Author: "Tsai, C" / Publication Type: Electronic Resources - Searchworks@Jio Institute Digital Library Search Results

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207 results on '"Tsai, C"'

1. Mitigation of the microbunching instability through transverse Landau damping

Author: Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., Di Mitri, S., Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., and Di Mitri, S.
Abstract: The microbunching instability has been a long-standing issue for high-brightness free-electron lasers (FELs) and is a significant showstopper to achieve full longitudinal coherence in the x-ray regime. This paper reports the first experimental demonstration of microbunching instability mitigation through transverse Landau damping, based on linear optics control in a dispersive region. Analytical predictions for the microbunching content are supported by numerical calculations of the instability gain. The effect is confirmed through the experimental characterization of the spectral brightness of the FERMI FEL under different transverse optics configurations of the transfer line between the linear accelerator and the FEL.
Published: 2024
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2. Mitigation of the microbunching instability through transverse Landau damping

Author: Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., Di Mitri, S., Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., and Di Mitri, S.
Abstract: The microbunching instability has been a long-standing issue for high-brightness free-electron lasers (FELs) and is a significant showstopper to achieve full longitudinal coherence in the x-ray regime. This paper reports the first experimental demonstration of microbunching instability mitigation through transverse Landau damping, based on linear optics control in a dispersive region. Analytical predictions for the microbunching content are supported by numerical calculations of the instability gain. The effect is confirmed through the experimental characterization of the spectral brightness of the FERMI FEL under different transverse optics configurations of the transfer line between the linear accelerator and the FEL.
Published: 2024
Full Text: View/download PDF

3. Mitigation of the microbunching instability through transverse Landau damping

Author: Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., Di Mitri, S., Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., and Di Mitri, S.
Abstract: The microbunching instability has been a long-standing issue for high-brightness free-electron lasers (FELs) and is a significant showstopper to achieve full longitudinal coherence in the x-ray regime. This paper reports the first experimental demonstration of microbunching instability mitigation through transverse Landau damping, based on linear optics control in a dispersive region. Analytical predictions for the microbunching content are supported by numerical calculations of the instability gain. The effect is confirmed through the experimental characterization of the spectral brightness of the FERMI FEL under different transverse optics configurations of the transfer line between the linear accelerator and the FEL.
Published: 2024
Full Text: View/download PDF

4. Mitigation of the microbunching instability through transverse Landau damping

Author: Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., Di Mitri, S., Brynes, A. D., Perosa, Giovanni, Tsai, C. -Y, Allaria, E., Badano, L., De Ninno, G., Ferrari, E., Garzella, D., Giannessi, L., Penco, G., Ribic, P. Rebernik, Roussel, E., Spampinati, S., Spezzani, C., Trovo, M., Veronese, M., and Di Mitri, S.
Abstract: The microbunching instability has been a long-standing issue for high-brightness free-electron lasers (FELs) and is a significant showstopper to achieve full longitudinal coherence in the x-ray regime. This paper reports the first experimental demonstration of microbunching instability mitigation through transverse Landau damping, based on linear optics control in a dispersive region. Analytical predictions for the microbunching content are supported by numerical calculations of the instability gain. The effect is confirmed through the experimental characterization of the spectral brightness of the FERMI FEL under different transverse optics configurations of the transfer line between the linear accelerator and the FEL.
Published: 2024
Full Text: View/download PDF

5. Early childhood caries sequelae and relapse rates in an Australian public dental hospital

Author: Tsai, C, Li, A, Brown, S, Deveridge, C, El Gana, R, Kucera, A, Irving, M, Kumar, H, Tsai, C, Li, A, Brown, S, Deveridge, C, El Gana, R, Kucera, A, Irving, M, and Kumar, H
Abstract: BACKGROUND: Early childhood caries (ECC) remains one of the most prevalent childhood diseases in Australia, disproportionately affecting disadvantaged populations. AIM: To investigate the ECC experience including risk factors, incidence of caries, pain and infection as well as relapse rates of caries and secondary dental general anaesthesia (GA). DESIGN: A retrospective cohort study included dental records of children with ECC, aged <72 months at an Australian public dental hospital paediatric dentistry department from 2013 to 2015 (n = 102). Dental caries, pain, infection, referral patterns, demographic and caries risk factor data were recorded for 24 months. Descriptive statistics were used for patient characteristics and clinical data, and Kaplan-Meier curves and parametric exponential survival models for time-to-event series. RESULTS: The study population demonstrated higher-than-national average dmft and disease progression at baseline. Major risk factors for the development of caries, pain and infection were daily consumption of sweetened beverages, poor oral hygiene, residing in lower socio-economic areas, older age and being male. Rates of caries relapse and new referral for secondary treatment under general anaesthesia were relatively high. CONCLUSION: A high degree of ECC progression and recurrence in this population indicates a need for a more comprehensive approach to ECC addressing multilevel root causes and systemic risk factors.
Published: 2023

6. Perioperative Pembrolizumab for Early-Stage Non-Small-Cell Lung Cancer

Author: Heather, W, Moishe, L, Terufumi, K, Masahiro, T, Se-Hoon, L, Shugeng, G, Ke-Neng, C, Christophe, D, Margarita, M, Ekkehard, E, Gastón L, M, Olivier, B, Delvys, R, Jamie E, C, Silvia, N, Jing, Y, Steven M, K, Ayman, S, Spicer, D Marcelo Tatangelo, J, Flores, M, Pastor, A, Puig, J, Martinengo, G, Varela, M, Brocca, C, Wong, M, Hui, R, Dooms, C, Vansteenkiste, J, Demedts, I, Sibille, A, Surmont, V, Deschepper, K, Lambrechts, M, Dias, J, Rafael Martins De Marchi, P, Alves, G, Henrique Araujo, L, Matias, D, Chaves, F, Franke, F, Teixeira, C, Tabacof, J, Faria, L, Morbeck, I, Henrique Cronemberger, E, Lima, I, Sardenberg, R, de Paiva Junior, T, Dutra, C, Luiz Guimaraes, J, Begin, P, Langleben, A, Liu, G, Liberman, M, Spicer, J, Gao, S, Zhao, G, Jiang, T, Yan, X, Hu, J, Chen, J, Tan, L, Wang, Q, Li, S, Chen, K, Yang, Y, Bai, J, Ma, S, Chen, H, Chen, Q, Wang, W, Zhang, L, Zhu, Y, Vanakesa, T, Zasadny, X, Duchemann, B, Girard, N, Bylicki, O, Berard, H, Thiberville, L, Mennecier, B, Mazieres, J, Eigendorff, E, Bonnet, R, Fix, P, Reck, M, Rittmeyer, A, Reinacher-Schick, A, Wehler, T, Lehmann, M, Serke, M, Wesseler, C, Täuscher, D, Lang, S, Wermke, M, Grohe, C, Wirtz, H, Kollmeier, J, Ritgen, M, Mueller, A, Frohling, K, Vogel, G, Faehling, M, Cuffe, S, Collins, D, Delmonte, A, Gilli, M, Piantedosi, F, Ogliari, F, Bulotta, A, Gregorc, V, Gianni, L, Grisanti, S, Intagliata, S, Roca, E, Ferrari, V, Berruti, A, Cortinovis, D, Lo Russo, G, Ferrara, R, Garassino, M, Rita Migliorino, M, Novello, S, Santoro, A, Signorelli, D, Tsuboi, M, Okada, M, Kato, T, Nishio, W, Kuroda, H, Shimizu, J, Sakao, Y, Sugio, K, Horinouchi, H, Takamochi, K, Saji, H, Tanaka, F, Ikeda, N, Muto, S, Shio, Y, Suzuki, H, Hegmane, A, Cicenas, S, Zemaitis, M, Kek Pang, Y, Yew Heng, F, Leong Yu, K, Lowczak, A, Makles, K, Bryl, M, Zurawski, B, Pawlak, I, Han, J, Lee, S, Kim, J, Yong Shim, B, Cebotaru, C, Ganea, D, Scheusan, R, Ciurescu, I, Mazilu, L, Ungureanu, A, Gal, C, Ciubotaru, E, Iordan, I, Berceanu-Ion, R, Ciuleanu, T, Laktionov, K, Karaseva, N, Smagina, M, Luft, A, Afanasyev, S, Nesterova, A, Levchenko, E, Arkhipov, A, Fedenko, A, Ruff, P, Jacobs, C, Fourie, S, Carcereny, E, Calles Blanco, A, Rodriguez Abreu, D, Majem Tarruella, M, Bosch Barrera, J, Bernabe Caro, R, Nadal Alforja, E, Martnez Marti, A, Liao, B, Huang, H, Chiu, C, Wang, C, Tsai, C, Voitko, N, Kryzhanivska, A, Kolesnik, O, Levenko, O, Bondarenko, I, Trukhin, D, Ursol, G, Paramonov, V, Sokur, I, Khan, S, Arora, A, Goranov, B, Greystoke, A, Ahmed, S, Pope, T, O'Brien, M, Charu, V, Cobb, P, Costin, D, Weksler, B, Schumacher, L, Finley, G, Furqan, M, Gentzler, R, Misleh, J, Guarino, M, Halmos, B, Keresztes, R, Jain, K, Yan Lou, Y, Molina, J, Liu-Dumlao, T, Zhao, Q, Niu, J, Taysir Hammoud, Z, Rybkin, I, Cuevo, R, Fernando, H, Schiller, J, Srkalovic, G, Koontz, M, Stampleman, L, Anderson, I, Villaruz, L, Wang, S, Komiya, T, Jain, S, Starodub, A, Wakelee, H, Kishor Ganti, A, Ernani, V, Kristedja, T, O'Day, S, Radhi, S, Sangal, A, Duvivier, H, Rich, P, Kazmi, S, Pollock, T, Chaft, J, Rathnasabapathy, C, Savvides, P, Costas, K, Kaywin, P, Villalona-Calero, M, Alekshun, T, Rao, S, Siegel, R, Wakelee, Heather, Liberman, Moishe, Kato, Terufumi, Tsuboi, Masahiro, Lee, Se-Hoon, Gao, Shugeng, Chen, Ke-Neng, Dooms, Christophe, Majem, Margarita, Eigendorff, Ekkehard, Martinengo, Gastón L, Bylicki, Olivier, Rodríguez-Abreu, Delvys, Chaft, Jamie E, Novello, Silvia, Yang, Jing, Keller, Steven M, Samkari, Ayman, Jonathan D Marcelo Tatangelo, Marcos Flores, Andrea Pastor, Juan Puig, Gaston Martinengo, Mirta Varela, Carlos Brocca, Mark Wong, Rina Hui, Christophe Dooms, Johan Vansteenkiste, Ingel Demedts, Anne Sibille, Veerle Surmont, Koenraad Deschepper, Marc Lambrechts, Josiane Dias, Pedro Rafael Martins De Marchi, Gustavo Alves, Luiz Henrique Araujo, Danielli Matias, Fabio Chaves, Fabio Franke, Carlos Teixeira, Jacques Tabacof, Luiza Faria, Igor Morbeck, Eduardo Henrique Cronemberger, Iane Lima, Rodrigo Sardenberg, Tadeu de Paiva Junior, Carolina Dutra, Jose Luiz Guimaraes, Paul Begin, Adrian Langleben, Geoffrey Liu, Moishe Liberman, Jonathan Spicer, Shugeng Gao, Guofang Zhao, Tao Jiang, Xiaolong Yan, Jian Hu, Jun Chen, Lijie Tan, Qun Wang, Shanqing Li, Keneng Chen, Yue Yang, Jie Bai, Shaohua Ma, Haiquan Chen, Qixun Chen, Wenxiang Wang, Lanjun Zhang, Yuming Zhu, Tonu Vanakesa, Xavier Zasadny, Boris Duchemann, Nicolas Girard, Olivier Bylicki, Henri Berard, Luc Thiberville, Bertrand Mennecier, Julien Mazieres, Ekkehard Eigendorff, Reiner Bonnet, Peter Fix, Martin Reck, Achim Rittmeyer, Anke Reinacher-Schick, Thomas Wehler, Markus Lehmann, Monika Serke, Claas Wesseler, Dagmar Täuscher, Susanne Lang, Martin Wermke, Christian Grohe, Hubert Wirtz, Jens Kollmeier, Mathias Ritgen, Annette Mueller, Klaus-Peter Frohling, Gunther Vogel, Martin Faehling, Sinead Cuffe, Dearbhaile Collins, Angelo Delmonte, Marina Gilli, Francovito Piantedosi, Francesca Ogliari, Alessandra Bulotta, Vanesa Gregorc, Luca Gianni, Salvatore Grisanti, Salvatore Intagliata, Elisa Roca, Vittorio Ferrari, Alfredo Berruti, Diego Cortinovis, Giuseppe Lo Russo, Roberto Ferrara, Marina Garassino, Maria Rita Migliorino, Silvia Novello, Armando Santoro, Diego Signorelli, Masahiro Tsuboi, Morihito Okada, Terufumi Kato, Wataru Nishio, Hiroaki Kuroda, Junichi Shimizu, Yukinori Sakao, Kenji Sugio, Hidehito Horinouchi, Kazuya Takamochi, Hisashi Saji, Fumihiro Tanaka, Norihiko Ikeda, Satoshi Muto, Yutaka Shio, Hiroyuki Suzuki, Alinta Hegmane, Saulius Cicenas, Marius Zemaitis, Yong Kek Pang, Fook Yew Heng, Kong Leong Yu, Anna Lowczak, Krytsyna Makles, Maciej Bryl, Bogdan Zurawski, Ireneusz Pawlak, Ji-Youn Han, Se-Hoon Lee, Jhingook Kim, Byoung Yong Shim, Cristina Cebotaru, Doina Ganea, Roxana Scheusan, Ioana Ciurescu, Laura Mazilu, Andrei Ungureanu, Cristian Gal, Elena Ciubotaru, Ingrid Iordan, Radu Berceanu-Ion, Tudor Ciuleanu, Konstantin Laktionov, Nina Karaseva, Maria Smagina, Alexander Luft, Sergey Afanasyev, Alfiya Nesterova, Evgeny Levchenko, Alexander Arkhipov, Alexander Fedenko, Paul Ruff, Conrad Jacobs, Samuel Fourie, Enric Carcereny, Antonio Calles Blanco, Delvys Rodriguez Abreu, Margarita Majem Tarruella, Joaquim Bosch Barrera, Reyes Bernabe Caro, Ernest Nadal Alforja, Alex Martnez Marti, Bin-Chi Liao, Hsu-Ching Huang, Chao-Hua Chiu, Chin-Chou Wang, Chen-Liang Tsai, Nataliia Voitko, Anna Kryzhanivska, Olena Kolesnik, Oleh Levenko, Oleksii Kolesnik, Igor Bondarenko, Dmytro Trukhin, Grygorii Ursol, Viktor Paramonov, Iryna Sokur, Sarah Khan, Arvind Arora, Bojidar Goranov, Alastair Greystoke, Samreen Ahmed, Tony Pope, Mary O'Brien, Veena Charu, Patrick Cobb, Dan Costin, Benny Weksler, Lana Schumacher, Gene Finley, Muhammad Furqan, Ryan Gentzler, Jamal Misleh, Michael Guarino, Balazs Halmos, Roger Keresztes, Kirti Jain, Yan Yan Lou, Julian Molina, Theresa Liu-Dumlao, Qing Zhao, Jiaxin Niu, Zane Taysir Hammoud, Igor Rybkin, Raymund Cuevo, Hiran Fernando, Joan Schiller, Gordan Srkalovic, Michael Koontz, Laura Stampleman, Ian Anderson, Liza Villaruz, Sarah Wang, Takefumi Komiya, Sushil Jain, Alexander Starodub, Heather Wakelee, Apar Kishor Ganti, Vinicius Ernani, Timothy Kristedja, Steven O'Day, Saba Radhi, Ashish Sangal, Herbert Duvivier, Patricia Rich, Shayma Kazmi, Theodore Pollock, Jamie Chaft, Chenthilmurugan Rathnasabapathy, Panayiotis Savvides, Kimberly Costas, Paul Kaywin, Miguel Villalona-Calero, Todd Alekshun, Kevin Chen, Suman Rao, Robert Siegel, Heather, W, Moishe, L, Terufumi, K, Masahiro, T, Se-Hoon, L, Shugeng, G, Ke-Neng, C, Christophe, D, Margarita, M, Ekkehard, E, Gastón L, M, Olivier, B, Delvys, R, Jamie E, C, Silvia, N, Jing, Y, Steven M, K, Ayman, S, Spicer, D Marcelo Tatangelo, J, Flores, M, Pastor, A, Puig, J, Martinengo, G, Varela, M, Brocca, C, Wong, M, Hui, R, Dooms, C, Vansteenkiste, J, Demedts, I, Sibille, A, Surmont, V, Deschepper, K, Lambrechts, M, Dias, J, Rafael Martins De Marchi, P, Alves, G, Henrique Araujo, L, Matias, D, Chaves, F, Franke, F, Teixeira, C, Tabacof, J, Faria, L, Morbeck, I, Henrique Cronemberger, E, Lima, I, Sardenberg, R, de Paiva Junior, T, Dutra, C, Luiz Guimaraes, J, Begin, P, Langleben, A, Liu, G, Liberman, M, Spicer, J, Gao, S, Zhao, G, Jiang, T, Yan, X, Hu, J, Chen, J, Tan, L, Wang, Q, Li, S, Chen, K, Yang, Y, Bai, J, Ma, S, Chen, H, Chen, Q, Wang, W, Zhang, L, Zhu, Y, Vanakesa, T, Zasadny, X, Duchemann, B, Girard, N, Bylicki, O, Berard, H, Thiberville, L, Mennecier, B, Mazieres, J, Eigendorff, E, Bonnet, R, Fix, P, Reck, M, Rittmeyer, A, Reinacher-Schick, A, Wehler, T, Lehmann, M, Serke, M, Wesseler, C, Täuscher, D, Lang, S, Wermke, M, Grohe, C, Wirtz, H, Kollmeier, J, Ritgen, M, Mueller, A, Frohling, K, Vogel, G, Faehling, M, Cuffe, S, Collins, D, Delmonte, A, Gilli, M, Piantedosi, F, Ogliari, F, Bulotta, A, Gregorc, V, Gianni, L, Grisanti, S, Intagliata, S, Roca, E, Ferrari, V, Berruti, A, Cortinovis, D, Lo Russo, G, Ferrara, R, Garassino, M, Rita Migliorino, M, Novello, S, Santoro, A, Signorelli, D, Tsuboi, M, Okada, M, Kato, T, Nishio, W, Kuroda, H, Shimizu, J, Sakao, Y, Sugio, K, Horinouchi, H, Takamochi, K, Saji, H, Tanaka, F, Ikeda, N, Muto, S, Shio, Y, Suzuki, H, Hegmane, A, Cicenas, S, Zemaitis, M, Kek Pang, Y, Yew Heng, F, Leong Yu, K, Lowczak, A, Makles, K, Bryl, M, Zurawski, B, Pawlak, I, Han, J, Lee, S, Kim, J, Yong Shim, B, Cebotaru, C, Ganea, D, Scheusan, R, Ciurescu, I, Mazilu, L, Ungureanu, A, Gal, C, Ciubotaru, E, Iordan, I, Berceanu-Ion, R, Ciuleanu, T, Laktionov, K, Karaseva, N, Smagina, M, Luft, A, Afanasyev, S, Nesterova, A, Levchenko, E, Arkhipov, A, Fedenko, A, Ruff, P, Jacobs, C, Fourie, S, Carcereny, E, Calles Blanco, A, Rodriguez Abreu, D, Majem Tarruella, M, Bosch Barrera, J, Bernabe Caro, R, Nadal Alforja, E, Martnez Marti, A, Liao, B, Huang, H, Chiu, C, Wang, C, Tsai, C, Voitko, N, Kryzhanivska, A, Kolesnik, O, Levenko, O, Bondarenko, I, Trukhin, D, Ursol, G, Paramonov, V, Sokur, I, Khan, S, Arora, A, Goranov, B, Greystoke, A, Ahmed, S, Pope, T, O'Brien, M, Charu, V, Cobb, P, Costin, D, Weksler, B, Schumacher, L, Finley, G, Furqan, M, Gentzler, R, Misleh, J, Guarino, M, Halmos, B, Keresztes, R, Jain, K, Yan Lou, Y, Molina, J, Liu-Dumlao, T, Zhao, Q, Niu, J, Taysir Hammoud, Z, Rybkin, I, Cuevo, R, Fernando, H, Schiller, J, Srkalovic, G, Koontz, M, Stampleman, L, Anderson, I, Villaruz, L, Wang, S, Komiya, T, Jain, S, Starodub, A, Wakelee, H, Kishor Ganti, A, Ernani, V, Kristedja, T, O'Day, S, Radhi, S, Sangal, A, Duvivier, H, Rich, P, Kazmi, S, Pollock, T, Chaft, J, Rathnasabapathy, C, Savvides, P, Costas, K, Kaywin, P, Villalona-Calero, M, Alekshun, T, Rao, S, Siegel, R, Wakelee, Heather, Liberman, Moishe, Kato, Terufumi, Tsuboi, Masahiro, Lee, Se-Hoon, Gao, Shugeng, Chen, Ke-Neng, Dooms, Christophe, Majem, Margarita, Eigendorff, Ekkehard, Martinengo, Gastón L, Bylicki, Olivier, Rodríguez-Abreu, Delvys, Chaft, Jamie E, Novello, Silvia, Yang, Jing, Keller, Steven M, Samkari, Ayman, Jonathan D Marcelo Tatangelo, Marcos Flores, Andrea Pastor, Juan Puig, Gaston Martinengo, Mirta Varela, Carlos Brocca, Mark Wong, Rina Hui, Christophe Dooms, Johan Vansteenkiste, Ingel Demedts, Anne Sibille, Veerle Surmont, Koenraad Deschepper, Marc Lambrechts, Josiane Dias, Pedro Rafael Martins De Marchi, Gustavo Alves, Luiz Henrique Araujo, Danielli Matias, Fabio Chaves, Fabio Franke, Carlos Teixeira, Jacques Tabacof, Luiza Faria, Igor Morbeck, Eduardo Henrique Cronemberger, Iane Lima, Rodrigo Sardenberg, Tadeu de Paiva Junior, Carolina Dutra, Jose Luiz Guimaraes, Paul Begin, Adrian Langleben, Geoffrey Liu, Moishe Liberman, Jonathan Spicer, Shugeng Gao, Guofang Zhao, Tao Jiang, Xiaolong Yan, Jian Hu, Jun Chen, Lijie Tan, Qun Wang, Shanqing Li, Keneng Chen, Yue Yang, Jie Bai, Shaohua Ma, Haiquan Chen, Qixun Chen, Wenxiang Wang, Lanjun Zhang, Yuming Zhu, Tonu Vanakesa, Xavier Zasadny, Boris Duchemann, Nicolas Girard, Olivier Bylicki, Henri Berard, Luc Thiberville, Bertrand Mennecier, Julien Mazieres, Ekkehard Eigendorff, Reiner Bonnet, Peter Fix, Martin Reck, Achim Rittmeyer, Anke Reinacher-Schick, Thomas Wehler, Markus Lehmann, Monika Serke, Claas Wesseler, Dagmar Täuscher, Susanne Lang, Martin Wermke, Christian Grohe, Hubert Wirtz, Jens Kollmeier, Mathias Ritgen, Annette Mueller, Klaus-Peter Frohling, Gunther Vogel, Martin Faehling, Sinead Cuffe, Dearbhaile Collins, Angelo Delmonte, Marina Gilli, Francovito Piantedosi, Francesca Ogliari, Alessandra Bulotta, Vanesa Gregorc, Luca Gianni, Salvatore Grisanti, Salvatore Intagliata, Elisa Roca, Vittorio Ferrari, Alfredo Berruti, Diego Cortinovis, Giuseppe Lo Russo, Roberto Ferrara, Marina Garassino, Maria Rita Migliorino, Silvia Novello, Armando Santoro, Diego Signorelli, Masahiro Tsuboi, Morihito Okada, Terufumi Kato, Wataru Nishio, Hiroaki Kuroda, Junichi Shimizu, Yukinori Sakao, Kenji Sugio, Hidehito Horinouchi, Kazuya Takamochi, Hisashi Saji, Fumihiro Tanaka, Norihiko Ikeda, Satoshi Muto, Yutaka Shio, Hiroyuki Suzuki, Alinta Hegmane, Saulius Cicenas, Marius Zemaitis, Yong Kek Pang, Fook Yew Heng, Kong Leong Yu, Anna Lowczak, Krytsyna Makles, Maciej Bryl, Bogdan Zurawski, Ireneusz Pawlak, Ji-Youn Han, Se-Hoon Lee, Jhingook Kim, Byoung Yong Shim, Cristina Cebotaru, Doina Ganea, Roxana Scheusan, Ioana Ciurescu, Laura Mazilu, Andrei Ungureanu, Cristian Gal, Elena Ciubotaru, Ingrid Iordan, Radu Berceanu-Ion, Tudor Ciuleanu, Konstantin Laktionov, Nina Karaseva, Maria Smagina, Alexander Luft, Sergey Afanasyev, Alfiya Nesterova, Evgeny Levchenko, Alexander Arkhipov, Alexander Fedenko, Paul Ruff, Conrad Jacobs, Samuel Fourie, Enric Carcereny, Antonio Calles Blanco, Delvys Rodriguez Abreu, Margarita Majem Tarruella, Joaquim Bosch Barrera, Reyes Bernabe Caro, Ernest Nadal Alforja, Alex Martnez Marti, Bin-Chi Liao, Hsu-Ching Huang, Chao-Hua Chiu, Chin-Chou Wang, Chen-Liang Tsai, Nataliia Voitko, Anna Kryzhanivska, Olena Kolesnik, Oleh Levenko, Oleksii Kolesnik, Igor Bondarenko, Dmytro Trukhin, Grygorii Ursol, Viktor Paramonov, Iryna Sokur, Sarah Khan, Arvind Arora, Bojidar Goranov, Alastair Greystoke, Samreen Ahmed, Tony Pope, Mary O'Brien, Veena Charu, Patrick Cobb, Dan Costin, Benny Weksler, Lana Schumacher, Gene Finley, Muhammad Furqan, Ryan Gentzler, Jamal Misleh, Michael Guarino, Balazs Halmos, Roger Keresztes, Kirti Jain, Yan Yan Lou, Julian Molina, Theresa Liu-Dumlao, Qing Zhao, Jiaxin Niu, Zane Taysir Hammoud, Igor Rybkin, Raymund Cuevo, Hiran Fernando, Joan Schiller, Gordan Srkalovic, Michael Koontz, Laura Stampleman, Ian Anderson, Liza Villaruz, Sarah Wang, Takefumi Komiya, Sushil Jain, Alexander Starodub, Heather Wakelee, Apar Kishor Ganti, Vinicius Ernani, Timothy Kristedja, Steven O'Day, Saba Radhi, Ashish Sangal, Herbert Duvivier, Patricia Rich, Shayma Kazmi, Theodore Pollock, Jamie Chaft, Chenthilmurugan Rathnasabapathy, Panayiotis Savvides, Kimberly Costas, Paul Kaywin, Miguel Villalona-Calero, Todd Alekshun, Kevin Chen, Suman Rao, and Robert Siegel
Abstract: BACKGROUND Among patients with resectable early-stage non-small-cell lung cancer (NSCLC), a perioperative approach that includes both neoadjuvant and adjuvant immune checkpoint inhibition may provide benefit beyond either approach alone. METHODS We conducted a randomized, double-blind, phase 3 trial to evaluate perioperative pembrolizumab in patients with early-stage NSCLC. Participants with resectable stage II, IIIA, or IIIB (N2 stage) NSCLC were assigned in a 1:1 ratio to receive neoadjuvant pembrolizumab (200 mg) or placebo once every 3 weeks, each of which was given with cisplatin-based chemotherapy for 4 cycles, followed by surgery and adjuvant pembrolizumab (200 mg) or placebo once every 3 weeks for up to 13 cycles. The dual primary end points were event-free survival (the time from randomization to the first occurrence of local progression that precluded the planned surgery, unresectable tumor, progression or recurrence, or death) and overall survival. Secondary end points included major pathological response, pathological complete response, and safety. RESULTS A total of 397 participants were assigned to the pembrolizumab group, and 400 to the placebo group. At the prespecified first interim analysis, the median follow-up was 25.2 months. Event-free survival at 24 months was 62.4% in the pembrolizumab group and 40.6% in the placebo group (hazard ratio for progression, recurrence, or death, 0.58; 95% confidence interval [CI], 0.46 to 0.72; P<0.001). The estimated 24-month overall survival was 80.9% in the pembrolizumab group and 77.6% in the placebo group (P = 0.02, which did not meet the significance criterion). A major pathological response occurred in 30.2% of the participants in the pembrolizumab group and in 11.0% of those in the placebo group (difference, 19.2 percentage points; 95% CI, 13.9 to 24.7; P<0.0001; threshold, P = 0.0001), and a pathological complete response occurred in 18.1% and 4.0%, respectively (difference, 14.2 percentage points
Published: 2023

7. Results and Limits of Time Division Multiplexing for the BICEP Array High Frequency Receivers

Author: Fatigoni, S., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Beck, D., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Filippini, J. P., Fortes, A., Gao, M., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J. A., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Handerson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J. H., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Lennox, A., Liu, T., Megerian, K. G., Miller, O. Y., Minutolo, L., Moncelsi, L., Nakato, Y., Nguyen, H. T., Brient, R. O, Palladino, S., Petroff, M. A., Polish, A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Romand, T., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Germaine, T. St., Steiger, A., Steinbach, B., Sudiwala, R., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vèrges, C., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, E., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Fatigoni, S., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Beck, D., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Filippini, J. P., Fortes, A., Gao, M., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J. A., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Handerson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J. H., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Lennox, A., Liu, T., Megerian, K. G., Miller, O. Y., Minutolo, L., Moncelsi, L., Nakato, Y., Nguyen, H. T., Brient, R. O, Palladino, S., Petroff, M. A., Polish, A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Romand, T., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Germaine, T. St., Steiger, A., Steinbach, B., Sudiwala, R., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vèrges, C., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, E., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.
Abstract: Time-Division Multiplexing is the readout architecture of choice for many ground and space experiments, as it is a very mature technology with proven outstanding low-frequency noise stability, which represents a central challenge in multiplexing. Once fully populated, each of the two BICEP Array high frequency receivers, observing at 150GHz and 220/270GHz, will have 7776 TES detectors tiled on the focal plane. The constraints set by these two receivers required a redesign of the warm readout electronics. The new version of the standard Multi Channel Electronics, developed and built at the University of British Columbia, is presented here for the first time. BICEP Array operates Time Division Multiplexing readout technology to the limits of its capabilities in terms of multiplexing rate, noise and crosstalk, and applies them in rigorously demanding scientific application requiring extreme noise performance and systematic error control. Future experiments like CMB-S4 plan to use TES bolometers with Time Division/SQUID-based readout for an even larger number of detectors., Comment: 10 pages, 7 figures, Submitted to Journal of Low Temperature Physics
Published: 2023

8. Ipsilateral radiation for squamous cell carcinoma of the tonsil: American Radium Society appropriate use criteria executive summary.

Author: Tsai, C Jillian, Tsai, C Jillian, Galloway, Thomas J, Margalit, Danielle N, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven, Chen, Allen, Cooper, Jay, Koyfman, Shlomo A, Ridge, John A, Robbins, Jared, Truong, Minh Tam, Yom, Sue S, Siddiqui, Farzan, Tsai, C Jillian, Tsai, C Jillian, Galloway, Thomas J, Margalit, Danielle N, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven, Chen, Allen, Cooper, Jay, Koyfman, Shlomo A, Ridge, John A, Robbins, Jared, Truong, Minh Tam, Yom, Sue S, and Siddiqui, Farzan
Abstract: BackgroundWe conducted the current systemic review to provide up-to-date literature summary and optimal evidence-based recommendations for ipsilateral radiation for squamous cell carcinoma of the tonsil.MethodsWe performed literature search of peer-reviewed journals through PubMed. The search strategy and subject-specific keywords were developed based on the expert panel's consensus. Articles published from January 2000 to May 2020 with full text available on PubMed and restricted to the English language and human subjects were included. Several prespecified search terms were used to identify relevant publications and additional evidence published since the initial American College of Radiology Appropriateness Criteria Ipsilateral Tonsil Radiation recommendation was finalized in 2012. The full bibliographies of identified articles were reviewed and irrelevant studies were removed.ResultsThe initial search and review returned 46 citations. The authors added three citations from bibliographies, websites, or books not found in the literature search. Of the 49 citations, 30 citations were retained for further detailed review, and 14 of them were added to the evidence table. Articles were removed from the bibliography if they were not relevant or generalizable to the topic, or focused on unknown primary disease. Several commonly encountered clinical case variants were created and panelists anonymously rated each treatment recommendation. The results were reviewed and disagreements discussed.ConclusionsThe panel provided updated evidence and recommendations for ipsilateral radiation for squamous cell carcinoma of the tonsil in the setting of primary radiation-based therapy and postoperative adjuvant radiotherapy. This committee did not reach agreements for some case variants due to a lack of strong evidence supporting specific treatment decisions, indicating a further need for research in these topics.
Published: 2021

9. Thatchtelithichnus on a pliocene grey whale mandible and barnacles as possible tracemakers

Author: Collareta, A, Tsai, C, Coletti, G, Bosselaers, M, Collareta A., Tsai C. -H., Coletti G., Bosselaers M., Collareta, A, Tsai, C, Coletti, G, Bosselaers, M, Collareta A., Tsai C. -H., Coletti G., and Bosselaers M.
Abstract: The ichnogenus Thatchtelithichnus Zonneveld, Bartels, Gunnell & McHugh was created for ring-shaped, roughly circular grooves affecting the outer surface of plastral bones of Eocene geoemydid turtles. Such traces were assumed to be attachment scars of aquatic ectoparasites (possibly ticks, leeches or liver flukes). Despite its well-distinctive aspect, Thatchtelithichnus has only been reported subsequently by few works and mostly from the plastron-bottom of freshwater turtles. Here we provide the first record of Thatchtelithichnus from a fossil mammal bone, namely, a partial grey whale mandible from the Belgian Pliocene. Thatchtelithichnus traces from this cetacean fossil commonly penetrate into the outermost portion of the cancellous bone, achieving a maximum depth of about 2 mm. The external margin of these grooves is sharply defined and commonly follows an elliptical, somewhat festooned path. A scrutiny of recent literature in palaeontological and forensic taphonomy as well as new first-hand observations reveal that Thatchtelithichnus-like structures can be produced by the attachment of barnacles on the surface of mammal bones that suffered long-lasting exposure on the seafloor. When encrusting bare bones in marine settings, barnacles can thus produce a variety of traces, including Anellusichnus Santos, Mayoral & Muñiz, Thatchtelithichnus and, possibly, Karethraichnus lakkos Zonneveld, Bartels, Gunnell & McHugh. The modes of trace formation are still largely to be understood, but observations on how barnacles damage paint coatings during growth might help us in envisaging how this kind of process works.
Published: 2021

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

Author: Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., Zhou Y., Segawa, Y, Hirose, H, Kaneko, D, Hasegawa, M, Adachi, S, Ade, P, Faundez, M, Akiba, Y, Arnold, K, Avva, J, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, De Haan, T, Dobbs, M, Dunner, R, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Ito, J, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Raum, C, Reichardt, C, Ross, C, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Segawa Y., Hirose H., Kaneko D., Hasegawa M., Adachi S., Ade P., Faundez M. A. O. A., Akiba Y., Arnold K., Avva J., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., De Haan T., Dobbs M., Dunner R., Bouhargani H. E., Elleflot T., Errard J., Fabbian G., Feeney S., Feng C., Fujino T., Galitzki N., Goeckner-Wald N., Groh J., Hall G., Halverson N., Hamada T., Hazumi M., Hill C., Howe L., Inoue Y., Ito J., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Montgomery J., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Raum C., Reichardt C. L., Ross C., Silva-Feaver M., Siritanasak P., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tsai C., Verges C., Westbrook B., and Zhou Y.
Abstract: POLARBEAR-2A is the first receiver for the Simons Array cosmic microwave background polarization experiment. POLARBEAR-2A has transition-edge sensor bolometers on the focal plane. Signals from bolometers are multiplexed and read out by a single SQUID. The receiver was deployed in late 2018 in Atacama, Chile, and operation started in 2019, where rapid confirmation of correspondence between bolometers and multiplexed readout channels was important as an initial step of performance validation. For this purpose, we devised a method using a coherent source that allows us to identify the frequency band and polarization sensitivity angle for each readout channel without detailed bolometer tuning.
Published: 2021

11. The Large Dispersion and Scattering of FRB 20190520B are Dominated by the Host Galaxy

Author: Ocker, S. K., Cordes, J. M., Chatterjee, S., Niu, C. -H., Li, D., McKee, J. W., Law, C. J., Tsai, C. -W., Anna-Thomas, R., Yao, J. -M., Cruces, M., Ocker, S. K., Cordes, J. M., Chatterjee, S., Niu, C. -H., Li, D., McKee, J. W., Law, C. J., Tsai, C. -W., Anna-Thomas, R., Yao, J. -M., and Cruces, M.
Abstract: The repeating FRB 20190520B is localized to a galaxy at $z=0.241$, much closer than expected given its dispersion measure $\rm DM=1205\pm4 pc\ cm^{-3}$. Here we assess implications of the large DM and scattering observed from FRB 20190520B for the host galaxy's plasma properties. A sample of 75 bursts detected with the Five-hundred-meter Aperture Spherical radio Telescope shows scattering on two scales: a mean temporal delay $\tau(1.41\ {\rm GHz})=10.9\pm1.5$ ms, which is attributed to the host galaxy, and a mean scintillation bandwidth $\nu_{\rm d}(1.41\ {\rm GHz})=0.21\pm0.01$ MHz, which is attributed to the Milky Way. Balmer line measurements for the host imply an H$\alpha$ emission measure (galaxy frame) $\rm EM_s=620$ pc cm$^{-6} \times (T/10^4 {\rm K})^{0.9}$, implying $\rm DM_{\rm H\alpha}$ of order the value inferred from the FRB DM budget, $\rm DM_h=1121^{+89}_{-138}$ pc cm$^{-3}$ for plasma temperatures greater than the typical value $10^4$ K. Combining $\tau$ and $\rm DM_h$ yields a nominal constraint on the scattering amplification from the host galaxy $\tilde{F} G=1.5^{+0.8}_{-0.3}$ (pc$^2$ km)$^{-1/3}$, where $\tilde{F}$ describes turbulent density fluctuations and $G$ represents the geometric leverage to scattering that depends on the location of the scattering material. For a two-screen scattering geometry where $\tau$ arises from the host galaxy and $\Delta \nu_{\rm d}$ from the Milky Way, the implied distance between the FRB source and dominant scattering material is $\lesssim100$ pc. The host galaxy scattering and DM contributions support a novel technique for estimating FRB redshifts using the $\tau-\rm DM$ relation, and are consistent with previous findings that scattering of localized FRBs is largely dominated by plasma within host galaxies and the Milky Way., Comment: 14 pages, 9 figures, accepted to ApJ
Published: 2022

12. Magnetic Field Reversal around an Active Fast Radio Burst

Author: Dai, S., Feng, Y., Yang, Y. P., Zhang, Y. K., Li, D., Niu, C. H., Wang, P., Xue, M. Y., Zhang, B., Burke-Spolaor, S., Law, C. J., Lynch, R. S., Connor, L., Anna-Thomas, R., Zhang, L., Duan, R., Yao, J. M., Tsai, C. W., Zhu, W. W., Cruces, M., Hobbs, G., Miao, C. C., Niu, J. R., Filipovic, M. D., Zhu, S. Q., Dai, S., Feng, Y., Yang, Y. P., Zhang, Y. K., Li, D., Niu, C. H., Wang, P., Xue, M. Y., Zhang, B., Burke-Spolaor, S., Law, C. J., Lynch, R. S., Connor, L., Anna-Thomas, R., Zhang, L., Duan, R., Yao, J. M., Tsai, C. W., Zhu, W. W., Cruces, M., Hobbs, G., Miao, C. C., Niu, J. R., Filipovic, M. D., and Zhu, S. Q.
Abstract: The environment of actively repeating fast radio bursts (FRBs) has been shown to be complex and varying. The recently localized FRB 20190520B is extremely active, has the largest confirmed host dispersion measure, and is only the second FRB source associated with a compact, persistent radio source (PRS). The main tracer of the magneto-ionic environments is the rotation measure (RM), a path-integral of the line-of-sight component of magnetic field strength (B) and electron density, which does not allow a direct probe of the B-field configuration. Here we report direct evidence for a B-field reversal based on the observed sign change and extreme variation of FRB 20190520B's RM, which changed from $\sim10000$ rad m$^{-2}$ to $\sim-16000$ rad m$^{-2}$ between June 2021 and January 2022. Such extreme RM reversal has never been observed before in any FRB nor in any astronomical object. The implied short-term change of the B-field configuration in or around the FRB could be due to the vicinity of massive black holes, or a magnetized companion star in binary systems, or a young supernova remnant along the line of sight., Comment: Submitted
Published: 2022

13. Relationships of familial sexual stigma and family support with internalized homonegativity among lesbian, gay and bisexual individuals : The mediating effect of self-identity disturbance and moderating effect of gender

Author: Lin, C. -Y, Griffiths, M. D., Pakpour, Amir H., Tsai, C. -S, Yen, C. -F, Lin, C. -Y, Griffiths, M. D., Pakpour, Amir H., Tsai, C. -S, and Yen, C. -F
Abstract: Background: The mediators of the association between familial attitudes toward sexual orientation and internalized homonegativity among lesbian, gay, and bisexual (LGB) individuals have not been well examined. Methods: A cross-sectional survey study was carried out to examine the (i) associations of familial sexual stigma and family support with internalized homonegativity among young adult LGB individuals in Taiwan, and (ii) mediating effect of self-identity disturbance and the moderating effect of gender. Self-identified LGB individuals (N = 1000; 50% males and 50% females; mean age = 24.6 years) participated in the study. Familial sexual stigma, family support, self-identity disturbance, and internalized homonegativity were assessed. Structural equation modeling was used to examine relationships between the variables. Results: The results indicated that familial sexual stigma was directly associated with increased internalized homonegativity, and indirectly associated with increased internalized homonegativity via the mediation of self-identity disturbance among LGB individuals. Family support was indirectly associated with decreased internalized homonegativity via the mediation of low self-identity disturbance. The direct association between family support and internalized homonegativity was only found among lesbian and bisexual women but not among gay and bisexual men. Conclusions: Program interventions for familial sexual stigma, family support, and self-identity disturbance are warranted to help reduce internalized homonegativity among LGB individuals.
Published: 2022
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14. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author: Westbrook, B., Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bender, A. N., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Coppi, G., Crowley, K., Cukierman, A., de, T., Dünner, R., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fuller, G., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Holzapfel, W., Howe, L., Inoue, Y., Jaehnig, G., Jaffe, A., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Le, M., Lee, A. T., Leon, D., Linder, E., Lowry, L., Madurowicz, A., Mak, D., Matsuda, F., May, A., Miller, N. J., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Peloton, J., Pham, A., Piccirillo, L., Plambeck, D., Poletti, D., Puglisi, G., Raum, C., Rebeiz, G., Reichardt, C. L., Richards, P. L., Roberts, H., Ross, C., Rotermund, K. M., Segawa, Y., Sherwin, B., Silva-Feaver, M., Siritanasak, P., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Tat, R., Teply, G. P., Tikhomirov, A., Tomaru, T., Tsai, C., Whitehorn, N., Zahn, A., Westbrook, B., Ade, P. A. R., Aguilar, M., Akiba, Y., Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bender, A. N., Bianchini, F., Boettger, D., Borrill, J., Chapman, S., Chinone, Y., Coppi, G., Crowley, K., Cukierman, A., de, T., Dünner, R., Dobbs, M., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fuller, G., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Holzapfel, W., Howe, L., Inoue, Y., Jaehnig, G., Jaffe, A., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kisner, T., Krachmalnicoff, N., Kusaka, A., Le, M., Lee, A. T., Leon, D., Linder, E., Lowry, L., Madurowicz, A., Mak, D., Matsuda, F., May, A., Miller, N. J., Minami, Y., Montgomery, J., Navaroli, M., Nishino, H., Peloton, J., Pham, A., Piccirillo, L., Plambeck, D., Poletti, D., Puglisi, G., Raum, C., Rebeiz, G., Reichardt, C. L., Richards, P. L., Roberts, H., Ross, C., Rotermund, K. M., Segawa, Y., Sherwin, B., Silva-Feaver, M., Siritanasak, P., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Tat, R., Teply, G. P., Tikhomirov, A., Tomaru, T., Tsai, C., Whitehorn, N., and Zahn, A.
Abstract: We present on the status of POLARBEAR-2 A (PB2-A) focal plane fabrication. The PB2-A is the first of three telescopes in the Simon Array (SA), which is an array of three cosmic microwave background (CMB) polarization sensitive telescopes located at the POLARBEAR (PB) site in Northern Chile. As the successor to the PB experiment, each telescope and receiver combination is named as PB2-A, PB2-B, and PB2-C. PB2-A and -B will have nearly identical receivers operating at 90 and 150 GHz while PB2-C will house a receiver operating at 220 and 270 GHz. Each receiver contains a focal plane consisting of seven close-hex packed lenslet coupled sinuous antenna transition edge sensor bolometer arrays. Each array contains 271 di-chroic optical pixels each of which have four TES bolometers for a total of 7588 detectors per receiver. We have produced a set of two types of candidate arrays for PB2-A. The first we call Version 11 (V11) and uses a silicon oxide (SiOx) for the transmission lines and cross-over process for orthogonal polarizations. The second we call Version 13 (V13) and uses silicon nitride (SiNx) for the transmission lines and cross-under process for orthogonal polarizations. We have produced enough of each type of array to fully populate the focal plane of the PB2-A receiver. The average wirebond yield for V11 and V13 arrays is 93.2% and 95.6% respectively. The V11 arrays had a superconducting transition temperature (Tc) of 452 +/- 15 mK, a normal resistance (Rn) of 1.25 +/- 0.20 Ohms, and saturations powers of 5.2 +/- 1.0 pW and 13 +/- 1.2 pW for the 90 and 150 GHz bands respectively. The V13 arrays had a superconducting transition temperature (Tc) of 456 +/-6 mK, a normal resistance (Rn) of 1.1 +/- 0.2 Ohms, and saturations powers of 10.8 +/- 1.8 pW and 22.9 +/- 2.6 pW for the 90 and 150 GHz bands respectively.
Published: 2022
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15. Thermal Testing for Cryogenic CMB Instrument Optical Design

Author: Goldfinger, D. C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayk, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Smith, A. G., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vergès, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Goldfinger, D. C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayk, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Smith, A. G., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vergès, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.
Abstract: Observations of the Cosmic Microwave Background rely on cryogenic instrumentation with cold detectors, readout, and optics providing the low noise performance and instrumental stability required to make more sensitive measurements. It is therefore critical to optimize all aspects of the cryogenic design to achieve the necessary performance, with low temperature components and acceptable system cooling requirements. In particular, we will focus on our use of thermal filters and cold optics, which reduce the thermal load passed along to the cryogenic stages. To test their performance, we have made a series of in situ measurements while integrating the third receiver for the BICEP Array telescope. In addition to characterizing the behavior of this receiver, these measurements continue to refine the models that are being used to inform design choices being made for future instruments., Comment: 9 pages, 8 figures, Proceedings of SPIE 2022
Published: 2022

16. Improved Polarization Calibration of the BICEP3 CMB Polarimeter at the South Pole

Author: Cornelison, J., Vergès, C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire IV, J. R., Connors, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Look, K., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reinsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Cornelison, J., Vergès, C., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Beck, D., Bischoff, C. A., Bock, J. J., Buza, V., Cheshire IV, J. R., Connors, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Look, K., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Prouve, T., Pryke, C., Racine, B., Reinsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Soliman, A., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.
Abstract: The BICEP3 Polarimeter is a small aperture, refracting telescope, dedicated to the observation of the Cosmic Microwave Background (CMB) at 95GHz. It is designed to target degree angular scale polarization patterns, in particular the very-much-sought-after primordial B-mode signal, which is a unique signature of cosmic inflation. The polarized signal from the sky is reconstructed by differencing co-localized, orthogonally polarized superconducting Transition Edge Sensor (TES) bolometers. In this work, we present absolute measurements of the polarization response of the detectors for more than $\sim 800$ functioning detector pairs of the BICEP3 experiment, out of a total of $\sim 1000$. We use a specifically designed Rotating Polarized Source (RPS) to measure the polarization response at multiple source and telescope boresight rotation angles, to fully map the response over 360 degrees. We present here polarization properties extracted from on-site calibration data taken in January 2022. A similar calibration campaign was performed in 2018, but we found that our constraint was dominated by systematics on the level of $\sim0.5^\circ$. After a number of improvements to the calibration set-up, we are now able to report a significantly lower level of systematic contamination. In the future, such precise measurements will be used to constrain physics beyond the standard cosmological model, namely cosmic birefringence., Comment: Submitted to: SPIE Astronomical Telescopes + Instrumentation (AS22)
Published: 2022

17. 2022 Upgrade and Improved Low Frequency Camera Sensitivity for CMB Observation at the South Pole

Author: Soliman, A., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Beck, D., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kangh, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Precup, N., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vergès, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., Zhang, S., Soliman, A., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Thakur, R. Basu, Bischoff, C. A., Beck, D., Bock, J. J., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A. J., Denison, E. V., Dierickx, M. I., Duband, L., Eiben, M., Fatigoni, S., Filippini, J. P., Giannakopoulos, C., Goeckner-Wald, N., Goldfinger, D. C., Grayson, J., Grimes, P. K., Hall, G., Halal, G., Halpern, M., Hand, E., Harrison, S. A., Henderson, S., Hildebrandt, S. R., Hilton, G. C., Hubmayr, J., Hui, H., Irwin, K. D., Kangh, J., Karkare, K. S., Kefeli, S., Kovac, J. M., Kuo, C. L., Lau, K., Leitch, E. M., Lennox, A., Liu, T., Megerian, K. G., Minutolo, L., Moncelsi, L., Nakato, Y., Namikawa, T., Nguyen, H. T., O'Brient, R., Palladino, S., Petroff, M. A., Precup, N., Prouve, T., Pryke, C., Racine, B., Reintsema, C. D., Salatino, M., Schillaci, A., Schmitt, B. L., Singari, B., Germaine, T. St., Steinbach, B., Sudiwala, R. V., Thompson, K. L., Tsai, C., Tucker, C., Turner, A. D., Umiltà, C., Vergès, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yang, H., Yoon, K. W., Young, E., Yu, C., Zeng, L., Zhang, C., and Zhang, S.
Abstract: Constraining the Galactic foregrounds with multi-frequency Cosmic Microwave Background (CMB) observations is an essential step towards ultimately reaching the sensitivity to measure primordial gravitational waves (PGWs), the sign of inflation after the Big-Bang that would be imprinted on the CMB. The BICEP Array telescope is a set of multi-frequency cameras designed to constrain the energy scale of inflation through CMB B-mode searches while also controlling the polarized galactic foregrounds. The lowest frequency BICEP Array receiver (BA1) has been observing from the South Pole since 2020 and provides 30 GHz and 40 GHz data to characterize the Galactic synchrotron in our CMB maps. In this paper, we present the design of the BA1 detectors and the full optical characterization of the camera including the on-sky performance at the South Pole. The paper also introduces the design challenges during the first observing season including the effect of out-of-band photons on detectors performance. It also describes the tests done to diagnose that effect and the new upgrade to minimize these photons, as well as installing more dichroic detectors during the 2022 deployment season to improve the BA1 sensitivity. We finally report background noise measurements of the detectors with the goal of having photon noise dominated detectors in both optical channels. BA1 achieves an improvement in mapping speed compared to the previous deployment season., Comment: Proceedings of SPIE Astronomical Telescopes + Instrumentation 2022 (AS22)
Published: 2022

18. Magnetic Field Reversal around an Active Fast Radio Burst

Author: Dai, S., Feng, Y., Yang, Y. P., Zhang, Y. K., Li, D., Niu, C. H., Wang, P., Xue, M. Y., Zhang, B., Burke-Spolaor, S., Law, C. J., Lynch, R. S., Connor, L., Anna-Thomas, R., Zhang, L., Duan, R., Yao, J. M., Tsai, C. W., Zhu, W. W., Cruces, M., Hobbs, G., Miao, C. C., Niu, J. R., Filipovic, M. D., Zhu, S. Q., Dai, S., Feng, Y., Yang, Y. P., Zhang, Y. K., Li, D., Niu, C. H., Wang, P., Xue, M. Y., Zhang, B., Burke-Spolaor, S., Law, C. J., Lynch, R. S., Connor, L., Anna-Thomas, R., Zhang, L., Duan, R., Yao, J. M., Tsai, C. W., Zhu, W. W., Cruces, M., Hobbs, G., Miao, C. C., Niu, J. R., Filipovic, M. D., and Zhu, S. Q.
Abstract: The environment of actively repeating fast radio bursts (FRBs) has been shown to be complex and varying. The recently localized FRB 20190520B is extremely active, has the largest confirmed host dispersion measure, and is only the second FRB source associated with a compact, persistent radio source (PRS). The main tracer of the magneto-ionic environments is the rotation measure (RM), a path-integral of the line-of-sight component of magnetic field strength (B) and electron density, which does not allow a direct probe of the B-field configuration. Here we report direct evidence for a B-field reversal based on the observed sign change and extreme variation of FRB 20190520B's RM, which changed from $\sim10000$ rad m$^{-2}$ to $\sim-16000$ rad m$^{-2}$ between June 2021 and January 2022. Such extreme RM reversal has never been observed before in any FRB nor in any astronomical object. The implied short-term change of the B-field configuration in or around the FRB could be due to the vicinity of massive black holes, or a magnetized companion star in binary systems, or a young supernova remnant along the line of sight., Comment: It was merged into arXiv:2202.11112. Science380,599-603(2023). DOI:10.1126/science.abo6526
Published: 2022

19. The Large Dispersion and Scattering of FRB 20190520B are Dominated by the Host Galaxy

Author: Ocker, S. K., Cordes, J. M., Chatterjee, S., Niu, C. -H., Li, D., McKee, J. W., Law, C. J., Tsai, C. -W., Anna-Thomas, R., Yao, J. -M., Cruces, M., Ocker, S. K., Cordes, J. M., Chatterjee, S., Niu, C. -H., Li, D., McKee, J. W., Law, C. J., Tsai, C. -W., Anna-Thomas, R., Yao, J. -M., and Cruces, M.
Abstract: The repeating FRB 20190520B is localized to a galaxy at $z=0.241$, much closer than expected given its dispersion measure $\rm DM=1205\pm4\ pc\ cm^{-3}$. Here we assess implications of the large DM and scattering observed from FRB 20190520B for the host galaxy's plasma properties. A sample of 75 bursts detected with the Five-hundred-meter Aperture Spherical radio Telescope shows scattering on two scales: a mean temporal delay $\tau(1.41\ {\rm GHz})=10.9\pm1.5$ ms, which is attributed to the host galaxy, and a mean scintillation bandwidth $\nu_{\rm d}(1.41\ {\rm GHz})=0.21\pm0.01$ MHz, which is attributed to the Milky Way. Balmer line measurements for the host imply an H$\alpha$ emission measure (galaxy frame) $\rm EM_s=620$ pc cm$^{-6} \times (T/10^4 {\rm K})^{0.9}$, implying $\rm DM_{\rm H\alpha}$ of order the value inferred from the FRB DM budget, $\rm DM_h=1121^{+89}_{-138}$ pc cm$^{-3}$ for plasma temperatures greater than the typical value $10^4$ K. Combining $\tau$ and $\rm DM_h$ yields a nominal constraint on the scattering amplification from the host galaxy $\tilde{F} G=1.5^{+0.8}_{-0.3}$ (pc$^2$ km)$^{-1/3}$, where $\tilde{F}$ describes turbulent density fluctuations and $G$ represents the geometric leverage to scattering that depends on the location of the scattering material. For a two-screen scattering geometry where $\tau$ arises from the host galaxy and $\Delta \nu_{\rm d}$ from the Milky Way, the implied distance between the FRB source and dominant scattering material is $\lesssim100$ pc. The host galaxy scattering and DM contributions support a novel technique for estimating FRB redshifts using the $\tau-\rm DM$ relation, and are consistent with previous findings that scattering of localized FRBs is largely dominated by plasma within host galaxies and the Milky Way., Comment: 14 pages, 9 figures, accepted to ApJ
Published: 2022
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20. Deployment of Polarbear-2A

Author: Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., Dobbs M., Dunner R., El-Bouhargani H., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Hall G., Halverson N. W., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Ross C., Segawa Y., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Verges C., Westbrook B., Zhou Y., Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko D., Adachi S., Ade P. A. R., Aguilar Faundez M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Carron J., Chapman S., Cheung K., Chinone Y., Crowley K., Cukierman A., Dobbs M., Dunner R., El-Bouhargani H., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Hall G., Halverson N. W., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jeong O., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Minami Y., Navaroli M., Nishino H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Ross C., Segawa Y., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Verges C., Westbrook B., and Zhou Y.
Abstract: Polarbear-2A is the first of three receivers in the Simons array, a cosmic microwave background experiment located on the Atacama Plateau in Chile. Polarbear-2A was deployed and achieved the first light in January 2019 by mapping the microwave emission from planet observations. Commissioning work is underway to prepare the receiver for science observations.
Published: 2020

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

Author: Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., Zhou Y., Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone Y., Adachi S., Ade P. A. R., Aguilar M., Akiba Y., Arnold K., Baccigalupi C., Barron D., Beck D., Beckman S., Bianchini F., Boettger D., Borrill J., Elbouhargani H., Carron J., Chapman S., Cheung K., Crowley K., Cukierman A., Dunner R., Dobbs M., Ducout A., Elleflot T., Errard J., Fabbian G., Feeney S. M., Feng C., Fujino T., Galitzki N., Gilbert A., Goeckner-Wald N., Groh J., Groh J. C., Hall G., Halverson N., Hamada T., Hasegawa M., Hazumi M., Hill C. A., Howe L., Inoue Y., Jaehnig G., Jaffe A. H., Jeong O., Lejeune M., Kaneko D., Katayama N., Keating B., Keskitalo R., Kikuchi S., Kisner T., Krachmalnicoff N., Kusaka A., Lee A. T., Leitch E. M., Leon D., Linder E., Lowry L. N., Mangu A., Matsuda F., Matsumura T., Minami Y., Montgomery J., Navaroli M., Nishino H., Paar H., Peloton J., Pham A. T. P., Poletti D., Puglisi G., Reichardt C. L., Richards P. L., Ross C., Segawa Y., Sherwin B. D., Silva-Feaver M., Siritanasak P., Stebor N., Stompor R., Suzuki A., Tajima O., Takakura S., Takatori S., Tanabe D., Teply G. P., Tomaru T., Tsai C., Tucker C., Verges C., Westbrook B., Whitehorn N., Zahn A., and Zhou Y.
Abstract: POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.
Published: 2020

22. A cross-sectional examination of a family history of Alzheimer's disease and ApoE epsilon 4 on physical fitness, molecular biomarkers, and neurocognitive performance

Author: Tsai, C-L, Erickson, K.I., Sun, H-S, Kuo, Y-M, Pai, M-C, Tsai, C-L, Erickson, K.I., Sun, H-S, Kuo, Y-M, and Pai, M-C
Abstract: Purpose The present study examined whether the ɛ4 allele of the apolipoprotein E (ApoE) gene impacts molecular biomarkers and neurocognitive performance among individuals at genetic risk for developing Alzheimer's disease (AD). The correlations between physical fitness and molecular/neurocognitive indices were also explored. Methods Fasting blood samples were collected from 162 individuals with a family history of AD (ADFH). There were twenty-two carriers of the ApoE-4 variant (ApoE-4 group). For comparison purposes we randomly selected 22 non-ɛ4 carriers (non-ApoE-4 group) from the ADFH individuals. Circulating inflammatory cytokines (e.g., TNF-α, IL-1β, IL-6, IL-8, and IL-15), neuroprotective growth factors (e.g., BDNF, IGF-1, IGF-2, VEGF, and FGF-2), and Amyloid-β peptides (e.g., Aβ1–40 and Aβ1–42), neurocognitive performance [e.g., behavior and brain even-related potentials (ERP)] during a task-switching paradigm, as well as physical fitness scores were measured. Results The ApoE-4 group relative to the non-ApoE-4 group was similar with respect to molecular biomarkers, physical fitness, and most measures of neurocognitive performance. However, ADFH individuals that were ɛ4 carriers exhibited significantly higher local switching accuracy costs, worse accuracy as well as smaller ERP P3 amplitudes for the memory-switching condition. Importantly, cardiorespiratory fitness levels were significantly correlated with accuracy for most task-switching conditions, and levels of BDNF, Aβ1–40, and Aβ1–42 collapsed across the two groups even when controlling for the age co-variable, while the ApoE-4 group revealed similar pattern of results. Conclusions These data suggest that individuals with ADFH that were carriers of the ApoE-4 variant performed worse on the task-switching paradigm and that this could be due to compromised task-set and memory updating processes. Physical exercise interventions aimed to enhance cardiorespiratory fitness levels could be a potential AD preven
Published: 2021

23. Systematic review of postoperative therapy for resected squamous cell carcinoma of the head and neck: Executive summary of the American Radium Society appropriate use criteria.

Author: Margalit, Danielle N, Margalit, Danielle N, Sacco, Assuntina G, Cooper, Jay S, Ridge, John A, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven S, Chen, Allen M, Galloway, Tom J, Koyfman, Shlomo A, Mita, Carol, Robbins, Jared R, Tsai, C Jillian, Truong, Minh T, Yom, Sue S, Siddiqui, Farzan, Margalit, Danielle N, Margalit, Danielle N, Sacco, Assuntina G, Cooper, Jay S, Ridge, John A, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven S, Chen, Allen M, Galloway, Tom J, Koyfman, Shlomo A, Mita, Carol, Robbins, Jared R, Tsai, C Jillian, Truong, Minh T, Yom, Sue S, and Siddiqui, Farzan
Abstract: BackgroundThe aims of this systematic review are to (a) evaluate the current literature on the impact of postoperative therapy for resected squamous cell carcinoma of the head and neck (SCCHN) on oncologic and non-oncologic outcomes and (b) identify the optimal evidence-based postoperative therapy recommendations for commonly encountered clinical scenarios.MethodsAn analysis of the medical literature from peer-reviewed journals was conducted using the Preferred Reporting Items for Systematic Reviews and Meta-analyses (PRISMA) guideline. Prospective studies and methodology-based systematic reviews and meta-analyses of postoperative therapy for SCCHN were identified by searching Medline (OVID) and EMBASE (Elsevier) using controlled vocabulary terms (ie, National Library of Medicine Medical Subject Headings [MeSH], EMTREE). Study screening and selection was performed with Covidence software and full-text review. The RAND/UCLA appropriateness method was used by the expert panel to rate the appropriate use of postoperative therapy, and the modified Delphi method was used to come to consensus.ResultsA total of 5660 studies were identified and screened using the title and abstract, leading to 201 studies assessed for relevance using full-text review. After limitation to the eligibility criteria, 101 studies from 1977 to 2020 were identified, including 77 with oncologic endpoints and 24 with function and quality of life endpoints. All studies reported staging prior to the implementation of American Joint Committee on Cancer (AJCC-8).ConclusionsProspective clinical studies and systematic reviews identified through the PRISMA systematic review provided good evidence for consensus statements regarding the appropriate use of postoperative therapy for resected SCCHN. Further research is needed in domains where consensus by the expert panel could not be achieved for the appropriateness of specific postoperative therapeutic interventions.
Published: 2021

24. A repeating fast radio burst associated with a persistent radio source

Author: Niu, C. -H., Aggarwal, K., Li, D., Zhang, X., Chatterjee, S., Tsai, C. -W., Yu, W., Law, C. J., Burke-Spolaor, S., Cordes, J. M., Zhang, Y. -K., Ocker, S., Yao, J. -M., Wang, P., Feng, Y., Niino, Y., Bochenek, C., Cruces, M., Connor, L., Jiang, J. -A., Dai, S., Luo, R., Li, G. -D., Miao, C. -C., Niu, J. -R., Anna-Thomas, R., Sydnor, J., Stern, D., Wang, W. -Y., Yuan, M., Yue, Y. -L., Zhou, D. -J., Yan, Z., Zhu, W. -W., Zhang, B., Niu, C. -H., Aggarwal, K., Li, D., Zhang, X., Chatterjee, S., Tsai, C. -W., Yu, W., Law, C. J., Burke-Spolaor, S., Cordes, J. M., Zhang, Y. -K., Ocker, S., Yao, J. -M., Wang, P., Feng, Y., Niino, Y., Bochenek, C., Cruces, M., Connor, L., Jiang, J. -A., Dai, S., Luo, R., Li, G. -D., Miao, C. -C., Niu, J. -R., Anna-Thomas, R., Sydnor, J., Stern, D., Wang, W. -Y., Yuan, M., Yue, Y. -L., Zhou, D. -J., Yan, Z., Zhu, W. -W., and Zhang, B.
Abstract: The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium, which is assumed to dominate the total extragalactic dispersion. While the host galaxy contributions to dispersion measure (DM) appear to be small for most FRBs, in at least one case there is evidence for an extreme magneto-ionic local environment and a compact persistent radio source. Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific star formation rate at a redshift $z=0.241\pm0.001$. The estimated host galaxy DM $\approx 903^{+72}_{-111}$ pc cm$^{-3}$, nearly an order of magnitude higher than the average of FRB host galaxies, far exceeds the DM contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host galaxy identifications., Comment: Accepted, Version 3
Published: 2021

25. K160 in the RNA-binding domain of the orf virus virulence factor OV20.0 is critical for its functions in counteracting host antiviral defense

Author: Greber, U, Liao, G-R, Tseng, Y-Y, Tseng, C-Y, Huang, Y-P, Tsai, C-H, Liu, H-P, Hsu, W-L, Greber, U, Liao, G-R, Tseng, Y-Y, Tseng, C-Y, Huang, Y-P, Tsai, C-H, Liu, H-P, and Hsu, W-L
Abstract: The OV20.0 virulence factor of orf virus antagonizes host antiviral responses. One mechanism through which it functions is by inhibiting activation of the dsRNA-activated protein kinase R (PKR) by sequestering dsRNA and by physically interacting with PKR. Sequence alignment indicated that several key residues critical for dsRNA binding were conserved in OV20.0, and their contribution to OV20.O function was investigated in this study. We found that residues F141, K160, and R164 were responsible for the dsRNA-binding ability of OV20.0. Interestingly, mutation at K160 (K160A) diminished the OV20.0-PKR interaction and further reduced the inhibitory effect of OV20.0 on PKR activation. Nevertheless, OV20.0 homodimerization was not influenced by K160A. The contribution of the dsRNA-binding domain and K160 to the suppression of RNA interference by OV20.0 was further demonstrated in plants. In summary, K160 is essential for the function of OV20.0, particularly its interaction with dsRNA and PKR that ultimately contributes to the suppression of PKR activation.
Published: 2021

26. Systematic review of postoperative therapy for resected squamous cell carcinoma of the head and neck: Executive summary of the American Radium Society appropriate use criteria.

Author: Margalit, Danielle N, Margalit, Danielle N, Sacco, Assuntina G, Cooper, Jay S, Ridge, John A, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven S, Chen, Allen M, Galloway, Tom J, Koyfman, Shlomo A, Mita, Carol, Robbins, Jared R, Tsai, C Jillian, Truong, Minh T, Yom, Sue S, Siddiqui, Farzan, Margalit, Danielle N, Margalit, Danielle N, Sacco, Assuntina G, Cooper, Jay S, Ridge, John A, Bakst, Richard L, Beadle, Beth M, Beitler, Jonathan J, Chang, Steven S, Chen, Allen M, Galloway, Tom J, Koyfman, Shlomo A, Mita, Carol, Robbins, Jared R, Tsai, C Jillian, Truong, Minh T, Yom, Sue S, and Siddiqui, Farzan
Abstract: BackgroundThe aims of this systematic review are to (a) evaluate the current literature on the impact of postoperative therapy for resected squamous cell carcinoma of the head and neck (SCCHN) on oncologic and non-oncologic outcomes and (b) identify the optimal evidence-based postoperative therapy recommendations for commonly encountered clinical scenarios.MethodsAn analysis of the medical literature from peer-reviewed journals was conducted using the Preferred Reporting Items for Systematic Reviews and Meta-analyses (PRISMA) guideline. Prospective studies and methodology-based systematic reviews and meta-analyses of postoperative therapy for SCCHN were identified by searching Medline (OVID) and EMBASE (Elsevier) using controlled vocabulary terms (ie, National Library of Medicine Medical Subject Headings [MeSH], EMTREE). Study screening and selection was performed with Covidence software and full-text review. The RAND/UCLA appropriateness method was used by the expert panel to rate the appropriate use of postoperative therapy, and the modified Delphi method was used to come to consensus.ResultsA total of 5660 studies were identified and screened using the title and abstract, leading to 201 studies assessed for relevance using full-text review. After limitation to the eligibility criteria, 101 studies from 1977 to 2020 were identified, including 77 with oncologic endpoints and 24 with function and quality of life endpoints. All studies reported staging prior to the implementation of American Joint Committee on Cancer (AJCC-8).ConclusionsProspective clinical studies and systematic reviews identified through the PRISMA systematic review provided good evidence for consensus statements regarding the appropriate use of postoperative therapy for resected SCCHN. Further research is needed in domains where consensus by the expert panel could not be achieved for the appropriateness of specific postoperative therapeutic interventions.
Published: 2021

27. Mechanism of activation and the rewired network: new drug design concepts

Author: Tunçbağ, Nurcan (ORCID 0000-0002-0389-9459 & YÖK ID 245513), Nussinov, R.; Zhang, M.; Maloney, R.; Tsai, C. J.; Yavuz, B. R.; Jang, H., Koç University Research Center for Translational Medicine (KUTTAM) / Koç Üniversitesi Translasyonel Tıp Araştırma Merkezi (KUTTAM), School of Medicine; College of Engineering, Department of Chemical and Biological Engineering, Tunçbağ, Nurcan (ORCID 0000-0002-0389-9459 & YÖK ID 245513), Nussinov, R.; Zhang, M.; Maloney, R.; Tsai, C. J.; Yavuz, B. R.; Jang, H., Koç University Research Center for Translational Medicine (KUTTAM) / Koç Üniversitesi Translasyonel Tıp Araştırma Merkezi (KUTTAM), School of Medicine; College of Engineering, and Department of Chemical and Biological Engineering
Abstract: Precision oncology benefits from effective early phase drug discovery decisions. Recently, drugging inactive protein conformations has shown impressive successes, raising the cardinal questions of which targets can profit and what are the principles of the active/inactive protein pharmacology. Cancer driver mutations have been established to mimic the protein activation mechanism. We suggest that the decision whether to target an inactive (or active) conformation should largely rest on the protein mechanism of activation. We next discuss the recent identification of double (multiple) same-allele driver mutations and their impact on cell proliferation and suggest that like single driver mutations, double drivers also mimic the mechanism of activation. We further suggest that the structural perturbations of double (multiple) in cis mutations may reveal new surfaces/pockets for drug design. Finally, we underscore the preeminent role of the cellular network which is deregulated in cancer. Our structure-based review and outlook updates the traditional Mechanism of Action, informs decisions, and calls attention to the intrinsic activation mechanism of the target protein and the rewired tumor-specific network, ushering innovative considerations in precision medicine., National Cancer Institute; National Institutes of Health; Intramural Research Program; Center for Cancer Research
Published: 2021

28. A repeating fast radio burst associated with a persistent radio source

Author: Niu, C. -H., Aggarwal, K., Li, D., Zhang, X., Chatterjee, S., Tsai, C. -W., Yu, W., Law, C. J., Burke-Spolaor, S., Cordes, J. M., Zhang, Y. -K., Ocker, S., Yao, J. -M., Wang, P., Feng, Y., Niino, Y., Bochenek, C., Cruces, M., Connor, L., Jiang, J. -A., Dai, S., Luo, R., Li, G. -D., Miao, C. -C., Niu, J. -R., Anna-Thomas, R., Sydnor, J., Stern, D., Wang, W. -Y., Yuan, M., Yue, Y. -L., Zhou, D. -J., Yan, Z., Zhu, W. -W., Zhang, B., Niu, C. -H., Aggarwal, K., Li, D., Zhang, X., Chatterjee, S., Tsai, C. -W., Yu, W., Law, C. J., Burke-Spolaor, S., Cordes, J. M., Zhang, Y. -K., Ocker, S., Yao, J. -M., Wang, P., Feng, Y., Niino, Y., Bochenek, C., Cruces, M., Connor, L., Jiang, J. -A., Dai, S., Luo, R., Li, G. -D., Miao, C. -C., Niu, J. -R., Anna-Thomas, R., Sydnor, J., Stern, D., Wang, W. -Y., Yuan, M., Yue, Y. -L., Zhou, D. -J., Yan, Z., Zhu, W. -W., and Zhang, B.
Abstract: The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium, which is assumed to dominate the total extragalactic dispersion. While the host galaxy contributions to dispersion measure (DM) appear to be small for most FRBs, in at least one case there is evidence for an extreme magneto-ionic local environment and a compact persistent radio source. Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific star formation rate at a redshift $z=0.241\pm0.001$. The estimated host galaxy DM $\approx 903^{+72}_{-111}$ pc cm$^{-3}$, nearly an order of magnitude higher than the average of FRB host galaxies, far exceeds the DM contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host galaxy identifications., Comment: Accepted, Version 3
Published: 2021
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29. The black hole masses of extremely luminous radio-WISE selected galaxies

Author: Ferris, E. R., Blain, A. W., Assef, R. J., Hatch, N. A., Kimball, A., Kim, M., Sajina, A., Silva, A., Stern, D., Diaz-Santos, T., Tsai, C-W., Wylezalek, D., Ferris, E. R., Blain, A. W., Assef, R. J., Hatch, N. A., Kimball, A., Kim, M., Sajina, A., Silva, A., Stern, D., Diaz-Santos, T., Tsai, C-W., and Wylezalek, D.
Abstract: We present near-IR photometry and spectroscopy of 30 extremely luminous radio and mid-IR selected galaxies. With bolometric luminosities exceeding $\sim10^{13}$ $\rm{L_{\odot}}$ and redshifts ranging from $z = 0.880-2.853$, we use VLT instruments X-shooter and ISAAC to investigate this unique population of galaxies. Broad multi-component emission lines are detected in 18 galaxies and we measure the near-IR lines $\rm{H\rm{\beta}}$, $\text{[OIII]}\rm{\lambda}\rm{\lambda}4959,5007$ and $\rm{H\rm{\alpha}}$ in six, 15 and 13 galaxies respectively, with 10 $\rm{Ly\alpha}$ and five CIV lines additionally detected in the UVB arm. We use the broad $\text{[OIII]}\rm{\lambda}5007$ emission lines as a proxy for the bolometric AGN luminosity, and derive lower limits to supermassive black hole masses of $10^{7.9}$-$10^{9.4}$ $\text{M}_{\odot}$ with expectations of corresponding host masses of $10^{10.4}$-$10^{12.0}$ $\text{M}_{\odot}$. We measure $\rm{\lambda}_{Edd}$ > 1 for eight of these sources at a $2\sigma$ significance. Near-IR photometry and SED fitting are used to compare stellar masses directly. We detect both Balmer lines in five galaxies and use these to infer a mean visual extinction of $A_{V}$ = 2.68 mag. Due to non-detections and uncertainties in our $\rm{H\rm{\beta}}$ emission line measurements, we simulate a broad $\rm{H\rm{\beta}}$ line of FWHM = 1480 $\rm{kms^{-1}}$ to estimate extinction for all sources with measured $\rm{H\rm{\alpha}}$ emission. We then use this to infer a mean $A_{V}=3.62$ mag, demonstrating the highly-obscured nature of these galaxies, with the consequence of increasing our estimates of black-hole masses by an 0.5 orders of magnitude in the most extreme and obscured cases., Comment: Accepted for publication in MNRAS. 14 pages (+8 page appendix), 11 figures and 9 tables
Published: 2021
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30. Design and characterization of the POLARBEAR-2b and POLARBEAR-2c cosmic microwave background cryogenic receivers

Author: Howe, L, Tsai, C, Lowry, L, Arnold, K, Coppi, G, Groh, J, Guo, X, Keating, B, Lee, A, May, A, Piccirillo, L, Stebor, N, Teply, G, Howe L., Tsai C., Lowry L., Arnold K., Coppi G., Groh J., Guo X., Keating B., Lee A., May A. J., Piccirillo L., Stebor N., Teply G., Howe, L, Tsai, C, Lowry, L, Arnold, K, Coppi, G, Groh, J, Guo, X, Keating, B, Lee, A, May, A, Piccirillo, L, Stebor, N, Teply, G, Howe L., Tsai C., Lowry L., Arnold K., Coppi G., Groh J., Guo X., Keating B., Lee A., May A. J., Piccirillo L., Stebor N., and Teply G.
Abstract: The POLARBEAR-2/Simons Array Cosmic Microwave Background (CMB) polarization experiment is an upgrade and expansion of the existing POLARBEAR-1 (PB-1) experiment, located in the Atacama desert in Chile. Along with the CMB temperature and E-mode polarization anisotropies, PB-1 and the Simons Array study the CMB B-mode polarization anisotropies produced at large angular scales by inflationary gravitational waves, and at small angular scales by gravitational lensing. These measurements provide constraints on various cosmological and particle physics parameters, such as the tensor-to-scalar ratio r, and the sum of the neutrino masses. The Simons Array consists of three 3.5 m diameter telescopes with upgraded POLARBEAR-2 (PB-2) cryogenic receivers, named PB-2a,-2b, and-2c. PB-2a and-2b will observe the CMB over multiple bands centered at 95 GHz and 150 GHz, while PB-2c will observe at 220 GHz and 270 GHz, which will enable enhanced foreground separation and de-lensing. Each Simons Array receiver consists of two cryostats which share the same vacuum space: an optics tube containing the cold reimaging lenses and Lyot stop, infrared-blocking filters, and cryogenic half-wave plate; and a backend which contains the focal plane detector array, cold readout components, and millikelvin refrigerator. Each PB-2 focal plane array is comprised of 7,588 dual-polarization, multi-chroic, lenslet-and antenna-coupled, Transition Edge Sensor (TES) bolometers which are cooled to 250 mK and read out using Superconducting Quantum Interference Devices (SQUIDs) through a digital frequency division multiplexing scheme with a multiplexing factor of 40. In this work we describe progress towards commissioning the PB-2b and-2c receivers including cryogenic design, characterization, and performance of both the PB-2b and-2c backend cryostats.
Published: 2018

31. The Simons Observatory: Instrument overview

Author: Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., Zhu N., Jonas Zmuidzinas, Jian-Rong Gao, Galitzki, N, Ali, A, Arnold, K, Ashton, P, Austermann, J, Baccigalupi, C, Baildon, T, Barron, D, Beall, J, Beckman, S, Bruno, S, Bryan, S, Calisse, P, Chesmore, G, Chinone, Y, Choi, S, Coppi, G, Crowley, K, Cukierman, A, Devlin, M, Dicker, S, Dober, B, Duff, S, Dunkley, J, Fabbian, G, Gallardo, P, Gerbino, M, Goeckner-Wald, N, Golec, J, Gudmundsson, J, Healy, E, Henderson, S, Hill, C, Hilton, G, Ho, S, Howe, L, Hubmayr, J, Jeong, O, Keating, B, Koopman, B, Kiuchi, K, Kusaka, A, Lashner, J, Lee, A, Li, Y, Limon, M, Lungu, M, Matsuda, F, Mauskopf, P, May, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Parshley, S, Piccirillo, L, Sathyanarayana Rao, M, Raum, C, Salatino, M, Seibert, J, Sierra, C, Silva-Feaver, M, Simon, S, Staggs, S, Stevens, J, Suzuki, A, Teply, G, Thornton, R, Tsai, C, Ullom, J, Vavagiakis, E, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, Galitzki N., Ali A., Arnold K. S., Ashton P. C., Austermann J. E., Baccigalupi C., Baildon T., Barron D., Beall J. A., Beckman S., Bruno S. M. M., Bryan S., Calisse P. G., Chesmore G. E., Chinone Y., Choi S. K., Coppi G., Crowley K. D., Crowley K. T., Cukierman A., Devlin M. J., Dicker S., Dober B., Duff S. M., Dunkley J., Fabbian G., Gallardo P. A., Gerbino M., Goeckner-Wald N., Golec J. E., Gudmundsson J. E., Healy E. E., Henderson S., Hill C. A., Hilton G. C., Ho S. -P. P., Howe L. A., Hubmayr J., Jeong O., Keating B., Koopman B. J., Kiuchi K., Kusaka A., Lashner J., Lee A. T., Li Y., Limon M., Lungu M., Matsuda F., Mauskopf P. D., May A. J., McCallum N., McMahon J., Nati F., Niemack M. D., Orlowski-Scherer J. L., Parshley S. C., Piccirillo L., Sathyanarayana Rao M., Raum C., Salatino M., Seibert J. S., Sierra C., Silva-Feaver M., Simon S. M., Staggs S. T., Stevens J. R., Suzuki A., Teply G., Thornton R., Tsai C., Ullom J. N., Vavagiakis E. M., Vissers M. R., Westbrook B., Wollack E. J., Xu Z., and Zhu N.
Abstract: The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 40,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 20,000 detectors along with an array of half-meter aperture refractive cameras, coupled to an additional 20,000+ detectors. The unique combination of large and small apertures in a single CMB observatory, which will be located in the Atacama Desert at an altitude of 5190 m, will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4 m in diameter and over 2 m long, creating a number of interesting technical challenges. Concurrently, we are designing an array of half-meter-aperture cryogenic cameras which also have compelling design challenges. We will give an overview of the drivers for and designs of the SO telescopes and the cryogenic cameras that will house the cold optical components and detector arrays.
Published: 2018

32. Cold Molecular Gas and Free-Free Emission from Hot, Dust-Obscured Galaxies at $z$~3

Author: Penney, J. I., Blain, A. W., Assef, R. J., Diaz-Santos, T., González-López, J. J., Tsai, C. -W., Aravena, M., Eisenhardt, P. R. M., Jones, S. F., Jun, H. D., Kim, M., Stern, D., Wu, J., Penney, J. I., Blain, A. W., Assef, R. J., Diaz-Santos, T., González-López, J. J., Tsai, C. -W., Aravena, M., Eisenhardt, P. R. M., Jones, S. F., Jun, H. D., Kim, M., Stern, D., and Wu, J.
Abstract: We report on observations of redshifted CO(1-0) line emission and observed-frame $\rm\sim$ 30GHz radio continuum emission from five ultra-luminous, mid-IR selected hot, Dust-Obscured Galaxies (Hot DOGs) at $z\rm\gtrsim$ 3 using the Karl G. Jansky Very Large Array. We detect CO(1-0) line emission in all five Hot DOGs, with one of them at high signal to noise. We analyse FIR-radio spectral energy distributions, including dust, free-free and synchrotron emission for the galaxies. We find that most of the 115 GHz rest-frame continuum is mostly due to synchrotron or free-free emission, with only a potentially small contribution from thermal emission. We see a deficit in the rest-frame 115 GHz continuum emission compared to dusty star-forming galaxies (DSFGs) and sub-millimetre galaxies (SMGs) at high redshift, suggesting that Hot DOGs do not have similar cold gas reserves compared with star-forming galaxies. One target, W2305-0039, is detected in the FIRST 1.4 GHz survey, and is likely to possess compact radio jets. We compare to the FIR-radio correlation, and find that at least half of the Hot DOGs in our sample are radio-quiet with respect to normal galaxies. These findings suggest that Hot DOGs have comparably less cold molecular gas than star-forming galaxies at lower, $z\rm\sim$ 2 redshifts, and are dominated by powerful, yet radio-quiet AGN., Comment: 15 pages, 12 figures, accepted for publication in MNRAS
Published: 2020
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33. A measurement of the CMB E-mode angular power spectrum at subdegree scales from 670 square degrees of POLARBEAR data

Author: Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Hasegawa, M., Hazumi, M., Hirose, H., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kikuchi, S., Kisner, T., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Reichardt, C. L., Segawa, Y., Siritanasak, P., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Vergès, C., Westbrook, B., Zhou, Y., Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Hasegawa, M., Hazumi, M., Hirose, H., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kikuchi, S., Kisner, T., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Reichardt, C. L., Segawa, Y., Siritanasak, P., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Vergès, C., Westbrook, B., and Zhou, Y.
Abstract: We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from July 2014 to December 2016 with the POLARBEAR experiment. We reach an effective polarization map noise level of $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range $500 \leq \ell <3000$, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is $\sim 2.3 \mu {\rm K}^2$ at $\ell \sim 1000$ with a systematic uncertainty of 0.5$\mu {\rm K}^2$. The data are consistent with the standard $\Lambda$CDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in $\Lambda$CDM as well as in extensions to $\Lambda$CDM. Adding the ground-based CMB polarization measurements to the Planck dataset reduces the uncertainty on the Hubble constant by a factor of 1.2 to $H_0 = 67.20 \pm 0.57 {\rm km\,s^{-1} \,Mpc^{-1}}$. When allowing the number of relativistic species ($N_{eff}$) to vary, we find $N_{eff} = 2.94 \pm 0.16$, which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance ($Y_{He}$) to vary, the data favor $Y_{He} = 0.248 \pm 0.012$. This is very close to the expectation of 0.2467 from Big Bang Nucleosynthesis. When varying both $Y_{He}$ and $N_{eff}$, we find $N_{eff} = 2.70 \pm 0.26$ and $Y_{He} = 0.262 \pm 0.015$., Comment: 15 pages, 5 figures, submitted to ApJ
Published: 2020
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34. Deployment of Polarbear-2A

Author: Kaneko, D, Adachi, S, Ade, PAR, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, NW, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Kaneko, D, Adachi, S, Ade, PAR, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, NW, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, and Zhou, Y
Published: 2020

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

Author: Chinone, Y, Adachi, S, Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, ElBouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Groh, JC, Hal, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, AH, Jeong, O, LeJeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leitch, EM, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Richards, PL, Ross, C, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, Chinone, Y, Adachi, S, Ade, PAR, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, ElBouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, SM, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Groh, JC, Hal, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, AH, Jeong, O, LeJeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, AT, Leitch, EM, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Richards, PL, Ross, C, Segawa, Y, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, GP, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, and Zhou, Y
Abstract: POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.
Published: 2020

36. Cold Molecular Gas and Free-Free Emission from Hot, Dust-Obscured Galaxies at $z$~3

Author: Penney, J. I., Blain, A. W., Assef, R. J., Diaz-Santos, T., González-López, J. J., Tsai, C. -W., Aravena, M., Eisenhardt, P. R. M., Jones, S. F., Jun, H. D., Kim, M., Stern, D., Wu, J., Penney, J. I., Blain, A. W., Assef, R. J., Diaz-Santos, T., González-López, J. J., Tsai, C. -W., Aravena, M., Eisenhardt, P. R. M., Jones, S. F., Jun, H. D., Kim, M., Stern, D., and Wu, J.
Abstract: We report on observations of redshifted CO(1-0) line emission and observed-frame $\rm\sim$ 30GHz radio continuum emission from five ultra-luminous, mid-IR selected hot, Dust-Obscured Galaxies (Hot DOGs) at $z\rm\gtrsim$ 3 using the Karl G. Jansky Very Large Array. We detect CO(1-0) line emission in all five Hot DOGs, with one of them at high signal to noise. We analyse FIR-radio spectral energy distributions, including dust, free-free and synchrotron emission for the galaxies. We find that most of the 115 GHz rest-frame continuum is mostly due to synchrotron or free-free emission, with only a potentially small contribution from thermal emission. We see a deficit in the rest-frame 115 GHz continuum emission compared to dusty star-forming galaxies (DSFGs) and sub-millimetre galaxies (SMGs) at high redshift, suggesting that Hot DOGs do not have similar cold gas reserves compared with star-forming galaxies. One target, W2305-0039, is detected in the FIRST 1.4 GHz survey, and is likely to possess compact radio jets. We compare to the FIR-radio correlation, and find that at least half of the Hot DOGs in our sample are radio-quiet with respect to normal galaxies. These findings suggest that Hot DOGs have comparably less cold molecular gas than star-forming galaxies at lower, $z\rm\sim$ 2 redshifts, and are dominated by powerful, yet radio-quiet AGN., Comment: 15 pages, 12 figures, accepted for publication in MNRAS
Published: 2020
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37. A measurement of the CMB E-mode angular power spectrum at subdegree scales from 670 square degrees of POLARBEAR data

Author: Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Hasegawa, M., Hazumi, M., Hirose, H., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kikuchi, S., Kisner, T., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Reichardt, C. L., Segawa, Y., Siritanasak, P., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Vergès, C., Westbrook, B., Zhou, Y., Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Hasegawa, M., Hazumi, M., Hirose, H., Jaffe, A. H., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Kikuchi, S., Kisner, T., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Matsumura, T., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Reichardt, C. L., Segawa, Y., Siritanasak, P., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Vergès, C., Westbrook, B., and Zhou, Y.
Abstract: We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from July 2014 to December 2016 with the POLARBEAR experiment. We reach an effective polarization map noise level of $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range $500 \leq \ell <3000$, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is $\sim 2.3 \mu {\rm K}^2$ at $\ell \sim 1000$ with a systematic uncertainty of 0.5$\mu {\rm K}^2$. The data are consistent with the standard $\Lambda$CDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in $\Lambda$CDM as well as in extensions to $\Lambda$CDM. Adding the ground-based CMB polarization measurements to the Planck dataset reduces the uncertainty on the Hubble constant by a factor of 1.2 to $H_0 = 67.20 \pm 0.57 {\rm km\,s^{-1} \,Mpc^{-1}}$. When allowing the number of relativistic species ($N_{eff}$) to vary, we find $N_{eff} = 2.94 \pm 0.16$, which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance ($Y_{He}$) to vary, the data favor $Y_{He} = 0.248 \pm 0.012$. This is very close to the expectation of 0.2467 from Big Bang Nucleosynthesis. When varying both $Y_{He}$ and $N_{eff}$, we find $N_{eff} = 2.70 \pm 0.26$ and $Y_{He} = 0.262 \pm 0.015$., Comment: 15 pages, 5 figures, submitted to ApJ
Published: 2020
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38. The Eighth Visual Object Tracking VOT2020 Challenge Results

Author: Kristan, M., Leonardis, A., Matas, J., Felsberg, Michael, Pflugfelder, R., Kämäräinen, J.-K., Danelljan, M., Zajc, L.C., Lukežic, A., Drbohlav, O., He, Linbo, Zhang, Yushan, Yan, S., Yang, J., Fernández, G., Hauptmann, A., Memarmoghadam, A., García-Martín, Á., Robinson, Andreas, Varfolomieiev, A., Gebrehiwot, A.H., Uzun, B., Yan, B., Li, B., Qian, C., Tsai, C.-Y., Micheloni, C., Wang, D., Wang, F., Xie, F., Järemo-Lawin, Felix, Gustafsson, F., Foresti, G.L., Bhat, G., Chen, G., Ling, H., Zhang, H., Cevikalp, H., Zhao, H., Bai, H., Kuchibhotla, H.C., Saribas, H., Fan, H., Ghanei-Yakhdan, H., Li, H., Peng, H., Lu, H., Khaghani, J., Bescos, J., Li, J., Fu, J., Yu, J., Xu, J., Kittler, J., Yin, J., Lee, J., Yu, K., Liu, K., Yang, K., Dai, K., Cheng, L., Zhang, L., Wang, L., Van, Gool L., Bertinetto, L., Dunnhofer, M., Cheng, M., Dasari, M.M., Wang, N., Zhang, P., Torr, P.H.S., Wang, Q., Timofte, R., Gorthi, R.K.S., Choi, S., Marvasti-Zadeh, S.M., Zhao, S., Kasaei, S., Qiu, S., Chen, S., Schön, T.B., Xu, T., Lu, W., Hu, W., Zhou, W., Qiu, X., Ke, X., Wu, X.-J., Zhang, X., Yang, X., Zhu, X., Jiang, Y., Wang, Y., Chen, Y., Ye, Y., Li, Y., Yao, Y., Lee, Y., Gu, Y., Wang, Z., Tang, Z., Feng, Z.-H., Mai, Z., Zhang, Z., Wu, Z., Ma, Z., Kristan, M., Leonardis, A., Matas, J., Felsberg, Michael, Pflugfelder, R., Kämäräinen, J.-K., Danelljan, M., Zajc, L.C., Lukežic, A., Drbohlav, O., He, Linbo, Zhang, Yushan, Yan, S., Yang, J., Fernández, G., Hauptmann, A., Memarmoghadam, A., García-Martín, Á., Robinson, Andreas, Varfolomieiev, A., Gebrehiwot, A.H., Uzun, B., Yan, B., Li, B., Qian, C., Tsai, C.-Y., Micheloni, C., Wang, D., Wang, F., Xie, F., Järemo-Lawin, Felix, Gustafsson, F., Foresti, G.L., Bhat, G., Chen, G., Ling, H., Zhang, H., Cevikalp, H., Zhao, H., Bai, H., Kuchibhotla, H.C., Saribas, H., Fan, H., Ghanei-Yakhdan, H., Li, H., Peng, H., Lu, H., Khaghani, J., Bescos, J., Li, J., Fu, J., Yu, J., Xu, J., Kittler, J., Yin, J., Lee, J., Yu, K., Liu, K., Yang, K., Dai, K., Cheng, L., Zhang, L., Wang, L., Van, Gool L., Bertinetto, L., Dunnhofer, M., Cheng, M., Dasari, M.M., Wang, N., Zhang, P., Torr, P.H.S., Wang, Q., Timofte, R., Gorthi, R.K.S., Choi, S., Marvasti-Zadeh, S.M., Zhao, S., Kasaei, S., Qiu, S., Chen, S., Schön, T.B., Xu, T., Lu, W., Hu, W., Zhou, W., Qiu, X., Ke, X., Wu, X.-J., Zhang, X., Yang, X., Zhu, X., Jiang, Y., Wang, Y., Chen, Y., Ye, Y., Li, Y., Yao, Y., Lee, Y., Gu, Y., Wang, Z., Tang, Z., Feng, Z.-H., Mai, Z., Zhang, Z., Wu, Z., and Ma, Z.
Abstract: The Visual Object Tracking challenge VOT2020 is the eighth annual tracker benchmarking activity organized by the VOT initiative. Results of 58 trackers are presented; many are state-of-the-art trackers published at major computer vision conferences or in journals in the recent years. The VOT2020 challenge was composed of five sub-challenges focusing on different tracking domains: (i) VOT-ST2020 challenge focused on short-term tracking in RGB, (ii) VOT-RT2020 challenge focused on “real-time” short-term tracking in RGB, (iii) VOT-LT2020 focused on long-term tracking namely coping with target disappearance and reappearance, (iv) VOT-RGBT2020 challenge focused on short-term tracking in RGB and thermal imagery and (v) VOT-RGBD2020 challenge focused on long-term tracking in RGB and depth imagery. Only the VOT-ST2020 datasets were refreshed. A significant novelty is introduction of a new VOT short-term tracking evaluation methodology, and introduction of segmentation ground truth in the VOT-ST2020 challenge – bounding boxes will no longer be used in the VOT-ST challenges. A new VOT Python toolkit that implements all these novelites was introduced. Performance of the tested trackers typically by far exceeds standard baselines. The source code for most of the trackers is publicly available from the VOT page. The dataset, the evaluation kit and the results are publicly available at the challenge website (http://votchallenge.net ).
Published: 2020
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39. The POLARBEAR Fourier transform spectrometer calibrator and spectroscopic characterization of the POLARBEAR instrument.

Author: Matsuda, F, 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, Westbrook, B, Matsuda, F, 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 cm2, optimized optical coupling to the POLARBEAR optics using a custom designed output parabolic mirror, and a continuously modulated output polarizer. The PB-FTS parabolic mirror is designed to mimic the shape of the 2.5 m-diameter HTT primary reflector, which allows for optimum optical coupling to the POLARBEAR receiver, reducing aberrations and systematics. One polarizing grid is placed at the output of the PB-FTS and modulated via continuous rotation. This modulation allows for decomposition of the signal into different harmonics that can be used to probe potentially pernicious sources of systematic error in a polarization-sensitive instrument. The high throughput and continuous output polarizer modulation features are unique compared to other FTS calibrators used in the CMB field. In-field characterization of the POLARBEAR receiver was accomplished using the PB-FTS in April 2014. We discuss the design, construction, and operation of the PB-FTS and present the spectral characterization of the POLARBEAR receiver. We introduce future applications for the PB-FTS in the next-generation CMB experiment, the Simons Array.
Published: 2019

40. The WISE Extended Source Catalogue (WXSC) I: The 100 Largest Galaxies

Author: Jarrett, T. H., Cluver, M. E., Brown, M. J. I., Dale, D. A., Tsai, C. W., Masci, F., Jarrett, T. H., Cluver, M. E., Brown, M. J. I., Dale, D. A., Tsai, C. W., and Masci, F.
Abstract: We present mid-infrared photometry and measured global properties of the 100 largest galaxies in the sky, including the Magellanic Clouds, Local Group galaxies M31 and M33, the Fornax and Virgo Galaxy Cluster giants, and many of the most spectacular Messier objects (e.g., M51 and M83). This is the first release of a larger catalog of extended sources as imaged in the mid-infrared, called the WISE Extended Source Catalogue (WXSC). In this study we measure their global attributes, including integrated flux, surface brightness and radial distribution. The largest of the large are the LMC, SMC and the Andromeda Galaxy, which are also the brightest mid-infrared galaxies in the sky. We interrogate the large galaxies using WISE colors, which serve as proxies for four general types of galaxies: bulge-dominated spheroidals, intermediate semi-quiescent disks, star-forming spirals, and AGN-dominated. The colors reveal a tight "sequence" that spans 5 magnitudes in W2-W3 color, ranging from early to late-types, and low to high star-forming activity; we fit the functional form given by: ${\rm (W1-W2)} = [0.015 \times {\rm e}^{ \frac{{\rm (W2-W3)}}{1.38} }] - 0.08$. Departures from this sequence may reveal nuclear, starburst, and merging events. Physical properties and luminosity attributes are computed, notably the diameter, aggregate stellar mass and the dust-obscured star formation activity. We introduce the 'pinwheel' diagram which depicts physical properties with respect to the median value observed for WISE galaxies in the local universe. Utilized with the WXSC, this diagram will delineate between different kinds of galaxies, identifying those with similar star formation and structural properties. Finally, we present the mid-infrared photometry of the 25 brightest globular clusters in the sky, including Omega Centauri, 47 Tucanae and a number of famed night-sky targets (e.g. M 13). (Abridged), Comment: 45 pages, 25 figures, 6 tables. Accepted for publication in ApJS. High quality graphics, tables and ancillary material are available at the following URL: https://vislab.idia.ac.za/research
Published: 2019
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41. A Measurement of the Degree Scale CMB B-mode Angular Power Spectrum with POLARBEAR

Author: Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Verges, C., Westbrook, B., Zhou, Y., Adachi, S., Faúndez, M. A. O. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Beckman, S., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Chapman, S., Cheung, K., Chinone, Y., Crowley, K., Cukierman, A., Dobbs, M., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Fujino, T., Galitzki, N., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Kaneko, D., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Segawa, Y., Silva-Feaver, M., Siritanasak, P., Stebor, N., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Tanabe, D., Teply, G. P., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.
Abstract: We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background (CMB) using taken from July 2014 to December 2016 with the POLARBEAR experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of $\mathrm{NET}_\mathrm{array}=23\, \mu \mathrm{K} \sqrt{\mathrm{s}}$ on a 670 square degree patch of sky centered at (RA, Dec)=($+0^\mathrm{h}12^\mathrm{m}0^\mathrm{s},-59^\circ18^\prime$). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ effective polarization map noise with a knee in sensitivity of $\ell = 90$, where the inflationary gravitational wave signal is expected to peak. The measured $B$-mode power spectrum is consistent with a $\Lambda$CDM lensing and single dust component foreground model over a range of multipoles $50 \leq \ell \leq 600$. The data disfavor zero $C_\ell^{BB}$ at $2.2\sigma$ using this $\ell$ range of POLARBEAR data alone. We cross-correlate our data with Planck high frequency maps and find the low-$\ell$ $B$-mode power in the combined dataset to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio $r < 0.90$ at 95% confidence level after marginalizing over foregrounds.
Published: 2019
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42. Hot Dust-Obscured Galaxies with Excess Blue Light

Author: Assef, R. J., Brightman, M., Walton, D. J., Stern, D., Bauer, F. E., Blain, A. W., Diaz-Santos, T., Eisenhardt, P. R. M., Hickox, R. C., Jun, H. D., Psychogyios, A., Tsai, C. -W., Wu, J. W., Assef, R. J., Brightman, M., Walton, D. J., Stern, D., Bauer, F. E., Blain, A. W., Diaz-Santos, T., Eisenhardt, P. R. M., Hickox, R. C., Jun, H. D., Psychogyios, A., Tsai, C. -W., and Wu, J. W.
Abstract: Hot Dust-Obscured Galaxies (Hot DOGs) are among the most luminous galaxies in the Universe. Powered by highly obscured, possibly Compton-thick, active galactic nuclei (AGNs), Hot DOGs are characterized by SEDs that are very red in the mid-IR yet dominated by the host galaxy stellar emission in the UV and optical. An earlier study identified a sub-sample of Hot DOGs with significantly enhanced UV emission. One target, W0204-0506, was studied in detail and, based on Chandra observations, it was concluded that the enhanced emission was most likely due to either extreme unobscured star-formation (${\rm SFR}>1000~M_{\odot}~\rm yr^{-1}$) or to light from the highly obscured AGN scattered by gas or dust into our line of sight. Here, we present a follow-up study of W0204-0506 as well as two more Hot DOGs with excess UV emission. For the two new objects we obtained Chandra/ACIS-S observations, and for all three targets we obtained HST/WFC3 F555W and F160W imaging. We conclude that the excess UV emission is primarily dominated by light from the central highly obscured, hyper-luminous AGN that has been scattered into our line of sight. We cannot rule out, however, that star-formation may significantly contribute to the UV excess of W0204-0506., Comment: 17 pages, 12 figures, 3 tables. Accepted for publication in The Astrophysical Journal
Published: 2019
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43. Cross-correlation of POLARBEAR CMB Polarization Lensing with High-$z$ Sub-mm Herschel-ATLAS galaxies

Author: Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., Verges, C., Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., and Verges, C.
Abstract: We report a 4.8$\sigma$ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the POLARBEAR experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of $b = 5.76 \pm 1.25$, corresponding to a host halo mass of $\log_{10}(M_h/M_\odot) =13.5^{+0.2}_{-0.3}$ at an effective redshift of $z \sim 2$ from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the sub-mm galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extra-galactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments., Comment: 14 pages, 6 figures, updated to match published version on ApJ
Published: 2019
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44. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from Polarbear and Cosmic Shear from Subaru Hyper Suprime-Cam

Author: Namikawa, T, Chinone, Y, Miyatake, H, Oguri, M, Takahashi, R, Kusaka, A, Katayama, N, Adachi, S, Aguilar, M, Aihara, H, Ali, A, Armstrong, R, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Corbett, L, Crowley, KT, El Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Groh, J, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Jeong, O, Kaneko, D, Keating, B, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Miyazaki, S, Murayama, H, Navaroli, M, Nishino, H, Nishizawa, AJ, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Speagle, JS, Stompor, R, Suzuki, A, Tait, PJ, Tajima, O, Takada, M, Takakura, S, Takatori, S, Tanabe, D, Tanaka, M, Teply, GP, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Namikawa, T, Chinone, Y, Miyatake, H, Oguri, M, Takahashi, R, Kusaka, A, Katayama, N, Adachi, S, Aguilar, M, Aihara, H, Ali, A, Armstrong, R, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Cheung, K, Corbett, L, Crowley, KT, El Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Galitzki, N, Goeckner-Wald, N, Groh, J, Hamada, T, Hasegawa, M, Hazumi, M, Hill, CA, Howe, L, Jeong, O, Kaneko, D, Keating, B, Lee, AT, Leon, D, Linder, E, Lowry, LN, Mangu, A, Matsuda, F, Minami, Y, Miyazaki, S, Murayama, H, Navaroli, M, Nishino, H, Nishizawa, AJ, Pham, ATP, Poletti, D, Puglisi, G, Reichardt, CL, Sherwin, BD, Silva-Feaver, M, Siritanasak, P, Speagle, JS, Stompor, R, Suzuki, A, Tait, PJ, Tajima, O, Takada, M, Takakura, S, Takatori, S, Tanabe, D, Tanaka, M, Teply, GP, Tsai, C, Verges, C, Westbrook, B, and Zhou, Y
Published: 2019

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

Author: Matsuda, F, 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, Westbrook, B, Matsuda, F, 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 cm2, optimized optical coupling to the POLARBEAR optics using a custom designed output parabolic mirror, and a continuously modulated output polarizer. The PB-FTS parabolic mirror is designed to mimic the shape of the 2.5 m-diameter HTT primary reflector, which allows for optimum optical coupling to the POLARBEAR receiver, reducing aberrations and systematics. One polarizing grid is placed at the output of the PB-FTS and modulated via continuous rotation. This modulation allows for decomposition of the signal into different harmonics that can be used to probe potentially pernicious sources of systematic error in a polarization-sensitive instrument. The high throughput and continuous output polarizer modulation features are unique compared to other FTS calibrators used in the CMB field. In-field characterization of the POLARBEAR receiver was accomplished using the PB-FTS in April 2014. We discuss the design, construction, and operation of the PB-FTS and present the spectral characterization of the POLARBEAR receiver. We introduce future applications for the PB-FTS in the next-generation CMB experiment, the Simons Array.
Published: 2019

46. Direct Detection of Multiple Backward Volume Modes in Yttrium Iron Garnet at Micron Scale Wavelengths

Author: Lim, Jinho, Bang, Wonbae, Trossmann, Jonathan, Kreisel, Andreas, Jungfleisch, Matthias Benjamin, Hoffmann, Axel, Tsai, C. C., Ketterson, John B., Lim, Jinho, Bang, Wonbae, Trossmann, Jonathan, Kreisel, Andreas, Jungfleisch, Matthias Benjamin, Hoffmann, Axel, Tsai, C. C., and Ketterson, John B.
Abstract: This article belongs to the Proceedings of The 37th International Symposium on Dynamical Properties of Solids.
Published: 2019

47. Allostery in Its Many Disguises: From Theory to Applications

Author: Wodak, S, Paci, E, Dokholyan, N, Berezovsky, I, Horovitz, A, Li, J, Hilser, V, Bahar, I, Karanicolas, J, Stock, G, Hamm, P, Stote, R, Eberhardt, J, Chebaro, Y, Dejaegere, A, Cecchini, M, Changeux, J, Bolhuis, P, Vreede, J, Faccioli, P, Orioli, S, Ravasio, R, Yan, L, Brito, C, Wyart, M, Gkeka, P, Rivalta, I, Palermo, G, Mccammon, J, Panecka-Hofman, J, Wade, R, Di Pizio, A, Niv, M, Nussinov, R, Tsai, C, Jang, H, Padhorny, D, Kozakov, D, Mcleish, T, Wodak, Shoshana J, Paci, Emanuele, Dokholyan, Nikolay V, Berezovsky, Igor N, Horovitz, Amnon, Li, Jing, Hilser, Vincent J, Bahar, Ivet, Karanicolas, John, Stock, Gerhard, Hamm, Peter, Stote, Roland H, Eberhardt, Jerome, Chebaro, Yassmine, Dejaegere, Annick, Cecchini, Marco, Changeux, Jean-Pierre, Bolhuis, Peter G, Vreede, Jocelyne, Faccioli, Pietro, Orioli, Simone, Ravasio, Riccardo, Yan, Le, Brito, Carolina, Wyart, Matthieu, Gkeka, Paraskevi, Rivalta, Ivan, Palermo, Giulia, McCammon, J Andrew, Panecka-Hofman, Joanna, Wade, Rebecca C, Di Pizio, Antonella, Niv, Masha Y, Nussinov, Ruth, Tsai, Chung-Jung, Jang, Hyunbum, Padhorny, Dzmitry, Kozakov, Dima, McLeish, Tom, Wodak, S, Paci, E, Dokholyan, N, Berezovsky, I, Horovitz, A, Li, J, Hilser, V, Bahar, I, Karanicolas, J, Stock, G, Hamm, P, Stote, R, Eberhardt, J, Chebaro, Y, Dejaegere, A, Cecchini, M, Changeux, J, Bolhuis, P, Vreede, J, Faccioli, P, Orioli, S, Ravasio, R, Yan, L, Brito, C, Wyart, M, Gkeka, P, Rivalta, I, Palermo, G, Mccammon, J, Panecka-Hofman, J, Wade, R, Di Pizio, A, Niv, M, Nussinov, R, Tsai, C, Jang, H, Padhorny, D, Kozakov, D, Mcleish, T, Wodak, Shoshana J, Paci, Emanuele, Dokholyan, Nikolay V, Berezovsky, Igor N, Horovitz, Amnon, Li, Jing, Hilser, Vincent J, Bahar, Ivet, Karanicolas, John, Stock, Gerhard, Hamm, Peter, Stote, Roland H, Eberhardt, Jerome, Chebaro, Yassmine, Dejaegere, Annick, Cecchini, Marco, Changeux, Jean-Pierre, Bolhuis, Peter G, Vreede, Jocelyne, Faccioli, Pietro, Orioli, Simone, Ravasio, Riccardo, Yan, Le, Brito, Carolina, Wyart, Matthieu, Gkeka, Paraskevi, Rivalta, Ivan, Palermo, Giulia, McCammon, J Andrew, Panecka-Hofman, Joanna, Wade, Rebecca C, Di Pizio, Antonella, Niv, Masha Y, Nussinov, Ruth, Tsai, Chung-Jung, Jang, Hyunbum, Padhorny, Dzmitry, Kozakov, Dima, and McLeish, Tom
Abstract: Allosteric regulation plays an important role in many biological processes, such as signal transduction, transcriptional regulation, and metabolism. Allostery is rooted in the fundamental physical properties of macromolecular systems, but its underlying mechanisms are still poorly understood. A collection of contributions to a recent interdisciplinary CECAM (Center Européen de Calcul Atomique et Moléculaire) workshop is used here to provide an overview of the progress and remaining limitations in the understanding of the mechanistic foundations of allostery gained from computational and experimental analyses of real protein systems and model systems. The main conceptual frameworks instrumental in driving the field are discussed. We illustrate the role of these frameworks in illuminating molecular mechanisms and explaining cellular processes, and describe some of their promising practical applications in engineering molecular sensors and informing drug design efforts.
Published: 2019

48. Direct Detection of Multiple Backward Volume Modes in Yttrium Iron Garnet at Micron Scale Wavelengths

Author: Lim, Jinho, Bang, Wonbae, Trossmann, Jonathan, Kreisel, Andreas, Jungfleisch, Matthias Benjamin, Hoffmann, Axel, Tsai, C. C., Ketterson, John B., Lim, Jinho, Bang, Wonbae, Trossmann, Jonathan, Kreisel, Andreas, Jungfleisch, Matthias Benjamin, Hoffmann, Axel, Tsai, C. C., and Ketterson, John B.
Abstract: This article belongs to the Proceedings of The 37th International Symposium on Dynamical Properties of Solids.
Published: 2019

49. Hot Dust-Obscured Galaxies with Excess Blue Light

Author: Assef, R. J., Brightman, M., Walton, D. J., Stern, D., Bauer, F. E., Blain, A. W., Diaz-Santos, T., Eisenhardt, P. R. M., Hickox, R. C., Jun, H. D., Psychogyios, A., Tsai, C. -W., Wu, J. W., Assef, R. J., Brightman, M., Walton, D. J., Stern, D., Bauer, F. E., Blain, A. W., Diaz-Santos, T., Eisenhardt, P. R. M., Hickox, R. C., Jun, H. D., Psychogyios, A., Tsai, C. -W., and Wu, J. W.
Abstract: Hot Dust-Obscured Galaxies (Hot DOGs) are among the most luminous galaxies in the Universe. Powered by highly obscured, possibly Compton-thick, active galactic nuclei (AGNs), Hot DOGs are characterized by SEDs that are very red in the mid-IR yet dominated by the host galaxy stellar emission in the UV and optical. An earlier study identified a sub-sample of Hot DOGs with significantly enhanced UV emission. One target, W0204-0506, was studied in detail and, based on Chandra observations, it was concluded that the enhanced emission was most likely due to either extreme unobscured star-formation (${\rm SFR}>1000~M_{\odot}~\rm yr^{-1}$) or to light from the highly obscured AGN scattered by gas or dust into our line of sight. Here, we present a follow-up study of W0204-0506 as well as two more Hot DOGs with excess UV emission. For the two new objects we obtained Chandra/ACIS-S observations, and for all three targets we obtained HST/WFC3 F555W and F160W imaging. We conclude that the excess UV emission is primarily dominated by light from the central highly obscured, hyper-luminous AGN that has been scattered into our line of sight. We cannot rule out, however, that star-formation may significantly contribute to the UV excess of W0204-0506., Comment: 17 pages, 12 figures, 3 tables. Accepted for publication in The Astrophysical Journal
Published: 2019
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50. Cross-correlation of POLARBEAR CMB Polarization Lensing with High-$z$ Sub-mm Herschel-ATLAS galaxies

Author: Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., Verges, C., Faundez, M. Aguilar, Arnold, K., Baccigalupi, C., Barron, D., Beck, D., Bianchini, F., Boettger, D., Borrill, J., Carron, J., Cheung, K., Chinone, Y., Bouhargani, H. El, Elleflot, T., Errard, J., Fabbian, G., Feng, C., Galitzki, N., Goeckner-Wald, N., Hasegawa, M., Hazumi, M., Howe, L., Kaneko, D., Katayama, N., Keating, B., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., Sherwin, B. D., Silva-Feaver, M., Stompor, R., Suzuki, A., Tajima, O., Takakura, S., Takatori, S., Teply, G. P., Tsai, C., and Verges, C.
Abstract: We report a 4.8$\sigma$ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the POLARBEAR experiment and the infrared-selected galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind. We infer a best-fit galaxy bias of $b = 5.76 \pm 1.25$, corresponding to a host halo mass of $\log_{10}(M_h/M_\odot) =13.5^{+0.2}_{-0.3}$ at an effective redshift of $z \sim 2$ from the cross-correlation power spectrum. Residual uncertainties in the redshift distribution of the sub-mm galaxies are subdominant with respect to the statistical precision. We perform a suite of systematic tests, finding that instrumental and astrophysical contaminations are small compared to the statistical error. This cross-correlation measurement only relies on CMB polarization information that, differently from CMB temperature maps, is less contaminated by galactic and extra-galactic foregrounds, providing a clearer view of the projected matter distribution. This result demonstrates the feasibility and robustness of this approach for future high-sensitivity CMB polarization experiments., Comment: 14 pages, 6 figures, updated to match published version on ApJ
Published: 2019
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