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37th International Cosmic Ray Conference, ICRC 2021

作者： Pronost, Guillaume Abe, K. Bronner, C. Hayato, Y. Hiraide, K. Ikeda, M. Kameda, J. Kanemura, Y. Kataoka, Y. Miki, S. Miura, M. Moriyama, S. Nagao, Y. Nakahata, M. Nakayama, S. Okamoto, K. Pronost, G. Sekiya, H. Shiozawa, M. Sonoda, Y. Suzuki, Y. Takeda, A. Takemoto, Y. Takenaka, A. Tanaka, H. Watanabe, S. Yano, T. Han, S. Kajita, T. Okumura, K. Tashiro, T. Xia, J. Megias, G.D. Labarga, L. Marti, Ll. Zaldivar, B. Pointon, B.W. Kearns, E. Raaf, J.L. Wan, L. Wester, T. Bian, J. Griskevich, N.J. Kropp, W.R. Locke, S. Mine, S. Smy, M.B. Sobel, H.W. Takhistov, V. Hill, J. Kim, J.Y. Lim, I.T. Park, R.G. Bodur, B. Scholberg, K. Walter, C.W. Bernard, L. Coffani, A. Drapier, O. El Hedri, S. Giampaolo, A. Gonin, M. Mueller, Th.A. Paganini, P. Quilain, B. Ishizuka, T. Nakamura, T. Jang, J.S. Learned, J.G. Cao, S. Anthony, L.H.V. Martin, D. Scott, M. Sztuc, A.A. Uchida, Y. Berardi, V. Catanesi, M.G. Radicioni, E. Calabria, N.F. Machado, L.N. De Rosa, G. Collazuol, G. Iacob, F. Lamoureux, M. Mattiazzi, M. Ospina, N. Ludovici, L. Maekawa, Y. Nishimura, Y. Friend, M. Hasegawa, T. Ishida, T. Kobayashi, T. Jakkapu, M. Matsubara, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Boschi, T. Di Lodovico, F. Gao, J. Migenda, J. Taani, M. Zsoldos, S. Nakano, Y. Ozaki, H. Suzuki, A.T. Takeuchi, Y. Yamamoto, S. Kotsar, Y. Ali, A. Feng, J. Kikawa, T. Mori, M. Nakaya, T. Wendell, R.A. Yasutome, K. Fernandez, P. McCauley, N. Mehta, P. Tsui, K.M. Fukuda, Y. Itow, Y. Menjo, H. Sato, K. Lagoda, J. Lakshmi, S.M. Mijakowski, P. Zalipska, J. Jiang, J. Jung, C.K. Vilela, C. Wilking, M.J. Yanagisawa, C. Harada, M. Ishino, H. Ito, S. Kitagawa, H. Koshio, Y. Ma, W. Piplani, N. Sakai, S. Barr, G. Barrow, D. Cook, L. Goldsack, A. Samani, S. Wark, D. Nova, F. Yang, J.Y. Jenkins, S.J. Malek, M. McElwee, J.M. Stone, O. Thiesse, M.D. Thompson, L.F. Okazawa, H. Kim, S.B. Kamioka Observatory ICRR The University of Tokyo Kamioka Gifu506-1205 Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba277-8582 Japan Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics British Columbia Institute of Technology BurnabyBCV5G 3H2 Canada Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Institute for Universe and Elementary Particles Chonnam National University Gwangju61186 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Junior College Fukuoka Institute of Technology Fukuoka Fukuoka811-0295 Japan Department of Physics Gifu University Gifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju500-712 Korea Republic of Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Institute For Interdisciplinary Research in Science and Education ICISE Quy Nhon55121 Viet Nam Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Università di Roma "La Sapienza" RomaI-00185 Italy Department of Physics Keio Unive

The radioactivity background are among the most dangerous background for low energy neutrino analysis in Super-Kamiokande (SK), like the solar neutrino analysis. Among them, the main contribution is coming from 222Rn, which is spread in the detector’s water due to the water source and to the photo multiplier (PMT) emanations. Up to now, its exact distribution in the detector was not known. Using our knowledge of the radon concentration in the detector water, and the SK-IV solar data, we developed a model of the radon distribution in the detector. The uncertainty on the Rn concentration associated with this model was estimated to be ∼ 0.1 mBq/m3 © Copyright owned by the author(s).

关键词： Radioactivity

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Diffuse Supernova Neutrino Background Search at Super-Kamiokande 37

Diffuse Supernova Neutrino Background Search at Super-Kamiok...

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37th International Cosmic Ray Conference, ICRC 2021

作者： El Hedri, S. Ashida, Y. Abe, K. Bronner, C. Hayato, Y. Hiraide, K. Ikeda, M. Kameda, J. Kanemura, Y. Kataoka, Y. Miki, S. Miura, M. Moriyama, S. Nagao, Y. Nakahata, M. Nakayama, S. Okamoto, K. Pronost, G. Sekiya, H. Shiozawa, M. Sonoda, Y. Suzuki, Y. Takeda, A. Takemoto, Y. Takenaka, A. Tanaka, H. Watanabe, S. Yano, T. Han, S. Kajita, T. Okumura, K. Tashiro, T. Xia, J. Megias, G.D. Labarga, L. Marti, Ll. Zaldivar, B. Pointon, B.W. Kearns, E. Raaf, J.L. Wan, L. Wester, T. Bian, J. Griskevich, N.J. Kropp, W.R. Locke, S. Mine, S. Smy, M.B. Sobel, H.W. Takhistov, V. Hill, J. Kim, J.Y. Lim, I.T. Park, R.G. Bodur, B. Scholberg, K. Walter, C.W. Bernard, L. Coffani, A. Drapier, O. El-Hedri, S. Gimpaolo, A. Gonin, M. Mueller, Th.A. Paganini, P. Quilain, B. Ishizuka, T. Nakamura, T. Jang, J.S. Learned, J.G. Cao, S. Anthony, L.H.V. Martin, D. Scott, M. Sztuc, A.A. Uchida, Y. Berardi, V. Catanesi, M.G. Radicioni, E. Calabria, N.F. Machado, L.N. De Rosa, G. Collazuol, G. Iacob, F. Lamoureux, M. Mattiazzi, M. Ospina, N. Ludovici, L. Maekawa, Y. Nishimura, Y. Friend, M. Hasegawa, T. Ishida, T. Kobayashi, T. Jakkapu, M. Matsubara, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Boschi, T. Di Lodovico, F. Gao, J. Migenda, J. Taani, M. Zsoldos, S. Nakano, Y. Ozaki, H. Suzuki, A.T. Takeuchi, Y. Yamamoto, S. Kotsar, Y. Ali, A. Feng, J. Kikawa, T. Mori, M. Nakaya, T. Wendell, R.A. Yasutome, K. Fernandez, P. McCauley, N. Mehta, P. Tsui, K.M. Fukuda, Y. Itow, Y. Menjo, H. Sato, K. Lagoda, J. Lakshmi, S.M. Mijakowski, P. Zalipska, J. Jiang, J. Jung, C.K. Vilela, C. Wilking, M.J. Yanagisawa, C. Harada, M. Ishino, H. Ito, S. Kitagawa, H. Koshio, Y. Ma, W. Piplani, N. Sakai, S. Barr, G. Barrow, D. Cook, L. Goldsack, A. Samani, S. Wark, D. Nova, F. Yang, J.Y. Jenkins, S.J. Malek, M. McElwee, J.M. Stone, O. Thiesse, M.D. Thompson, L.F. Okazawa, H. Ecole Polytechnique IN2P3-CNRS Laaoratoire Leprince-Ringuet PalaiseauF-91120 France Kyoto University Department of Physics Kyoto Kyoto606-8502 Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics British Columbia Institute of Technology BurnabyBCV5G 3H2 Canada Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Institute for Universe and Elementary Particles Chonnam National University Gwangju61186 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3 CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Junior College Fukuoka Institute of Technology Fukuoka Fukuoka811-0295 Japan Department of Physics Gifu University Gifu Gifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju500-712 Korea Republic of Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Institute For Interdisciplinary Research in Science and Education ICISE Quy Nhon55121 Viet Nam Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Unive

We present the results of a search for the Diffuse Supernova Neutrino Background (DSNB) at Super-Kamiokande (SK) that incorporates 22.5 × 2970 *** of data from its fourth data-taking phase. Two analyses, with different energy regimes covering the 9.3−81.3 MeV antineutrino energy range, have been developed based on previous SK searches, with substantially improved background modeling and data reduction techniques. Moreover, a combined analysis of nearly 20 years of SK data (1996-2018) has been performed, with a 90% C.L. sensitivity to the DSNB flux comparable to various DSNB predictions. No significant evidence for a DSNB signal has been observed, and both analyses set world-leading limits on the DSNB flux that can reach about 2.7ν***−2.s−1 for a wide range of models. © Copyright owned by the author(s).

关键词： Supernovae

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Designing the Application of Security Text Messages Into Audio Files Using Data Encryption Standard (DES) Algorithms Using the End Of File (EOF) Method

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Journal of Physics: Conference Series 2019年第1期1363卷

作者： A M H Pardede Anggi Pramana Muhammad Zarlis Akbar Iskandar Rosida Tiurma Manurung S Sriadhi Citra Kurniawan Abdurrozzaq Hasibuan Nurintan Asyiah Siregar Ayu Esteka Sari Indrya Mulyaningsih Teguh Hidayat Iskandar Alam Ibrahim Tri Listyorini Edy Winarno Tulus STMIK Kaputama Binjai Sumatera Utara Indonesia Department of Computer Science Universitas Sumatera Utara Medan Indonesia Department of Informatics STMIK AKBA Makassar Indonesia Graduate Program in Scientific Psychology Universitas Kristen Maranatha Indonesia Department of Electrical Engineering Universitas Negeri Medan Indonesia Department of Electrical Engineering Sekolah Tinggi Teknik Malang Indonesia Faculty of Engineering Universitas Islam Sumatera Utara Medan Indonesia Department of Management STIE Labuhanbatu Sumatera Utara Indonesia Department of Management STIE Sakti Alam Kerinci Jambi Indonesia Department of Indonesian Language Teaching Institut Agama Islam Negeri Syekh Nurjati Cirebon Indonesia Department of Informatics Engineering Universitas Muhammadiyah Sorong Sorong Indonesia Department of English Education Universitas Muhammadiyah Sorong Sorong Indonesia Department of Informatics Universitas Muria Kudus Indonesia Faculty of Information Technology Universitas Stikubank Semarang Indonesia Department of Mathematics Universitas Sumatera Utara Medan Indonesia

There are several ways to deal with security issues of confidential data sent via the internet, including using cryptographic techniques and steganography. Steganography is the science and art of concealing information / messages in a media in such a way that its existence is not detected by other parties who are not entitled to the information. Instead, cryptography disguises the meaning of a message, but does not hide that there is a message because the file looks suspicious. The Steganography technique used here was End Of File (EOF). The EOF technique described how to add data or files at the end of the image file. For this technique, the size of data or files that will be hidden could be larger than the size of the image file. The hidden data will be inserted at the end of the file so that it will not affect the image. This steganography application is also equipped with a cryptographic function Data Encryption Standard (DES) at the time of insertion of data that functions as a generator code and encrypts data, so that the security of a data in the file is more protected and protected from those who are not entitled to know the data.

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Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector 37

Measurements of the charge ratio and polarization of cosmic-...

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37th International Cosmic Ray Conference, ICRC 2021

作者： Kitagawa, Hussain Nakano, Yuuki Koshio, Yusuke Abe, K. Bronner, C. Hayato, Y. Hiraide, K. Ikeda, M. Kameda, J. Kanemura, Y. Kataoka, Y. Miki, S. Miura, M. Moriyama, S. Nagao, Y. Nakahata, M. Nakayama, S. Okamoto, K. Pronost, G. Sekiya, H. Shiozawa, M. Sonoda, Y. Suzuki, Y. Takeda, A. Takemoto, Y. Takenaka, A. Tanaka, H. Watanabe, S. Yano, T. Han, S. Kajita, T. Okumura, K. Tashiro, T. Xia, J. Megias, G.D. Labarga, L. Marti, Ll. Zaldivar, B. Pointon, B.W. Kearns, E. Raaf, J.L. Wan, L. Wester, T. Bian, J. Griskevich, N.J. Kropp, W.R. Locke, S. Mine, S. Smy, M.B. Sobel, H.W. Takhistov, V. Hill, J. Kim, J.Y. Lim, I.T. Park, R.G. Bodur, B. Scholberg, K. Walter, C.W. Bernard, L. Coffani, A. Drapier, O. El Hedri, S. Giampaolo, A. Gonin, M. Mueller, Th.A. Paganini, P. Quilain, B. Ishizuka, T. Nakamura, T. Jang, J.S. Learned, J.G. Cao, S. Anthony, L.H.V. Martin, D. Scott, M. Sztuc, A.A. Uchida, Y. Berardi, V. Catanesi, M.G. Radicioni, E. Calabria, N.F. Machado, L.N. De Rosa, G. Collazuol, G. Iacob, F. Lamoureux, M. Mattiazzi, M. Ospina, N. Ludovici, L. Maekawa, Y. Nishimura, Y. Friend, M. Hasegawa, T. Ishida, T. Kobayashi, T. Jakkapu, M. Matsubara, T. Nakadaira, T. Nakamura, K. Oyama, Y. Sakashita, K. Sekiguchi, T. Tsukamoto, T. Boschi, T. Di Lodovico, F. Gao, J. Migenda, J. Taani, M. Zsoldos, S. Ozaki, H. Suzuki, A.T. Takeuchi, Y. Yamamoto, S. Kotsar, Y. Ali, A. Feng, J. Kikawa, T. Mori, M. Nakaya, T. Wendell, R.A. Yasutome, K. Fernandez, P. McCauley, N. Mehta, P. Tsui, K.M. Fukuda, Y. Itow, Y. Menjo, H. Sato, K. Lagoda, J. Lakshmi, S.M. Mijakowski, P. Zalipska, J. Jiang, J. Jung, C.K. Vilela, C. Wilking, M.J. Yanagisawa, C. Harada, M. Ishino, H. Ito, S. Ma, W. Piplani, N. Sakai, S. Barr, G. Barrow, D. Cook, L. Goldsack, A. Samani, S. Wark, D. Nova, F. Yang, J.Y. Jenkins, S.J. Malek, M. McElwee, J.M. Stone, O. Thiesse, M.D. Thompson, L.F. Okazawa, H. Kim, S.B. Okayama University Department of Physics Tsushimanaka Kita-ku Okayama Japan Kobe University Department of Physics Rokko-dai Nada-ku Kobe Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu506-1205 Japan Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Institute for Cosmic Ray Research University of Tokyo Chiba Kashiwa277-8582 Japan Department of Theoretical Physics University Autonoma Madrid Madrid28049 Spain Department of Physics Boston University BostonMA02215 United States Department of Physics British Columbia Institute of Technology BurnabyBCV5G 3H2 Canada Department of Physics and Astronomy University of California Irvine IrvineCA92697-4575 United States Department of Physics California State University Dominguez Hills CarsonCA90747 United States Institute for Universe and Elementary Particles Chonnam National University Gwangju61186 Korea Republic of Department of Physics Duke University DurhamNC27708 United States Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet PalaiseauF-91120 France Junior College Fukuoka Institute of Technology Fukuoka Fukuoka811-0295 Japan Department of Physics Gifu University Gifu Gifu501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju500-712 Korea Republic of Department of Physics and Astronomy University of Hawaii HonoluluHI96822 United States Institute For Interdisciplinary Research in Science and Education ICISE Quy Nhon55121 Viet Nam Department of Physics Imperial College London LondonSW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Bari Università e Politecnico di Bari BariI-70125 Italy Dipartimento di Fisica INFN Sezione di Napoli Università di Napoli NapoliI-80126 Italy Dipartimento di Fisica INFN Sezione di Padova Università di Padova PadovaI-35131 Italy INFN Sezione di Roma Università

Cosmic-ray muons arise from the showers of secondary particles produced via the interactions of primary cosmic particles with air nuclei at the top of the atmosphere. The interaction products, pions and kaons composing showers mostly decay to muons reflect the details of the hadronic interactions depending on their energy. Measurements of the charge ratio and polarization of cosmic-ray muons can be used to constrain high energy hadronic interaction models in the atmosphere. In this presentation, we will report the current status of the measurement of the charge ratio using data collected by the Super-Kamiokande (SK) detector located at a depth of 2700 m of water equivalent. Using the data taken in the fourth phase of SK (SK-IV), the charge ratio is measured to be 1.42 ± 0.02 (statistical uncertainty only), at the energy of 1.3 TeV. This result for the charge ratio is in good agreement with those previously obtained by deep underground experiments. © Copyright owned by the author(s) under the terms of the Creative Commons.

关键词： Cosmology

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Sustainable Revitalization in Cultural Heritage Kampong Kauman Surakarta Supported by Spatial Analysis

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IOP Conference Series: Earth and Environmental Science 2018年第1期123卷

作者： M Musyawaroh T S Pitana M Masykuri Nandariyah Doctoral Candidate Study Program of Environmental Science Graduate School of Universitas Sebelas Maret Surakarta Indonesia Study Program of Architecture Faculty of Engineering Universitas Sebelas Maret Surakarta Indonesia Study Program of Environmental Science Graduate School of Universitas Sebelas Maret Surakarta Indonesia Study Program of Agronomy Graduate School of Universitas Sebelas Maret Surakarta Indonesia

Revitalization is a much-needed for a historic kampong as a settlement, place of business, and as tourist destinations. The research was conducted in Kauman as one of the cultural heritage kampong which was formerly as a residence of abdidalemulamaKeraton who also work as batik entrepreneurs. This study aims to formulate a sustainable revitalization step based on the character of the area and the building. Aspects of sustainable revitalization that analyzed are the physical and non-physical condition of the environment. This research is an applied research with qualitative rationalistic approach supported with spatial distribution analysis through satellite imagery and Arch-GIS. The results revealed that sustainable revitalization for Kaumancan be done through: 1) Physical condition of the environment consists of land and building use, green open space, recreational park and sport activities, streets, drainage network, sewer network, the garbage disposal network; 2) Non-physical of the environment consists of economy, heritage socio-cultural, and the engagement of relevant stakeholders. The difference of this study with others is, this study is a continuation of the Kauman revitalization assistance program which involves community participation to produce a more appropriate solution for the problem of kampong.

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The Black Hole Explorer: Motivation and Vision

arXiv

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arXiv 2024年

作者： Johnson, Michael D. Akiyama, Kazunori Baturin, Rebecca Bilyeu, Bryan Blackburn, Lindy Boroson, Don Cárdenas-Avendaño, Alejandro Chael, Andrew Chan, Chi-Kwan Chang, Dominic Cheimets, Peter Chou, Cathy Doeleman, Sheperd S. Farah, Joseph Galison, Peter Gamble, Ronald Gammie, Charles F. Gelles, Zachary Gómez, José L. Gralla, Samuel E. Grimes, Paul Gurvits, Leonid I. Hadar, Shahar Haworth, Kari Hada, Kazuhiro Hecht, Michael H. Honma, Mareki Houston, Janice Hudson, Ben Issaoun, Sara Jia, He Jorstad, Svetlana Kauffmann, Jens Kovalev, Yuri Y. Kurczynski, Peter Lafon, Robert Lupsasca, Alexandru Lehmensiek, Robert Ma, Chung-Pei Marrone, Daniel P. Marscher, Alan P. Melnick, Gary J. Narayan, Ramesh Niinuma, Kotaro Noble, Scott C. Palmer, Eric J. Palumbo, Daniel C.M. Paritsky, Lenny Peretz, Eliad Pesce, Dominic Plavin, Alexander Quataert, Eliot Rana, Hannah Ricarte, Angelo Roelofs, Freek Shtyrkova, Katia Sinclair, Laura C. Small, Jeffrey Kumara, Sridharan Tirupati Srinivasan, Ranjani Strominger, Andrew Tiede, Paul Tong, Edward Wang, Jade Weintroub, Jonathan Wielgus, Maciek Wong, George Zhang, Xinyue Alice Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Black Hole Initiative Harvard University 20 Garden Street CambridgeMA02138 United States Haystack Observatory Massachusetts Institute of Technology WestfordMA01886 United States Mizusawa VLBI Observatory National Astronomical Observatory of Japan Iwate023-0861 Japan MIT Lincoln Laboratory LexingtonMA02421 United States Princeton Gravity Initiative Princeton University PrincetonNJ08544 United States Steward Observatory and Department of Astronomy University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Data Science Institute University of Arizona 1230 N. Cherry Ave. TucsonAZ85721 United States Program in Applied Mathematics University of Arizona 617 N. Santa Rita TucsonAZ85721 United States Las Cumbres Observatory 6740 Cortona Drive GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Department of History of Science Harvard University CambridgeMA02138 United States Department of Physics Harvard University CambridgeMA02138 United States NASA Goddard Space Flight Center GreenbeltMD20771 United States Departments of Astronomy and of Physics University of Illinois UrbanaIL61801 United States Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía s/n GranadaE-18008 Spain Department of Physics University of Arizona TucsonAZ85719 United States Joint Institute for VLBI ERIC Dwingeloo7991PD Netherlands Faculty of Aerospace Engineering Delft University of Technology Delft2629 HS Netherlands Department of Mathematics and Physics University of Haifa at Oranim Kiryat Tivon3600600 Israel Haifa Research Center for Theoretical Physics and Astrophysics University of Haifa Haifa3498838 Israel 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-

We present the Black Hole Explorer (BHEX), a mission that will produce the sharpest images in the history of astronomy by extending submillimeter Very-Long-Baseline Interferometry (VLBI) to space. BHEX will discover and measure the bright and narrow "photon ring" that is predicted to exist in images of black holes, produced from light that has orbited the black hole before escaping. This discovery will expose universal features of a black hole's spacetime that are distinct from the complex astrophysics of the emitting plasma, allowing the first direct measurements of a supermassive black hole's spin. In addition to studying the properties of the nearby supermassive black holes M87*and Sgr A*, BHEX will measure the properties of dozens of additional supermassive black holes, providing crucial insights into the processes that drive their creation and growth. BHEX will also connect these supermassive black holes to their relativistic jets, elucidating the power source for the brightest and most efficient engines in the universe. BHEX will address fundamental open questions in the physics and astrophysics of black holes that cannot be answered without submillimeter space VLBI. The mission is enabled by recent technological breakthroughs, including the development of ultra-high-speed downlink using laser communications, and it leverages billions of dollars of existing ground infrastructure. We present the motivation for BHEX, its science goals and associated requirements, and the pathway to launch within the next decade. © 2024, CC BY.

关键词： Photons

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DEA and Fuzzy Simple Additive Weighting for Benchmarking Qualitative Data

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Journal of Physics: Conference Series 2019年第1期1361卷

作者： Dahlan Abdullah H Hartono Erianto Ongko Cut Ita Erliana Defi Irwansyah Akbar Iskandar Ayu Esteka Sari Abdussakir Yuniningsih Nurintan Asyiah Siregar Muhammad Syahrul Kahar Raditya Faisal Waliulu Ainna Amalia Nuning Kurniasih Muhammad Arifin Syafiul Muzid Department of Informatics Universitas Malikussaleh Aceh Indonesia Department of Computer Science STMIK IBBI Medan Indonesia Department of Informatics Akademi Teknologi Industri Immanuel Medan Indonesia Department of Industrial Engineering Universitas Malikussaleh Aceh Indonesia Department of Informatics STMIK AKBA Makassar Indonesia Department of Management STIE Sakti Alam Kerinci Jambi Indonesia Department of Mathematics Education State Islamic University of Malang MalangIndonesia Department of Economic and Business Universitas Pembangunan Nasional 'Veteran' Surabaya Indonesia Department of Management STIE Labuhanbatu Sumatera Utara Indonesia Mathematics Education Department Universitas Muhammadiyah Sorong Sorong Indonesia Informatics Engineering Department Universitas Muhammadiyah Sorong Sorong Indonesia Islamic Institut of Miftahul Ula Kertosono Nganjuk East Java Indonesia Faculty of Communication Sciences Library and Information Science Program Universitas Padjadjaran Bandung Indonesia Department of Information System Faculty of Engineering Universitas Muria Kudus Indonesia Information System Department Universitas Muria Kudus Indonesia

Data Envelopment Analysis (DEA) is one method that is often used in the benchmarking process. The benchmarking process with DEA is often faced with problems where there is a Decision Making Unit (DMU) both Input and Output which is not in the form of qualitative data but in the form of qualitative data. Qualitative data requires an assessment from the appraiser so that it can become quantitative data. This study will use the Fuzzy Simple Additive Weighting method to convert qualitative data into quantitative. The results of this study will produce a model that integrates DEA with Fuzzy Simple Additive Weighting.

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Geochemical Approach to Reveal The Genetic Occurrence of Gibbsite, Relative to The Parent Rock Type in Lateritic Bauxites

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Journal of Physics: Conference Series 2019年第1期1363卷

作者： R D Nugraheni D Sunjaya Geological Engineering Study Program Faculty of Earth Technology and Energy Universitas Trisakti Jl. Kyai Tapa No.1 Grogol Jakarta Barat Indonesia PT Aneka Tambang Tbk. Unit Geomin Jl. Letjen T.B. Simatupang No.1 Lingkar Selatan Tanjung Barat Jakarta Selatan

Situating in a tropical climate, will be favourable for Indonesia and Malaysia to have an intensive weathering and a concentration of lateritic bauxite. The study area takes place in Kuantan, Pahang State, Malaysia and Landak area, West Kalimantan, Indonesia. The study area has different type of parent rock, topography and drainage condition, which will also cause the different characteristics of alumina minerals in bauxite. One of the common form of alumina minerals is known as Gibbsite [Al(OH)3]. The objective of this research is to investigate the genesis of gibbsite from two different parent rocks. Samples were taken and collected from pitting, analyzed for Al2O3, Fe2O3, SiO2 and TiO2 using XRF and XRD examination. The parent rock of bauxite in Kuantan is basalt, meanwhile, in Landak, ranges from granodiorite to andesite. Petrography and XRD analyses of Kuantan bauxite shows predominant gibbsite, with minor amount of geothite, hematite, kaolinite, illite, quartz and feldspar, while in Landak, mineralogically consists of variant amount of gibbsite, goethite, hematite, kaolinite, illite and quartz. In Kuantan, the amount of Al2O3 varies from 23.6% - 51.01%, nearly similar than that in Landak that varies from 31.35% - 55.03%. Gibbsite in Kuantan is assumed as a transformation of Ca-rich plagioclase and Ferromagnesian- silicate minerals, on the other hand, gibbsite in Landak was produced from direct weathering of primary Al- silicate minerals (Na- plagioclase and K-feldspar). From study, it can be inferred that gibbsite formed from a layer of silicates and will concentrated in finer clay as a weathering product. Moreover, the different types of parent rock will produce different types and amount of alumina minerals. The study will be beneficial to predict the existence of potential alumina minerals in lateritic bauxite.

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Measurement of the neutrino-oxygen neutral-current quasielastic cross section using atmospheric neutrinos in the SK-Gd experiment

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Physical Review D 2024年第1期109卷 L011101-L011101页

作者： S. Sakai K. Abe C. Bronner Y. Hayato K. Hiraide K. Hosokawa K. Ieki M. Ikeda J. Kameda Y. Kanemura R. Kaneshima Y. Kashiwagi Y. Kataoka S. Miki S. Mine M. Miura S. Moriyama Y. Nakano M. Nakahata S. Nakayama Y. Noguchi K. Sato H. Sekiya H. Shiba K. Shimizu M. Shiozawa Y. Sonoda Y. Suzuki A. Takeda Y. Takemoto H. Tanaka T. Yano S. Han T. Kajita K. Okumura T. Tashiro T. Tomiya X. Wang S. Yoshida P. Fernandez L. Labarga N. Ospina B. Zaldivar B. W. Pointon E. Kearns J. L. Raaf L. Wan T. Wester J. Bian N. J. Griskevich S. Locke M. B. Smy H. W. Sobel V. Takhistov A. Yankelevich J. Hill M. C. Jang S. H. Lee D. H. Moon R. G. Park B. Bodur K. Scholberg C. W. Walter A. Beauchêne O. Drapier A. Giampaolo Th. A. Mueller A. D. Santos P. Paganini B. Quilain T. Nakamura J. S. Jang L. N. Machado J. G. Learned K. Choi N. Iovine S. Cao L. H. V. Anthony D. Martin N. W. Prouse M. Scott A. A. Sztuc Y. Uchida V. Berardi N. F. Calabria M. G. Catanesi E. Radicioni A. Langella G. De Rosa G. Collazuol F. Iacob M. Mattiazzi L. Ludovici M. Gonin G. Pronost C. Fujisawa Y. Maekawa Y. Nishimura R. Okazaki R. Akutsu M. Friend T. Hasegawa T. Ishida T. Kobayashi M. Jakkapu T. Matsubara T. Nakadaira K. Nakamura Y. Oyama K. Sakashita T. Sekiguchi T. Tsukamoto N. Bhuiyan G. T. Burton F. Di Lodovico J. Gao A. Goldsack T. Katori J. Migenda R. M. Ramsden Z. Xie S. Zsoldos A. T. Suzuki Y. Takagi H. Zhong Y. Takeuchi J. Feng L. Feng J. R. Hu Z. Hu M. Kawaue T. Kikawa M. Mori T. Nakaya R. A. Wendell K. Yasutome S. J. Jenkins N. McCauley P. Mehta A. Tarant Y. Fukuda Y. Itow H. Menjo K. Ninomiya Y. Yoshioka J. Lagoda S. M. Lakshmi M. Mandal P. Mijakowski Y. S. Prabhu J. Zalipska M. Jia J. Jiang C. K. Jung W. Shi M. J. Wilking C. Yanagisawa M. Harada Y. Hino H. Ishino Y. Koshio F. Nakanishi T. Tada T. Tano T. Ishizuka G. Barr D. Barrow L. Cook S. Samani D. Wark A. Holin F. Nova S. Jung B. S. Yang J. Y. Yang J. Yoo J. E. P. Fannon L. Kneale M. Malek J. M. McElwee M. D. Thiesse L. F. Thompson S. T. Wilson H. Okazawa S. B. Kim E. Kwon J. W. Seo I. Yu A. K. Ichika Department of Physics Okayama University Okayama 700-8530 Japan Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu 506-1205 Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI) The University of Tokyo Institutes for Advanced Study University of Tokyo Kashiwa Chiba 277-8583 Japan Department of Physics and Astronomy University of California Irvine Irvine California 92697-4575 USA Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba 277-8582 Japan ILANCE CNRS—University of Tokyo International Research Laboratory Kashiwa Chiba 277-8582 Japan Department of Theoretical Physics University Autonoma Madrid 28049 Madrid Spain Department of Physics British Columbia Institute of Technology Burnaby British Columbia V5G 3H2 Canada TRIUMF 4004 Wesbrook Mall Vancouver British Columbia V6T2A3 Canada Department of Physics Boston University Boston Massachusetts 02215 USA High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan Department of Physics California State University Dominguez Hills Carson California 90747 USA Institute for Universe and Elementary Particles Chonnam National University Gwangju 61186 South Korea Department of Physics Duke University Durham North Carolina 27708 USA Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet F-91120 Palaiseau France Department of Physics Gifu University Gifu 501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju 500-712 South Korea School of Physics and Astronomy University of Glasgow Glasgow Scotland G12 8QQ United Kingdom Department of Physics and Astronomy University of Hawaii Honolulu Hawaii 96822 USA Institute for Basic Science (IBS) Daejeon 34126 South Korea Institute for Interdisciplinary Research in Science and Education ICISE Quy Nhon 55121 Vietnam Department of Physics Imperial College London London SW7 2AZ United Kingdom Dipa

We report the first measurement of the atmospheric neutrino-oxygen neutral-current quasielastic (NCQE) cross section in the gadolinium-loaded Super-Kamiokande (SK) water Cherenkov detector. In June 2020, SK began a new experimental phase, named SK-Gd, by loading 0.011% by mass of gadolinium into the ultrapure water of the SK detector. The introduction of gadolinium to ultrapure water has the effect of improving the neutron-tagging efficiency. Using a 552.2 day dataset from August 2020 to June 2022, we measure the NCQE cross section to be 0.74±0.22(stat)−0.15+0.85(syst)×10−38 cm2/oxygen in the energy range from 160 MeV to 10 GeV, which is consistent with the atmospheric neutrino-flux-averaged theoretical NCQE cross section and the measurement in the SK pure-water phase within the uncertainties. Furthermore, we compare the models of the nucleon-nucleus interactions in water and find that the binary cascade model and the Liège intranuclear cascade model provide a somewhat better fit to the observed data than the Bertini cascade model. Since the atmospheric neutrino-oxygen NCQE reactions are one of the main backgrounds in the search for diffuse supernova neutrino background (DSNB), these new results will contribute to future studies—and the potential discovery—of the DSNB in SK.

关键词： Total cross sections Neutrinos Cherenkov detectors

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Atmospheric neutrino oscillation analysis with neutron tagging and an expanded fiducial volume in Super-Kamiokande I–V

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Physical Review D 2024年第7期109卷 072014-072014页

作者： T. Wester K. Abe C. Bronner Y. Hayato K. Hiraide K. Hosokawa K. Ieki M. Ikeda J. Kameda Y. Kanemura R. Kaneshima Y. Kashiwagi Y. Kataoka S. Miki S. Mine M. Miura S. Moriyama Y. Nakano M. Nakahata S. Nakayama Y. Noguchi K. Sato H. Sekiya H. Shiba K. Shimizu M. Shiozawa Y. Sonoda Y. Suzuki A. Takeda Y. Takemoto H. Tanaka T. Yano S. Han T. Kajita K. Okumura T. Tashiro T. Tomiya X. Wang S. Yoshida P. Fernandez L. Labarga N. Ospina B. Zaldivar B. W. Pointon E. Kearns J. L. Raaf L. Wan J. Bian N. J. Griskevich S. Locke M. B. Smy H. W. Sobel V. Takhistov A. Yankelevich J. Hill S. H. Lee D. H. Moon R. G. Park B. Bodur K. Scholberg C. W. Walter A. Beauchêne O. Drapier A. Giampaolo Th. A. Mueller A. D. Santos P. Paganini B. Quilain T. Nakamura J. S. Jang L. N. Machado J. G. Learned K. Choi N. Iovine S. Cao L. H. V. Anthony D. Martin N. W. Prouse M. Scott A. A. Sztuc Y. Uchida V. Berardi M. G. Catanesi E. Radicioni N. F. Calabria A. Langella G. De Rosa G. Collazuol F. Iacob M. Mattiazzi L. Ludovici M. Gonin G. Pronost C. Fujisawa Y. Maekawa Y. Nishimura R. Okazaki R. Akutsu M. Friend T. Hasegawa T. Ishida T. Kobayashi M. Jakkapu T. Matsubara T. Nakadaira K. Nakamura Y. Oyama K. Sakashita T. Sekiguchi T. Tsukamoto N. Bhuiyan G. T. Burton F. Di Lodovico J. Gao A. Goldsack T. Katori J. Migenda R. Ramsden Z. Xie S. Zsoldos A. T. Suzuki Y. Takagi Y. Takeuchi H. Zhong J. Feng L. Feng J. R. Hu Z. Hu M. Kawaue T. Kikawa M. Mori T. Nakaya R. A. Wendell K. Yasutome S. J. Jenkins N. McCauley P. Mehta A. Tarrant Y. Fukuda Y. Itow H. Menjo K. Ninomiya J. Lagoda S. M. Lakshmi M. Mandal P. Mijakowski Y. S. Prabhu J. Zalipska M. Jia J. Jiang C. K. Jung W. Shi M. J. Wilking C. Yanagisawa M. Harada Y. Hino H. Ishino Y. Koshio F. Nakanishi S. Sakai T. Tada T. Tano T. Ishizuka G. Barr D. Barrow L. Cook A. Holin F. Nova S. Samani D. Wark S. Jung B. S. Yang J. Y. Yang J. Yoo J. E. P. Fannon L. Kneale M. Malek J. M. McElwee M. D. Thiesse L. F. Thompson S. T. Wilson H. Okazawa S. B. Kim E. Kwon J. W. Seo I. Yu A. K. Ichikawa K. D. Nakamura S. Tair Department of Physics Boston University Boston Massachusetts 02215 USA Kamioka Observatory Institute for Cosmic Ray Research University of Tokyo Kamioka Gifu 506-1205 Japan Kavli Institute for the Physics and Mathematics of the Universe (WPI) The University of Tokyo Institutes for Advanced Study University of Tokyo Kashiwa Chiba 277-8583 Japan Department of Physics and Astronomy University of California Irvine Irvine California 92697-4575 USA Research Center for Cosmic Neutrinos Institute for Cosmic Ray Research University of Tokyo Kashiwa Chiba 277-8582 Japan ILANCE CNRS—University of Tokyo International Research Laboratory Kashiwa Chiba 277-8582 Japan Department of Theoretical Physics University Autonoma Madrid 28049 Madrid Spain Department of Physics British Columbia Institute of Technology Burnaby British Columbia V5G 3H2 Canada TRIUMF 4004 Wesbrook Mall Vancouver British Columbia V6T2A3 Canada High Energy Accelerator Research Organization (KEK) Tsukuba Ibaraki 305-0801 Japan Department of Physics California State University Dominguez Hills Carson California 90747 USA Institute for Universe and Elementary Particles Chonnam National University Gwangju 61186 Korea Department of Physics Duke University Durham North Carolina 27708 USA Ecole Polytechnique IN2P3-CNRS Laboratoire Leprince-Ringuet F-91120 Palaiseau France Department of Physics Gifu University Gifu Gifu 501-1193 Japan GIST College Gwangju Institute of Science and Technology Gwangju 500-712 Korea School of Physics and Astronomy University of Glasgow Glasgow G12 8QQ United Kingdom Department of Physics and Astronomy University of Hawaii Honolulu Hawaii 96822 USA Center for Underground Physics Institute for Basic Science (IBS) Daejeon 34126 Korea Institute For Interdisciplinary Research in Science and Education ICISE Quy Nhon 55121 Vietnam Department of Physics Imperial College London London SW7 2AZ United Kingdom Dipartimento Interuniversitario di Fisica INFN Sezione di Ba

We present a measurement of neutrino oscillation parameters with the Super-Kamiokande detector using atmospheric neutrinos from the complete pure-water SK I–V (April 1996–July 2020) dataset, including events from an expanded fiducial volume. The dataset corresponds to 6511.3 live days and an exposure of 484.2 kiloton-years. Measurements of the neutrino oscillation parameters Δm322, sin2θ23, sin2θ13, δCP, and the preference for the neutrino mass ordering are presented with atmospheric neutrino data alone, and with constraints on sin2θ13 from reactor neutrino experiments. Our analysis including constraints on sin2θ13 favors the normal mass ordering at the 92.3% level.

关键词： Neutrinos Cherenkov detectors Neutrino detection Particle detectors Particle mixing & oscillations

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