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1. Overview of the Medium and High Frequency Telescopes of the LiteBIRD Satellite Mission

Author: L. Montier, B. Mot, P. de Bernardis, B. Maffei, G. Pisano, F. Columbro, J. E. Gudmundsson, S. Henrot-Versillé, L. Lamagna, J. Montgomery, T. Prouvé, M. Russell, G. Savini, S. Stever, K. L. Thompson, M. Tsujimoto, C. Tucker, B. Westbrook, P. A.R. Ade, A. Adler, E. Allys, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. Austermann, C. Baccigalupi, A. J. Banda, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, D. Beck, S. Beckman, J. Bermejo, M. Bersanelli, J. Bonis, J. Borrill, F. Boulanger, S. Bounissou, M. Brilenkov, M. Brown, M. Bucher, E. Calabrese, P. Campeti, A. Carones, F. J. Casas, A. Challinor, V. Chan, K. Cheung, Y. Chinone, J. F. Cliché, L. Colombo, J. Cubas, A. Cukierman, D. Curtis, G. D’Alessandro, N. Dachlythra, M. De Petris, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, L. Duband, S. Duff, J. M. Duval, K. Ebisawa, T. Elleflot, H. K. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, M. Galloway, K. Ganga, J. R. Gao, R. Genova-Santos, M. Gerbino, M. Gervasi, T. Ghigna, E. Gjerløw, M. L. Gradziel, J. Grain, F. Grupp, A. Gruppuso, T. de Haan, N. W. Halverson, P. Hargrave, T. Hasebe, M. Hasegawa, M. Hattori, M. Hazumi, D. Herman, D. Herranz, C. A. Hill, G. Hilton, Y. Hirota, E. Hivon, R. A. Hlozek, Y. Hoshino, E. de la Hoz, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, K. Ishimura, H. Ishino, G. Jaehnig, T. Kaga, S. Kashima, N. Katayama, A. Kato, T. Kawasaki, R. Keskitalo, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, I. Kreykenbohm, C. L. Kuo, A. Kushino, J. V. Lanen, M. Lattanzi, A.T. Lee, C. Leloup, F. Levrier, E. Linder, T. Louis, G. Luzzi, T. Maciaszek, D. Maino, M. Maki, S. Mandelli, E. Martinez-Gonzalez, S. Masi, T. Matsumura, A. Mennella, M. Migliaccio, Y. Minami, K. Mitsuda, G. Morgante, Y. Murata, J. A. Murphy, M. Nagai, Y. Nagano, T. Nagasaki, R. Nagata, S. Nakamura, T. Namikawa, P. Natoli, S. Nerval, T. Nishibori, H. Nishino, C. O’Sullivan, H. Ogawa, S. Oguri, H. Ohsaki, I. S. Ohta, N. Okada, L. Pagano, A. Paiella, D. Paoletti, G. Patanchon, J. Peloton, F. Piacentini, G. Polenta, D. Poletti, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Reinecke, M. Remazeilles, A. Ritacco, G. Roudil, J. A. Rubino-Martin, H. Sakurai, Y. Sakurai, M. Sandri, M. Sasaki, D. Scott, J. Seibert, Y. Sekimoto, B. Sherwin, K. Shinozaki, M. Shiraishi, P. J. Shirron, G. Signorelli, G. Smecher, R. Stompor, H. Sugai, S. Sugiyama, A. Suzuki, J. Suzuki, T. L. Svalheim, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takase, Y. Takeda, A. Tartari, E. Taylor, Y. Terao, H. Thommesen, B. Thorne, T. Toda, M. Tomasi, M. Tominaga, N. Trappe, M. Tristram, M. Tsuji, J. Ullom, G. Vermeulen, P. Vielva, F. Villa, M. Vissers, N. Vittorio, I. Wehus, J. Weller, J. Wilms, B. Winter, E. J. Wollack, N. Y. Yamasaki, T. Yoshida, J. Yumoto, M. Zannoni, and A. Zonca
Subjects: Instrumentation And Photography, Astrophysics
Abstract: LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium- and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89–224 GHz) and the High-Frequency Telescope (166–448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.
Published: 2020
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2. Optical Characterization of OMT-Coupled TES Bolometers for LiteBIRD

Author: J. Hubmayr, P. A. R. Ade, A. Adler, E. Allys, D. Alonso, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. E. Austermann, S. Azzoni, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, N. Bartolo, S. Basak, E. Battistelli, L. Bautista, J. A. Beall, D. Beck, S. Beckman, K. Benabed, J. Bermejo-Ballesteros, M. Bersanelli, J. Bonis, J. Borrill, F. Bouchet, F. Boulanger, S. Bounissou, M. Brilenkov, M. L. Brown, M. Bucher, E. Calabrese, M. Calvo, P. Campeti, A. Carones, F. J. Casas, A. Catalano, A. Challinor, V. Chan, K. Cheung, Y. Chinone, C. Chiocchetta, S. E. Clark, L. Clermont, S. Clesse, J. Cliche, F. Columbro, J. A. Connors, A. Coppolecchia, W. Coulton, J. Cubas, A. Cukierman, D. Curtis, F. Cuttaia, G. D’Alessandro, K. Dachlythra, P. de Bernardis, T. de Haan, E. de la Hoz, M. De Petris, S. Della Torre, J. J. Daz Garca, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, D. Douillet, E. Doumayrou, L. Duband, A. Ducout, S. M. Duff, J. M. Duval, K. Ebisawa, T. Elleflot, H. K. Eriksen, J. Errard, T. Essinger-Hileman, S. Farrens, F. Finelli, R. Flauger, K. Fleury-Frenette, C. Franceschet, U. Fuskeland, L. Galli, S. Galli, M. Galloway, K. Ganga, J. R. Gao, R. T. Genova-Santos, M. Georges, M. Gerbino, M. Gervasi, T. Ghigna, S. Giardiello, E. Gjerlw, R. Gonzlez Gonzles, M. L. Gradziel, J. Grain, L. Grandsire, F. Grupp, A. Gruppuso, J. E. Gudmundsson, N. W. Halverson, J. Hamilton, P. Hargrave, T. Hasebe, M. Hasegawa, M. Hattori, M. Hazumi, S. Henrot-Versill, B. Hensley, D. Herman, D. Herranz, G. C. Hilton, E. Hivon, R. A. Hlozek, D. Hoang, A. L. Hornsby, Y. Hoshino, K. Ichiki, T. Iida, T. Ikemoto, H. Imada, K. Ishimura, H. Ishino, G. Jaehnig, M. Jones, T. Kaga, S. Kashima, N. Katayama, A. Kato, T. Kawasaki, R. Keskitalo, C. Kintziger, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, I. Kreykenbohm, C. L. Kuo, A. Kushino, L. Lamagna, J. V. Lanen, G. Laquaniello, M. Lattanzi, A. T. Lee, C. Leloup, F. Levrier, E. Linder, M. J. Link, A. I. Lonappan, T. Louis, G. Luzzi, J. Macias-Perez, T. Maciaszek, B. Maffei, D. Maino, M. Maki, S. Mandelli, M. Maris, B. Marquet, E. Martnez-Gonzlez, F. A. Martire, S. Masi, M. Massa, M. Masuzawa, S. Matarrese, F. T. Matsuda, T. Matsumura, L. Mele, A. Mennella, M. Migliaccio, Y. Minami, K. Mitsuda, A. Moggi, M. Monelli, A. Monfardini, J. Montgomery, L. Montier, G. Morgante, B. Mot, Y. Murata, J. A. Murphy, M. Nagai, Y. Nagano, T. Nagasaki, R. Nagata, S. Nakamura, R. Nakano, T. Namikawa, F. Nati, P. Natoli, S. Nerval, N. Neto Godry Farias, T. Nishibori, H. Nishino, F. Noviello, G. C. O’Neil, C. O’Sullivan, K. Odagiri, H. Ochi, H. Ogawa, S. Oguri, H. Ohsaki, I. S. Ohta, N. Okada, L. Pagano, A. Paiella, D. Paoletti, G. Pascual Cisneros, A. Passerini, G. Patanchon, V. Pelgrim, J. Peloton, V. Pettorino, F. Piacentini, M. Piat, G. Piccirilli, F. Pinsard, G. Pisano, J. Plesseria, G. Polenta, D. Poletti, T. Prouv, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Reinecke, C. D. Reintsema, M. Remazeilles, A. Ritacco, P. Rosier, G. Roudil, J. Rubino-Martin, M. Russell, H. Sakurai, Y. Sakurai, M. Sandri, M. Sasaki, G. Savini, D. Scott, J. Seibert, Y. Sekimoto, B. Sherwin, K. Shinozaki, M. Shiraishi, P. Shirron, A. Shitvov, G. Signorelli, G. Smecher, F. Spinella, J. Starck, S. Stever, R. Stompor, R. Sudiwala, S. Sugiyama, R. Sullivan, A. Suzuki, J. Suzuki, T. Suzuki, T. L. Svalheim, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takase, Y. Takeda, A. Tartari, D. Tavagnacco, A. Taylor, E. Taylor, Y. Terao, L. Terenzi, J. Thermeau, H. Thommesen, K. L. Thompson, B. Thorne, T. Toda, M. Tomasi, M. Tominaga, N. Trappe, M. Tristram, M. Tsuji, M. Tsujimoto, C. Tucker, R. Ueki, J. N. Ullom, K. Umemori, L. Vacher, J. Van Lanen, G. Vermeulen, P. Vielva, F. Villa, M. R. Vissers, N. Vittorio, B. Wandelt, W. Wang, I. K. Wehus, J. Weller, B. Westbrook, G. Weymann-Despres, J. Wilms, B. Winter, E. J. Wollack, N. Y. Yamasaki, T. Yoshida, J. Yumoto, K. Watanuki, A. Zacchei, M. Zannoni, A. Zonca, Hubmayr, J, Ade, P, Adler, A, Allys, E, Alonso, D, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Azzoni, S, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, 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, Bucher, M, Calabrese, E, Calvo, M, Campeti, P, Carones, A, Casas, F, Catalano, A, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Chiocchetta, C, Clark, S, Clermont, L, Clesse, S, Cliche, J, Columbro, F, Connors, J, 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, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Douillet, D, Doumayrou, E, Duband, L, Ducout, A, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, 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, Genova-Santos, R, Georges, M, Gerbino, M, Gervasi, M, Ghigna, T, Giardiello, S, Gjerlw, E, Gonzles, R, Gradziel, M, Grain, J, Grandsire, L, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, Hamilton, J, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versill, S, Hensley, B, Herman, D, Herranz, D, Hilton, G, Hivon, E, Hlozek, R, Hoang, D, Hornsby, A, 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, Kushino, A, Lamagna, L, Lanen, J, Laquaniello, G, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Link, M, Lonappan, A, 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, Masi, S, Massa, M, Masuzawa, M, Matarrese, S, Matsuda, F, 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, 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, O’Sullivan, C, Odagiri, K, Ochi, H, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, 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, 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, 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, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ueki, R, Ullom, J, Umemori, K, Vacher, L, Van Lanen, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wandelt, B, Wang, W, Wehus, I, Weller, J, Westbrook, B, Weymann-Despres, G, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Watanuki, K, Zacchei, A, Zannoni, M, Zonca, A, and National Aeronautics and Space Administration (US)
Subjects: CMB, TES, OMT, Low temperature detector, Bolometer, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, General Materials Science, Condensed Matter Physics, CMB, TES, OMT, Low temperature detector, Bolometer, Atomic and Molecular Physics, and Optics
Abstract: et al., Feedhorn- and orthomode transducer- (OMT) coupled transition edge sensor (TES) bolometers have been designed and micro-fabricated to meet the optical specifications of the LiteBIRD high frequency telescope (HFT) focal plane. We discuss the design and optical characterization of two LiteBIRD HFT detector types: dual-polarization, dual-frequency-band pixels with 195/280 GHz and 235/337 GHz band centers. Results show well-matched passbands between orthogonal polarization channels and frequency centers within 3% of the design values. The optical efficiency of each frequency channel is conservatively reported to be within the range 0.64−0.72, determined from the response to a cryogenic, temperature-controlled thermal source. These values are in good agreement with expectations and either exceed or are within 10% of the values used in the LiteBIRD sensitivity forecast. Lastly, we report a measurement of loss in Nb/SiNx/Nb microstrip at 100 mK and over the frequency range 200–350 GHz, which is comparable to values previously reported in the literature., This work is supported by NASA under grant no. 80NSSC18K0132.
Published: 2022

3. Updated design of the CMB polarization experiment satellite LiteBIRD

Author: H. Sugai, P. A. R. Ade, Y. Akiba, D. Alonso, K. Arnold, J. Aumont, J. Austermann, C. Baccigalupi, A. J. Banday, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, S. Beckman, M. Bersanelli, J. Borrill, F. Boulanger, M. L. Brown, M. Bucher, A. Buzzelli, E. Calabrese, F. J. Casas, A. Challinor, V. Chan, Y. Chinone, J.-F. Cliche, F. Columbro, A. Cukierman, D. Curtis, P. Danto, P. de Bernardis, T. de Haan, M. De Petris, C. Dickinson, M. Dobbs, T. Dotani, L. Duband, A. Ducout, S. Duff, A. Duivenvoorden, J.-M. Duval, K. Ebisawa, T. Elleflot, H. Enokida, H. K. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, K. Ganga, J.-R. Gao, R. Génova-Santos, T. Ghigna, A. Gomez, M. L. Gradziel, J. Grain, F. Grupp, A. Gruppuso, J. E. Gudmundsson, N. W. Halverson, P. Hargrave, T. Hasebe, M. Hasegawa, M. Hattori, M. Hazumi, S. Henrot-Versille, D. Herranz, C. Hill, G. Hilton, Y. Hirota, E. Hivon, R. Hlozek, D.-T. Hoang, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, K. Ishimura, H. Ishino, G. C. Jaehnig, M. Jones, T. Kaga, S. Kashima, Y. Kataoka, N. Katayama, T. Kawasaki, R. Keskitalo, A. Kibayashi, T. Kikuchi, K. Kimura, T. Kisner, Y. Kobayashi, N. Kogiso, A. Kogut, K. Kohri, E. Komatsu, K. Komatsu, K. Konishi, N. Krachmalnicoff, C. L. Kuo, N. Kurinsky, A. Kushino, M. Kuwata-Gonokami, L. Lamagna, M. Lattanzi, A. T. Lee, E. Linder, B. Maffei, D. Maino, M. Maki, A. Mangilli, E. Martínez-González, S. Masi, R. Mathon, T. Matsumura, A. Mennella, M. Migliaccio, Y. Minami, K. Mistuda, D. Molinari, L. Montier, G. Morgante, B. Mot, Y. Murata, J. A. Murphy, M. Nagai, R. Nagata, S. Nakamura, T. Namikawa, P. Natoli, S. Nerval, T. Nishibori, H. Nishino, Y. Nomura, F. Noviello, C. O’Sullivan, H. Ochi, H. Ogawa, H. Ohsaki, I. Ohta, N. Okada, L. Pagano, A. Paiella, D. Paoletti, G. Patanchon, F. Piacentini, G. Pisano, G. Polenta, D. Poletti, T. Prouvé, G. Puglisi, D. Rambaud, C. Raum, S. Realini, M. Remazeilles, G. Roudil, J. A. Rubiño-Martín, M. Russell, H. Sakurai, Y. Sakurai, M. Sandri, G. Savini, D. Scott, Y. Sekimoto, B. D. Sherwin, K. Shinozaki, M. Shiraishi, P. Shirron, G. Signorelli, G. Smecher, P. Spizzi, S. L. Stever, R. Stompor, S. Sugiyama, A. Suzuki, J. Suzuki, E. Switzer, R. Takaku, H. Takakura, S. Takakura, Y. Takeda, A. Taylor, E. Taylor, Y. Terao, K. L. Thompson, B. Thorne, M. Tomasi, H. Tomida, N. Trappe, M. Tristram, M. Tsuji, M. Tsujimoto, C. Tucker, J. Ullom, S. Uozumi, S. Utsunomiya, J. Van Lanen, G. Vermeulen, P. Vielva, F. Villa, M. Vissers, N. Vittorio, F. Voisin, I. Walker, N. Watanabe, I. Wehus, J. Weller, B. Westbrook, B. Winter, E. Wollack, R. Yamamoto, N. Y. Yamasaki, M. Yanagisawa, T. Yoshida, J. Yumoto, M. Zannoni, A. Zonca, Sugai, H, Ade, P, Akiba, Y, Alonso, D, Arnold, K, Aumont, J, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beckman, S, Bersanelli, M, Borrill, J, Boulanger, F, Brown, M, Bucher, M, Buzzelli, A, Calabrese, E, Casas, F, Challinor, A, Chan, V, Chinone, Y, Cliche, J, 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, Ebisawa, K, Elleflot, T, Enokida, H, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Ganga, K, Gao, J, Génova-Santos, R, Ghigna, T, Gomez, A, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, Halverson, N, 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, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, 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, Kurinsky, N, Kushino, A, Kuwata-Gonokami, M, Lamagna, L, Lattanzi, M, Lee, A, 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, 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, Ohsaki, H, Ohta, I, 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, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Savini, G, Scott, D, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Spizzi, P, Stever, S, 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, 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, Yanagisawa, M, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, World Premier International Research Center (Japan), Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), European Space Agency, Canadian Space Agency, National Aeronautics and Space Administration (US), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Sugai, H. [0000-0001-6501-3871], and Apollo - University of Cambridge Repository
Subjects: Passive cooling, Cosmic Microwave Background, Cosmology, Polarimetry, Instrumentation, Inflation, Cosmic microwave background, cosmic background radiation: polarization, 7. Clean energy, 01 natural sciences, Polarization, General Materials Science, 010303 astronomy & astrophysics, media_common, Physics, Settore FIS/01, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, suppression, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Infation, adiabatic, Astrophysics - Instrumentation and Methods for Astrophysics, signature, Astrophysics and Astronomy, media_common.quotation_subject, Lagrangian point, Inflation, Primordial gravitational wave, Satellite, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Noise (electronics), Article, NO, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, noise: thermal, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Gravitational wave, PE9_14, beam: width, gravitational radiation: primordial, Astronomy, 13. Climate action, Sky, spectral, galaxy, astro-ph.IM
Abstract: H. Sugai, et al., Recent developments of transition-edge sensors (TESs), based on extensive experience in ground-based experiments, have been making the sensor techniques mature enough for their application on future satellite cosmic microwave background (CMB) polarization experiments. LiteBIRD is in the most advanced phase among such future satellites, targeting its launch in Japanese Fiscal Year 2027 (2027FY) with JAXA’s H3 rocket. It will accommodate more than 4000 TESs in focal planes of reflective low-frequency and refractive medium-and-high-frequency telescopes in order to detect a signature imprinted on the CMB by the primordial gravitational waves predicted in cosmic inflation. The total wide frequency coverage between 34 and 448 GHz enables us to extract such weak spiral polarization patterns through the precise subtraction of our Galaxy’s foreground emission by using spectral differences among CMB and foreground signals. Telescopes are cooled down to 5 K for suppressing thermal noise and contain polarization modulators with transmissive half-wave plates at individual apertures for separating sky polarization signals from artificial polarization and for mitigating from instrumental 1/f noise. Passive cooling by using V-grooves supports active cooling with mechanical coolers as well as adiabatic demagnetization refrigerators. Sky observations from the second Sun–Earth Lagrangian point, L2, are planned for 3 years. An international collaboration between Japan, the USA, Canada, and Europe is sharing various roles. In May 2019, the Institute of Space and Astronautical Science, JAXA, selected LiteBIRD as the strategic large mission No. 2., This work was supported by World Premier International Research Center Initiative (WPI), MEXT, Japan, by JSPS Core-to-Core Program, A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian contribution to the LiteBIRD phase A is supported by the Italian Space Agency (ASI Grant No. 2016-24- H.1-2018) and the National Institute for Nuclear Physics (INFN). The French contribution to the LiteBIRD phase A is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifque (CNRS), and by the Commissariat à l’Energie Atomique (CEA). A Concurrent Design Facility study focused on the MHFT and Sub-Kelvin coolers has been led by the European Space Agency (ESA). The Canadian contribution to LiteBIRD is supported by the Canadian Space Agency. The US contribution is supported by NASA Grant no. 80NSSC18K0132
Published: 2020
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4. The LiteBIRD Satellite Mission: Sub-Kelvin Instrument

Author: A. Suzuki, P. A. R. Ade, Y. Akiba, D. Alonso, K. Arnold, J. Aumont, C. Baccigalupi, D. Barron, S. Basak, S. Beckman, J. Borrill, F. Boulanger, M. Bucher, E. Calabrese, Y. Chinone, S. Cho, B. Crill, A. Cukierman, D. W. Curtis, T. de Haan, M. Dobbs, A. Dominjon, T. Dotani, L. Duband, A. Ducout, J. Dunkley, J. M. Duval, T. Elleflot, H. K. Eriksen, J. Errard, J. Fischer, T. Fujino, T. Funaki, U. Fuskeland, K. Ganga, N. Goeckner-Wald, J. Grain, N. W. Halverson, T. Hamada, T. Hasebe, M. Hasegawa, K. Hattori, M. Hattori, L. Hayes, M. Hazumi, N. Hidehira, C. A. Hill, G. Hilton, J. Hubmayr, K. Ichiki, T. Iida, H. Imada, M. Inoue, Y. Inoue, K. D. Irwin, H. Ishino, O. Jeong, H. Kanai, D. Kaneko, S. Kashima, N. Katayama, T. Kawasaki, S. A. Kernasovskiy, R. Keskitalo, A. Kibayashi, Y. Kida, K. Kimura, T. Kisner, K. Kohri, E. Komatsu, K. Komatsu, C. L. Kuo, N. A. Kurinsky, A. Kusaka, A. Lazarian, A. T. Lee, D. Li, E. Linder, B. Maffei, A. Mangilli, M. Maki, T. Matsumura, S. Matsuura, D. Meilhan, S. Mima, Y. Minami, K. Mitsuda, L. Montier, M. Nagai, T. Nagasaki, R. Nagata, M. Nakajima, S. Nakamura, T. Namikawa, M. Naruse, H. Nishino, T. Nitta, T. Noguchi, H. Ogawa, S. Oguri, N. Okada, A. Okamoto, T. Okamura, C. Otani, G. Patanchon, G. Pisano, G. Rebeiz, M. Remazeilles, P. L. Richards, S. Sakai, Y. Sakurai, Y. Sato, N. Sato, M. Sawada, Y. Segawa, Y. Sekimoto, U. Seljak, B. D. Sherwin, T. Shimizu, K. Shinozaki, R. Stompor, H. Sugai, H. Sugita, J. Suzuki, O. Tajima, S. Takada, R. Takaku, S. Takakura, S. Takatori, D. Tanabe, E. Taylor, K. L. Thompson, B. Thorne, T. Tomaru, T. Tomida, N. Tomita, M. Tristram, C. Tucker, P. Turin, M. Tsujimoto, S. Uozumi, S. Utsunomiya, Y. Uzawa, F. Vansyngel, I. K. Wehus, B. Westbrook, M. Willer, N. Whitehorn, Y. Yamada, R. Yamamoto, N. Yamasaki, T. Yamashita, M. Yoshida, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio spectrum, law.invention, Antenna array, Telescope, Optics, bolometer, Settore FIS/05 - Astronomia e Astrofisica, law, Polarization, 0103 physical sciences, B-mode, Inflation, Satellite, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, activity report, detector: design, Physics, 010308 nuclear & particles physics, business.industry, Gravitational wave, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Astrophysics - Astrophysics of Galaxies, Atomic and Molecular Physics, and Optics, cryogenics, Astrophysics of Galaxies (astro-ph.GA), electronics: readout, interference: quantum, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, cosmic background radiation: anisotropy
Abstract: 著者人数: 153名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 羽澄, 昌史; 今田, 大皓; 満田, 和久; 坂井, 真一郎; Tomida, T.; 辻本, 匡弘; Yamamoto, R.; 山崎, 典子）, Accepted: 2018-04-30, 資料番号: SA1180210000
Published: 2018
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5. POLARBEAR-2: an instrument for CMB polarization measurements

Author: Y. Inoue, P. Ade, Y. Akiba, C. Aleman, K. Arnold, C. Baccigalupi, B. Barch, D. Barron, A. Bender, D. Boettger, J. Borrill, S. Chapman, Y. Chinone, A. Cukierman, T. de Haan, M. A. Dobbs, A. Ducout, R. Dünner, T. Elleflot, J. Errard, G. Fabbian, S. Feeney, C. Feng, G. Fuller, A. J. Gilbert, N. Goeckner-Wald, J. Groh, G. Hall, N. Halverson, T. Hamada, M. Hasegawa, K. Hattori, M. Hazumi, C. Hill, W. L. Holzapfel, Y. Hori, L. Howe, F. Irie, G. Jaehnig, A. Jaffe, O. Jeong, N. Katayama, J. P. Kaufman, K. Kazemzadeh, B. G. Keating, Z. Kermish, R. Keskitalo, T. S. Kisner, A. Kusaka, M. Le Jeune, A. T. Lee, D. Leon, E. V. Linder, L. Lowry, F. Matsuda, T. Matsumura, N. Miller, K. Mizukami, J. Montgomery, M. Navaroli, H. Nishino, H. Paar, J. Peloton, D. Poletti, G. Puglisi, C. R. Raum, G. M. Rebeiz, C. L. Reichardt, P. L. Richards, C. Ross, K. M. Rotermund, Y. Segawa, B. D. Sherwin, I. Shirley, P. Siritanasak, N. Stebor, R. Stompor, J. Suzuki, A. Suzuki, O. Tajima, S. Takada, S. Takatori, G. P. Teply, A. Tikhomirov, T. Tomaru, N. Whitehorn, A. Zahn, O. Zahn, Holland, Wayne S, Zmuidzinas, Jonas, Institut Lagrange de Paris, Sorbonne Université (SU), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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, Ducout, A, Dunner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fuller, G, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, W, Hori, Y, Howe, L, Irie, F, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, J, Kazemzadeh, K, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, A, Leon, D, Linder, E, 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, Rebeiz, G, Reichardt, C, Richards, P, Ross, C, Rotermund, K, Segawa, Y, Sherwin, B, Shirley, I, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, G, Tikhomirov, A, Tomaru, T, Whitehorn, N, Zahn, A, Zahn, O, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, cosmic background radiation: polarization, Gravitational Wave, Astrophysics, 01 natural sciences, law.invention, law, Polarization, Cosmic Microwave Background, neutrino: mass, mirror, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Weak gravitational lensing, Physics, Equipment and services, Settore FIS/05, superconductivity, Astrophysics::Instrumentation and Methods for Astrophysics, Bolometers, Polarization (waves), vacuum system, astro-ph.CO, readout, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, IR filter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Bolometer, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 010309 optics, POLARBEAR-2, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Sensors, Gravitational wave, gravitational radiation: primordial, temperature, millimeter wave, optics, Gravitational lens, Extremely high frequency, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
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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6. The Simons Array CMB polarization experiment

Author: N. Stebor, P. Ade, Y. Akiba, C. Aleman, K. Arnold, C. Baccigalupi, B. Barch, D. Barron, S. Beckman, A. Bender, D. Boettger, J. Borrill, S. Chapman, Y. Chinone, A. Cukierman, T. de Haan, M. Dobbs, A. Ducout, R. Dunner, T. Elleflot, J. Errard, G. Fabbian, S. Feeney, C. Feng, T. Fujino, G. Fuller, A. J. Gilbert, N. Goeckner-Wald, J. Groh, G. Hall, N. Halverson, T. Hamada, M. Hasegawa, K. Hattori, M. Hazumi, C. Hill, W. L. Holzapfel, Y. Hori, L. Howe, Y. Inoue, F. Irie, G. Jaehnig, A. Jaffe, O. Jeong, N. Katayama, J. P. Kaufman, K. Kazemzadeh, B. G. Keating, Z. Kermish, R. Keskitalo, T. Kisner, A. Kusaka, M. Le Jeune, A. T. Lee, D. Leon, E. V. Linder, L. Lowry, F. Matsuda, T. Matsumura, N. Miller, J. Montgomery, M. Navaroli, H. Nishino, H. Paar, J. Peloton, D. Poletti, G. Puglisi, C. R. Raum, G. M. Rebeiz, C. L. Reichardt, P. L. Richards, C. Ross, K. M. Rotermund, Y. Segawa, B. D. Sherwin, I. Shirley, P. Siritanasak, L. Steinmetz, R. Stompor, A. Suzuki, O. Tajima, S. Takada, S. Takatori, G. P. Teply, A. Tikhomirov, T. Tomaru, B. Westbrook, N. Whitehorn, A. Zahn, O. Zahn, Institut Lagrange de Paris, Sorbonne Universités, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Sorbonne Université (SU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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, Dunner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Fuller, G, Gilbert, A, Goeckner-Wald, N, Groh, J, 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, Le Jeune, M, Lee, A, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, C, Richards, P, Ross, C, Rotermund, K, Segawa, Y, Sherwin, B, Shirley, I, Siritanasak, P, Steinmetz, L, Stompor, R, Suzuki, A, Tajima, O, Takada, S, Takatori, S, Teply, G, Tikhomirov, A, Tomaru, T, Westbrook, B, Whitehorn, N, Zahn, A, Zahn, O, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Holland, Wayne S, Zmuidzinas, Jonas, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Gark energy, Cosmic microwave background, Observatories, cosmic background radiation: polarization, 01 natural sciences, Receivers, Multiplexing, law.invention, Cosmic microwave background radiation, law, Observatory, Polarization, Superconductors, dark energy, Physics, Settore FIS/05, precision measurement, superconductivity, polarimeters, Astrophysics::Instrumentation and Methods for Astrophysics, neutrinos, Polarization (waves), Bolometers, cryogenics, amplifier, interference: quantum, Dark matter, gravitational lensing, Gravitational lensing, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter, cosmic background radiation: B-mode, Settore FIS/05 - Astronomia e Astrofisica, bolometer, 0103 physical sciences, Neutrino, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, 010306 general physics, detector: design, activity report, cosmic microwave background radiation, polarization, 010308 nuclear & particles physics, Gravitational wave, Sensors, Bolometer, Astronomy, Polarimeter, Inflation, Amplifiers, Gravitational lens, Antennas, Transition edge sensor, Telescopes
Abstract: International audience; 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.© (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Published: 2016
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7. THE Q/U IMAGING EXPERIMENT INSTRUMENT

Author: C. Bischoff, A. Brizius, I. Buder, Y. Chinone, K. Cleary, R. N. Dumoulin, A. Kusaka, R. Monsalve, S. K. Nxe6ss, L. B. Newburgh, G. Nixon, R. Reeves, K. M. Smith, K. Vanderlinde, I. K. Wehus, M. Bogdan, R. Bustos, S. E. Church, R. Davis, and C. Dickinson et al.
Published: 2013

8. Efficacité et fiabilité de la sédation. Un travail d’observation multicentrique, prospectif mené dans les unités de soins palliatifs au Japon

Author: T. Morita, M. Ikenaga, and Y. Chinone
Subjects: Anesthesiology and Pain Medicine, Oncology, Oncology (nursing)
Published: 2006
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9. Validité de la démarche éthique de la sédation palliative. Un travail d’observation multicentrique, prospectif mené dans les unités de soins palliatifs au Japon

Author: T. Morita, Y. Chinone, and M. Ikenaga
Subjects: Anesthesiology and Pain Medicine, Oncology, Oncology (nursing)
Published: 2006
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10. THE Q/U IMAGING EXPERIMENT INSTRUMENT.

Author: BISCHOFF, C., BRIZIUS, A., BUDER, I., Y. CHINONE, CLEARY, K., DUMOULIN, R. N., KUSAKA, A., MONSALVE, R., NÆSS, S. K., NEWBURGH, L. B., NIXON, G., REEVES, R., SMITH, K. M., VANDERLINDE, K., WEHUS, I. K., BOGDAN, M., BUSTOS, R., CHURCH, S. E., DAVIS, R., and DICKINSON, C.
Subjects: COSMIC background radiation, GRAVITATIONAL waves, BINARY pulsars, POLARISCOPE, FOCAL planes, ELECTRON mobility
Abstract: The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(~1°). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs½) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs½ at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range l ~ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument. [ABSTRACT FROM AUTHOR]
Published: 2013
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11. Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum from Two Years of POLARBEAR Data.

Author: M. Aguilar Faúndez, K. Arnold, C. Baccigalupi, D. Barron, D. Beck, S. Beckman, F. Bianchini, J. Carron, K. Cheung, Y. Chinone, H. El Bouhargani, T. Elleflot, J. Errard, G. Fabbian, C. Feng, T. Fujino, N. Goeckner-Wald, T. Hamada, M. Hasegawa, and M. Hazumi
Subjects: POWER spectra, COSMIC background radiation, MICROWAVE measurements, DARK matter, GRAVITATIONAL lenses
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 AL = 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. [ABSTRACT FROM AUTHOR]
Published: 2020
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12. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment.

Author: Y Chinone, S Adachi, PAR Ade, M Aguilar, Y Akiba, K Arnold, C Baccigalupi, D Barron, D Beck, S Beckman, F Bianchini, D Boettger, J Borrill, H ElBouhargani, J Carron, S Chapman, K Cheung, K Crowley, A Cukierman, and R Dünner
Published: 2020
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13. Applications of High Purity SiC Prepared by Chemical Vapor Deposition

Author: K. Matsumoto, Y. Chinone, F. Fujita, and S. Ezaki
Subjects: Materials science, Hybrid physical-chemical vapor deposition, Chemical engineering, Graphite substrate, Substrate (chemistry), Graphite, Chemical vapor deposition, Combustion chemical vapor deposition
Abstract: Applications of free-standing CVD-SiC films are presented. After the growth of the CVD-SiC on a graphite substrate, we can get freestanding films with various thicknesses by burning off the substrate at high temperature. Three-dimensional complex free-standing products are obtained by using the machined complex graphite. The grown layers are yellow in color and cubic in structure.
Published: 1989
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14. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam.

Author: T. Namikawa, Y. Chinone, H. Miyatake, M. Oguri, R. Takahashi, A. Kusaka, N. Katayama, S. Adachi, M. Aguilar, H. Aihara, A. Ali, R. Armstrong, K. Arnold, C. Baccigalupi, D. Barron, D. Beck, S. Beckman, F. Bianchini, D. Boettger, and J. Borrill
Subjects: *COSMIC background radiation, *DARK matter, *NULL hypothesis, *TEMPERATURE measurements
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. [ABSTRACT FROM AUTHOR]
Published: 2019
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15. Measurements of Tropospheric Ice Clouds with a Ground-based CMB Polarization Experiment, POLARBEAR.

Author: S. Takakura, M. A. O. Aguilar-Faúndez, Y. Akiba, K. Arnold, C. Baccigalupi, D. Barron, D. Beck, F. Bianchini, D. Boettger, J. Borrill, K. Cheung, Y. Chinone, T. Elleflot, J. Errard, G. Fabbian, C. Feng, N. Goeckner-Wald, T. Hamada, M. Hasegawa, and M. Hazumi
Subjects: ICE clouds, ICE crystals, POLARIZATION (Nuclear physics), COSMIC background radiation, TROPOSPHERE, HEAT radiation & absorption, SCATTERING (Physics)
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. [ABSTRACT FROM AUTHOR]
Published: 2019
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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: Collaboration, The POLARBEAR, P. A. R. Ade, M. Aguilar, Y. Akiba, K. Arnold, C. Baccigalupi, D. Barron, D. Beck, F. Bianchini, D. Boettger, J. Borrill, S. Chapman, Y. Chinone, K. Crowley, A. Cukierman, R. Dünner, M. Dobbs, A. Ducout, T. Elleflot, and J. Errard
Subjects: COSMIC background radiation, GRAVITATIONAL lenses, POLARIZATION (Nuclear physics)
Abstract: We report an improved measurement of the cosmic microwave background B-mode polarization power spectrum with the Polarbear experiment at 150 GHz. By adding new data collected during the second season of observations (2013–2014) to re-analyzed data from the first season (2012–2013), we have reduced twofold the band-power uncertainties. The band powers are reported over angular multipoles , where the dominant B-mode signal is expected to be due to the gravitational lensing of E-modes. We reject the null hypothesis of no B-mode polarization at a confidence of 3.1σ including both statistical and systematic uncertainties. We test the consistency of the measured B-modes with the Λ Cold Dark Matter (ΛCDM) framework by fitting for a single lensing amplitude parameter AL relative to the Planck 2015 best-fit model prediction. We obtain ± 0.14(foreground) ± 0.04(multi), where is the fiducial ΛCDM value. [ABSTRACT FROM AUTHOR]
Published: 2017
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17. THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF THE GALACTIC PLANE AT 43 AND 95 GHz.

Author: T. M. Ruud, U. Fuskeland, I. K. Wehus, M. Vidal, D. Araujo, C. Bischoff, I. Buder, Y. Chinone, K. Cleary, R. N. Dumoulin, A. Kusaka, R. Monsalve, S. K. Næss, L. B. Newburgh, R. A. Reeves, J. T. L. Zwart, L. Bronfman, R. D. Davies, R. Davis, and C. Dickinson
Subjects: COSMIC background radiation, METAPHYSICAL cosmology, GALACTIC coordinates, POLARIZATION spectroscopy, FARADAY effect
Abstract: We present polarization observations of two Galactic plane fields centered on Galactic coordinates (l, b) = (0°, 0°) and (329°, 0°) at both Q (43 GHz) and W bands (95 GHz), covering between 301 and 539 square degrees depending on frequency and field. These measurements were made with the QUIET instrument between 2008 October and 2010 December, and include a total of 1263 hr of observations. The resulting maps represent the deepest large-area Galactic polarization observations published to date at the relevant frequencies with instrumental rms noise varying between 1.8 and 2.8 μK deg, 2.3–6 times deeper than corresponding WMAP and Planck maps. The angular resolution is 27.′3 and 12.′8 FWHM at Q and W bands, respectively. We find excellent agreement between the QUIET and WMAP maps over the entire fields, and no compelling evidence for significant residual instrumental systematic errors in either experiment, whereas the Planck 44 GHz map deviates from these in a manner consistent with reported systematic uncertainties for this channel. We combine QUIET and WMAP data to compute inverse-variance-weighted average maps, effectively retaining small angular scales from QUIET and large angular scales from WMAP. From these combined maps, we derive constraints on several important astrophysical quantities, including a robust detection of polarized synchrotron spectral index steepening of ≈0.2 off the plane, as well as the Faraday rotation measure toward the Galactic center (RM = −4000 ± 200 rad m−2), all of which are consistent with previously published results. Both the raw QUIET and the co-added QUIET+WMAP maps are made publicly available together with all necessary ancillary information. [ABSTRACT FROM AUTHOR]
Published: 2015
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18. MODELING ATMOSPHERIC EMISSION FOR CMB GROUND-BASED OBSERVATIONS.

Author: J. Errard, P. A. R. Ade, Y. Akiba, K. Arnold, M. Atlas, C. Baccigalupi, D. Barron, D. Boettger, J. Borrill, S. Chapman, Y. Chinone, A. Cukierman, J. Delabrouille, M. Dobbs, A. Ducout, T. Elleflot, G. Fabbian, C. Feng, S. Feeney, and A. Gilbert
Subjects: COSMIC background radiation, ASTROPHYSICAL radiation, ATMOSPHERIC effects on remote sensing, METEOROLOGICAL optics, SIGNAL detection
Abstract: Atmosphere is one of the most important noise sources for ground-based cosmic microwave background (CMB) experiments. By increasing optical loading on the detectors, it amplifies their effective noise, while its fluctuations introduce spatial and temporal correlations between detected signals. We present a physically motivated 3D-model of the atmosphere total intensity emission in the millimeter and sub-millimeter wavelengths. We derive a new analytical estimate for the correlation between detectors time-ordered data as a function of the instrument and survey design, as well as several atmospheric parameters such as wind, relative humidity, temperature and turbulence characteristics. Using an original numerical computation, we examine the effect of each physical parameter on the correlations in the time series of a given experiment. We then use a parametric-likelihood approach to validate the modeling and estimate atmosphere parameters from the polarbear-i project first season data set. We derive a new 1.0% upper limit on the linear polarization fraction of atmospheric emission. We also compare our results to previous studies and weather station measurements. The proposed model can be used for realistic simulations of future ground-based CMB observations. [ABSTRACT FROM AUTHOR]
Published: 2015
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19. THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF RADIO SOURCES AT 43 AND 95 GHz.

Author: K. M. Huffenberger, D. Araujo, C. Bischoff, I. Buder, Y. Chinone, K. Cleary, A. Kusaka, R. Monsalve, S. K. Næss, L. B. Newburgh, R. Reeves, T. M. Ruud, I. K. Wehus, J. T. L. Zwart, C. Dickinson, H. K. Eriksen, T. Gaier, J. O. Gundersen, M. Hasegawa, and M. Hazumi
Subjects: POLARIZATION microscopy, ASTROCHEMISTRY, GALACTIC center, RADIO galaxies, RADIO astronomy, RADIO sources (Astronomy)
Abstract: We present polarization measurements of extragalactic radio sources observed during the cosmic microwave background polarization survey of the Q/U Imaging Experiment (QUIET), operating at 43 GHz (Q-band) and 95 GHz (W-band). We examine sources selected at 20 GHz from the public, >40 mJy catalog of the Australia Telescope (AT20G) survey. There are ∼480 such sources within QUIET’s four low-foreground survey patches, including the nearby radio galaxies Centaurus A and Pictor A. The median error on our polarized flux density measurements is 30–40 mJy per Stokes parameter. At signal-to-noise ratio > 3 significance, we detect linear polarization for seven sources in Q-band and six in W-band; only 1.3 ± 1.1 detections per frequency band are expected by chance. For sources without a detection of polarized emission, we find that half of the sources have polarization amplitudes below 90 mJy (Q-band) and 106 mJy (W-band), at 95% confidence. Finally, we compare our polarization measurements to intensity and polarization measurements of the same sources from the literature. For the four sources with WMAP and Planck intensity measurements >1 Jy, the polarization fractions are above 1% in both QUIET bands. At high significance, we compute polarization fractions as much as 10%–20% for some sources, but the effects of source variability may cut that level in half for contemporaneous comparisons. Our results indicate that simple models—ones that scale a fixed polarization fraction with frequency—are inadequate to model the behavior of these sources and their contributions to polarization maps. [ABSTRACT FROM AUTHOR]
Published: 2015
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20. Characterization of a half-wave plate for cosmic microwave background circular polarization measurement with POLARBEAR.

Author: Fujino T, Takakura S, Chinone Y, Hasegawa M, Hazumi M, Katayama N, Lee AT, Matsumura T, Minami Y, and Nishino H
Abstract: A half-wave plate (HWP) is often used as a modulator to suppress systematic error in the measurements of cosmic microwave background (CMB) polarization. A HWP can also be used to measure circular polarization (CP) through its optical leakage from CP to linear polarization. The CP of the CMB is predicted from various sources, such as interactions in the Universe and extension of the standard model. Interaction with supernova remnants of population III stars is one of the brightest CP sources. Thus, the observation of the CP of CMB is a new tool for searching for population III stars. In this paper, we demonstrate the improved measurement of the leakage coefficient using the transmission measurement of an actual HWP in the laboratory. We measured the transmittance of linearly polarized light through the HWP used in Polarbear in the frequency range of 120-160 GHz. We evaluate the properties of the HWP by fitting the data with a physical model using the Markov Chain Monte Carlo method. We then estimate the band-averaged CP leakage coefficient using the physical model. We find that the leakage coefficient strongly depends on the spectra of CP sources. We thus calculate the maximum fractional leakage coefficient from CP to linear polarization as 0.133 ± 0.009 in the Rayleigh-Jeans spectrum. The nonzero value shows that Polarbear has a sensitivity to CP. Additionally, because we use the bandpass of detectors installed in the telescope to calculate the band-averaged values, we also consider systematic effects in the experiment., (© 2023 Author(s). Published under an exclusive license by AIP Publishing.)
Published: 2023
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21. C -Methylation of S -adenosyl-L-Methionine Occurs Prior to Cyclopropanation in the Biosynthesis of 1-Amino-2-Methylcyclopropanecarboxylic Acid (Norcoronamic Acid) in a Bacterium.

Author: Maruyama C, Chinone Y, Sato S, Kudo F, Ohsawa K, Kubota J, Hashimoto J, Kozone I, Doi T, Shin-Ya K, Eguchi T, and Hamano Y
Subjects: Bacterial Proteins genetics, Bacterial Proteins metabolism, Cyclopropanes, Lyases genetics, Lyases metabolism, Methyltransferases genetics, Methyltransferases metabolism, Amino Acids biosynthesis, S-Adenosylmethionine metabolism, Streptomyces metabolism
Abstract: Many pharmacologically important peptides are bacterial or fungal in origin and contain nonproteinogenic amino acid (NPA) building blocks. Recently, it was reported that, in bacteria, a cyclopropane-containing NPA 1-aminocyclopropanecarboxylic acid (ACC) is produced from the L-methionine moiety of S -adenosyl-L-methionine (SAM) by non-canonical ACC-forming enzymes. On the other hand, it has been suggested that a monomethylated ACC analogue, 2-methyl-ACC (MeACC), is derived from L-valine. Therefore, we have investigated the MeACC biosynthesis by identifying a gene cluster containing bacterial MeACC synthase genes. In this gene cluster, we identified two genes, orf29 and orf30 , which encode a cobalamin (B12)-dependent radical SAM methyltransferase and a bacterial ACC synthase, respectively, and were found to be involved in the MeACC biosynthesis. In vitro analysis using their recombinant enzymes (rOrf29 and rOrf30) further revealed that the ACC structure of MeACC was derived from the L-methionine moiety of SAM, rather than L-valine. In addition, rOrf29 was found to catalyze the C -methylation of the L-methionine moiety of SAM. The resulting methylated derivative of SAM was then converted into MeACC by rOrf30. Thus, we demonstrate that C -methylation of SAM occurs prior to cyclopropanation in the biosynthesis of a bacterial MeACC (norcoronamic acid).
Published: 2020
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22. Internal Delensing of Cosmic Microwave Background Polarization B-Modes with the POLARBEAR Experiment.

Author: Adachi S, Aguilar Faúndez MAO, Akiba Y, Ali A, Arnold K, Baccigalupi C, Barron D, Beck D, Bianchini F, Borrill J, Carron J, Cheung K, Chinone Y, Crowley K, El Bouhargani H, 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
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
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23. 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
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 cm 2 , 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
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24. Measurement of the cosmic microwave background polarization lensing power spectrum with the POLARBEAR experiment.

Author: Ade PA, Akiba Y, Anthony AE, Arnold K, Atlas M, Barron D, Boettger D, Borrill J, Chapman S, Chinone Y, Dobbs M, Elleflot T, Errard J, Fabbian G, Feng C, Flanigan D, Gilbert A, Grainger W, Halverson NW, Hasegawa M, Hattori K, Hazumi M, Holzapfel WL, Hori Y, Howard J, Hyland P, Inoue Y, Jaehnig GC, Jaffe A, Keating B, Kermish Z, Keskitalo R, Kisner T, Le Jeune M, Lee AT, Linder E, Leitch EM, Lungu M, Matsuda F, Matsumura T, Meng X, Miller NJ, Morii H, Moyerman S, Myers MJ, Navaroli M, Nishino H, Paar H, Peloton J, Quealy E, Rebeiz G, Reichardt CL, Richards PL, Ross C, Schanning I, Schenck DE, Sherwin B, Shimizu A, Shimmin C, Shimon M, Siritanasak P, Smecher G, Spieler H, Stebor N, Steinbach B, Stompor R, Suzuki A, Takakura S, Tomaru T, Wilson B, Yadav A, and Zahn O
Abstract: Gravitational lensing due to the large-scale distribution of matter in the cosmos distorts the primordial cosmic microwave background (CMB) and thereby induces new, small-scale B-mode polarization. This signal carries detailed information about the distribution of all the gravitating matter between the observer and CMB last scattering surface. We report the first direct evidence for polarization lensing based on purely CMB information, from using the four-point correlations of even- and odd-parity E- and B-mode polarization mapped over ∼30 square degrees of the sky measured by the POLARBEAR experiment. These data were analyzed using a blind analysis framework and checked for spurious systematic contamination using null tests and simulations. Evidence for the signal of polarization lensing and lensing B modes is found at 4.2σ (stat+sys) significance. The amplitude of matter fluctuations is measured with a precision of 27%, and is found to be consistent with the Lambda cold dark matter cosmological model. This measurement demonstrates a new technique, capable of mapping all gravitating matter in the Universe, sensitive to the sum of neutrino masses, and essential for cleaning the lensing B-mode signal in searches for primordial gravitational waves.
Published: 2014
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25. Evidence for gravitational lensing of the cosmic microwave background polarization from cross-correlation with the cosmic infrared background.

Author: Ade PA, Akiba Y, Anthony AE, Arnold K, Atlas M, Barron D, Boettger D, Borrill J, Borys C, Chapman S, Chinone Y, Dobbs M, Elleflot T, Errard J, Fabbian G, Feng C, Flanigan D, Gilbert A, Grainger W, Halverson NW, Hasegawa M, Hattori K, Hazumi M, Holzapfel WL, Hori Y, Howard J, Hyland P, Inoue Y, Jaehnig GC, Jaffe A, Keating B, Kermish Z, Keskitalo R, Kisner T, Le Jeune M, Lee AT, Leitch EM, Linder E, Lungu M, Matsuda F, Matsumura T, Meng X, Miller NJ, Morii H, Moyerman S, Myers MJ, Navaroli M, Nishino H, Paar H, Peloton J, Poletti D, Quealy E, Rebeiz G, Reichardt CL, Richards PL, Ross C, Rotermund K, Schanning I, Schenck DE, Sherwin BD, Shimizu A, Shimmin C, Shimon M, Siritanasak P, Smecher G, Spieler H, Stebor N, Steinbach B, Stompor R, Suzuki A, Takakura S, Tikhomirov A, Tomaru T, Wilson B, Yadav A, and Zahn O
Abstract: We reconstruct the gravitational lensing convergence signal from cosmic microwave background (CMB) polarization data taken by the Polarbear experiment and cross-correlate it with cosmic infrared background maps from the Herschel satellite. From the cross spectra, we obtain evidence for gravitational lensing of the CMB polarization at a statistical significance of 4.0σ and indication of the presence of a lensing B-mode signal at a significance of 2.3σ. We demonstrate that our results are not biased by instrumental and astrophysical systematic errors by performing null tests, checks with simulated and real data, and analytical calculations. This measurement of polarization lensing, made via the robust cross-correlation channel, not only reinforces POLARBEAR auto-correlation measurements, but also represents one of the early steps towards establishing CMB polarization lensing as a powerful new probe of cosmology and astrophysics.
Published: 2014
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26. Effect of parenteral hydration therapy based on the Japanese national clinical guideline on quality of life, discomfort, and symptom intensity in patients with advanced cancer.

Author: Yamaguchi T, Morita T, Shinjo T, Inoue S, Takigawa C, Aruga E, Tani K, Hara T, Tamura Y, Suga A, Adachi S, Katayama H, Osaka I, Saito Y, Nakajima N, Higashiguchi T, Hayashi T, Okabe T, Kohara H, Tamaki T, Chinone Y, Aragane H, Kanai Y, Tokura N, Yamaguchi T, Asada T, and Uchitomi Y
Subjects: Aged, Comorbidity, Female, Humans, Japan, Male, Pain mortality, Pain prevention & control, Patient Satisfaction statistics & numerical data, Practice Guidelines as Topic, Prevalence, Risk Factors, Stress, Psychological epidemiology, Stress, Psychological prevention & control, Survival Analysis, Survival Rate, Terminal Care standards, Treatment Outcome, Fluid Therapy mortality, Fluid Therapy standards, Neoplasms mortality, Neoplasms nursing, Parenteral Nutrition mortality, Parenteral Nutrition standards, Quality of Life, Terminal Care statistics & numerical data
Abstract: Context: Although an evidence-based clinical guideline for parenteral hydration therapy was established in Japan, the efficacy of the guideline has not been assessed., Objectives: Our purpose was to explore the effect of parenteral hydration therapy based on this clinical guideline on quality of life (QoL), discomfort, symptoms, and fluid retention signs in patients with advanced cancer., Methods: This multicenter, prospective, observational study included 161 patients with advanced abdominal cancer who received guideline-based hydration therapy. We evaluated the longitudinal changes of the global QoL (Item 30 of European Organization for Research and Treatment of Cancer Quality-of-Life Questionnaire-C30); the Discomfort Scale; the intensity of seven physical symptoms; and the severity of fluid retention signs. We also evaluated patient satisfaction and the feeling of benefit from hydration one week after the study commenced, and bronchial secretions, hyperactive delirium, communication capacity, and agitation 48 hours before a patient's death., Results: The global QoL, the Discomfort Scale, and the intensities of all physical symptoms, except for vomiting and drowsiness, were stable throughout the study period. More than 80% of patients maintained all fluid retention signs. Patient global satisfaction was 76.4 (0-100) and feeling of benefit was 5.43 (range 0-7)., Conclusion: Guideline-based parenteral hydration therapy contributed to maintaining global QoL and provided satisfaction and a feeling of benefit without increasing discomfort and worsening symptoms and fluid retention signs in patients with advanced cancer., (Copyright © 2012 U.S. Cancer Pain Relief Committee. Published by Elsevier Inc. All rights reserved.)
Published: 2012
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27. Note: innovative demodulation scheme for coherent detectors in cosmic microwave background experiments.

Author: Ishidoshiro K, Chinone Y, Hasegawa M, Hazumi M, Nagai M, and Tajima O
Abstract: We propose an innovative demodulation scheme for coherent detectors used in cosmic microwave background polarization experiments. Removal of non-white noise, e.g., narrow-band noise, in detectors is one of the key requirements for the experiments. A combination of modulation and demodulation is used to extract polarization signals as well as to suppress such noise. Traditional demodulation, which is based on the two-point numerical differentiation, works as a first-order high pass filter for the noise. The proposed demodulation is based on the three-point numerical differentiation. It works as a second-order high pass filter. By using a real detector, we confirmed significant improvements of suppression power for the narrow-band noise. We also found improvement of the noise floor.
Published: 2012
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28. Calibration system with cryogenically-cooled loads for cosmic microwave background polarization detectors.

Author: Hasegawa M, Tajima O, Chinone Y, Hazumi M, Ishidoshiro K, and Nagai M
Abstract: We present a novel system to calibrate millimeter-wave polarimeters for cosmic microwave background (CMB) polarization measurements. This technique is an extension of the conventional metal mirror rotation approach, however, it employs cryogenically-cooled blackbody absorbers. The primary advantage of this system is that it can generate a slightly polarized signal (∼100 mK) in the laboratory; this is at a similar level to that measured by ground-based CMB polarization experiments observing a ∼10 K sky. It is important to reproduce the observing condition in the laboratory for reliable characterization of polarimeters before deployment. In this paper, we present the design and principle of the system and demonstrate its use with a coherent-type polarimeter used for an actual CMB polarization experiment. This technique can also be applied to incoherent-type polarimeters and it is very promising for the next-generation CMB polarization experiments.
Published: 2011
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29. Efficacy and safety of palliative sedation therapy: a multicenter, prospective, observational study conducted on specialized palliative care units in Japan.

Author: Morita T, Chinone Y, Ikenaga M, Miyoshi M, Nakaho T, Nishitateno K, Sakonji M, Shima Y, Suenaga K, Takigawa C, Kohara H, Tani K, Kawamura Y, Matsubara T, Watanabe A, Yagi Y, Sasaki T, Higuchi A, Kimura H, Abo H, Ozawa T, Kizawa Y, and Uchitomi Y
Subjects: Adult, Aged, Aged, 80 and over, Female, Humans, Japan, Male, Middle Aged, Palliative Care organization & administration, Prospective Studies, Hypnotics and Sedatives administration & dosage, Hypnotics and Sedatives adverse effects, Neoplasms therapy, Palliative Care methods, Stress, Psychological drug therapy
Abstract: Although palliative sedation therapy is often required in terminally ill cancer patients, its efficacy and safety are not sufficiently understood. The primary aims of this multicenter observational study were to 1) explore the efficacy and safety of palliative sedation therapy, and 2) identify the factors contributing to inadequate symptom relief and complications, using a prospective study design, clearly defined measurement methods, and a consecutive sample from 21 specialized palliative care units in Japan. A sample of 102 consecutive adult cancer patients who received continuous deep sedation were enrolled. Physicians prospectively evaluated the intensity of patient symptoms, communication capacity, respiratory rate, and complications related to sedation. Symptoms were measured on the Agitation Distress Scale, the Memorial Delirium Assessment Scale, and the ad hoc symptom severity scale (0 = no symptoms, 1 = mild and tolerable symptoms, 2 = intolerable symptoms for less than 15 minutes in the previous one hour, and 3 = intolerable symptoms continuing for more than 15 minutes in the previous one hour). Inadequate symptom relief was defined as presence of hyperactive delirium (item 9 of the Memorial Delirium Assessment Scale >or=2) or grade 2 or 3 symptom intensity 4 hours after sedation. The degree of communication capacity was measured on the Communication Capacity Scale. Palliative sedation therapy succeeded in symptom alleviation in 83% of the cases. Median time elapsed before patients initially had one continuous hour of deep sedation was 60 minutes, but 49% of the patients awakened once after falling into a deeply sedated state. The percentage of patients who were capable of explicit communication decreased from 40% before sedation to 7.1% 4 hours after sedation, and the mean Communication Capacity Score significantly decreased to the level of 15 points (P < 0.001). The respiratory rates did not significantly decrease after sedation (18 +/- 9.0 to 16 +/- 9.4/min, P = 0.62), but respiratory and/or circulatory suppression (respiratory rate
Published: 2005
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30. Ethical validity of palliative sedation therapy: a multicenter, prospective, observational study conducted on specialized palliative care units in Japan.

Author: Morita T, Chinone Y, Ikenaga M, Miyoshi M, Nakaho T, Nishitateno K, Sakonji M, Shima Y, Suenaga K, Takigawa C, Kohara H, Tani K, Kawamura Y, Matsubara T, Watanabe A, Yagi Y, Sasaki T, Higuchi A, Kimura H, Abo H, Ozawa T, Kizawa Y, and Uchitomi Y
Subjects: Adult, Aged, Aged, 80 and over, Female, Humans, Japan, Male, Middle Aged, Palliative Care organization & administration, Prospective Studies, Hypnotics and Sedatives therapeutic use, Neoplasms therapy, Palliative Care ethics, Palliative Care methods, Stress, Psychological drug therapy
Abstract: Although palliative sedation therapy is often required in terminally ill cancer patients to achieve acceptable symptom relief, empirical data supporting the ethical validity of this approach are lacking. The primary aim of this study was to systematically investigate whether empirical evidence supports the ethical validity of sedation. This was a multicenter, prospective, observational study, which was conducted by 21 specialized palliative care units in Japan. One-hundred two consecutive adult cancer patients who received continuous deep sedation were enrolled. Continuous deep sedation was defined as the continuous use of sedative medications to relieve intolerable and refractory distress by achieving almost or complete unconsciousness until death. Prior to the study, we conceptualized the ethical validity of sedation from the viewpoints of physicians' intent, proportionality, and autonomy. Sedation was performed mainly with midazolam and phenobarbital. The initial doses of midazolam and phenobarbital were 1.5 mg/hour and 20 mg/hour, respectively. Main administration routes were continuous subcutaneous infusion and continuous intravenous infusion, and no rapid intravenous injection was reported. Of 59 patients who received artificial hydration or could intake adequate fluids/foods orally before sedation, 63% received artificial hydration therapy after sedation, and in the remaining patients, artificial hydration was withheld or withdrawn due to fluid retention symptoms and/or patient wishes. Of 66 patients who were able to verbally express themselves, 95% explicitly stated that symptoms were intolerable. The etiologies of the symptoms requiring sedation were primarily related to the progression of the underlying malignancy, such as cancer cachexia and organ failure, and standard palliative treatments had failed: steroids in 68% of patients with fatigue, opioids in 95% of patients with dyspnea, antisecretion medications in 75% of patients with bronchial secretion, antipsychotic medications in 74% of patients with delirium, and opioids in all patients with pain. On the basis of the Palliative Prognostic Index, 94% of the patients were predicted to die within 3 weeks. Before sedation, 67% of the patients expressed explicit wishes for sedation. In the remaining 34 patients, previous wishes for sedation were noted in 4 patients, and in the other 30 patients, the families were involved in the decision-making process. The chief reason for patient non-involvement in the decision making was cognitive impairment. These data indicate that palliative sedation therapy performed in specialized palliative care units in Japan generally followed the principles of double effect, proportionality, and autonomy.
Published: 2005
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30 results on '"Y. Chinone"'

1. Overview of the Medium and High Frequency Telescopes of the LiteBIRD Satellite Mission

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

3. Updated design of the CMB polarization experiment satellite LiteBIRD

4. The LiteBIRD Satellite Mission: Sub-Kelvin Instrument

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

6. The Simons Array CMB polarization experiment

7. THE Q/U IMAGING EXPERIMENT INSTRUMENT

8. Efficacité et fiabilité de la sédation. Un travail d’observation multicentrique, prospectif mené dans les unités de soins palliatifs au Japon

9. Validité de la démarche éthique de la sédation palliative. Un travail d’observation multicentrique, prospectif mené dans les unités de soins palliatifs au Japon

10. THE Q/U IMAGING EXPERIMENT INSTRUMENT.

11. Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum from Two Years of POLARBEAR Data.

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

13. Applications of High Purity SiC Prepared by Chemical Vapor Deposition

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

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

16. A Measurement of the Cosmic Microwave Background B-mode Polarization Power Spectrum at Subdegree Scales from Two Years of polarbear Data.

17. THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF THE GALACTIC PLANE AT 43 AND 95 GHz.

18. MODELING ATMOSPHERIC EMISSION FOR CMB GROUND-BASED OBSERVATIONS.

19. THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF RADIO SOURCES AT 43 AND 95 GHz.

20. Characterization of a half-wave plate for cosmic microwave background circular polarization measurement with POLARBEAR.

21. C -Methylation of S -adenosyl-L-Methionine Occurs Prior to Cyclopropanation in the Biosynthesis of 1-Amino-2-Methylcyclopropanecarboxylic Acid (Norcoronamic Acid) in a Bacterium.

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

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

24. Measurement of the cosmic microwave background polarization lensing power spectrum with the POLARBEAR experiment.

25. Evidence for gravitational lensing of the cosmic microwave background polarization from cross-correlation with the cosmic infrared background.

26. Effect of parenteral hydration therapy based on the Japanese national clinical guideline on quality of life, discomfort, and symptom intensity in patients with advanced cancer.

27. Note: innovative demodulation scheme for coherent detectors in cosmic microwave background experiments.

28. Calibration system with cryogenically-cooled loads for cosmic microwave background polarization detectors.

29. Efficacy and safety of palliative sedation therapy: a multicenter, prospective, observational study conducted on specialized palliative care units in Japan.

30. Ethical validity of palliative sedation therapy: a multicenter, prospective, observational study conducted on specialized palliative care units in Japan.

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30 results on '"Y. Chinone"'

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