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1. Unravelling the asphericities in the explosion and multi-faceted circumstellar matter of SN 2023ixf

Author

Singh, Avinash, Teja, R. S., Moriya, T. J., Maeda, K., Kawabata, K. S., Tanaka, M., Imazawa, R., Nakaoka, T., Gangopadhyay, A., Yamanaka, M., Swain, V., Sahu, D. K., Anupama, G. C., Kumar, B., Anche, R. M., Sano, Y., Raj, A., Agnihotri, V. K., Bhalerao, V., Bisht, D., Bisht, M. S., Belwal, K., Chakrabarti, S. K., Fujii, M., Nagayama, T., Matsumoto, K., Hamada, T., Kawabata, M., Kumar, A., Kumar, R., Malkan, B. K., Smith, P., Sakagami, Y., Taguchi, K., Tominaga, N., and Watanabe, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present a detailed investigation of photometric, spectroscopic, and polarimetric observations of the Type II SN 2023ixf. Earlier studies have provided compelling evidence for a delayed shock breakout from a confined dense circumstellar matter (CSM) enveloping the progenitor star. The temporal evolution of polarization in SN~2023ixf revealed three distinct peaks in polarization evolution at 1.4 d, 6.4 d, and 79.2 d, indicating an asymmetric dense CSM, an aspherical shock front and clumpiness in the low-density extended CSM, and an aspherical inner ejecta/He-core. SN 2023ixf displayed two dominant axes, one along the CSM-outer ejecta and the other along the inner ejecta/He-core, showcasing the independent origin of asymmetry in the early and late evolution. The argument for an aspherical shock front is further strengthened by the presence of a high-velocity broad absorption feature in the blue wing of the Balmer features in addition to the P-Cygni absorption post 16 d. Hydrodynamical light curve modeling indicated a progenitor of 10 solar mass with a radius of 470 solar radii and explosion energy of 2e51 erg, along with 0.06 solar mass of 56-Ni, though these properties are not unique due to modeling degeneracies. The modeling also indicated a two-zone CSM: a confined dense CSM extending up to 5e14 cm, with a mass-loss rate of 1e-2 solar mass per year, and an extended CSM spanning from 5e14 cm to at least 1e16cm with a mass-loss rate of 1e-4 solar mass per year, both assuming a wind-velocity of 10 km/s. The early nebular phase observations display an axisymmetric line profile of [OI], red-ward attenuation of the emission of Halpha post 125 days, and flattening in the Ks-band, marking the onset of dust formation., Comment: 32 pages, 15 figures, 1 Table, Accepted in the Astrophysical Journal

Published
2024

2. 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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4. 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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5. 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

6. Measurement of the cosmic microwave background polarization lensing power spectrum from two years of polarbear data

Author

Faúndez, MA, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Carron, J, Cheung, K, Chinone, Y, Bouhargani, HE, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Goeckner-Wald, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Hirose, H, Jeong, O, Katayama, N, Keating, B, Kikuchi, S, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Matsuda, F, Matsumura, T, Minami, Y, Navaroli, M, Nishino, H, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takatori, S, Tanabe, D, Teply, GP, and Tsai, C

Subjects
Cosmic microwave background radiation, Gravitational lensing, 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 gravitational lensing deflection power spectrum reconstructed with two seasons of cosmic microwave background polarization data from the Polarbear experiment. Observations were taken at 150 GHz from 2012 to 2014 and surveyed three patches of sky totaling 30 square degrees. We test the consistency of the lensing spectrum with a cold dark matter cosmology and reject the no-lensing hypothesis at a confidence of 10.9σ, including statistical and systematic uncertainties. We observe a value of A L = 1.33 ± 0.32 (statistical) ±0.02 (systematic) ±0.07 (foreground) using all polarization lensing estimators, which corresponds to a 24% accurate measurement of the lensing amplitude. Compared to the analysis of the first-year data, we have improved the breadth of both the suite of null tests and the error terms included in the estimation of systematic contamination.

Published
2020

7. The LiteBIRD Satellite Mission - Sub-Kelvin Instrument

Author

Suzuki, A., Ade, P. A. R., Akiba, Y., Alonso, D., Arnold, K., Aumont, J., Baccigalupi, C., Barron, D., Basak, S., Beckman, S., Borrill, J., Boulanger, F., Bucher, M., Calabrese, E., Chinone, Y., Cho, H-M., Cukierman, A., Curtis, D. W., de Haan, T., Dobbs, M., Dominjon, A., Dotani, T., Duband, L., Ducout, A., Dunkley, J., Duval, J. M., Elleflot, T., Eriksen, H. K., Errard, J., Fischer, J., Fujino, T., Funaki, T., Fuskeland, U., Ganga, K., Goeckner-Wald, N., Grain, J., Halverson, N. W., Hamada, T., Hasebe, T., Hasegawa, M., Hattori, K., Hattori, M., Hayes, L., Hazumi, M., Hidehira, N., Hill, C. A., Hilton, G., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Inoue, M., Inoue, Y., D., K., Ishino, H., Jeong, O., Kanai, H., Kaneko, D., Kashima, S., Katayama, N., Kawasaki, T., Kernasovskiy, S. A., Keskitalo, R., Kibayashi, A., Kida, Y., Kimura, K., Kisner, T., Kohri, K., Komatsu, E., Komatsu, K., Kuo, C. L., Kurinsky, N. A., Kusaka, A., Lazarian, A., Lee, A. T., Li, D., Linder, E., Maffei, B., Mangilli, A., Maki, M., Matsumura, T., Matsuura, S., Meilhan, D., Mima, S., Minami, Y., Mitsuda, K., Montier, L., Nagai, M., Nagasaki, T., Nagata, R., Nakajima, M., Nakamura, S., Namikawa, T., Naruse, M., Nishino, H., Nitta, T., Noguchi, T., Ogawa, H., Oguri, S., Okada, N., Okamoto, A., Okamura, T., Otani, C., Patanchon, G., Pisano, G., Rebeiz, G., Remazeilles, M., Richards, P. L., Sakai, S., Sakurai, Y., Sato, Y., Sato, N., Sawada, M., Segawa, Y., Sekimoto, Y., Seljak, U., Sherwin, B. D., Shimizu, T., Shinozaki, K., Stompor, R., Sugai, H., Sugita, H., Suzuki, J., Tajima, O., Takada, S., Takaku, R., Takakura, S., Takatori, S., Tanabe, D., Taylor, E., Thompson, K. L., Thorne, B., Tomaru, T., Tomida, T., Tomita, N., Tristram, M., Tucker, C., Turin, P., Tsujimoto, M., Uozumi, S., Utsunomiya, S., Uzawa, Y., Vansyngel, F., Wehus, I. K., Westbrook, B., Willer, M., Whitehorn, N., Yamada, Y., Yamamoto, R., Yamasaki, N., Yamashita, T., and Yoshida, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Inflation is the leading theory of the first instant of the universe. Inflation, which postulates that the universe underwent a period of rapid expansion an instant after its birth, provides convincing explanation for cosmological observations. Recent advancements in detector technology have opened opportunities to explore primordial gravitational waves generated by the inflation through B-mode (divergent-free) polarization pattern embedded in the Cosmic Microwave Background anisotropies. If detected, these signals would provide strong evidence for inflation, point to the correct model for inflation, and open a window to physics at ultra-high energies. LiteBIRD is a satellite mission with a goal of detecting degree-and-larger-angular-scale B-mode polarization. LiteBIRD will observe at the second Lagrange point with a 400 mm diameter telescope and 2,622 detectors. It will survey the entire sky with 15 frequency bands from 40 to 400 GHz to measure and subtract foregrounds. The U.S. LiteBIRD team is proposing to deliver sub-Kelvin instruments that include detectors and readout electronics. A lenslet-coupled sinuous antenna array will cover low-frequency bands (40 GHz to 235 GHz) with four frequency arrangements of trichroic pixels. An orthomode-transducer-coupled corrugated horn array will cover high-frequency bands (280 GHz to 402 GHz) with three types of single frequency detectors. The detectors will be made with Transition Edge Sensor (TES) bolometers cooled to a 100 milli-Kelvin base temperature by an adiabatic demagnetization refrigerator.The TES bolometers will be read out using digital frequency multiplexing with Superconducting QUantum Interference Device (SQUID) amplifiers. Up to 78 bolometers will be multiplexed with a single SQUID amplidier. We report on the sub-Kelvin instrument design and ongoing developments for the LiteBIRD mission., Comment: 7 pages 2 figures Journal of Low Temperature Physics - Special edition - LTD17 Proceeding

Published
2018
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8. 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

9. 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

10. The LiteBIRD Satellite Mission: Sub-Kelvin Instrument

Author

Suzuki, A, Ade, PAR, Akiba, Y, Alonso, D, Arnold, K, Aumont, J, Baccigalupi, C, Barron, D, Basak, S, Beckman, S, Borrill, J, Boulanger, F, Bucher, M, Calabrese, E, Chinone, Y, Cho, S, Crill, B, Cukierman, A, Curtis, DW, de Haan, T, Dobbs, M, Dominjon, A, Dotani, T, Duband, L, Ducout, A, Dunkley, J, Duval, JM, Elleflot, T, Eriksen, HK, Errard, J, Fischer, J, Fujino, T, Funaki, T, Fuskeland, U, Ganga, K, Goeckner-Wald, N, Grain, J, Halverson, NW, Hamada, T, Hasebe, T, Hasegawa, M, Hattori, K, Hattori, M, Hayes, L, Hazumi, M, Hidehira, N, Hill, CA, Hilton, G, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Inoue, M, Inoue, Y, Irwin, KD, Ishino, H, Jeong, O, Kanai, H, Kaneko, D, Kashima, S, Katayama, N, Kawasaki, T, Kernasovskiy, SA, Keskitalo, R, Kibayashi, A, Kida, Y, Kimura, K, Kisner, T, Kohri, K, Komatsu, E, Komatsu, K, Kuo, CL, Kurinsky, NA, Kusaka, A, Lazarian, A, Lee, AT, Li, D, Linder, E, Maffei, B, Mangilli, A, Maki, M, Matsumura, T, Matsuura, S, Meilhan, D, Mima, S, Minami, Y, Mitsuda, K, Montier, L, Nagai, M, Nagasaki, T, Nagata, R, Nakajima, M, Nakamura, S, Namikawa, T, Naruse, M, Nishino, H, Nitta, T, Noguchi, T, Ogawa, H, and Oguri, S

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

Inflation is the leading theory of the first instant of the universe. Inflation, which postulates that the universe underwent a period of rapid expansion an instant after its birth, provides convincing explanation for cosmological observations. Recent advancements in detector technology have opened opportunities to explore primordial gravitational waves generated by the inflation through “B-mode” (divergent-free) polarization pattern embedded in the cosmic microwave background anisotropies. If detected, these signals would provide strong evidence for inflation, point to the correct model for inflation, and open a window to physics at ultra-high energies. LiteBIRD is a satellite mission with a goal of detecting degree-and-larger-angular-scale B-mode polarization. LiteBIRD will observe at the second Lagrange point with a 400 mm diameter telescope and 2622 detectors. It will survey the entire sky with 15 frequency bands from 40 to 400 GHz to measure and subtract foregrounds. The US LiteBIRD team is proposing to deliver sub-Kelvin instruments that include detectors and readout electronics. A lenslet-coupled sinuous antenna array will cover low-frequency bands (40–235 GHz) with four frequency arrangements of trichroic pixels. An orthomode-transducer-coupled corrugated horn array will cover high-frequency bands (280–402 GHz) with three types of single frequency detectors. The detectors will be made with transition edge sensor (TES) bolometers cooled to a 100 milli-Kelvin base temperature by an adiabatic demagnetization refrigerator. The TES bolometers will be read out using digital frequency multiplexing with Superconducting QUantum Interference Device (SQUID) amplifiers. Up to 78 bolometers will be multiplexed with a single SQUID amplifier. We report on the sub-Kelvin instrument design and ongoing developments for the LiteBIRD mission.

Published
2018

11. 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

12. Concept Study of Optical Configurations for High-Frequency Telescope for LiteBIRD

Author

Hasebe, T, Kashima, S, Ade, PAR, Akiba, Y, Alonso, D, Arnold, K, Aumont, J, Baccigalupi, C, Barron, D, Basak, S, Beckman, S, Borrill, J, Boulanger, F, Bucher, M, Calabrese, E, Chinone, Y, Cho, H-M, Cukierman, A, Curtis, DW, de Haan, T, Dobbs, M, Dominjon, A, Dotani, T, Duband, L, Ducout, A, Dunkley, J, Duval, JM, Elleflot, T, Eriksen, HK, Errard, J, Fischer, J, Fujino, T, Funaki, T, Fuskeland, U, Ganga, K, Goeckner-Wald, N, Grain, J, Halverson, NW, Hamada, T, Hasegawa, M, Hattori, K, Hattori, M, Hayes, L, Hazumi, M, Hidehira, N, Hill, CA, Hilton, G, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Inoue, M, Inoue, Y, Irwin, KD, Ishino, H, Jeong, O, Kanai, H, Kaneko, D, Katayama, N, Kawasaki, T, Kernasovskiy, SA, Keskitalo, R, Kibayashi, A, Kida, Y, Kimura, K, Kisner, T, Kohri, K, Komatsu, E, Komatsu, K, Kuo, CL, Kurinsky, NA, Kusaka, A, Lazarian, A, Lee, AT, Li, D, Linder, E, Maffei, B, Mangilli, A, Maki, M, Matsumura, T, Matsuura, S, Meilhan, D, Mima, S, Minami, Y, Mitsuda, K, Montier, L, Nagai, M, Nagasaki, T, Nagata, R, Nakajima, M, Nakamura, S, Namikawa, T, Naruse, M, Nishino, H, Nitta, T, Noguchi, T, Ogawa, H, Oguri, S, Okada, N, and Okamoto, A

Subjects
Physical Sciences, Classical Physics, Condensed Matter Physics, Cosmic microwave background radiation, Inflation, Satellite, Telescope, Mathematical Physics, General Physics, Classical physics, Condensed matter physics
Abstract

The high-frequency telescope for LiteBIRD is designed with refractive and reflective optics. In order to improve sensitivity, this paper suggests the new optical configurations of the HFT which have approximately 7 times larger focal planes than that of the original design. The sensitivities of both the designs are compared, and the requirement of anti-reflection (AR) coating on the lens for the refractive option is derived. We also present the simulation result of a sub-wavelength AR structure on both surfaces of silicon, which shows a band-averaged reflection of 1.1–3.2% at 101–448 GHz.

Published
2018

13. 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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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. 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

17. Molecular behavior of DNA in a cell-sized compartment coated by lipids

Author

Hamada, T., Fujimoto, R., Shimobayashi, S. F., Ichikawa, M., and Takagi, M.

Subjects
Physics - Biological Physics, Condensed Matter - Soft Condensed Matter, Quantitative Biology - Biomolecules
Abstract

The behavior of long DNA molecules in a cell-sized confined space was investigated. We prepared water-in-oil droplets covered by phospholipids, which mimic the inner space of a cell, following the encapsulation of DNA molecules with unfolded coil and folded globule conformations. Microscopic observation revealed that the adsorption of coiled DNA onto the membrane surface depended on the size of the vesicular space. Globular DNA showed a cell-size-dependent unfolding transition after adsorption on the membrane. Furthermore, when DNA interacted with a two-phase membrane surface, DNA selectively adsorbed on the membrane phase, such as an ordered or disordered phase, depending on its conformation. We discuss the mechanism of these trends by considering the free energy of DNA together with a polyamine in the solution. The free energy of our model was consistent with the present experimental data. The cooperative interaction of DNA and polyamines with a membrane surface leads to the size-dependent behavior of molecular systems in a small space. These findings may contribute to a better understanding of the physical mechanism of molecular events and reactions inside a cell., Comment: 5 pages, 5 figures

Published
2015

18. 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

19. 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

20. 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

23. 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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26. SPH Simulations with Reconfigurable Hardware Accelerator

Author

Nakasato, N., Hamada, T., and Fukushige, T.

Subjects
Astrophysics
Abstract

We present a novel approach to accelerate astrophysical hydrodynamical simulations. In astrophysical many-body simulations, GRAPE (GRAvity piPE) system has been widely used by many researchers. However, in the GRAPE systems, its function is completely fixed because specially developed LSI is used as a computing engine. Instead of using such LSI, we are developing a special purpose computing system using Field Programmable Gate Array (FPGA) chips as the computing engine. Together with our developed programming system, we have implemented computing pipelines for the Smoothed Particle Hydrodynamics (SPH) method on our PROGRAPE-3 system. The SPH pipelines running on PROGRAPE-3 system have the peak speed of 85 GFLOPS and in a realistic setup, the SPH calculation using one PROGRAPE-3 board is 5-10 times faster than the calculation on the host computer. Our results clearly shows for the first time that we can accelerate the speed of the SPH simulations of a simple astrophysical phenomena using considerable computing power offered by the hardware., Comment: 27 pages, 13 figures, submitted to PASJ

Published
2006
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27. LiteBIRD: A Satellite for the Studies of B-Mode Polarization and Inflation from Cosmic Background Radiation Detection

Author

Hazumi, M., Ade, P. A. R., Akiba, Y., Alonso, D., Arnold, K., Aumont, J., Baccigalupi, C., Barron, D., Basak, S., Beckman, S., Borrill, J., Boulanger, F., Bucher, M., Calabrese, E., Chinone, Y., Cho, S., Cukierman, A., Curtis, D. W., de Haan, T., Dobbs, M., Dominjon, A., Dotani, T., Duband, L., Ducout, A., Dunkley, J., Duval, J. M., Elleflot, T., Eriksen, H. K., Errard, J., Fischer, J., Fujino, T., Funaki, T., Fuskeland, U., Ganga, K., Goeckner-Wald, N., Grain, J., Halverson, N. W., Hamada, T., Hasebe, T., Hasegawa, M., Hattori, K., Hattori, M., Hayes, L., Hidehira, N., Hill, C. A., Hilton, G., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Inoue, M., Inoue, Y., Irwin, K. D., Ishino, H., Jeong, O., Kanai, H., Kaneko, D., Kashima, S., Katayama, N., Kawasaki, T., Kernasovskiy, S. A., Keskitalo, R., Kibayashi, A., Kida, Y., Kimura, K., Kisner, T., Kohri, K., Komatsu, E., Komatsu, K., Kuo, C. L., Kurinsky, N. A., Kusaka, A., Lazarian, A., Lee, A. T., Li, D., Linder, E., Maffei, B., Mangilli, A., Maki, M., Matsumura, T., Matsuura, S., Meilhan, D., Mima, S., Minami, Y., Mitsuda, K., Montier, L., Nagai, M., Nagasaki, T., Nagata, R., Nakajima, M., Nakamura, S., Namikawa, T., Naruse, M., Nishino, H., Nitta, T., Noguchi, T., Ogawa, H., Oguri, S., Okada, N., Okamoto, A., Okamura, T., Otani, C., Patanchon, G., Pisano, G., Rebeiz, G., Remazeilles, M., Richards, P. L., Sakai, S., Sakurai, Y., Sato, Y., Sato, N., Sawada, M., Segawa, Y., Sekimoto, Y., Seljak, U., Sherwin, B. D., Shimizu, T., Shinozaki, K., Stompor, R., Sugai, H., Sugita, H., Suzuki, A., Suzuki, J., Tajima, O., Takada, S., Takaku, R., Takakura, S., Takatori, S., Tanabe, D., Taylor, E., Thompson, K. L., Thorne, B., Tomaru, T., Tomida, T., Tomita, N., Tristram, M., Tucker, C., Turin, P., Tsujimoto, M., Uozumi, S., Utsunomiya, S., Uzawa, Y., Vansyngel, F., Wehus, I. K., Westbrook, B., Willer, M., Whitehorn, N., Yamada, Y., Yamamoto, R., Yamasaki, N., Yamashita, T., and Yoshida, M.

Published
2019
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32. Soft- and Hard-Error Radiation Reliability of 228 KB $3\mathrm{T}+1\mathrm{C}$ Oxide Semiconductor Memory

Author

Takahashi, H., primary, Okamoto, Y., additional, Hamada, T., additional, Komura, Y., additional, Watanabe, S., additional, Tsuda, K., additional, Sawai, H., additional, Matsuzaki, T., additional, Ando, Y., additional, Onuki, T., additional, Kunitake, H., additional, Yamazaki, S., additional, Kobayashi, D., additional, Ikuta, A., additional, Makino, T., additional, and Ohshima, T., additional

Published
2023
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33. Bayesian risk prediction model for colorectal cancer mortality through integration of clinicopathologic and genomic data

Author

Zhao, M. (Melissa), Lau, M. C. (Mai Chan), Haruki, K. (Koichiro), Väyrynen, J. P. (Juha P.), Gurjao, C. (Carino), Väyrynen, S. A. (Sara A.), Costa, A. D. (Andressa Dias), Borowsky, J. (Jennifer), Fujiyoshi, K. (Kenji), Arima, K. (Kota), Hamada, T. (Tsuyoshi), Lennerz, J. K. (Jochen K.), Fuchs, C. S. (Charles S.), Nishihara, R. (Reiko), Chan, A. T. (Andrew T.), Ng, K. (Kimmie), Zhang, X. (Xuehong), Meyerhardt, J. A. (Jeffrey A.), Song, M. (Mingyang), Wang, M. (Molin), Giannakis, M. (Marios), Nowak, J. A. (Jonathan A.), Yu, K.-H. (Kun-Hsing), Ugai, T. (Tomotaka), Ogino, S. (Shuji), Zhao, M. (Melissa), Lau, M. C. (Mai Chan), Haruki, K. (Koichiro), Väyrynen, J. P. (Juha P.), Gurjao, C. (Carino), Väyrynen, S. A. (Sara A.), Costa, A. D. (Andressa Dias), Borowsky, J. (Jennifer), Fujiyoshi, K. (Kenji), Arima, K. (Kota), Hamada, T. (Tsuyoshi), Lennerz, J. K. (Jochen K.), Fuchs, C. S. (Charles S.), Nishihara, R. (Reiko), Chan, A. T. (Andrew T.), Ng, K. (Kimmie), Zhang, X. (Xuehong), Meyerhardt, J. A. (Jeffrey A.), Song, M. (Mingyang), Wang, M. (Molin), Giannakis, M. (Marios), Nowak, J. A. (Jonathan A.), Yu, K.-H. (Kun-Hsing), Ugai, T. (Tomotaka), and Ogino, S. (Shuji)

Abstract

Routine tumor-node-metastasis (TNM) staging of colorectal cancer is imperfect in predicting survival due to tumor pathobiological heterogeneity and imprecise assessment of tumor spread. We leveraged Bayesian additive regression trees (BART), a statistical learning technique, to comprehensively analyze patient-specific tumor characteristics for the improvement of prognostic prediction. Of 75 clinicopathologic, immune, microbial, and genomic variables in 815 stage II–III patients within two U.S.-wide prospective cohort studies, the BART risk model identified seven stable survival predictors. Risk stratifications (low risk, intermediate risk, and high risk) based on model-predicted survival were statistically significant (hazard ratios 0.19–0.45, vs. higher risk; P < 0.0001) and could be externally validated using The Cancer Genome Atlas (TCGA) data (P = 0.0004). BART demonstrated model flexibility, interpretability, and comparable or superior performance to other machine-learning models. Integrated bioinformatic analyses using BART with tumor-specific factors can robustly stratify colorectal cancer patients into prognostic groups and be readily applied to clinical oncology practice.

Published
2023

34. A c-axis aligned crystalline IGZO FET and a 0.06-μm2 HfO2-based Capacitor 1T1C FeRAM with High Voltage Tolerance and 10-ns Write Time

Author

Endo, M., primary, Numata, S., additional, Ohshima, K., additional, Egi, Y., additional, Isaka, F., additional, Ohno, T., additional, Tezuka, S., additional, Hamada, T., additional, Furutani, K., additional, Tsuda, K., additional, Matsuzaki, T., additional, Onuki, T., additional, Murakawa, T., additional, Kunitake, H., additional, Kobayashi, M., additional, and Yamazaki, S., additional

Published
2022
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37. Method for rapid performance validation of large TES bolometer array for POLARBEAR-2A using a coherent millimeter-wave source

Author

Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, 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, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., 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., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., 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., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., Zhou Y., Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, 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, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., 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., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., 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., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., and Zhou Y.

Abstract

POLARBEAR-2A is the first receiver for the Simons Array cosmic microwave background polarization experiment. POLARBEAR-2A has transition-edge sensor bolometers on the focal plane. Signals from bolometers are multiplexed and read out by a single SQUID. The receiver was deployed in late 2018 in Atacama, Chile, and operation started in 2019, where rapid confirmation of correspondence between bolometers and multiplexed readout channels was important as an initial step of performance validation. For this purpose, we devised a method using a coherent source that allows us to identify the frequency band and polarization sensitivity angle for each readout channel without detailed bolometer tuning.

Published
2021

39. P1212: PERSONALIZED TREATMENT FOR ELDERLY PATIENTS WITH DIFFUSE LARGE B-CELL LYMPHOMA

Author

Nukariya, H., primary, Miura, K., additional, Takahashi, H., additional, Nakagawa, M., additional, Hamada, T., additional, Itho, S., additional, Ichinohe, T., additional, Endo, T., additional, Kurihara, K., additional, Koike, T., additional, Iizuka, K., additional, Ohtake, S., additional, Yoshihito, U., additional, Iriyama, N., additional, Hatta, Y., additional, and Nakamura, H., additional

Published
2022
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40. Deployment of Polarbear-2A

Author

Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, 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, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, 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, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez 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., Dunner 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., Zhou Y., Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, 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, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, 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, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez 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., Dunner 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.

Abstract

Polarbear-2A is the first of three receivers in the Simons array, a cosmic microwave background experiment located on the Atacama Plateau in Chile. Polarbear-2A was deployed and achieved the first light in January 2019 by mapping the microwave emission from planet observations. Commissioning work is underway to prepare the receiver for science observations.

Published
2020

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

Author

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

Abstract

POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.

Published
2020

42. Preparation of Microfiltration Hollow Fiber Membranes from Cellulose Triacetate by Thermally Induced Phase Separation.

Author

Takao, S, Rajabzadeh, S, Otsubo, C, Hamada, T, Kato, N, Nakagawa, K, Shintani, T, Matsuyama, H, Yoshioka, T, Takao, S, Rajabzadeh, S, Otsubo, C, Hamada, T, Kato, N, Nakagawa, K, Shintani, T, Matsuyama, H, and Yoshioka, T

Abstract

For the first time, self-standing microfiltration (MF) hollow fiber membranes were prepared from cellulose triacetate (CTA) via the thermally induced phase separation (TIPS) method. The resultant membranes were compared with counterparts prepared from cellulose diacetate (CDA) and cellulose acetate propionate (CAP). Extensive solvent screening by considering the Hansen solubility parameters of the polymer and solvent, the polymer's solubility at high temperature, solidification of the polymer solution at low temperature, viscosity, and processability of the polymeric solution, is the most challenging issue for cellulose membrane preparation. Different phase separation mechanisms were identified for CTA, CDA, and CAP polymer solutions prepared using the screened solvents for membrane preparation. CTA solutions in binary organic solvents possessed the appropriate properties for membrane preparation via liquid-liquid phase separation, followed by a solid-liquid phase separation (polymer crystallization) mechanism. For the prepared CTA hollow fiber membranes, the maximum stress was 3-5 times higher than those of the CDA and CAP membranes. The temperature gap between the cloud point and crystallization onset in the polymer solution plays a crucial role in membrane formation. All of the CTA, CDA, and CAP membranes had a very porous bulk structure with a pore size of ∼100 nm or larger, as well as pores several hundred nanometers in size at the inner surface. Using an air gap distance of 0 mm, the appropriate organic solvents mixed in an optimized ratio, and a solvent for cellulose derivatives as the quench bath media, it was possible to obtain a CTA MF hollow fiber membrane with high pure water permeance and notably high rejection of 100 nm silica nanoparticles. It is expected that these membranes can play a great role in pharmaceutical separation.

Published
2022

43. Preparation of Chemically Resistant Cellulose Benzoate Hollow Fiber Membrane via Thermally Induced Phase Separation Method.

Author

Takao, S, Rajabzadeh, S, Shibata, M, Otsubo, C, Hamada, T, Kato, N, Nakagawa, K, Kitagawa, T, Matsuyama, H, Yoshioka, T, Takao, S, Rajabzadeh, S, Shibata, M, Otsubo, C, Hamada, T, Kato, N, Nakagawa, K, Kitagawa, T, Matsuyama, H, and Yoshioka, T

Abstract

For the first time, we have successfully fabricated microfiltration (MF) hollow fiber membranes by the thermally induced phase separation (TIPS) and non-solvent induced phase separation (NIPS) methods using cellulose acetate benzoate (CBzOH), which is a cellulose derivative with considerable chemical resistance. To obtain an appropriate CBzOH TIPS membrane, a comprehensive solvent screening was performed to choose the appropriate solvent to obtain a membrane with a porous structure. In parallel, the CBzOH membrane was prepared by the NIPS method to compare and evaluate the effect of membrane structure using the same polymer material. Prepared CBzOH membrane by TIPS method showed high porosity, pore size around 100 nm or larger and high pure water permeability (PWP) with slightly low rection performance compared to that by NIPS. On the contrary, CBzOH membranes prepared with the NIPS method showed three times lower PWP with higher rejection. The chemical resistance of the prepared CBzOH membranes was compared with that of cellulose triacetate (CTA) hollow fiber membrane, which is a typical cellulose derivative as a control membrane, using a 2000 ppm sodium hypochlorite (NaClO) solution. CBzOH membranes prepared with TIPS and NIPS methods showed considerable resistance against the NaClO solution regardless of the membrane structure, porosity and pore size. On the other hand, when the CTA membrane, as the control membrane, was subjected to the NaClO solution, membrane mechanical strength sharply decreased over the exposure time to NaClO. It is interesting that although the CBzOH TIPS membrane showed three times higher pure water permeability than other membranes with slightly lower rejection and considerably higher NaClO resistance, the mechanical strength of this membrane is more than two times higher than other membranes. While CBzOH samples showed no change in chemical structure and contact angle, CTA showed considerable change in chemical structure and a sharp decr

Published
2022

46. The tale of TILs in breast cancer: A report from The International Immuno-Oncology Biomarker Working Group

Author

El Bairi, K., Haynes, H. R., Blackley, E., Fineberg, S., Shear, J., Turner, S., de Freitas, J. R., Sur, D., Amendola, L. C., Gharib, M., Kallala, A., Arun, I., Azmoudeh-Ardalan, F., Fujimoto, L., Sua, L. F., Liu, S. -W., Lien, H. -C., Kirtani, P., Balancin, M., El Attar, H., Guleria, P., Yang, W., Shash, E., Chen, I. -C., Bautista, V., Do Prado Moura, J. F., Rapoport, B. L., Castaneda, C., Spengler, E., Acosta-Haab, G., Frahm, I., Sanchez, J., Castillo, M., Bouchmaa, N., Md Zin, R. R., Shui, R., Onyuma, T., Husain, Z., Willard-Gallo, K., Coosemans, A., Perez, E. A., Provenzano, E., Ericsson, P. G., Richardet, E., Mehrotra, R., Sarancone, S., Ehinger, A., Rimm, D. L., Bartlett, J. M. S., Viale, G., Denkert, C., Hida, A. I., Sotiriou, C., Loibl, S., Hewitt, S. M., Badve, S., Symmans, W. F., Kim, R. S., Pruneri, G., Goel, S., Francis, P. A., Inurrigarro, G., Yamaguchi, R., Garcia-Rivello, H., Horlings, H., Afqir, S., Salgado, R., Adams, S., Kok, M., Dieci, M. V., Michiels, S., Demaria, S., Loi, S., Schelfhout, V., Arbzadeh, E., Bondanar, A., Reyes, S. A. G., Ruz, J. R., Kang, J., Xiang, L., Zimovjanova, M., Togores, P., Ozturk, T., Patil, A., Corpa, M., Whitehouse, A., Tan, B., de Paula, A., Rossetti, C., Lang-Schwarz, C., Mahon, S., Giacometti, C., Linderholm, B., Deman, F., Montagna, G., Gong, G., Pavcovich, M., Chaer, Y., Cabrero, I. A., de Brito, M. L., Ilieva, N., Fulop, A., Souza, M., Bilancia, D., Idowu, M., Johri, R., Szpor, J., Bachani, L., Schmitt, F., Giannotti, M., Kurebayashi, Y., Ramirez, B. E. A., Salido, E., Bortesi, L., Bonetto, S., Elomina, K., Lopez, P., Sharma, V., Edirisinghe, A., Mathur, D., Sahay, A., Mouloud, M. A., Giang, C. H., Mukolwe, E., Kiruka, E., Samberg, N., Abe, N., Brown, M., Millar, E., X. B., Li, Yuan, Z., Pasupathy, A., Miele, R., Luff, R., e Porfirio, M. M. A., Ajemba, O., Soni, R., Orvieto, E., Dimaio, M., Thomas, J., Merard, R., Subramaniam, M. M., Apolinario, T., Preda, O., Preda, R., Makanga, A., Maior, M. S., Li, L., Saghatchian, M., Saurine, T., Janssen, E., Cochran, J., Vlada, N., Cappellesso, R., Elfer, K., Hollick, M., Desai, S., Oner, G., Schreurs, A., Liu, S., Perera, R., Mercurio, P., Garcia, F., Hosny, K., Matsumoto, H., van Deurzen, C., Bianchini, G., Coban, I., Jahangir, A., Rahman, A., Stover, D., Luz, P., Martel, A., Waumans, Y., Stenzinger, A., Cortes, J., Dimitrova, P., Nauwelaers, I., Velasco, M., Fan, F., Akturk, G., Firer, M., Roxanis, I., Schneck, M., Wen, H., Cockenpot, V., Konstantinov, A., Calatrava, A., Vidya, M. N., Choi, H. J., Jank, P., Ciinen, A. H., Sabanathan, D., Floris, G., Hoeflmayer, D., Hamada, T., Laudus, N., Grigoriadis, A., Porcellato, I., Acs, B., Miglietta, F., Parrodi, J., Clunie, D., Calhoun, B., F. -I., Lu, Lefevre, A., Tabbarah, S., Tran, W., Garcia-murillas, I., Jelinic, P., Boeckx, C., Souza, S., Cebollero, M. C., Felip, E., Rendon, J. L. S., El Gabry, E., Saltz, J., Bria, E., Garufi, G., Hartman, J., Sebastian, M., Olofsson, H., Kooreman, L., Cucherousset, J., Mathieu, M. -C., Ballesteros-Merino, C., Siziopikou, P., Fong, J., Klein, M., Qulis, I. R. I., Wesseling, J., Bellolio, E., Araya, J. C., Naber, S., Cheang, M., Castellano, I., Ales, A., Laenkholm, A. -V., Kulka, J., Quinn, C., Sapino, A., Amendoeira, I., Marchio, C., Braybrooke, J., Vincent-Salomon, A., Korski, K. P., Sofopoulos, M., Stovgaard, E. I. S., Bianchi, S., Bago-Horvath, Z., Yu, C., Regitnig, P., Hall, S., Kos, Z., Sant, S., Tille, J. -C., Gallas, B., Bethmann, D., Savas, P., Mendes, L., Soler, T., van Seijen, M., Gruosso, T., Quintana, A., Giltnane, J., Van den Eynden, G., Duregon, E., de Cabo, R., Recamo, P. C., Gaboury, L., Zimmerman, J., Pop, C. S., Wernicke, A., Williams, D., Gill, A., Solomon, B., Thapa, B., Farshid, G., Gilham, L., Christie, M., O'Toole, S., Hendry, S., Fox, S. B., Luen, S. J., Lakhani, S. R., Fuchs, T., John, T., Brcic, I., Hainfellner, J., Sigurd, L., Preusser, M., Poortmans, P., Decaluwe, A., Carey, C., Colpaert, C., Larsimont, D., Peeters, D., Broeckx, G., van de Vijver, K., Buisseret, L., Dirix, L., Hertoghs, M., Piccart, M., Ignatiadis, M., Van Bockstal, M., Sirtaine, N., Vermeulen, P., de Wind, R., Declercq, S., Gevaert, T., Haibe-Kans, B., Nelson, B. H., Watson, P. H., Leung, S., Nielsen, T., Shi, L., Balslev, E., Thagaard, J., Almangush, A., Makitie, A., Joensuu, H., Lundin, J., Drubay, D., Roblin, E., Andre, F., Penault-Llorca, F., Lemonnier, J., Adam, J., Lacroix-Triki, M., Ternes, N., Radosevic-Robin, N., Klaushen, F., Weber, K., Harbeck, N., Gluz, O., Wienert, S., Cserni, G., Vingiani, A., Criscitiello, C., Solinas, C., Curigliano, G., Konishi, E., Suzuki, E., Yoshikawa, K., Kawaguchi, K., Takada, M., Toi, M., Ishida, M., Shibata, N., Saji, S., Kogawa, T., Sakatani, T., Okamoto, T., Moriya, T., Kataoka, T., Shimoi, T., Sugie, T., Mukohara, T., Shu, Y., Kikawa, Y., Kozuka, Y., Sayed, S., Rahayu, R., Ramsaroop, R., Senkus-Konefka, E., Chmielik, E., Cardoso, F., Ribeiro, J., Chan, J., Dent, R., Martin, M., Hagen, C., Guerrero, A., Rojo, F., Comerma, L., Nuciforo, P., Serrano, V. V., Camaea, V. P., Steenbruggen, T., Ciompi, F., Nederlof, I., Jan, Hudecek, van der Laak, J., van den Berg, J., Voorwerk, L., van de Vijver, M., de Maaker, M., Linn, S., Mckenzie, H., Somaiah, N., Tutt, A., Swanton, C., Hiley, C., Moore, D. A., Hall, J. A., Le Quesne, J., Jabbar, K. A., al Bakir, M., Hills, R., Irshad, S., Yuan, Y., Li, Z., Liu, M., Klein, J., Fadare, O., Thompson, A., Lazar, A. J., Gown, A., Lo, A., Garrido Castro, A. C., Madabhushi, A., Moreira, A., Richardson, A., Beck, A. H., Bellizzi, A. M., Wolff, A., Harbhajanka, A., Sharma, A., Cimino-Mathews, A., Srinivasan, A., Singh, B., Chennubhotla, C. S., Chauhan, C., Dillon, D. A., Zardavas, D., Johnson, D. B., Thompson, A. E., Brogi, E., Reisenbichler, E., Huang, E., Hirsch, F. R., Mcarthur, H., Ziai, J., Brock, J., Kerner, J., Zha, J., Lennerz, J. K., Carter, J. M., Reis-Filho, J., Sparano, J., Balko, J. M., Pogue-Geile, K., Steele, K. E., Blenman, K. R. M., Allison, K. H., Pusztai, L., Cooper, L., Estrada, V. M., Flowers, M., Robson, M., Rebelatto, M. C., Hanna, M. G., Goetz, M. P., Khojasteh, M., Sanders, M. E., Regan, M. M., Misialek, M., Amgad, M., Tung, N., Singh, R., Huang, R., Pierce, R. H., Leon-Ferre, R., Swain, S., Ely, S., Kim, S. -R., Bedri, S., Paik, S., Schnitt, S., D'Alfons, T., Kurkure, U., Bossuyt, V., Tong, W., Wang, Y., Dos Anjos, C. H., Gaire, F., Van Diest, P. J., El Bairi, Khalid [0000-0002-8414-4145], de Freitas, Juliana Ribeiro [0000-0003-4978-7273], Sur, Daniel [0000-0002-0926-4614], Amendola, Luis Claudio [0000-0002-6404-450X], Azmoudeh-Ardalan, Farid [0000-0003-4701-0532], Kirtani, Pawan [0000-0002-2343-7016], Yang, Wenxian [0000-0002-5349-9680], Castillo, Miluska [0000-0002-0111-3176], Provenzano, Elena [0000-0003-3345-3965], Mehrotra, Ravi [0000-0001-9453-1408], Ehinger, Anna [0000-0001-9225-7396], Rimm, David L [0000-0001-5820-4397], Bartlett, John MS [0000-0002-0347-3888], Denkert, Carsten [0000-0002-2249-0982], Hida, Akira I [0000-0002-4486-8819], Sotiriou, Christos [0000-0002-5745-9977], Hewitt, Stephen M [0000-0001-8283-1788], Badve, Sunil [0000-0001-8861-9980], Symmans, William Fraser [0000-0002-1526-184X], Goel, Shom [0000-0001-8329-9084], Francis, Prudence A [0000-0002-7207-9286], Horlings, Hugo [0000-0003-4782-8828], Salgado, Roberto [0000-0002-1110-3801], Demaria, Sandra [0000-0003-4426-0499], Loi, Sherene [0000-0001-6137-9171], Apollo - University of Cambridge Repository, UCL - SSS/IREC/SLUC - Pôle St.-Luc, UCL - (SLuc) Service d'anatomie pathologique, Imagerie Moléculaire et Stratégies Théranostiques (IMoST), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Clermont Auvergne (UCA), Centre Jean Perrin [Clermont-Ferrand] (UNICANCER/CJP), and UNICANCER

Subjects
Oncology, medicine.medical_treatment, [SDV]Life Sciences [q-bio], TRASTUZUMAB, Improved survival, MICROENVIRONMENT, Review Article, SUBTYPES, NEOADJUVANT CHEMOTHERAPY, 0302 clinical medicine, Breast cancer, Ecology,Evolution & Ethology, PROGNOSTIC-SIGNIFICANCE, Medicine and Health Sciences, Pharmacology (medical), TUMOR-INFILTRATING LYMPHOCYTES, Stage (cooking), RC254-282, Chemical Biology & High Throughput, 0303 health sciences, Human Biology & Physiology, Genome Integrity & Repair, Neoplasms. Tumors. Oncology. Including cancer and carcinogens, ASSOCIATION, 3. Good health, 030220 oncology & carcinogenesis, Biomarker (medicine), Life Sciences & Biomedicine, Genetics & Genomics, medicine.medical_specialty, chemical and pharmacologic phenomena, International Immuno-Oncology Biomarker Working Group, Predictive markers, 03 medical and health sciences, Signalling & Oncogenes, SDG 3 - Good Health and Well-being, Internal medicine, 692/53/2423, medicine, Radiology, Nuclear Medicine and imaging, In patient, 030304 developmental biology, Computational & Systems Biology, Science & Technology, IDENTIFICATION, business.industry, review-article, Cancer, 03.01. Általános orvostudomány, Immunotherapy, Tumour Biology, medicine.disease, PREDICTIVE-VALUE, 692/4028/67/1347, Programmed death 1, business, FREE SURVIVAL
Abstract

The advent of immune-checkpoint inhibitors (ICI) in modern oncology has significantly improved survival in several cancer settings. A subgroup of women with breast cancer (BC) has immunogenic infiltration of lymphocytes with expression of programmed death-ligand 1 (PD-L1). These patients may potentially benefit from ICI targeting the programmed death 1 (PD-1)/PD-L1 signaling axis. The use of tumor-infiltrating lymphocytes (TILs) as predictive and prognostic biomarkers has been under intense examination. Emerging data suggest that TILs are associated with response to both cytotoxic treatments and immunotherapy, particularly for patients with triple-negative BC. In this review from The International Immuno-Oncology Biomarker Working Group, we discuss (a) the biological understanding of TILs, (b) their analytical and clinical validity and efforts toward the clinical utility in BC, and (c) the current status of PD-L1 and TIL testing across different continents, including experiences from low-to-middle-income countries, incorporating also the view of a patient advocate. This information will help set the stage for future approaches to optimize the understanding and clinical utilization of TIL analysis in patients with BC. ispartof: NPJ BREAST CANCER vol:7 issue:1 ispartof: location:United States status: published

Published
2021

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