Search

Your search keyword '"Puglisi, G"' showing total 514 results
Start Over Author "Puglisi, G" Publication Type Academic Journals
514 results on '"Puglisi, G"'

1. In-flight polarization angle calibration for LiteBIRD: blind challenge and cosmological implications

Author

collaboration, The LiteBIRD, Krachmalnicoff, N, Matsumura, T, de la Hoz, E, Basak, S, Gruppuso, A, Minami, Y, Baccigalupi, C, Komatsu, E, Martínez-González, E, Vielva, P, Aumont, J, Aurlien, R, Azzoni, S, Banday, AJ, Barreiro, RB, Bartolo, N, Bersanelli, M, Calabrese, E, Carones, A, Casas, FJ, Cheung, K, Chinone, Y, Columbro, F, de Bernardis, P, Diego-Palazuelos, P, Errard, J, Finelli, F, Fuskeland, U, Galloway, M, Genova-Santos, RT, Gerbino, M, Ghigna, T, Giardiello, S, Gjerløw, E, Hazumi, M, Henrot-Versillé, S, Kisner, T, Lamagna, L, Lattanzi, M, Levrier, F, Luzzi, G, Maino, D, Masi, S, Migliaccio, M, Montier, L, Morgante, G, Mot, B, Nagata, R, Nati, F, Natoli, P, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Remazeilles, M, Rubino-Martin, J, Sasaki, M, Shiraishi, M, Signorelli, G, Stever, S, Tartari, A, Tristram, M, Tsuji, M, Vacher, L, Wehus, IK, and Zannoni, M

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics
Abstract

We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to the 22 (partially overlapping) LiteBIRD frequency channels. Our in-flight angle calibration relies on nulling the EB cross correlation of the polarized signal in each channel. This calibration step has been carried out by two independent groups with a blind analysis, allowing an accuracy of the order of a few arc-minutes to be reached on the estimate of the angle offsets. Both the corrected and uncorrected multi-frequency maps are propagated through the foreground cleaning step, with the goal of computing clean CMB maps. We employ two component separation algorithms, the Bayesian-Separation of Components and Residuals Estimate Tool (B-SeCRET), and the Needlet Internal Linear Combination (NILC). We find that the recovered CMB maps obtained with algorithms that do not make any assumptions about the foreground properties, such as NILC, are only mildly affected by the angle miscalibration. However, polarization angle offsets strongly bias results obtained with the parametric fitting method. Once the miscalibration angles are corrected by EB nulling prior to the component separation, both component separation algorithms result in an unbiased estimation of the r parameter. While this work is motivated by the conceptual design study for LiteBIRD, its framework can be broadly applied to any CMB polarization experiment. In particular, the combination of simulation plus blind analysis provides a robust forecast by taking into account not only detector sensitivity but also systematic effects.

Published
2022

2. The Simons Observatory: Gain, bandpass and polarization-angle calibration requirements for B-mode searches

Author

Abitbol, MH, Alonso, D, Simon, SM, Lashner, J, Crowley, KT, Ali, AM, Azzoni, S, Baccigalupi, C, Barron, D, Brown, ML, Calabrese, E, Carron, J, Chinone, Y, Chluba, J, Coppi, G, Crowley, KD, Devlin, M, Dunkley, J, Errard, J, Fanfani, V, Galitzki, N, Gerbino, M, Hill, JC, Johnson, BR, Jost, B, Keating, B, Krachmalnicoff, N, Kusaka, A, Lee, AT, Louis, T, Madhavacheril, MS, McCarrick, H, McMahon, J, Meerburg, PD, Nati, F, Nishino, H, Page, LA, Poletti, D, Puglisi, G, Randall, MJ, Rotti, A, Spisak, J, Suzuki, A, Teply, GP, Verges, C, Wollack, EJ, Xu, Z, and Zannoni, M

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

We quantify the calibration requirements for systematic uncertainties for next-generation ground-based observatories targeting the large-angle B-mode polarization of the Cosmic Microwave Background, with a focus on the Simons Observatory (SO). We explore uncertainties on gain calibration, bandpass center frequencies, and polarization angles, including the frequency variation of the latter across the bandpass. We find that gain calibration and bandpass center frequencies must be known to percent levels or less to avoid biases on the tensor-to-scalar ratio r on the order of Δ r∼10-3, in line with previous findings. Polarization angles must be calibrated to the level of a few tenths of a degree, while their frequency variation between the edges of the band must be known to O(10) degrees. Given the tightness of these calibration requirements, we explore the level to which residual uncertainties on these systematics would affect the final constraints on r if included in the data model and marginalized over. We find that the additional parameter freedom does not degrade the final constraints on r significantly, broadening the error bar by O(10%) at most. We validate these results by reanalyzing the latest publicly available data from the collaboration within an extended parameter space covering both cosmological, foreground and systematic parameters. Finally, our results are discussed in light of the instrument design and calibration studies carried out within SO.

Published
2021

4. Sensitivity Modeling for LiteBIRD

Author

Hasebe, T., Ade, P. A. R., Adler, A., Allys, E., Alonso, D., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Basak, S., Battistelli, E., Bautista, L., Beall, J., Beck, D., Beckman, S., Benabed, K., Bermejo-Ballesteros, J., Bersanelli, M., Bonis, J., Borrill, J., Bouchet, F., Boulanger, F., Bounissou, S., Brilenkov, M., Brown, M. L., Bucher, M., Calabrese, E., Calvo, M., Campeti, P., Carones, A., Casas, F. J., Catalano, A., Challinor, A., Chan, V., Cheung, K., Chinone, Y., Cliche, J., Columbro, F., Coulton, W., Cubas, J., Cukierman, A., Curtis, D., D’Alessandro, G., Dachlythra, K., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Torre, S. Della, Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Douillet, D., Duband, L., Ducout, A., Duff, S., Duval, J. M., Ebisawa, K., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Finelli, F., Flauger, R., Franceschet, C., Fuskeland, U., Galli, S., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R. T., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerløw, E., Gradziel, M. L., Grain, J., Grandsire, L., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hamilton, J., Hargrave, P., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Herman, D., Herranz, D., Hill, C. A., Hilton, G., Hivon, E., Hlozek, R. A., Hoang, T. D., Hornsby, A. L., Hoshino, Y., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., Jones, M., Kaga, T., Kashima, S., Katayama, N., Kato, A., Kawasaki, T., Keskitalo, R., Kisner, T., Kobayashi, Y., Kogiso, N., Kogut, A., Kohri, K., Komatsu, E., Komatsu, K., Konishi, K., Krachmalnicoff, N., Kreykenbohm, I., Kuo, C. L., Kushino, A., Lamagna, L., Lanen, J. V., Laquaniello, G., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Louis, T., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Maris, M., Martínez-González, E., Masi, S., Massa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Moggi, A., Monfardini, A., Montgomery, J., Montier, L., Morgante, G., Mot, B., Murata, Y., Murphy, J. A., Nagai, M., Nagano, Y., Nagasaki, T., Nagata, R., Nakamura, S., Nakano, R., Namikawa, T., Nati, F., Natoli, P., Nerval, S., Nishibori, T., Nishino, H., Noviello, F., O’Sullivan, C., Odagiri, K., Ogawa, H., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Passerini, A., Patanchon, G., Pelgrim, V., Peloton, J., Piacentini, F., Piat, M., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J., Russell, M., Sakurai, H., Sakurai, Y., Sandri, M., Sasaki, M., Savini, G., Scott, D., Seibert, J., Sekimoto, Y., Sherwin, B., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Smecher, G., Spinella, F., Stever, S., Stompor, R., Sugiyama, S., Sullivan, R., Suzuki, A., Suzuki, J., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takase, Y., Takeda, Y., Tartari, A., Tavagnacco, D., Taylor, A., Taylor, E., Terao, Y., Thermeau, J., Thommesen, H., Thompson, K. L., Thorne, B., Toda, T., Tomasi, M., Tominaga, M., Trappe, N., Tristram, M., Tsuji, M., Tsujimoto, M., Tucker, C., Ullom, J., Vacher, L., Vermeulen, G., Vielva, P., Villa, F., Vissers, M., Vittorio, N., Wandelt, B., Wang, W., Watanuki, K., Wehus, I. K., Weller, J., Westbrook, B., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Zacchei, A., Zannoni, M., and Zonca, A.

Published
2022
Full Text
View/download PDF

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. Internal Delensing of Cosmic Microwave Background Polarization B-Modes with the POLARBEAR Experiment

Author

Adachi, S, Faúndez, MAO Aguilar, Akiba, Y, Ali, A, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Borrill, J, Carron, J, Cheung, K, Chinone, Y, Crowley, K, Bouhargani, H El, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Goeckner-Wald, N, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Katayama, N, Keating, B, Kikuchi, S, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Matsuda, F, Matsumura, T, Minami, Y, Namikawa, T, Navaroli, M, Nishino, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stompor, R, Tajima, O, Takatori, S, Tanabe, D, Teply, GP, and Vergès, C

Subjects
Particle and High Energy Physics, Physical Sciences, POLARBEAR Collaboration, astro-ph.CO, astro-ph.IM, gr-qc, Mathematical Sciences, Engineering, General Physics, Mathematical sciences, Physical sciences
Abstract

Using only cosmic microwave background polarization data from the polarbear experiment, we measure B-mode polarization delensing on subdegree scales at more than 5σ significance. We achieve a 14% B-mode power variance reduction, the highest to date for internal delensing, and improve this result to 22% by applying for the first time an iterative maximum a posteriori delensing method. Our analysis demonstrates the capability of internal delensing as a means of improving constraints on inflationary models, paving the way for the optimal analysis of next-generation primordial B-mode experiments.

Published
2020

8. Optical Characterization of OMT-Coupled TES Bolometers for LiteBIRD

Author

Hubmayr, J., Ade, P. A. R., Adler, A., Allys, E., Alonso, D., Arnold, K., Auguste, D., Aumont, J., Aurlien, R., Austermann, J. E., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Basak, S., Battistelli, E., Bautista, L., Beall, J. A., Beck, D., Beckman, S., Benabed, K., Bermejo-Ballesteros, J., Bersanelli, M., Bonis, J., Borrill, J., Bouchet, F., Boulanger, F., Bounissou, S., Brilenkov, M., Brown, M. L., Bucher, M., Calabrese, E., Calvo, M., Campeti, P., Carones, A., Casas, F. J., Catalano, A., Challinor, A., Chan, V., Cheung, K., Chinone, Y., Chiocchetta, C., Clark, S. E., Clermont, L., Clesse, S., Cliche, J., Columbro, F., Connors, J. A., Coppolecchia, A., Coulton, W., Cubas, J., Cukierman, A., Curtis, D., Cuttaia, F., D’Alessandro, G., Dachlythra, K., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Daz Garca, J. J., Dickinson, C., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Douillet, D., Doumayrou, E., Duband, L., Ducout, A., Duff, S. M., Duval, J. M., Ebisawa, K., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farrens, S., Finelli, F., Flauger, R., Fleury-Frenette, K., Franceschet, C., Fuskeland, U., Galli, L., Galli, S., Galloway, M., Ganga, K., Gao, J. R., Genova-Santos, R. T., Georges, M., Gerbino, M., Gervasi, M., Ghigna, T., Giardiello, S., Gjerlw, E., Gonzles, R. Gonzlez, Gradziel, M. L., Grain, J., Grandsire, L., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hamilton, J., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versill, S., Hensley, B., Herman, D., Herranz, D., Hilton, G. C., Hivon, E., Hlozek, R. A., Hoang, D., Hornsby, A. L., Hoshino, Y., Ichiki, K., Iida, T., Ikemoto, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G., Jones, M., Kaga, T., Kashima, S., Katayama, N., Kato, A., Kawasaki, T., Keskitalo, R., Kintziger, C., Kisner, T., Kobayashi, Y., Kogiso, N., Kogut, A., Kohri, K., Komatsu, E., Komatsu, K., Konishi, K., Krachmalnicoff, N., Kreykenbohm, I., Kuo, C. L., Kushino, A., Lamagna, L., Lanen, J. V., Laquaniello, G., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Link, M. J., Lonappan, A. I., Louis, T., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Maki, M., Mandelli, S., Maris, M., Marquet, B., Martnez-Gonzlez, E., Martire, F. A., Masi, S., Massa, M., Masuzawa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Mennella, A., Migliaccio, M., Minami, Y., Mitsuda, K., Moggi, A., Monelli, M., Monfardini, A., Montgomery, J., Montier, L., Morgante, G., Mot, B., Murata, Y., Murphy, J. A., Nagai, M., Nagano, Y., Nagasaki, T., Nagata, R., Nakamura, S., Nakano, R., Namikawa, T., Nati, F., Natoli, P., Nerval, S., Neto Godry Farias, N., Nishibori, T., Nishino, H., Noviello, F., O’Neil, G. C., O’Sullivan, C., Odagiri, K., Ochi, H., Ogawa, H., Ogawa, H., Oguri, S., Ohsaki, H., Ohta, I. S., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Pascual Cisneros, G., Passerini, A., Patanchon, G., Pelgrim, V., Peloton, J., Pettorino, V., Piacentini, F., Piat, M., Piccirilli, G., Pinsard, F., Pisano, G., Plesseria, J., Polenta, G., Poletti, D., Prouv, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Reintsema, C. D., Remazeilles, M., Ritacco, A., Rosier, P., Roudil, G., Rubino-Martin, J., Russell, M., Sakurai, H., Sakurai, Y., Sandri, M., Sasaki, M., Savini, G., Scott, D., Seibert, J., Sekimoto, Y., Sherwin, B., Shinozaki, K., Shiraishi, M., Shirron, P., Shitvov, A., Signorelli, G., Smecher, G., Spinella, F., Starck, J., Stever, S., Stompor, R., Sudiwala, R., Sugiyama, S., Sullivan, R., Suzuki, A., Suzuki, J., Suzuki, T., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takase, Y., Takeda, Y., Tartari, A., Tavagnacco, D., Taylor, A., Taylor, E., Terao, Y., Terenzi, L., Thermeau, J., Thommesen, H., Thompson, K. L., Thorne, B., Toda, T., Tomasi, M., Tominaga, M., Trappe, N., Tristram, M., Tsuji, M., Tsujimoto, M., Tucker, C., Ueki, R., Ullom, J. N., Umemori, K., Vacher, L., Van Lanen, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M. R., Vittorio, N., Wandelt, B., Wang, W., Wehus, I. K., Weller, J., Westbrook, B., Weymann-Despres, G., Wilms, J., Winter, B., Wollack, E. J., Yamasaki, N. Y., Yoshida, T., Yumoto, J., Watanuki, K., Zacchei, A., Zannoni, M., and Zonca, A.

Published
2022
Full Text
View/download PDF

9. 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

10. The POLARBEAR Fourier transform spectrometer calibrator and spectroscopic characterization of the POLARBEAR instrument.

Author

Matsuda, F, Lowry, L, Suzuki, A, Aguilar Fáundez, M, Arnold, K, Barron, D, Bianchini, F, Cheung, K, Chinone, Y, Elleflot, T, Fabbian, G, Goeckner-Wald, N, Hasegawa, M, Kaneko, D, Katayama, N, Keating, B, Lee, AT, Navaroli, M, Nishino, H, Paar, H, Puglisi, G, Richards, PL, Seibert, J, Siritanasak, P, Tajima, O, Takatori, S, Tsai, C, and Westbrook, B

Subjects
astro-ph.IM, Physical Sciences, Chemical Sciences, Engineering, Applied Physics
Abstract

We describe the Fourier Transform Spectrometer (FTS) used for in-field testing of the POLARBEAR receiver, an experiment located in the Atacama Desert of Chile which measures the cosmic microwave background (CMB) polarization. The POLARBEAR-FTS (PB-FTS) is a Martin-Puplett interferometer designed to couple to the Huan Tran Telescope (HTT) on which the POLARBEAR receiver is installed. The PB-FTS measured the spectral response of the POLARBEAR receiver with signal-to-noise ratio >20 for ∼69% of the focal plane detectors due to three features: a high throughput of 15.1 sr cm2, optimized optical coupling to the POLARBEAR optics using a custom designed output parabolic mirror, and a continuously modulated output polarizer. The PB-FTS parabolic mirror is designed to mimic the shape of the 2.5 m-diameter HTT primary reflector, which allows for optimum optical coupling to the POLARBEAR receiver, reducing aberrations and systematics. One polarizing grid is placed at the output of the PB-FTS and modulated via continuous rotation. This modulation allows for decomposition of the signal into different harmonics that can be used to probe potentially pernicious sources of systematic error in a polarization-sensitive instrument. The high throughput and continuous output polarizer modulation features are unique compared to other FTS calibrators used in the CMB field. In-field characterization of the POLARBEAR receiver was accomplished using the PB-FTS in April 2014. We discuss the design, construction, and operation of the PB-FTS and present the spectral characterization of the POLARBEAR receiver. We introduce future applications for the PB-FTS in the next-generation CMB experiment, the Simons Array.

Published
2019

11. 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

12. 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

13. 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

17. 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

18. 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

19. Making maps of cosmic microwave background polarization for B-mode studies: The POLARBEAR example

Author

Poletti, D, Fabbian, G, Le Jeune, M, Peloton, J, Arnold, K, Baccigalupi, C, Barron, D, Beckman, S, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, Ducout, A, Elleflot, T, Errard, J, Feeney, S, Goeckner-Wald, N, Groh, J, Hall, G, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaffe, AH, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, L, Matsuda, F, Navaroli, M, Paar, H, Puglisi, G, Reichardt, CL, Ross, C, Siritanasak, P, Stebor, N, Steinbach, B, Stompor, R, Suzuki, A, Tajima, O, Teply, G, and Whitehorn, N

Subjects
cosmic background radiation, cosmology: observations, astro-ph.IM, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. For instance, in the context of ground-based observations, filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this work we have explicitly constructed a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigated the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then discuss the potential implications of these observations on the choice of map-making and power spectrum estimation approaches in the context of B-mode polarization studies. Specifically, we have studied the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may haveon the performance of the popular pseudo-spectrum estimators. We conclude that although maps produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focused on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR. Our analysis and conclusions are however more generally applicable.

Published
2017

22. 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

23. 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

24. 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

25. 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

26. Updated Design of the CMB Polarization Experiment Satellite LiteBIRD

Author

Sugai, H., Ade, P. A. R., Akiba, Y., Alonso, D., Arnold, K., Aumont, J., Austermann, J., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Basak, S., Beall, J., Beckman, S., Bersanelli, M., Borrill, J., Boulanger, F., Brown, M. L., Bucher, M., Buzzelli, A., Calabrese, E., Casas, F. J., Challinor, A., Chan, V., Chinone, Y., Cliche, J.-F., Columbro, F., Cukierman, A., Curtis, D., Danto, P., de Bernardis, P., de Haan, T., De Petris, M., Dickinson, C., Dobbs, M., Dotani, T., Duband, L., Ducout, A., Duff, S., Duivenvoorden, A., Duval, J.-M., Ebisawa, K., Elleflot, T., Enokida, H., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Finelli, F., Flauger, R., Franceschet, C., Fuskeland, U., Ganga, K., Gao, J.-R., Génova-Santos, R., Ghigna, T., Gomez, A., Gradziel, M. L., Grain, J., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hattori, M., Hazumi, M., Henrot-Versille, S., Herranz, D., Hill, C., Hilton, G., Hirota, Y., Hivon, E., Hlozek, R., Hoang, D.-T., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishimura, K., Ishino, H., Jaehnig, G. C., Jones, M., Kaga, T., Kashima, S., Kataoka, Y., Katayama, N., Kawasaki, T., Keskitalo, R., Kibayashi, A., Kikuchi, T., Kimura, K., Kisner, T., Kobayashi, Y., Kogiso, N., Kogut, A., Kohri, K., Komatsu, E., Komatsu, K., Konishi, K., Krachmalnicoff, N., Kuo, C. L., Kurinsky, N., Kushino, A., Kuwata-Gonokami, M., Lamagna, L., Lattanzi, M., Lee, A. T., Linder, E., Maffei, B., Maino, D., Maki, M., Mangilli, A., Martínez-González, E., Masi, S., Mathon, R., Matsumura, T., Mennella, A., Migliaccio, M., Minami, Y., Mistuda, K., Molinari, D., Montier, L., Morgante, G., Mot, B., Murata, Y., Murphy, J. A., Nagai, M., Nagata, R., Nakamura, S., Namikawa, T., Natoli, P., Nerval, S., Nishibori, T., Nishino, H., Nomura, Y., Noviello, F., O’Sullivan, C., Ochi, H., Ogawa, H., Ogawa, H., Ohsaki, H., Ohta, I., Okada, N., Okada, N., Pagano, L., Paiella, A., Paoletti, D., Patanchon, G., Piacentini, F., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Remazeilles, M., Roudil, G., Rubiño-Martín, J. A., Russell, M., Sakurai, H., Sakurai, Y., Sandri, M., Savini, G., Scott, D., Sekimoto, Y., Sherwin, B. D., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Smecher, G., Spizzi, P., Stever, S. L., Stompor, R., Sugiyama, S., Suzuki, A., Suzuki, J., Switzer, E., Takaku, R., Takakura, H., Takakura, S., Takeda, Y., Taylor, A., Taylor, E., Terao, Y., Thompson, K. L., Thorne, B., Tomasi, M., Tomida, H., Trappe, N., Tristram, M., Tsuji, M., Tsujimoto, M., Tucker, C., Ullom, J., Uozumi, S., Utsunomiya, S., Van Lanen, J., Vermeulen, G., Vielva, P., Villa, F., Vissers, M., Vittorio, N., Voisin, F., Walker, I., Watanabe, N., Wehus, I., Weller, J., Westbrook, B., Winter, B., Wollack, E., Yamamoto, R., Yamasaki, N. Y., Yanagisawa, M., Yoshida, T., Yumoto, J., Zannoni, M., and Zonca, A.

Published
2020
Full Text
View/download PDF

27. 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
Full Text
View/download PDF

38. Polarization fraction of Planck Galactic cold clumps and forecasts for the Simons Observatory.

Author

Clancy, J, Puglisi, G, Clark, S E, Coppi, G, Fabbian, G, Hervías-Caimapo, C, Hill, J C, Nati, F, and Reichardt, C L

Subjects
*FRACTIONS, *GALACTIC magnetic fields, *OBSERVATORIES, *ACTINIC flux, *SIGNAL-to-noise ratio
Abstract

We measure the mean-squared polarization fraction of a sample of 6282 Galactic cold clumps at 353 GHz, consisting of Planck Galactic cold clump (PGCC) catalogue category 1 objects [flux densities measured with signal-to-noise ratio (S/N) > 4]. At 353 GHz, we find the mean-squared polarization fraction, which we define as the mean-squared polarization divided by the mean-squared intensity, to be (4.79 ± 0.44) × 10−4 equation to an |$11\, \sigma$| detection of polarization. We test if the polarization fraction depends on the clumps' physical properties, including flux density, luminosity, Galactic latitude, and physical distance. We see a trend towards increasing polarization fraction with increasing Galactic latitude, but find no evidence that polarization depends on the other tested properties. The Simons Observatory, with angular resolution of order 1 arcmin and noise levels between 22 and |$54\, \mu$| K−arcmin at high frequencies, will substantially enhance our ability to determine the magnetic field structure in Galactic cold clumps. At |$\ge 5\, \sigma$| significance, we predict the Simons Observatory will detect at least ∼12 000 cold clumps in intensity and ∼430 cold clumps in polarization. This number of polarization detections would represent a two orders of magnitude increase over the current Planck results. We also release software that can be used to mask these Galactic cold clumps in other analyses. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results