, S, Aguilar-Faúndez, MAO, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Chinone, Y, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Goeckner-Wald, N, Hamada, T, Hasegawa, M, Hazumi, M, Howe, L, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Lowry, LN, Matsuda, FT, May, AJ, Minami, Y, Navaroli, M, Nishino, H, Piccirillo, L, Poletti, D, Puglisi, G, Reichardt, CL, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Suzuki, A, Tajima, O, Takatori, S, Tanabe, D, Teply, GP, and Tsai, C

Subjects
Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, atmospheric effects, scattering, cosmology: observations, cosmic background radiation, polarization, astro-ph.IM, astro-ph.CO, physics.ao-ph, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The polarization of the atmosphere has been a long-standing concern for ground-based experiments targeting cosmic microwave background (CMB) polarization. Ice crystals in upper tropospheric clouds scatter thermal radiation from the ground and produce a horizontally polarized signal. We report a detailed analysis of the cloud signal using a ground-based CMB experiment, Polarbear, located at the Atacama desert in Chile and observing at 150 GHz. We observe horizontally polarized temporal increases of low-frequency fluctuations ("polarized bursts," hereafter) of ≲0.1 K when clouds appear in a webcam monitoring the telescope and the sky. The hypothesis of no correlation between polarized bursts and clouds is rejected with >24σ statistical significance using three years of data. We consider many other possibilities including instrumental and environmental effects, and find no reasons other than clouds that can explain the data better. We also discuss the impact of the cloud polarization on future ground-based CMB polarization experiments.

Published
2019

9. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author

Westbrook, B, Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bender, AN, Bianchini, F, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Coppi, G, Crowley, K, Cukierman, A, de Haan, T, Dünner, R, Dobbs, M, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fuller, G, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Halverson, NW, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Holzapfel, W, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Le Jeune, M, Lee, AT, Leon, D, Linder, E, Lowry, L, Madurowicz, A, Mak, D, Matsuda, F, May, A, Miller, NJ, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Piccirillo, L, Plambeck, D, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, CL, Richards, PL, Roberts, H, Ross, C, Rotermund, KM, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Tat, R, Teply, GP, Tikhomirov, A, Tomaru, T, Tsai, C, Whitehorn, N, and Zahn, A

Subjects
Physical Sciences, Classical Physics, Condensed Matter Physics, CMB, Fabrication, Instrumentation, Detectors, Transition edge sensor, Sinuous antenna, Polarization, Inflation, Mathematical Physics, General Physics, Classical physics, Condensed matter physics
Abstract

We present on the status of POLARBEAR-2 A (PB2-A) focal plane fabrication. The PB2-A is the first of three telescopes in the Simons Array, which is an array of three cosmic microwave background polarization-sensitive telescopes located at the POLARBEAR site in Northern Chile. As the successor to the PB experiment, each telescope and receiver combination is named as PB2-A, PB2-B, and PB2-C. PB2-A and -B will have nearly identical receivers operating at 90 and 150 GHz while PB2-C will house a receiver operating at 220 and 270 GHz. Each receiver contains a focal plane consisting of seven close-hex packed lenslet-coupled sinuous antenna transition edge sensor bolometer arrays. Each array contains 271 dichroic optical pixels, each of which has four TES bolometers for a total of 7588 detectors per receiver. We have produced a set of two types of candidate arrays for PB2-A. The first we call Version 11 (V11) uses a silicon oxide (SiOx) for the transmission lines and crossover process for orthogonal polarizations. The second we call Version 13 (V13) uses silicon nitride (SiNx) for the transmission lines and cross-under process for orthogonal polarizations. We have produced enough of each type of array to fully populate the focal plane of the PB2-A receiver. The average wirebond yield for V11 and V13 arrays is 93.2% and 95.6%, respectively. The V11 arrays had a superconducting transition temperature (Tc) of 452±15 mK, a normal resistance (Rn) of 1.25±0.20Ω, and saturation powers of 5.2 ± 1.0 pW and 13 ± 1.2 pW for the 90 and 150 GHz bands, respectively. The V13 arrays had a superconducting transition temperature (Tc) of 456 ± 6 mK, a normal resistance (Rn) of 1.1±0.2Ω, and saturation powers of 10.8 ± 1.8 pW and 22.9 ± 2.6 pW for the 90 and 150 GHz bands, respectively. Production and characterization of arrays for PB2-B are ongoing and are expected to be completed by the summer of 2018. We have fabricated the first three candidate arrays for PB2-C but do not have any characterization results to present at this time.

Published
2018

11. A Measurement of the Cosmic Microwave Background $B$-Mode Polarization Power Spectrum at Sub-Degree Scales from 2 years of POLARBEAR Data

Author

The POLARBEAR Collaboration, Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Ducout, A., Dünner, R., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hamada, T., Hall, G., Halverson, N. W., Hasegawa, M., Hazumi, M., Hill, C., Howe, L., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Jeune, M. Le, Lee, A. T., Leitch, E. M., Leon, D., Linder, E., Lowry, L., Matsuda, F., Matsumura, T., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Richards, P. L., Ross, C., Segawa, Y., Sherwin, B. D., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tomaru, T., Tucker, C., Whitehorn, N., and Zahn, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report an improved measurement of the cosmic microwave background (CMB) $B$-mode polarization power spectrum with the POLARBEAR experiment at 150 GHz. By adding new data collected during the second season of observations (2013-2014) to re-analyzed data from the first season (2012-2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles $500 \leq \ell \leq 2100$, where the dominant $B$-mode signal is expected to be due to the gravitational lensing of $E$-modes. We reject the null hypothesis of no $B$-mode polarization at a confidence of 3.1$\sigma$ including both statistical and systematic uncertainties. We test the consistency of the measured $B$-modes with the $\Lambda$ Cold Dark Matter ($\Lambda$CDM) framework by fitting for a single lensing amplitude parameter $A_L$ relative to the Planck best-fit model prediction. We obtain $A_L = 0.60 ^{+0.26} _{-0.24} ({\rm stat}) ^{+0.00} _{-0.04}({\rm inst}) \pm 0.14 ({\rm foreground}) \pm 0.04 ({\rm multi})$, where $A_{L}=1$ is the fiducial $\Lambda$CDM value, and the details of the reported uncertainties are explained later in the manuscript., Comment: 16 pages, 10 figures. Minor changes to match the published version. For data and figures, see http://bolo.berkeley.edu/polarbear/data/polarbear_BB_2017/

Published
2017
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12. A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of POLARBEAR Data

Author

Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, JC, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, AH, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Le Jeune, M, Lee, AT, Leitch, EM, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Richards, PL, Ross, C, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tucker, C, Whitehorn, N, and Zahn, A

Subjects
cosmic background radiation, cosmology: observations, large-scale structure of universe
Published
2017

13. Erratum: “A Measurement of the Cosmic Microwave Background B-Mode Polarization Power Spectrum at Sub-degree Scales with POLARBEAR” (2014, ApJ, 794, 171)

Author

Ade, The Polarbear Collaboration PAR, Akiba, Y, Anthony, AE, Arnold, K, Atlas, M, Barron, D, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Dobbs, M, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Flanigan, D, Gilbert, A, Grainger, W, Halverson, NW, Hasegawa, M, Hattori, K, Hazumi, M, Holzapfel, WL, Hori, Y, Howard, J, Hyland, P, Inoue, Y, Jaehnig, GC, Jaffe, AH, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Le Jeune, M, Lee, AT, Leitch, EM, Linder, E, Lungu, M, Matsuda, F, Matsumura, T, Meng, X, Miller, NJ, Morii, H, Moyerman, S, Myers, MJ, Navaroli, M, Nishino, H, Orlando, A, Paar, H, Peloton, J, Poletti, D, Quealy, E, Rebeiz, G, Reichardt, CL, Richards, PL, Ross, C, Schanning, I, Schenck, DE, Sherwin, BD, Shimizu, A, Shimmin, C, Shimon, M, Siritanasak, P, Smecher, G, Spieler, H, Stebor, N, Steinbach, B, Stompor, R, Suzuki, A, Takakura, S, Tomaru, T, Wilson, B, Yadav, A, and Zahn, O

Subjects
Particle and High Energy Physics, Physical Sciences, cosmic background radiation, cosmology: observations, large-scale structure of universe, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We report an improved measurement of the cosmic microwave background B-mode polarization power spectrum with the Polarbear experiment at 150 GHz. By adding new data collected during the second season of observations (2013-2014) to re-analyzed data from the first season (2012-2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles 500 ≤ ℓ ≤ 2100, where the dominant B-mode signal is expected to be due to the gravitational lensing of E-modes. We reject the null hypothesis of no B-mode polarization at a confidence of 3.1σ including both statistical and systematic uncertainties. We test the consistency of the measured B-modes with the Λ Cold Dark Matter (ΛCDM) framework by fitting for a single lensing amplitude parameter A L = 0.60 +0.26-0.24(stat)+0.00-0.04 (inst) ± 0.14(foreground) ± 0.04(multi), where A L = 1 relative to the Planck 2015 best-fit model prediction. We obtain ±0.14(foreground) ±0.04(multi), where is the fiducial ΛCDM value.

Published
2017

14. POLARBEAR-2: an instrument for CMB polarization measurements

Author

Inoue, Y., 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., de Haan, T., Dobbs, M. A., Ducout, A., Dunner, R., Elleflot, T., Errard, J., Fabbian, G., Feeney, S., Feng, C., Fuller, G., Gilbert, A. J., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N., Hamada, T., Hasegawa, M., Hattori, K., Hazumi, M., Hill, C., Holzapfel, W. L., Hori, Y., Howe, L., Irie, F., Jaehnig, G., Jaffe, A., Jeongh, O., Katayama, N., Kaufman, J. P., Kazemzadeh, K., Keating, B. G., Kermish, Z., Keskital, R., Kisner, T., Kusaka, A., Jeune, M. Le, Lee, A. T., Leon, D., Linder, E. V., Lowry, L., Matsuda, F., Matsumura, T., Miller, N., Mizukami, K., Montgomery, J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Poletti, D., Puglisi, G., Raum, C. R., Rebeiz, G. M., Reichardt, C. L., Richards, P. L., Ross, C., Rotermund, K. M., Segaw, Y., Sherwin, B. D., Shirley, I., Siritanasak, P., Stebor, N., Suzuki, R. Stompor A., Tajima, O., Takada, S., Takatori, S., Teply, G. P., Tikhomirol, A., Tomaru, T., Whitehorn, N., Zahn, A., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

POLARBEAR-2 (PB-2) is a cosmic microwave background (CMB) polarization experiment that will be located in the Atacama highland in Chile at an altitude of 5200 m. Its science goals are to measure the CMB polarization signals originating from both primordial gravitational waves and weak lensing. PB-2 is designed to measure the tensor to scalar ratio, r, with precision {\sigma}(r) < 0.01, and the sum of neutrino masses, {\Sigma}m{\nu}, with {\sigma}({\Sigma}m{\nu}) < 90 meV. To achieve these goals, PB-2 will employ 7588 transition-edge sensor bolometers at 95 GHz and 150 GHz, which will be operated at the base temperature of 250 mK. Science observations will begin in 2017., Comment: 9pages,8figures

Published
2016
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15. The POLARBEAR-2 and the Simons Array Experiment

Author

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., De Haan, T., 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. Le, 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., 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., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an overview of the design and status of the \Pb-2 and the Simons Array experiments. \Pb-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~milli-Kelvin. The focal plane is filled with 7,588 dichroic lenslet-antenna coupled polarization sensitive Transition Edge Sensor (TES) bolometric pixels that are sensitive to 95~GHz 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~$\mu$K$_{CMB}\sqrt{s}$ in each frequency band. \Pb-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three \Pb-2 type receivers. The Simons Array will cover 95~GHz, 150~GHz 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 $\sigma(r) = 6\times 10^{-3}$ at $r = 0.1$ and $\sum m_\nu (\sigma =1)$ to 40 meV., Comment: Accepted to Journal of Low Temperature Physics LTD16 Special Issue, Low Temperature Detector 16 Conference Proceedings, 5 pages, 1 figure

Published
2015
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16. Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

Author

Takakura, S, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beckman, S, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Fujino, T, Galitzki, N, Goeckner-Wald, N, Halverson, NW, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaffe, AH, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Lowry, L, Matsuda, F, Matsumura, T, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Reichardt, CL, Ross, C, Siritanasak, P, Suzuki, A, Tajima, O, Takatori, S, and Teply, G

Subjects
CMBR experiments, gravitational waves and CMBR polarization, astro-ph.IM, astro-ph.CO, physics.ins-det, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

A continuously rotating half-wave plate (CRHWP) is a promising tool to improve the sensitivity to large angular scales in cosmic microwave background (CMB) polarization measurements. With a CRHWP, single detectors can measure three of the Stokes parameters, I, Q and U, thereby avoiding the set of systematic errors that can be introduced by mismatches in the properties of orthogonal detector pairs. We focus on the implementation of CRHWPs in large aperture telescopes (i.e. the primary mirror is larger than the current maximum half-wave plate diameter of ∼0.5 m), where the CRHWP can be placed between the primary mirror and focal plane. In this configuration, one needs to address the intensity to polarization (I→P) leakage of the optics, which becomes a source of 1/f noise and also causes differential gain systematics that arise from CMB temperature fluctuations. In this paper, we present the performance of a CRHWP installed in the {\scshape Polarbear} experiment, which employs a Gregorian telescope with a 2.5 m primary illumination pattern. The CRHWP is placed near the prime focus between the primary and secondary mirrors. We find that the I→P leakage is larger than the expectation from the physical properties of our primary mirror, resulting in a 1/f knee of 100 mHz. The excess leakage could be due to imperfections in the detector system, i.e. detector non-linearity in the responsivity and time-constant. We demonstrate, however, that by subtracting the leakage correlated with the intensity signal, the 1/f noise knee frequency is reduced to 32 mHz (ℓ ∼ 39 for our scan strategy), which is very promising to probe the primordial B-mode signal. We also discuss methods for further noise subtraction in future projects where the precise temperature control of instrumental components and the leakage reduction will play a key role.

Published
2017

17. Modeling atmospheric emission for CMB ground-based observations

Author

Errard, J., Ade, P. A. R., Akiba, Y., Arnold, K., Atlas, M., Baccigalupi, C., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Cukierman, A., Delabrouille, J., Dobbs, M., Ducout, A., Elleflot, T., Fabbian, G., Feng, C., Feeney, S., Gilbert, A., Goeckner-Wald, N., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Hill, C., Holzapfel, W. L., Hori, Y., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Jeong, O., Katayama, N., Kaufman, J., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Leitch, E. M., Leon, D., Linder, E., Matsuda, F., Matsumura, T., Miller, N. J., Myers, M. J., Navaroli, M., Nishino, H., Okamura, T., Paar, H., Peloton, J., Poletti, D., Puglisi, G., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Rotermund, K. M., Schenck, D. E., Sherwin, B. D., Siritanasak, P., Smecher, G., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Tikhomirov, A., Tomaru, T., Whitehorn, N., Wilson, B., Yadav, A., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Atmosphere is one of the most important noise sources for ground-based cosmic microwave background (CMB) experiments. By increasing optical loading on the detectors, it amplifies their effective noise, while its fluctuations introduce spatial and temporal correlations between detected signals. We present a physically motivated 3d-model of the atmosphere total intensity emission in the millimeter and sub-millimeter wavelengths. We derive a new analytical estimate for the correlation between detectors time-ordered data as a function of the instrument and survey design, as well as several atmospheric parameters such as wind, relative humidity, temperature and turbulence characteristics. Using an original numerical computation, we examine the effect of each physical parameter on the correlations in the time series of a given experiment. We then use a parametric-likelihood approach to validate the modeling and estimate atmosphere parameters from the POLARBEAR-I project first season data set. We derive a new 1.0% upper limit on the linear polarization fraction of atmospheric emission. We also compare our results to previous studies and weather station measurements. The proposed model can be used for realistic simulations of future ground-based CMB observations., Comment: 20 pages, 16 figures

Published
2015
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18. Development and characterization of the readout system for POLARBEAR-2

Author

Barron, D., Ade, P. A. R., Akiba, Y., Aleman, C., Arnold, K., Atlas, M., Bender, A., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Cukierman, A., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Gilbert, A., Goeckner-Wald, N., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Katayama, N., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Leitch, E. M., Linder, E., Matsuda, F., Matsumura, T., Meng, X., Morii, H., Myers, M. J., Navaroli, M., Nishino, H., Okamura, T., Paar, H., Peloton, J., Poletti, D., Raum, C., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Rotermund, K., Schenck, D. E., Sherwin, B. D., Shirley, I., Sholl, M., Siritanasak, P., Smecher, G., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Suzuki, J., Takada, S., Takakura, S., Tomaru, T., Wilson, B., Yadav, A., Yamaguchi, H., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

POLARBEAR-2 is a next-generation receiver for precision measurements of the polarization of the cosmic microwave background (Cosmic Microwave Background (CMB)). Scheduled to deploy in early 2015, it will observe alongside the existing POLARBEAR-1 receiver, on a new telescope in the Simons Array on Cerro Toco in the Atacama desert of Chile. For increased sensitivity, it will feature a larger area focal plane, with a total of 7,588 polarization sensitive antenna-coupled Transition Edge Sensor (TES) bolometers, with a design sensitivity of 4.1 uKrt(s). The focal plane will be cooled to 250 milliKelvin, and the bolometers will be read-out with 40x frequency domain multiplexing, with 36 optical bolometers on a single SQUID amplifier, along with 2 dark bolometers and 2 calibration resistors. To increase the multiplexing factor from 8x for POLARBEAR-1 to 40x for POLARBEAR-2 requires additional bandwidth for SQUID readout and well-defined frequency channel spacing. Extending to these higher frequencies requires new components and design for the LC filters which define channel spacing. The LC filters are cold resonant circuits with an inductor and capacitor in series with each bolometer, and stray inductance in the wiring and equivalent series resistance from the capacitors can affect bolometer operation. We present results from characterizing these new readout components. Integration of the readout system is being done first on a small scale, to ensure that the readout system does not affect bolometer sensitivity or stability, and to validate the overall system before expansion into the full receiver. We present the status of readout integration, and the initial results and status of components for the full array., Comment: Presented at SPIE Astronomical Telescopes and Instrumentation 2014: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII. Published in Proceedings of SPIE Volume 9153

Published
2014
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19. POLARBEAR-2: an instrument for CMB polarization measurements

Author

Inoue, Y, 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, de Haan, T, Dobbs, MA, Ducout, A, Dünner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fuller, G, Gilbert, AJ, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, WL, Hori, Y, Howe, L, Irie, F, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, JP, Kazemzadeh, K, Keating, BG, Kermish, Z, Keskitalo, R, Kisner, TS, Kusaka, A, Le Jeune, M, Lee, AT, Leon, D, Linder, EV, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Mizukami, K, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Raum, CR, Rebeiz, GM, Reichardt, CL, Richards, PL, Ross, C, Rotermund, KM, Segawa, Y, Sherwin, BD, Shirley, I, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, J, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, GP, Tikhomirov, A, Tomaru, T, Whitehorn, N, Zahn, A, and Zahn, O

Subjects
Engineering, Communications Engineering, Electronics, Sensors and Digital Hardware, Physical Sciences, Atomic, Molecular and Optical Physics, Cosmic Microwave Background, IR filter, POLARBEAR-2, Polarization, Bolometer, Gravitational Wave, millimeter wave, astro-ph.IM, astro-ph.CO, Communications engineering, Electronics, sensors and digital hardware, Atomic, molecular and optical physics
Abstract

POLARBEAR-2 (PB-2) is a cosmic microwave background (CMB) polarization experiment that will be located in the Atacama highland in Chile at an altitude of 5200 m. Its science goals are to measure the CMB polarization signals originating from both primordial gravitational waves and weak lensing. PB-2 is designed to measure the tensor to scalar ratio, r, with precision σ(r) > 0:01, and the sum of neutrino masses, Σmz, with σ(Σmv) < 90 meV. To achieve these goals, PB-2 will employ 7588 transition-edge sensor bolometers at 95 GHz and 150 GHz, which will be operated at the base temperature of 250 mK. Science observations will begin in 2017.

Published
2016

20. The Polarbear-2 and the Simons Array Experiments

Author

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 De, 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 Le, 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, and Zahn, O

Subjects
Particle and High Energy Physics, Physical Sciences, Cosmic microwave background, Inflation, Gravitational weak lensing, Polarization, B-mode, astro-ph.IM, astro-ph.CO, Mathematical Physics, Classical Physics, Condensed Matter Physics, General Physics, Classical physics, Condensed matter physics
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.

Published
2016

21. The Simons Array CMB polarization experiment

Author

Stebor, N, Ade, P, Akiba, Y, Aleman, C, Arnold, K, Baccigalupi, C, Barch, B, Barron, D, Beckman, S, Bender, A, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, de Haan, T, Dobbs, M, Ducout, A, Planella, R Dünner, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Fuller, G, Gilbert, AJ, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, WL, Hori, Y, Howe, L, Inoue, Y, Irie, F, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, JP, Kazemzadeh, K, Keating, BG, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, AT, Leon, D, Linder, EV, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Raum, CR, Rebeiz, GM, Reichardt, CL, Richards, PL, Ross, C, Rotermund, KM, Segawa, Y, Sherwin, BD, Shirley, I, Siritanasak, P, Steinmetz, L, Stompor, R, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, GP, Tikhomirov, A, Tomaru, T, Westbrook, B, Whitehorn, N, Zahn, A, and Zahn, O

Subjects
cosmic microwave background radiation, polarization, polarimeters, inflation, neutrinos, dark matter, dark energy, gravitational lensing
Abstract

The Simons Array is a next generation cosmic microwave background (CMB) polarization experiment whose science target is a precision measurement of the B-mode polarization pattern produced both by inflation and by gravitational lensing. As a continuation and extension of the successful POLARBEAR experimental program, the Simons Array will consist of three cryogenic receivers each featuring multichroic bolometer arrays mounted onto separate 3.5m telescopes. The first of these, also called POLARBEAR-2A, will be the first to deploy in late 2016 and has a large diameter focal plane consisting of dual-polarization dichroic pixels sensitive at 95 GHz and 150 GHz. The POLARBEAR-2A focal plane will utilize 7,588 antenna-coupled superconducting transition edge sensor (TES) bolometers read out with SQUID amplifiers using frequency domain multiplexing techniques. The next two receivers that will make up the Simons Array will be nearly identical in overall design but will feature extended frequency capability. The combination of high sensitivity, multichroic frequency coverage and large sky area available from our mid-latitude Chilean observatory will allow Simons Array to produce high quality polarization sky maps over a wide range of angular scales and to separate out the CMB B-modes from other astrophysical sources with high fidelity. After accounting for galactic foreground separation, the Simons Array will detect the primordial gravitational wave B-mode signal to r > 0.01 with a significance of > 5σ and will constrain the sum of neutrino masses to 40 meV (1σ) when cross-correlated with galaxy surveys. We present the current status of this funded experiment, its future, and discuss its projected science return.

Published
2016

22. A Measurement of the Cosmic Microwave Background B-Mode Polarization Power Spectrum at Sub-Degree Scales with POLARBEAR

Author

The POLARBEAR Collaboration, Ade, P. A. R., Akiba, Y., Anthony, A. E., Arnold, K., Atlas, M., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Flanigan, D., Gilbert, A., Grainger, W., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Howard, J., Hyland, P., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Leitch, E. M., Linder, E., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Poletti, D., Quealy, E., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Schanning, I., Schenck, D. E., Sherwin, B. D., Shimizu, A., Shimmin, C., Shimon, M., Siritanasak, P., Smecher, G., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Takakura, S., Tomaru, T., Wilson, B., Yadav, A., and Zahn, O.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We report a measurement of the B-mode polarization power spectrum in the cosmic microwave background (CMB) using the POLARBEAR experiment in Chile. The faint B-mode polarization signature carries information about the Universe's entire history of gravitational structure formation, and the cosmic inflation that may have occurred in the very early Universe. Our measurement covers the angular multipole range 500 < l < 2100 and is based on observations of an effective sky area of 25 square degrees with 3.5 arcmin resolution at 150 GHz. On these angular scales, gravitational lensing of the CMB by intervening structure in the Universe is expected to be the dominant source of B-mode polarization. Including both systematic and statistical uncertainties, the hypothesis of no B-mode polarization power from gravitational lensing is rejected at 97.1% confidence. The band powers are consistent with the standard cosmological model. Fitting a single lensing amplitude parameter A_BB to the measured band powers, A_BB = 1.12 +/- 0.61 (stat) +0.04/-0.12 (sys) +/- 0.07 (multi), where A_BB = 1 is the fiducial WMAP-9 LCDM value. In this expression, "stat" refers to the statistical uncertainty, "sys" to the systematic uncertainty associated with possible biases from the instrument and astrophysical foregrounds, and "multi" to the calibration uncertainties that have a multiplicative effect on the measured amplitude A_BB., Comment: 22 pages, 12 figures. v3 is updated to reflect the erratum published in ApJ 2017 848:73, which changed the rejection of the hypothesis of no B-mode polarization power from gravitational lensing from 97.2% to 97.1%

Published
2014
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23. POLARBEAR constraints on cosmic birefringence and primordial magnetic fields

Author

Ade, PAR, Arnold, K, Atlas, M, Baccigalupi, C, Barron, D, 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, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, NW, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, WL, Hori, Y, Howe, L, Inoue, Y, Jaehnig, GC, Jaffe, AH, Jeong, O, Katayama, N, Kaufman, JP, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, AT, Leitch, EM, Leon, D, Li, Y, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Montgomery, J, Myers, MJ, Navaroli, M, Nishino, H, Okamura, T, Paar, H, Peloton, J, Pogosian, L, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, CL, Richards, PL, Ross, C, Rotermund, KM, Schenck, DE, Sherwin, BD, Shimon, M, Shirley, I, Siritanasak, P, Smecher, G, Stebor, N, Steinbach, B, Suzuki, A, Suzuki, JI, Tajima, O, Takakura, S, Tikhomirov, A, Tomaru, T, Whitehorn, N, Wilson, B, Yadav, A, Zahn, A, and Zahn, O

Subjects
astro-ph.CO, Nuclear & Particles Physics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

We constrain anisotropic cosmic birefringence using four-point correlations of even-parity E-mode and odd-parity B-mode polarization in the cosmic microwave background measurements made by the POLARization of the Background Radiation (POLARBEAR) experiment in its first season of observations. We find that the anisotropic cosmic birefringence signal from any parity-violating processes is consistent with zero. The Faraday rotation from anisotropic cosmic birefringence can be compared with the equivalent quantity generated by primordial magnetic fields if they existed. The POLARBEAR nondetection translates into a 95% confidence level (C.L.) upper limit of 93 nanogauss (nG) on the amplitude of an equivalent primordial magnetic field inclusive of systematic uncertainties. This four-point correlation constraint on Faraday rotation is about 15 times tighter than the upper limit of 1380 nG inferred from constraining the contribution of Faraday rotation to two-point correlations of B-modes measured by Planck in 2015. Metric perturbations sourced by primordial magnetic fields would also contribute to the B-mode power spectrum. Using the POLARBEAR measurements of the B-mode power spectrum (two-point correlation), we set a 95% C.L. upper limit of 3.9 nG on primordial magnetic fields assuming a flat prior on the field amplitude. This limit is comparable to what was found in the Planck 2015 two-point correlation analysis with both temperature and polarization. We perform a set of systematic error tests and find no evidence for contamination. This work marks the first time that anisotropic cosmic birefringence or primordial magnetic fields have been constrained from the ground at subdegree scales.

Published
2015

24. Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum with the POLARBEAR experiment

Author

POLARBEAR Collaboration, Ade, P. A. R., Akiba, Y., Anthony, A. E., Arnold, K., Atlas, M., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Flanigan, D., Gilbert, A., Grainger, W., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Howard, J., Hyland, P., Inoue, Y., Jaehnig, G. C., Jaffe, A., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Linder, E., Leitch, E. M., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Quealy, E., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Schanning, I., Schenck, D. E., Sherwin, B., Shimizu, A., Shimmin, C., Shimon, M., Siritanasak, P., Smecher, G., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Takakura, S., Tomaru, T., Wilson, B., Yadav, A., and Zahn, O.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational lensing due to the large-scale distribution of matter in the cosmos distorts the primordial Cosmic Microwave Background (CMB) and thereby induces new, small-scale $B$-mode polarization. This signal carries detailed information about the distribution of all the gravitating matter between the observer and CMB last scattering surface. We report the first direct evidence for polarization lensing based on purely CMB information, from using the four-point correlations of even- and odd-parity $E$- and $B$-mode polarization mapped over $\sim30$ square degrees of the sky measured by the POLARBEAR experiment. These data were analyzed using a blind analysis framework and checked for spurious systematic contamination using null tests and simulations. Evidence for the signal of polarization lensing and lensing $B$-modes is found at 4.2$\sigma$ (stat.+sys.) significance. The amplitude of matter fluctuations is measured with a precision of $27\%$, and is found to be consistent with the Lambda Cold Dark Matter ($\Lambda$CDM) cosmological model. This measurement demonstrates a new technique, capable of mapping all gravitating matter in the Universe, sensitive to the sum of neutrino masses, and essential for cleaning the lensing $B$-mode signal in searches for primordial gravitational waves., Comment: 7 pages, 3 figures. Matches Physical Review Letters accepted version. Submitted on 11 March 2014; accepted on 25 April 2014. The companion paper (arXiv:1312.6645) describes a measurement of polarization lensing in cross-correlation

Published
2013
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25. Evidence for Gravitational Lensing of the Cosmic Microwave Background Polarization from Cross-correlation with the Cosmic Infrared Background

Author

POLARBEAR Collaboration, Ade, P. A. R., Akiba, Y., Anthony, A. E., Arnold, K., Atlas, M., Barron, D., Boettger, D., Borrill, J., Borys, C., Chapman, S., Chinone, Y., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Flanigan, D., Gilbert, A., Grainger, W., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Howard, J., Hyland, P., Inoue, Y., Jaehnig, G. C., Jaffe, A., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Leitch, E. M., Linder, E., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Quealy, E., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Rotermund, K., Schanning, I., Schenck, D. E., Sherwin, B. D., Shimizu, A., Shimmin, C., Shimon, M., Siritanasak, P., Smecher, G., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Takakura, S., Tikhomirov, A., Tomaru, T., Wilson, B., Yadav, A., and Zahn, O.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We reconstruct the gravitational lensing convergence signal from Cosmic Microwave Background (CMB) polarization data taken by the POLARBEAR experiment and cross-correlate it with Cosmic Infrared Background (CIB) maps from the Herschel satellite. From the cross-spectra, we obtain evidence for gravitational lensing of the CMB polarization at a statistical significance of 4.0$\sigma$ and evidence for the presence of a lensing $B$-mode signal at a significance of 2.3$\sigma$. We demonstrate that our results are not biased by instrumental and astrophysical systematic errors by performing null-tests, checks with simulated and real data, and analytical calculations. This measurement of polarization lensing, made via the robust cross-correlation channel, not only reinforces POLARBEAR auto-correlation measurements, but also represents one of the early steps towards establishing CMB polarization lensing as a powerful new probe of cosmology and astrophysics., Comment: 6 pages, 2 figures. v2: replaced with version accepted for publication in Physical Review Letters. The companion paper (arXiv:1312.6646) describes a measurement of the polarization lensing power spectrum

Published
2013
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26. Deployment of Polarbear-2A

Author

Kaneko, Daisuke, Adachi, S., Ade, P. A. R., Aguilar Faúndez, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Dűnner, R., El-Bouhargani, H., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Ross, C., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tomaru, T., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.

Published
2020
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27. The bolometric focal plane array of the Polarbear CMB experiment

Author

Arnold, K., Ade, P. A. R., Anthony, A. E., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M. A., Errard, J., Fabbian, G., Flanigan, D., Fuller, G., Ghribi, A., Grainger, W., Halverson, N., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Howard, J., Hyland, P., Jaffe, A., Keating, B., Kermish, Z., Kisner, T., Jeune, M. Le, Lee, A. T., Linder, E., Lungu, M., Matsuda, F., Matsumura, T., Miller, N. J., Meng, X., Morii, H., Moyerman, S., Myers, M. J., Nishino, H., Paar, H., Quealy, E., Reichardt, C., Richards, P. L., Ross, C., Shimizu, A., Shimmin, C., Shimon, M., Sholl, M., Siritanasak, P., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Tomaru, T., Tucker, C., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Polarbear Cosmic Microwave Background (CMB) polarization experiment is currently observing from the Atacama Desert in Northern Chile. It will characterize the expected B-mode polarization due to gravitational lensing of the CMB, and search for the possible B-mode signature of inflationary gravitational waves. Its 250 mK focal plane detector array consists of 1,274 polarization-sensitive antenna-coupled bolometers, each with an associated lithographed band-defining filter. Each detector's planar antenna structure is coupled to the telescope's optical system through a contacting dielectric lenslet, an architecture unique in current CMB experiments. We present the initial characterization of this focal plane.

Published
2012
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28. The POLARBEAR Experiment

Author

Kermish, Z., Ade, P., Anthony, A., Arnold, K., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M. A., Errard, J., Fabbian, G., Flanigan, D., Fuller, G., Ghribi, A., Grainger, W., Halverson, N., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Howard, J., Hyland, P., Jaffe, A., Keating, B., Kisner, T., Lee, A. T., Jeune, M. Le, Linder, E., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Nishino, H., Paar, H., Quealy, E., Reichardt, C. L., Richards, P. L., Ross, C., Shimizu, A., Shimon, M., Shimmin, C., Sholl, M., Siritanasak, P., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Tomaru, T., Tucker, C., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present the design and characterization of the POLARBEAR experiment. POLARBEAR will measure the polarization of the cosmic microwave background (CMB) on angular scales ranging from the experiment's 3.5 arcminute beam size to several degrees. The experiment utilizes a unique focal plane of 1,274 antenna-coupled, polarization sensitive TES bolometers cooled to 250 milliKelvin. Employing this focal plane along with stringent control over systematic errors, POLARBEAR has the sensitivity to detect the expected small scale B-mode signal due to gravitational lensing and search for the large scale B-mode signal from inflationary gravitational waves. POLARBEAR was assembled for an engineering run in the Inyo Mountains of California in 2010 and was deployed in late 2011 to the Atacama Desert in Chile. An overview of the instrument is presented along with characterization results from observations in Chile., Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, July 6, 2012. To be published in Proceedings of SPIE Volume 8452

Published
2012
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29. Ultra High Energy Cosmology with POLARBEAR

Author

Keating, B., Moyerman, S., Boettger, D., Edwards, J., Fuller, G., Matsuda, F., Miller, N., Paar, H., Rebeiz, G., Schanning, I., Shimon, M., Stebor, N., Arnold, K., Flanigan, D., Holzapfel, W., Howard, J., Kermish, Z., Lee, A., Lungu, M., Myers, M., Nishino, H., O'Brient, R., Quealy, E., Reichardt, C., Richards, P., Shimmin, C., Steinbach, B., Suzuki, A., Zahn, O., Borrill, J., Cantalupo, C., Kisner, E., Linder, E., Sholl, M., Spieler, H., Anthony, A., Halverson, N., Errard, J., Fabbian, G., Jeune, M. Le, Stompor, R., Jaffe, A., O'Dea, D., Chinone, Y., Hasegawa, M., Hazumi, M., Matsumura, T., Morii, H., Shimizu, A., Tomaru, T., Hyland, P., Dobbs, M., Ade, P., Grainger, W., and Tucker, C.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

Observations of the temperature anisotropy of the Cosmic Microwave Background (CMB) lend support to an inflationary origin of the universe, yet no direct evidence verifying inflation exists. Many current experiments are focussing on the CMB's polarization anisotropy, specifically its curl component (called "B-mode" polarization), which remains undetected. The inflationary paradigm predicts the existence of a primordial gravitational wave background that imprints a unique B-mode signature on the CMB's polarization at large angular scales. The CMB B-mode signal also encodes gravitational lensing information at smaller angular scales, bearing the imprint of cosmological large scale structures (LSS) which in turn may elucidate the properties of cosmological neutrinos. The quest for detection of these signals; each of which is orders of magnitude smaller than the CMB temperature anisotropy signal, has motivated the development of background-limited detectors with precise control of systematic effects. The POLARBEAR experiment is designed to perform a deep search for the signature of gravitational waves from inflation and to characterize lensing of the CMB by LSS. POLARBEAR is a 3.5 meter ground-based telescope with 3.8 arcminute angular resolution at 150 GHz. At the heart of the POLARBEAR receiver is an array featuring 1274 antenna-coupled superconducting transition edge sensor (TES) bolometers cooled to 0.25 Kelvin. POLARBEAR is designed to reach a tensor-to-scalar ratio of 0.025 after two years of observation -- more than an order of magnitude improvement over the current best results, which would test physics at energies near the GUT scale. POLARBEAR had an engineering run in the Inyo Mountains of Eastern California in 2010 and will begin observations in the Atacama Desert in Chile in 2011., Comment: 8 pages, 6 figures, DPF 2011 conference proceedings

Published
2011

30. The new generation CMB B-mode polarization experiment: POLARBEAR

Author

The Polarbear Collaboration, Errard, J., Ade, P. A. R., Anthony, A., Arnold, K., Aubin, F., Boettger, D., Borrill, J., Cantalupo, C., Dobbs, M. A., Flanigan, D., Ghribi, A., Halverson, N., Hazumi, M., Holzapfel, W. L., Howard, J., Hyland, P., Jaffe, A., Keating, B., Kisner, T., Kermish, Z., Lee, A. T., Linder, E., Lungu, M., Matsumura, T., Miller, N., Meng, X., Myers, M., Nishino, H., O'Brient, R., O'Dea, D., Reichardt, C., Schanning, I., Shimizu, A., Shimmin, C., Shimon, M., Spieler, H., Steinbach, B., Stompor, R., Suzuki, A., Tomaru, T., Tran, H. T., Tucker, C., Quealy, E., Richards, P. L., and Zahn, O.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We describe the Cosmic Microwave Background (CMB) polarization experiment called Polarbear. This experiment will use the dedicated Huan Tran Telescope equipped with a powerful 1,200-bolometer array receiver to map the CMB polarization with unprecedented accuracy. We summarize the experiment, its goals, and current status.

Published
2010

31. The POLARBEAR Cosmic Microwave Background Polarization Experiment

Author

Barron, D, Ade, P, Anthony, A, Arnold, K, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Dobbs, M, Edwards, J, Errard, J, Fabbian, G, Flanigan, D, Fuller, G, Ghribi, A, Grainger, W, Halverson, N, Hasegawa, M, Hattori, K, Hazumi, M, Holzapfel, W, Howard, J, Hyland, P, Jaehnig, G, Jaffe, A, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Lee, AT, Le Jeune, M, Linder, E, Lungu, M, Matsuda, F, Matsumura, T, Meng, X, Miller, NJ, Morii, H, Moyerman, S, Myers, M, Nishino, H, Paar, H, Peloton, J, Quealy, E, Rebeiz, G, Reichardt, CL, Richards, PL, Ross, C, Shimizu, A, Shimmin, C, Shimon, M, Sholl, M, Siritanasak, P, Spieler, H, Stebor, N, Steinbach, B, Stompor, R, Suzuki, A, Tomaru, T, Tucker, C, Yadav, A, and Zahn, O

Subjects
Particle and High Energy Physics, Physical Sciences, Cosmic microwave background, CMB polarization, Millimeter-wave, Mathematical Physics, Classical Physics, Condensed Matter Physics, General Physics, Classical physics, Condensed matter physics
Abstract

The polarbear cosmic microwave background (CMB) polarization experiment has been observing since early 2012 from its 5,200 m site in the Atacama Desert in Northern Chile. polarbear's measurements will characterize the expected CMB polarization due to gravitational lensing by large scale structure, and search for the possible B-mode polarization signature of inflationary gravitational waves. polarbear's 250 mK focal plane detector array consists of 1,274 polarization-sensitive antenna-coupled bolometers, each with an associated lithographed band-defining filter and contacting dielectric lenslet, an architecture unique in current CMB experiments. The status of the polarbear instrument, its focal plane, and the analysis of its measurements are presented. © 2014 Springer Science+Business Media New York.

Published
2014

32. The POLARBEAR experiment

Author

Kermish, ZD, Ade, P, Anthony, A, Arnold, K, Barron, D, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Dobbs, MA, Errard, J, Fabbian, G, Flanigan, D, Fuller, G, Ghribi, A, Grainger, W, Halverson, N, Hasegawa, M, Hattori, K, Hazumi, M, Holzapfel, WL, Howard, J, Hyland, P, Jaffe, A, Keating, B, Kisner, T, Lee, AT, Le Jeune, M, Linder, E, Lungu, M, Matsuda, F, Matsumura, T, Meng, X, Miller, NJ, Morii, H, Moyerman, S, Myers, MJ, Nishino, H, Paar, H, Quealy, E, Reichardt, CL, Richards, PL, Ross, C, Shimizu, A, Shimon, M, Shimmin, C, Sholl, M, Siritanasak, P, Spieler, H, Stebor, N, Steinbach, B, Stompor, R, Suzuki, A, Tomaru, T, Tucker, C, and Zahn, O

Subjects
Cosmic Microwave Background, Inflation, Polarization, Bolometer, astro-ph.IM
Abstract

We present the design and characterization of the polarbear experiment. polarbear will measure the polarization of the cosmic microwave background (CMB) on angular scales ranging from the experiment's 3.5′ beam size to several degrees. The experiment utilizes a unique focal plane of 1,274 antenna-coupled, polarization sensitive TES bolometers cooled to 250 milliKelvin. Employing this focal plane along with stringent control over systematic errors, polarbear has the sensitivity to detect the expected small scale B-mode signal due to gravitational lensing and search for the large scale B-mode signal from inflationary gravitational waves. polarbear was assembled for an engineering run in the Inyo Mountains of California in 2010 and was deployed in late 2011 to the Atacama Desert in Chile. An overview of the instrument is presented along with characterization results from observations in Chile. © 2012 SPIE.

Published
2012

33. The new generation CMB B-mode polarization experiment: POLARBEAR

Author

Collaboration, The Polarbear, Errard, J, Ade, PAR, Anthony, A, Arnold, K, Aubin, F, Boettger, D, Borrill, J, Cantalupo, C, Dobbs, MA, Flanigan, D, Ghribi, A, Halverson, N, Hazumi, M, Holzapfel, WL, Howard, J, Hyland, P, Jaffe, A, Keating, B, Kisner, T, Kermish, Z, Lee, AT, Linder, E, Lungu, M, Matsumura, T, Miller, N, Meng, X, Myers, M, Nishino, H, O'Brient, R, O'Dea, D, Reichardt, C, Schanning, I, Shimizu, A, Shimmin, C, Shimon, M, Spieler, H, Steinbach, B, Stompor, R, Suzuki, A, Tomaru, T, Tran, HT, Tucker, C, Quealy, E, Richards, PL, and Zahn, O

Subjects
astro-ph.IM, astro-ph.CO
Abstract

We describe the Cosmic Microwave Background (CMB) polarization experimentcalled Polarbear. This experiment will use the dedicated Huan Tran Telescopeequipped with a powerful 1,200-bolometer array receiver to map the CMBpolarization with unprecedented accuracy. We summarize the experiment, itsgoals, and current status.

Published
2010

34. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author

Chinone, Y, primary, Adachi, S, additional, Ade, PAR, additional, Aguilar, M, additional, Akiba, Y, additional, Arnold, K, additional, Baccigalupi, C, additional, Barron, D, additional, Beck, D, additional, Beckman, S, additional, Bianchini, F, additional, Boettger, D, additional, Borrill, J, additional, ElBouhargani, H, additional, Carron, J, additional, Chapman, S, additional, Cheung, K, additional, Crowley, K, additional, Cukierman, A, additional, Dünner, R, additional, Dobbs, M, additional, Ducout, A, additional, Elleflot, T, additional, Errard, J, additional, Fabbian, G, additional, Feeney, S M, additional, Feng, C, additional, Fujino, T, additional, Galitzki, N, additional, Gilbert, A, additional, Goeckner-Wald, N, additional, Groh, J, additional, Groh, J C, additional, Hall, G, additional, Halverson, N, additional, Hamada, T, additional, Hasegawa, M, additional, Hazumi, M, additional, Hill, C A, additional, Howe, L, additional, Inoue, Y, additional, Jaehnig, G, additional, Jaffe, A H, additional, Jeong, O, additional, LeJeune, M, additional, Kaneko, D, additional, Katayama, N, additional, Keating, B, additional, Keskitalo, R, additional, Kikuchi, S, additional, Kisner, T, additional, Krachmalnicoff, N, additional, Kusaka, A, additional, Lee, A T, additional, Leitch, E M, additional, Leon, D, additional, Linder, E, additional, Lowry, L N, additional, Mangu, A, additional, Matsuda, F, additional, Matsumura, T, additional, Minami, Y, additional, Montgomery, J, additional, Navaroli, M, additional, Nishino, H, additional, Paar, H, additional, Peloton, J, additional, Pham, ATP, additional, Poletti, D, additional, Puglisi, G, additional, Reichardt, C L, additional, Richards, P L, additional, Ross, C, additional, Segawa, Y, additional, Sherwin, B D, additional, Silva-Feaver, M, additional, Siritanasak, P, additional, Stebor, N, additional, Stompor, R, additional, Suzuki, A, additional, Tajima, O, additional, Takakura, S, additional, Takatori, S, additional, Tanabe, D, additional, Teply, G P, additional, Tomaru, T, additional, Tsai, C, additional, Tucker, C, additional, Verges, C, additional, Westbrook, B, additional, Whitehorn, N, additional, Zahn, A, additional, and Zhou, Y, additional

Published
2020
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36. Kolmogorov-Smirnov like test for time-frequency Fourier spectrogram analysis in LISA Pathfinder

Author

Errard, J., Ade, P., Akiba, Y., Arnold, K., Atlas, M., Baccigalupi, C., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Cukierman, A., Delabrouille, J., Dobbs, M., Ducout, A., Elleflot, T., Fabbian, G., Feng, C., Feeney, S., Gilbert, A., Goeckner-Wald, N., Halverson, N., Hasegawa, M., Hattori, K., Hazumi, M., Hill, C., Holzapfel, W., Hori, Y., Inoue, Y., Jaehnig, G., Jaffe, A., Jeong, O., Katayama, N., Kaufman, J., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A., Leitch, E., Leon, D., Linder, E., Matsuda, F., Matsumura, T., Miller, N., Myers, M., Navaroli, M., Nishino, H., Okamura, T., Paar, H., Peloton, J., Poletti, D., Rebeiz, G., Reichardt, C., Richards, P., Ross, C., Rotermund, K., Schenck, D., Sherwin, B., Siritanasak, P., Smecher, G., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Tikhomirov, A., Tomaru, T., Whitehorn, N., Wilson, B., Yadav, A., Zahn, O., Ferraioli, Luigi, Armano, Michele, Audley, Heather, Congedo, Giuseppe, Diepholz, Ingo, Gibert, Ferran, Hewitson, Martin, Hueller, Mauro, Karnesis, Nikolaos, Korsakova, Natalia, Nofrarías, Miquel, Plagnol, Eric, Vitale, Stefano, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Department of Geological Sciences [BYU], Brigham Young University (BYU), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Queen Mary University of London (QMUL), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, McGill University = Université McGill [Montréal, Canada], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Mathematics Research Institute, School of Engineering, Computing and Mathematics, University of Exeter, Advanced Fusion Research Center, Kyushu University-Research Institute for Applied Mechanics, RIKEN IFREQ, National Astronomical Observatory of Japan (NAOJ), Imperial College London, Department of Advanced Materials, University of Tokyo, Department of Advanced Materials, PowerTech Labs, California Institute of Technology (CALTECH), Department of surgery and cancer - Faculty of medecine, KEK (High energy accelerator research organization), Dept. of Physics, University of Wisconsin-Madison, Institute for Advanced Study [Princeton] (IAS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre de Recerca en Sanitat Animal (CReSA), Department of Physics and INFN, University of Trento [Trento], Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Kyushu University [Fukuoka]-Research Institute for Applied Mechanics, Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), McGill University, High Energy Accelerator Research Organization (KEK), University of Tsukuba, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Computer science, Monte Carlo method, Kolmogorov–Smirnov test, Noise analysis, 01 natural sciences, LISA Pathfinder, Synthetic data, Gravitational waves, symbols.namesake, Time-frequency map, 0103 physical sciences, Test statistic, 010306 general physics, Spectrogram, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], LISA, 010308 nuclear & particles physics, eLISA, Astronomy and Astrophysics, Time–frequency analysis, Kolmogorov-Smirnov test, Noise, Pathfinder, Space and Planetary Science, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm
Abstract

A statistical procedure for the analysis of time-frequency noise maps is presented and applied to LISA Pathfinder mission synthetic data. The procedure is based on the Kolmogorov-Smirnov like test that is applied to the analysis of time-frequency noise maps produced with the spectrogram technique. The influence of the finite size windowing on the statistic of the test is calculated with a Monte Carlo simulation for 4 different windows type. Such calculation demonstrate that the test statistic is modified by the correlations introduced in the spectrum by the finite size of the window and by the correlations between different time bins originated by overlapping between windowed segments. The application of the test procedure to LISA Pathfinder data demonstrates the test capability of detecting non-stationary features in a noise time series that is simulating low frequency non-stationary noise in the system., Experimental Astronomy, 39 (1), ISSN:0922-6435, ISSN:1572-9508

Published
2014

37. ENDEAVOUR:Towards a flexible software-defined network ecosystem: Implementation of the Monitoring Platform

Author

Fernandes, Eder Leao, Boettger, D., Antichi, Gianni, Lapeyrade, Rémy, Owezarski, Philippe, Queen Mary University of London (QMUL), Computer Laboratory [Cambridge], University of Cambridge [UK] (CAM), Équipe Services et Architectures pour Réseaux Avancés (LAAS-SARA), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Queen Mary University london, University of Cambridge, LAAS-CNRS, European Project: 644960,H2020,H2020-ICT-2014-1,ENDEAVOUR(2015), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), and Université de Toulouse (UT)

Subjects
[INFO.INFO-NI]Computer Science [cs]/Networking and Internet Architecture [cs.NI], ComputingMilieux_THECOMPUTINGPROFESSION
Abstract

This is the accompanying report of the demonstrator of Work Package 3 for month 24, where the implementation of the ENDEAVOUR monitoring platform is documented. In this report, we briefly discuss the organization of the code development, we then describe the implementation of the ele- ments of the ENDEAVOUR monitoring platform, and finally, present and document the demonstrators.

Published
2017

38. A Measurement of the Cosmic Microwave Background $B$-Mode Polarization Power Spectrum at Sub-Degree Scales from 2 years of POLARBEAR Data

Author

Polarbear, The Collaboration, Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Ducout, A., Dünner, R., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hamada, T., Hall, G., Halverson, N. W., Hasegawa, M., Hazumi, M., Hill, C., Howe, L., Inoue, Y., Jaehnig, G. C., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Le Jeune, M., Lee, A. T., Leitch, E. M., Leon, D., Linder, E., Lowry, L., Matsuda, F., Matsumura, T., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Richards, P. L., Ross, C., Segawa, Y., Sherwin, B. D., Silva, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tomaru, T., Carole Tucker, Whitehorn, N., Zahn, A., AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), POLARBEAR, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'astrophysique spatiale ( IAS ), and Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
large-scale structure of universe, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, cosmic background radiation, gravitation: lens, cosmology: observations, cosmic background radiation: multipole, polarization: power spectrum, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report an improved measurement of the cosmic microwave background (CMB) $B$-mode polarization power spectrum with the POLARBEAR experiment at 150 GHz. By adding new data collected during the second season of observations (2013-2014) to re-analyzed data from the first season (2012-2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles $500 \leq \ell \leq 2100$, where the dominant $B$-mode signal is expected to be due to the gravitational lensing of $E$-modes. We reject the null hypothesis of no $B$-mode polarization at a confidence of 3.1$\sigma$ including both statistical and systematic uncertainties. We test the consistency of the measured $B$-modes with the $\Lambda$ Cold Dark Matter ($\Lambda$CDM) framework by fitting for a single lensing amplitude parameter $A_L$ relative to the Planck best-fit model prediction. We obtain $A_L = 0.60 ^{+0.26} _{-0.24} ({\rm stat}) ^{+0.00} _{-0.04}({\rm inst}) \pm 0.14 ({\rm foreground}) \pm 0.04 ({\rm multi})$, where $A_{L}=1$ is the fiducial $\Lambda$CDM value, and the details of the reported uncertainties are explained later in the manuscript., Comment: 16 pages, 10 figures. Minor changes to match the published version. For data and figures, see http://bolo.berkeley.edu/polarbear/data/polarbear_BB_2017/

Published
2017

39. A Measurement of the Degree-scale CMB B-mode Angular Power Spectrum with Polarbear.

Author

tion, Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., El Bouhargani, H., and Elleflot, T.

Subjects
COSMIC background radiation, POWER spectra
Abstract

We present a measurement of the B-mode polarization power spectrum of the cosmic microwave background (CMB) using data taken from 2014 July to 2016 December with the Polarbear experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of on a 670 square degree patch of sky centered at (R.A., decl.) = (+0h12m0s, −59°18′). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve 32 μK arcmin effective polarization map noise with a knee in sensitivity of ℓ = 90, where the inflationary gravitational-wave signal is expected to peak. The measured B-mode power spectrum is consistent with a ΛCDM lensing and single dust component foreground model over a range of multipoles 50 ≤ ℓ ≤ 600. The data disfavor zero at 2.2σ using this ℓ range of Polarbear data alone. We cross-correlate our data with Planck full mission 143, 217, and 353 GHz frequency maps and find the low-ℓ B-mode power in the combined data set to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio r < 0.90 at the 95% confidence level after marginalizing over foregrounds. [ABSTRACT FROM AUTHOR]

Published
2020
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40. Electrical characterization and tuning of the integrated POLARBEAR-2a focal plane and readout (Conference Presentation)

Author

Barron, Darcy, primary, Arnold, Kam, additional, Elleflot, Tucker, additional, Groh, John C., additional, Kaneko, Daisuke, additional, Katayama, Nobuhiko, additional, Lee, Adrian T., additional, Lowry, Lindsay N., additional, Nishino, Haruki, additional, Suzuki, Aritoki, additional, Takatori, Sayuri, additional, Ade, P., additional, Akiba, Y., additional, Ali, A., additional, Aguilar, M., additional, Anderson, A., additional, Ashton, P., additional, Avva, J., additional, Beck, D., additional, Baccigalupi, C., additional, Beckman, S., additional, Bender, A., additional, Bianchini, F., additional, Boettger, D., additional, Borrill, J., additional, Carron, J., additional, Chapman, S., additional, Chinone, Y., additional, Coppi, G., additional, Crowley, K., additional, Cukierman, A., additional, de Haan, T., additional, Dobbs, M., additional, Dunner, R., additional, Errard, J., additional, Fabbian, G., additional, Feeney, S., additional, Feng, C., additional, Fuller, G., additional, Galitzki, N., additional, Gilbert, A., additional, Goeckner-Wald, N., additional, Hamada, T., additional, Halverson, N., additional, Hasegawa, M., additional, Hazumi, M., additional, Hill, C., additional, Holzapfel, W., additional, Howe, L., additional, Inoue, Y., additional, Ito, J., additional, Jaehnig, G., additional, Jeong, O., additional, Keating, B., additional, Keskitalo, R., additional, Kisner, T., additional, Krachmalnicoff, N., additional, Kusaka, A., additional, Le Jeune, M., additional, Leon, D., additional, Linder, E., additional, Lowitz, A., additional, Madurowicz, A., additional, Mak, D., additional, Matsuda, F., additional, Matsumura, T., additional, May, A., additional, Miller, N., additional, Minami, Y., additional, Montgomery, J., additional, Natoli, T., additional, Navroli, M., additional, Peloton, J., additional, Pham, A., additional, Piccirillo, L., additional, Plambeck, D., additional, Poletti, D., additional, Puglisi, G., additional, Raum, C., additional, Rebeiz, G., additional, Reichardt, C., additional, Richards, P., additional, Roberts, H., additional, Ross, C., additional, Rotermund, K., additional, Silva Feaver, Max, additional, Segawa, Y., additional, Sherwin, B., additional, Siritanasak, P., additional, Steinmetz, L., additional, Stompor, R., additional, Tajima, O., additional, Takakura, S., additional, Tanabe, D., additional, Tat, R., additional, Teply, G., additional, Tikhomirov, A., additional, Tomaru, T., additional, Tsai, C., additional, Verges, C., additional, Westbrook, B., additional, Whitehorn, N., additional, and Zahn, A., additional

Published
2018
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41. Erratum: “A Measurement of the Cosmic Microwave Background B-Mode Polarization Power Spectrum at Sub-degree Scales with POLARBEAR” (2014, ApJ, 794, 171)

Author

P. A. R. Ade, The Polarbear Collaboration:, primary, Akiba, Y., additional, Anthony, A. E., additional, Arnold, K., additional, Atlas, M., additional, Barron, D., additional, Boettger, D., additional, Borrill, J., additional, Chapman, S., additional, Chinone, Y., additional, Dobbs, M., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feng, C., additional, Flanigan, D., additional, Gilbert, A., additional, Grainger, W., additional, Halverson, N. W., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Holzapfel, W. L., additional, Hori, Y., additional, Howard, J., additional, Hyland, P., additional, Inoue, Y., additional, Jaehnig, G. C., additional, Jaffe, A. H., additional, Keating, B., additional, Kermish, Z., additional, Keskitalo, R., additional, Kisner, T., additional, Jeune, M. Le, additional, Lee, A. T., additional, Leitch, E. M., additional, Linder, E., additional, Lungu, M., additional, Matsuda, F., additional, Matsumura, T., additional, Meng, X., additional, Miller, N. J., additional, Morii, H., additional, Moyerman, S., additional, Myers, M. J., additional, Navaroli, M., additional, Nishino, H., additional, Orlando, A., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Quealy, E., additional, Rebeiz, G., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Schanning, I., additional, Schenck, D. E., additional, Sherwin, B. D., additional, Shimizu, A., additional, Shimmin, C., additional, Shimon, M., additional, Siritanasak, P., additional, Smecher, G., additional, Spieler, H., additional, Stebor, N., additional, Steinbach, B., additional, Stompor, R., additional, Suzuki, A., additional, Takakura, S., additional, Tomaru, T., additional, Wilson, B., additional, Yadav, A., additional, and Zahn, O., additional

Published
2017
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43. Measurement of the cosmic microwave background polarization lensing power spectrum with the POLARBEAR experiment

Author

POLARBEAR Collaboration, Ade, P. A. R., Akiba, Y., Anthony, A. E., Arnold, K., Atlas, M., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Flanigan, D., Gilbert, A., Grainger, W., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Howard, J., Hyland, P., Inoue, Y., Jaehnig, G. C., Jaffe, A., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Jeune, M. Le, Lee, A. T., Linder, E., Leitch, E. M., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Quealy, E., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Schanning, I., Schenck, D. E., Sherwin, B., Shimizu, A., Shimmin, C., Shimon, M., Siritanasak, P., Smecher, G., Spieler, H., Stebor, N., Steinbach, B., Stompor, R., Suzuki, A., Takakura, S., Tomaru, T., Wilson, B., Yadav, A., Zahn, O., Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Queen Mary University of London (QMUL), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cavendish Laboratory, University of Cambridge [UK] (CAM), Advanced Fusion Research Center, Kyushu University [Fukuoka]-Research Institute for Applied Mechanics, RIKEN IFREQ, National Astronomical Observatory of Japan (NAOJ), National Institute for Laser, Plasma and Radiation Physics (INFLPR), Department of Applied Chemistry (Faculty of Engineering, Hiroshima University), Hiroshima University, National Institute for Environmental Studies (NIES), McGill University = Université McGill [Montréal, Canada], Institute for Advanced Study [Princeton] (IAS), Dalhousie University [Halifax], Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), The University of Tokyo (UTokyo), University of California [San Diego] (UC San Diego), University of California, POLARBEAR, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California (UC), and The University of Tokyo

Subjects
Physics, [PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, Cosmic microwave background, Strong gravitational lensing, Dark matter, Gravitational lensing formalism, FOS: Physical sciences, General Physics and Astronomy, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Gravitational lens, 13. Climate action, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Weak gravitational lensing, ComputingMilieux_MISCELLANEOUS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational lensing due to the large-scale distribution of matter in the cosmos distorts the primordial Cosmic Microwave Background (CMB) and thereby induces new, small-scale $B$-mode polarization. This signal carries detailed information about the distribution of all the gravitating matter between the observer and CMB last scattering surface. We report the first direct evidence for polarization lensing based on purely CMB information, from using the four-point correlations of even- and odd-parity $E$- and $B$-mode polarization mapped over $\sim30$ square degrees of the sky measured by the POLARBEAR experiment. These data were analyzed using a blind analysis framework and checked for spurious systematic contamination using null tests and simulations. Evidence for the signal of polarization lensing and lensing $B$-modes is found at 4.2$\sigma$ (stat.+sys.) significance. The amplitude of matter fluctuations is measured with a precision of $27\%$, and is found to be consistent with the Lambda Cold Dark Matter ($\Lambda$CDM) cosmological model. This measurement demonstrates a new technique, capable of mapping all gravitating matter in the Universe, sensitive to the sum of neutrino masses, and essential for cleaning the lensing $B$-mode signal in searches for primordial gravitational waves., Comment: 7 pages, 3 figures. Matches Physical Review Letters accepted version. Submitted on 11 March 2014; accepted on 25 April 2014. The companion paper (arXiv:1312.6645) describes a measurement of polarization lensing in cross-correlation

Published
2014

44. Gravitational Lensing of Cosmic Microwave Background Polarization

Author

Ade, P. A. R., Akiba, Y., Anthony, A. E., Arnold, K., Barron, D., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feng, C., Flanigan, D., Gilbert, A., Grainger, W., Halverson, N. W., Hasegawa, M., Hattori, K., Hazumi, M., Holzapfel, W. L., Hori, Y., Howard, J., Hyland, P., Inoue, Y., Jaehnig, G. C., Jaffe, A., Keating, B., Kermish, Z., Keskitalo, R., Kisner, T., Le Jeune, M., Lee, A. T., Linder, E., Lungu, M., Matsuda, F., Matsumura, T., Meng, X., Miller, N. J., Morii, H., Moyerman, S., Myers, M. J., Navaroli, M., Nishino, H., Paar, H., Peloton, J., Quealy, E., Rebeiz, G., Reichardt, C. L., Richards, P. L., Ross, C., Schanning, I., Schenck, D. E., Sherwin, B., Shimizu, A., Shimmin, C., Shimon, M., Siritanasak, P., Smecher, G., Spieler, H., Stebor, N., Steinbach, B., Stompor, Radek, Suzuki, A., Takakura, S., Tomaru, T., Wilson, B., Yadav, A., Zahn, O., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, POLARBEAR, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

8 pages, 4 figures. The companion paper describes a measurement of polarization lensing in cross-correlation; Primary fluctuations in both temperature and polarization of the Cosmic Microwave Background (CMB) reflect the properties of the Universe from the Big Bang until the photons decoupled from matter 380,000 years later. These primary fluctuations are then lensed by large-scale structures (such as clusters of galaxies and filaments of dark matter), with the result that the distribution and properties of dark matter, including the masses of neutrinos, can be determined more accurately by extracting the lensing information than through studying the primary fluctuations alone. Polarization lensing can give cleaner, higher resolution results than temperature lensing. The correlation of lensed CMB polarization with large-scale structure, traced through the Cosmic Infrared Background, was recently detected; however, this correlation does not trace all structure and depends on the relationship between the infrared flux from the galaxies and the underlying mass distribution. Here we report the detection of gravitational lensing directly from CMB polarization measurements. With these data, we have made a census of essentially all structure integrated along the line of sight through the full depth of the observable Universe on 30 square degrees of the sky, and we find good agreement with expectations from the standard Lambda cold-dark matter cosmology.

Published
2013

45. POLARBEAR-2: an instrument for CMB polarization measurements

Author

Inoue, Y., additional, Ade, P., additional, Akiba, Y., additional, Aleman, C., additional, Arnold, K., additional, Baccigalupi, C., additional, Barch, B., additional, Barron, D., additional, Bender, A., additional, Boettger, D., additional, Borrill, J., additional, Chapman, S., additional, Chinone, Y., additional, Cukierman, A., additional, de Haan, T., additional, Dobbs, M. A., additional, Ducout, A., additional, Dünner, R., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feeney, S., additional, Feng, C., additional, Fuller, G., additional, Gilbert, A. J., additional, Goeckner-Wald, N., additional, Groh, J., additional, Hall, G., additional, Halverson, N., additional, Hamada, T., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Hill, C., additional, Holzapfel, W. L., additional, Hori, Y., additional, Howe, L., additional, Irie, F., additional, Jaehnig, G., additional, Jaffe, A., additional, Jeong, O., additional, Katayama, N., additional, Kaufman, J. P., additional, Kazemzadeh, K., additional, Keating, B. G., additional, Kermish, Z., additional, Keskitalo, R., additional, Kisner, T. S., additional, Kusaka, A., additional, Le Jeune, M., additional, Lee, A. T., additional, Leon, D., additional, Linder, E. V., additional, Lowry, L., additional, Matsuda, F., additional, Matsumura, T., additional, Miller, N., additional, Mizukami, K., additional, Montgomery, J., additional, Navaroli, M., additional, Nishino, H., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Puglisi, G., additional, Raum, C. R., additional, Rebeiz, G. M., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Rotermund, K. M., additional, Segawa, Y., additional, Sherwin, B. D., additional, Shirley, I., additional, Siritanasak, P., additional, Stebor, N., additional, Stompor, R., additional, Suzuki, J., additional, Suzuki, A., additional, Tajima, O., additional, Takada, S., additional, Takatori, S., additional, Teply, G. P., additional, Tikhomirov, A., additional, Tomaru, T., additional, Whitehorn, N., additional, Zahn, A., additional, and Zahn, O., additional

Published
2016
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46. The Simons Array CMB polarization experiment

Author

Stebor, N., additional, Ade, P., additional, Akiba, Y., additional, Aleman, C., additional, Arnold, K., additional, Baccigalupi, C., additional, Barch, B., additional, Barron, D., additional, Beckman, S., additional, Bender, A., additional, Boettger, D., additional, Borrill, J., additional, Chapman, S., additional, Chinone, Y., additional, Cukierman, A., additional, de Haan, T., additional, Dobbs, M., additional, Ducout, A., additional, Dunner, R., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feeney, S., additional, Feng, C., additional, Fujino, T., additional, Fuller, G., additional, Gilbert, A. J., additional, Goeckner-Wald, N., additional, Groh, J., additional, Hall, G., additional, Halverson, N., additional, Hamada, T., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Hill, C., additional, Holzapfel, W. L., additional, Hori, Y., additional, Howe, L., additional, Inoue, Y., additional, Irie, F., additional, Jaehnig, G., additional, Jaffe, A., additional, Jeong, O., additional, Katayama, N., additional, Kaufman, J. P., additional, Kazemzadeh, K., additional, Keating, B. G., additional, Kermish, Z., additional, Keskitalo, R., additional, Kisner, T., additional, Kusaka, A., additional, Le Jeune, M., additional, Lee, A. T., additional, Leon, D., additional, Linder, E. V., additional, Lowry, L., additional, Matsuda, F., additional, Matsumura, T., additional, Miller, N., additional, Montgomery, J., additional, Navaroli, M., additional, Nishino, H., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Puglisi, G., additional, Raum, C. R., additional, Rebeiz, G. M., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Rotermund, K. M., additional, Segawa, Y., additional, Sherwin, B. D., additional, Shirley, I., additional, Siritanasak, P., additional, Steinmetz, L., additional, Stompor, R., additional, Suzuki, A., additional, Tajima, O., additional, Takada, S., additional, Takatori, S., additional, Teply, G. P., additional, Tikhomirov, A., additional, Tomaru, T., additional, Westbrook, B., additional, Whitehorn, N., additional, Zahn, A., additional, and Zahn, O., additional

Published
2016
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47. A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION WITH POLARBEAR

Author

ADE, P.A.R., primary, AKIBA, Y., additional, ANTHONY, A.E., additional, ARNOLD, K., additional, ATLAS, M., additional, BARRON, D., additional, BOETTGER, D., additional, BORRILL, J., additional, CHAPMAN, S., additional, CHINONE, Y., additional, DOBBS, M., additional, ELLEFLOT, T., additional, ERRARD, J., additional, FABBIAN, G., additional, FENG, C., additional, FLANIGAN, D., additional, GILBERT, A., additional, GRAINGER, W., additional, HALVERSON, N.W., additional, HASEGAWA, M., additional, HATTORI, K., additional, HAZUMI, M., additional, HOLZAPFEL, W.L., additional, HORI, Y., additional, HOWARD, J., additional, HYLAND, P., additional, INOUE, Y., additional, JAEHNIG, G.C., additional, JAFFE, A.H., additional, KEATING, B., additional, KERMISH, Z., additional, KESKITALO, R., additional, KISNER, T., additional, JEUNE, M. LE, additional, LEE, A.T., additional, LEITCH, E.M., additional, LINDER, E., additional, LUNGU, M., additional, MATSUDA, F., additional, MATSUMURA, T., additional, MENG, X., additional, MILLER, N.J., additional, MORII, H., additional, MOYERMAN, S., additional, MYERS, M.J., additional, NAVAROLI, M., additional, NISHINO, H., additional, ORLANDO, A., additional, PAAR, H., additional, PELOTON, J., additional, POLETTI, D., additional, QUEALY, E., additional, and REBEIZ, G., additional

Published
2015
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48. A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUNDB-MODE POLARIZATION POWER SPECTRUM AT SUB-DEGREE SCALES WITH POLARBEAR

Author

P. A. R. Ade, The Polarbear Collaboration:, primary, Akiba, Y., additional, Anthony, A. E., additional, Arnold, K., additional, Atlas, M., additional, Barron, D., additional, Boettger, D., additional, Borrill, J., additional, Chapman, S., additional, Chinone, Y., additional, Dobbs, M., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feng, C., additional, Flanigan, D., additional, Gilbert, A., additional, Grainger, W., additional, Halverson, N. W., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Holzapfel, W. L., additional, Hori, Y., additional, Howard, J., additional, Hyland, P., additional, Inoue, Y., additional, Jaehnig, G. C., additional, Jaffe, A. H., additional, Keating, B., additional, Kermish, Z., additional, Keskitalo, R., additional, Kisner, T., additional, Le Jeune, M., additional, Lee, A. T., additional, Leitch, E. M., additional, Linder, E., additional, Lungu, M., additional, Matsuda, F., additional, Matsumura, T., additional, Meng, X., additional, Miller, N. J., additional, Morii, H., additional, Moyerman, S., additional, Myers, M. J., additional, Navaroli, M., additional, Nishino, H., additional, Orlando, A., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Quealy, E., additional, Rebeiz, G., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Schanning, I., additional, Schenck, D. E., additional, Sherwin, B. D., additional, Shimizu, A., additional, Shimmin, C., additional, Shimon, M., additional, Siritanasak, P., additional, Smecher, G., additional, Spieler, H., additional, Stebor, N., additional, Steinbach, B., additional, Stompor, R., additional, Suzuki, A., additional, Takakura, S., additional, Tomaru, T., additional, Wilson, B., additional, Yadav, A., additional, and Zahn, O., additional

Published
2014
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49. Thermal and optical characterization for POLARBEAR-2 optical system

Author

Inoue, Y., additional, Stebor, N., additional, Ade, P. A. R., additional, Akiba, Y., additional, Arnold, K., additional, Anthony, A. E., additional, Atlas, M., additional, Barron, D., additional, Bender, A., additional, Boettger, D., additional, Borrilll, J., additional, Chapman, S., additional, Chinone, Y., additional, Cukierman, A., additional, Dobbs, M., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feng, C., additional, Gilbert, A., additional, Halverson, N. W., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Holzapfel, W. L., additional, Hori, Y., additional, Jaehnig, G. C., additional, Jaffe, A. H., additional, Katayama, N., additional, Keating, B., additional, Kermish, Z., additional, Keskitalo, Reijo, additional, Kisner, T., additional, Le Jeune, M., additional, Lee, A. T., additional, Leitch, E. M., additional, Linder, E., additional, Matsuda, F., additional, Matsumura, T., additional, Meng, X., additional, Morii, H., additional, Myers, M. J., additional, Navaroli, M., additional, Nishino, H., additional, Okamura, T., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Rebeiz, G., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Schenck, D. E., additional, Sherwin, B. D., additional, Siritanasak, P., additional, Smecher, G., additional, Sholl, M., additional, Steinbach, B., additional, Stompor, R., additional, Suzuki, A., additional, Suzuki, J., additional, Takada, S., additional, Takakura, S., additional, Tomaru, T., additional, Wilson, B., additional, Yadav, A., additional, Yamaguchi, H., additional, and Zahn, O., additional

Published
2014
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50. The Simons Array: expanding POLARBEAR to three multi-chroic telescopes

Author

Arnold, K., additional, Stebor, N., additional, Ade, P. A. R., additional, Akiba, Y., additional, Anthony, A. E., additional, Atlas, M., additional, Barron, D., additional, Bender, A., additional, Boettger, D., additional, Borrill, J., additional, Chapman, S., additional, Chinone, Y., additional, Cukierman, A., additional, Dobbs, M., additional, Elleflot, T., additional, Errard, J., additional, Fabbian, G., additional, Feng, C., additional, Gilbert, A., additional, Goeckner-Wald, N., additional, Halverson, N. W., additional, Hasegawa, M., additional, Hattori, K., additional, Hazumi, M., additional, Holzapfel, W. L., additional, Hori, Y., additional, Inoue, Y., additional, Jaehnig, G. C., additional, Jaffe, A. H., additional, Katayama, N., additional, Keating, B., additional, Kermish, Z., additional, Keskitalo, R., additional, Kisner, T., additional, Le Jeune, M., additional, Lee, A. T., additional, Leitch, E. M., additional, Linder, E., additional, Matsuda, F., additional, Matsumura, T., additional, Meng, X., additional, Miller, N. J., additional, Morii, H., additional, Myers, M. J., additional, Navaroli, M., additional, Nishino, H., additional, Okamura, T., additional, Paar, H., additional, Peloton, J., additional, Poletti, D., additional, Raum, C., additional, Rebeiz, G., additional, Reichardt, C. L., additional, Richards, P. L., additional, Ross, C., additional, Rotermund, K. M., additional, Schenck, D. E., additional, Sherwin, B. D., additional, Shirley, I., additional, Sholl, M., additional, Siritanasak, P., additional, Smecher, G., additional, Steinbach, B., additional, Stompor, R., additional, Suzuki, A., additional, Suzuki, J., additional, Takada, S., additional, Takakura, S., additional, Tomaru, T., additional, Wilson, B., additional, Yadav, A., additional, and Zahn, O., additional

Published
2014
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