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6,470 results on '"Wada, K."'

1. Development of a data overflow protection system for Super-Kamiokande to maximize data from nearby supernovae

Author: Mori, M., Abe, K., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Jang, M. C., Lee, S. H., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchene, A., Drapier, O., Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Rogly, R., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., Iovine, N., 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., Langella, A., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Perisse, L., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Okazaki, R., Akutsu, R., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Burton, G. T., Edwards, R., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Ramsden, R. M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takagi, Y., Takeuchi, Y., Zhong, H., Bronner, C., Feng, J., Hu, J. R., Hu, Z., Kawaune, M., Kikawa, T., LiCheng, F., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarant, A., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Yoshioka, Y., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Shi, W., Wilking, M. J., Yanagisawa, C., Harada, M., Hino, Y., Ishino, H., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Tada, T., Tano, T., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Jung, S., Yang, B. S., Yang, J. Y., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Thiesse, M. D., Thompson, L. F., Wilson, S., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Eguchi, A., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Watanabe, E., Yokoyama, M., de Perio, P., Fujita, S., Martens, K., Tsui, K. M., Vagins, M. R., Valls, C. J., Xia, J., Kuze, M., Izumiyama, S., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Yoshida, T., Martin, J. F., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., Flaherty, M. O', Richards, B., Ali, A., Jamieson, B., Amanai, S., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics, High Energy Physics - Experiment
Abstract: Neutrinos from very nearby supernovae, such as Betelgeuse, are expected to generate more than ten million events over 10\,s in Super-Kamokande (SK). At such large event rates, the buffers of the SK analog-to-digital conversion board (QBEE) will overflow, causing random loss of data that is critical for understanding the dynamics of the supernova explosion mechanism. In order to solve this problem, two new DAQ modules were developed to aid in the observation of very nearby supernovae. The first of these, the SN module, is designed to save only the number of hit PMTs during a supernova burst and the second, the Veto module, prescales the high rate neutrino events to prevent the QBEE from overflowing based on information from the SN module. In the event of a very nearby supernova, these modules allow SK to reconstruct the time evolution of the neutrino event rate from beginning to end using both QBEE and SN module data. This paper presents the development and testing of these modules together with an analysis of supernova-like data generated with a flashing laser diode. We demonstrate that the Veto module successfully prevents DAQ overflows for Betelgeuse-like supernovae as well as the long-term stability of the new modules. During normal running the Veto module is found to issue DAQ vetos a few times per month resulting in a total dead time less than 1\,ms, and does not influence ordinary operations. Additionally, using simulation data we find that supernovae closer than 800~pc will trigger Veto module resulting in a prescaling of the observed neutrino data., Comment: 28 pages, 18 figures. Submitted to PTEP
Published: 2024
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2. Measurements of the charge ratio and polarization of cosmic-ray muons with the Super-Kamiokande detector

Author: Kitagawa, H., Tada, T., Abe, K., Bronner, C., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Jang, M. C., Lee, S. H., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchêne, A., Drapier, O., Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Rogly, R., Nakamura, T., Jang, J. S., Machado, L. N., Learned, J. G., Choi, K., Iovine, N., Cao, S., Anthony, L. H. V., Martin, D., Prouse, N. W., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Calabria, N. F., Catanesi, M. G., Radicioni, E., Langella, A., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Périssé, L., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Okazaki, R., Akutsu, R., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Ramsden, R. M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takagi, Y., Takeuchi, Y., Zhong, H., Feng, J., Feng, L., Hu, J. R., Hu, Z., Kawaue, M., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarant, A., Wilking, M. J., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Yoshioka, Y., Lagoda, J., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Shi, W., Yanagisawa, C., Harada, M., Hino, Y., Ishino, H., Koshio, Y., Nakanishi, F., Sakai, S., Tano, T., Ishizuka, T., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Jung, S., Yang, B. S., Yang, J. Y., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Thiesse, M. D., Thompson, L. F., Wilson, S. T., Okazawa, H., Lakshmi, S. M., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Eguchi, A., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Watanabe, E., Yokoyama, M., de Perio, P., Fujita, S., Jesús-Valls, C., Martens, K., Tsui, K. M., Vagins, M. R., Xia, J., Izumiyama, S., Kuze, M., Matsumoto, R., Terada, K., Ishitsuka, M., Ito, H., Kinoshita, T., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Yoshida, T., Martin, J. F., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Edwards, R., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Amanai, S., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results of the charge ratio ($R$) and polarization ($P^{\mu}_{0}$) measurements using the decay electron events collected from 2008 September to 2022 June by the Super-Kamiokande detector. Because of its underground location and long operation, we performed high precision measurements by accumulating cosmic-ray muons. We measured the muon charge ratio to be $R=1.32 \pm 0.02$ $(\mathrm{stat.}{+}\mathrm{syst.})$ at $E_{\mu}\cos \theta_{\mathrm{Zenith}}=0.7^{+0.3}_{-0.2}$ $\mathrm{TeV}$, where $E_{\mu}$ is the muon energy and $\theta_{\mathrm{Zenith}}$ is the zenith angle of incoming cosmic-ray muons. This result is consistent with the Honda flux model while this suggests a tension with the $\pi K$ model of $1.9\sigma$. We also measured the muon polarization at the production location to be $P^{\mu}_{0}=0.52 \pm 0.02$ $(\mathrm{stat.}{+}\mathrm{syst.})$ at the muon momentum of $0.9^{+0.6}_{-0.1}$ $\mathrm{TeV}/c$ at the surface of the mountain; this also suggests a tension with the Honda flux model of $1.5\sigma$. This is the most precise measurement ever to experimentally determine the cosmic-ray muon polarization near $1~\mathrm{TeV}/c$. These measurement results are useful to improve the atmospheric neutrino simulations., Comment: 29 pages, 45 figures
Published: 2024

3. Solar neutrino measurements using the full data period of Super-Kamiokande-IV

Author: Collaboration, Super-Kamiokande, Abe, K., Bronner, C., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Imaizumi, S., Iyogi, K., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Kato, Y., Kishimoto, Y., Miki, S., Mine, S., Miura, M., Mochizuki, T., Moriyama, S., Nagao, Y., Nakahata, M., Nakano, Y., Nakayama, S., Noguchi, Y., Okada, T., Okamoto, K., Orii, A., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, R., Wang, X., Yoshida, S., Bravo-Berguno, D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Blaszczyk, F. d. M., Kachulis, C., Kearns, E., Raaf, J. L., Stone, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Weatherly, P., Yankelevich, A., Ganezer, K. S., Hill, J., Jang, M. C., Kim, J. Y., Lee, S., Lim, I. T., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchene, A., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Imber, J., Mueller, Th. A., Paganini, P., Rogly, R., Quilain, B., Santos, A., Nakamura, T., Jang, J. S., Machado, L. N., Learned, J. G., Matsuno, S., Iovine, N., Choi, K., Cao, S., Anthony, L. H. V., Litchfield, R. P., Prouse, N., Marin, D., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Catanesi, M. G., Intonti, R. A., Radicioni, E., Calabria, N. F., De Rosa, G., Langella, A., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Perisse, L., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Okazaki, R., Friend, M., Hasegawa, T., Ishida, T., Jakkapu, M., Kobayashi, T., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Boschi, T., Bhuiyan, N., Burton, G. T., Gao, J., Goldsack, A., Katori, T., Di Lodovico, F., Migenda, J., Sedgwick, S. Molina, Ramsden, R. M., Taani, M., Xie, Z., Zsoldos, S., Abe, KE., Hasegawa, M., Isobe, Y., Kotsar, Y., Miyabe, H., Ozaki, H., Shiozawa, T., Sugimoto, T., Suzuki, A. T., Takagi, Y., Takeuchi, Y., Yamamoto, S., Zhong, H., Ashida, Y., Feng, J., Feng, L., Hayashino, T., Hirota, S., Hu, J. R., Hu, Z., Jiang, M., Kawaue, M., Kikawa, T., Mori, M., Nakamura, KE., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Pritchard, A., Tarrant, A., Wilking, M. J., Fukuda, Y., Itow, Y., Menjo, H., Murase, M., Ninomiya, K., Niwa, T., Tsukada, M., Yoshioka, Y., Frankiewicz, K., Lagoda, J., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jiang, J., Jia, M., Jung, C. K., Palomino, J. L., Santucci, G., Shi, W., Vilela, C., Yanagisawa, C., Fukuda, D., Hagiwara, K., Harada, M., Hino, Y., Horai, T., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Piplani, N., Sakai, S., Sakuda, M., Tada, T., Tano, T., Xu, C., Yamaguchi, R., Ishizuka, T., Kuno, Y., Barr, G., Barrow, D., Cook, L., Samani, S., Simpson, C., Wark, D., Holin, A. M., Nova, F., Jung, S., Yang, B., Yang, J. Y., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Wilson, S. T., Okazawa, H., Lakshmi, S. M., Choi, Y., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Tairahune, S., Nishijima, K., Eguchi, A., Iwamoto, K., Nakagiri, K., Nakajima, Y., Ogawa, N., Shima, S., Watanabe, E., Yokoyama, M., Calland, R. G., Fujita, S., Jesus-Valls, C., Junjie, X., Ming, T. K., de Perio, P., Martens, K., Murdoch, M., Vagins, M. R., Izumiyama, S., Kuze, M., Matsumoto, R., Okajima, Y., Tanaka, M., Yoshida, T., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Ohta, K., Ommura, Y., Shinoki, M., Shigeta, N., Suganuma, T., Yamaguchi, K., Martin, J. F., Nantais, C. M., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Chen, S., Xu, B. D., Zhang, B., Berkman, S., Posiadala-Zezula, M., Boyd, S. B., Edwards, R., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Walker, J., Amanai, S., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Sasaki, R., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment
Abstract: An analysis of solar neutrino data from the fourth phase of Super-Kamiokande~(SK-IV) from October 2008 to May 2018 is performed and the results are presented. The observation time of the data set of SK-IV corresponds to $2970$~days and the total live time for all four phases is $5805$~days. For more precise solar neutrino measurements, several improvements are applied in this analysis: lowering the data acquisition threshold in May 2015, further reduction of the spallation background using neutron clustering events, precise energy reconstruction considering the time variation of the PMT gain. The observed number of solar neutrino events in $3.49$--$19.49$ MeV electron kinetic energy region during SK-IV is $65,443^{+390}_{-388}\,(\mathrm{stat.})\pm 925\,(\mathrm{syst.})$ events. Corresponding $\mathrm{^{8}B}$ solar neutrino flux is $(2.314 \pm 0.014\, \rm{(stat.)} \pm 0.040 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$, assuming a pure electron-neutrino flavor component without neutrino oscillations. The flux combined with all SK phases up to SK-IV is $(2.336 \pm 0.011\, \rm{(stat.)} \pm 0.043 \, \rm{(syst.)}) \times 10^{6}~\mathrm{cm^{-2}\,s^{-1}}$. Based on the neutrino oscillation analysis from all solar experiments, including the SK $5805$~days data set, the best-fit neutrino oscillation parameters are $\rm{sin^{2} \theta_{12,\,solar}} = 0.306 \pm 0.013 $ and $\Delta m^{2}_{21,\,\mathrm{solar}} = (6.10^{+ 0.95}_{-0.81}) \times 10^{-5}~\rm{eV}^{2}$, with a deviation of about 1.5$\sigma$ from the $\Delta m^{2}_{21}$ parameter obtained by KamLAND. The best-fit neutrino oscillation parameters obtained from all solar experiments and KamLAND are $\sin^{2} \theta_{12,\,\mathrm{global}} = 0.307 \pm 0.012 $ and $\Delta m^{2}_{21,\,\mathrm{global}} = (7.50^{+ 0.19}_{-0.18}) \times 10^{-5}~\rm{eV}^{2}$., Comment: 47 pages, 61 figures
Published: 2023
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4. Hydrogen embrittlement susceptibility of additively manufactured 316L stainless steel: influence of post-processing, printing direction, temperature and pre-straining

Author: Álvarez, G., Harris, Z., Wada, K., Rodríguez, C., and Martínez-Pañeda, E.
Subjects: Physics - Chemical Physics
Abstract: The influence of post-build processing on the hydrogen embrittlement behavior of additively manufactured (AM) 316L stainless steel fabricated using laser powder bed fusion was assessed at both room temperature and -50$^\circ$ C via uniaxial tensile experiments. In the absence of hydrogen at ambient temperature, all four evaluated AM conditions (as-built (AB), annealed (ANN), hot isostatic pressed (HIP), and HIP plus cold worked (CW) to 30\%) exhibit notably reduced ductility relative to conventionally manufactured (CM) 316L stainless steel. The AM material exhibits sensitivity to the build direction, both in the presence and absence of hydrogen, with a notable increase in yield strength in the X direction and enhanced ductility in the Z direction. Conversely, testing of non-charged specimens at -50$^\circ$ C revealed similar ductility between the CM, AB, ANN, and HIP conditions. Upon hydrogen charging, the ductility of all four AM conditions was found to be similar to that of CM 316L at ambient temperature, with the HIP condition actually exceeding the CM material. Critically, testing of hydrogen-charged samples at -50$^\circ$ C revealed that the ductility of the HIP AM 316L condition was nearly double that observed in the CM 316L. This improved performance persisted even after cold working, as the CW AM 316L exhibited comparable ductility to CM 316L at -50 C after hydrogen charging, despite having a 2-fold higher yield strength. Feritscope measurements suggest this increased performance is related to the reduced propensity for AM 316L to form strain-induced martensite during deformation, even after significant post-processing treatments. These results demonstrate that AM 316L can be post-processed using typical procedures to exhibit similar to or even improved resistance to hydrogen embrittlement relative to CM 316L.
Published: 2023

5. Laser cooling of positronium

Author: Shu, K., Tajima, Y., Uozumi, R., Miyamoto, N., Shiraishi, S., Kobayashi, T., Ishida, A., Yamada, K., Gladen, R. W., Namba, T., Asai, S., Wada, K., Mochizuki, I., Hyodo, T., Ito, K., Michishio, K., O'Rourke, B. E., Oshima, N., and Yoshioka, K.
Subjects: Physics - Atomic Physics, High Energy Physics - Experiment
Abstract: When laser radiation is skilfully applied, atoms and molecules can be cooled allowing precise measurements and control of quantum systems. This is essential in fundamental studies of physics as well as practical applications such as precision spectroscopy, quantum-statistical-property manifesting ultracold gases, and quantum computing. In laser cooling, repeated cycles of laser photon absorption and direction-independent spontaneous emission can slow atoms and molecules to otherwise unattainable velocities. Simple systems can provide a rigorous testing ground for fundamental theories of physics; one such system is the purely leptonic positronium, an exotic atom of an electron and its antiparticle, the positron. However, the cooling of positronium has hitherto remained unrealised. Here, we demonstrate laser cooling of positronium. A novel laser system of a train of broadband pulses with successively increasing central frequencies was used to overcome major challenges presented by the short lifetime of positronium and the significant Doppler broadening and recoil as a consequence of its very light mass. One-dimensional chirp cooling of the dilute positronium gas in a counter-propagating configuration gave a final velocity distribution corresponding to approximately 1 K in a short time of 100 ns. This study on a pure leptonic system is a major step in the field of low-temperature fundamental physics of antimatter, and is complementary to the laser cooling of antihydrogen, a hadron-containing exotic atom. Progress in this field is vital in elucidating the origin of the matter-antimatter asymmetry in the universe. The application of laser cooling to positronium may afford a unique opportunity to rigorously test bound-state quantum electrodynamics. Moreover, laser cooling of positronium is key to the realisation of Bose-Einstein condensation in this matter-antimatter system.
Published: 2023

6. Search for astrophysical electron antineutrinos in Super-Kamiokande with 0.01wt% gadolinium-loaded water

Author: Harada, M., Abe, K., Bronner, C., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Lee, S. H., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchene, A., Drapier, O., Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., Iovine, N., 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., Langella, A., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Okazaki, R., Akutsu, R., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takagi, Y., Takeuchi, Y., Feng, J., Feng, L., Hu, J. R., Hu, Z., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarrant, A., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Hino, Y., Ishino, H., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Tada, T., Tano, T., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, B. S., Yang, J. Y., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Thiesse, M. D., Thompson, L. F., Wilson, S. T., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Watanabe, E., Yokoyama, M., de Perio, P., Martens, K., Tsui, K. M., Vagins, M. R., Xia, J., Kuze, M., Izumiyama, S., Matsumoto, R., Ishitsuka, M., Ito, H., Kinoshita, T., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Edwards, R., Hadley, D., Nicholson, M., Flaherty, M. O, Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Nuclear Experiment, Physics - Instrumentation and Detectors
Abstract: We report the first search result for the flux of astrophysical electron antineutrinos for energies O(10) MeV in the gadolinium-loaded Super-Kamiokande (SK) detector. In June 2020, gadolinium was introduced to the ultra-pure water of the SK detector in order to detect neutrons more efficiently. In this new experimental phase, SK-Gd, we can search for electron antineutrinos via inverse beta decay with efficient background rejection and higher signal efficiency thanks to the high efficiency of the neutron tagging technique. In this paper, we report the result for the initial stage of SK-Gd with a $22.5\times552$ $\rm kton\cdot day$ exposure at 0.01% Gd mass concentration. No significant excess over the expected background in the observed events is found for the neutrino energies below 31.3 MeV. Thus, the flux upper limits are placed at the 90% confidence level. The limits and sensitivities are already comparable with the previous SK result with pure-water ($22.5 \times 2970 \rm kton\cdot day$) owing to the enhanced neutron tagging.
Published: 2023
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7. Measurement of the cosmogenic neutron yield in Super-Kamiokande with gadolinium loaded water

Author: Collaboration, Super-Kamiokande, Shinoki, M., Abe, K., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Lee, S. H., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchêne, A., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., 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., Langella, A., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Akutsu, R., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Boschi, T., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarrant, A., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, J. Y., Yang, B. S., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Xia, J., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment
Abstract: Cosmic-ray muons that enter the Super-Kamiokande detector cause hadronic showers due to spallation in water, producing neutrons and radioactive isotopes. Those are a major background source for studies of MeV-scale neutrinos and searches for rare events. Since 2020, gadolinium was introduced in the ultra-pure water in the Super-Kamiokande detector to improve the detection efficiency of neutrons. In this study, the cosmogenic neutron yield was measured using data acquired during the period after the gadolinium loading. The yield was found to be $(2.76 \pm 0.02\,\mathrm{(stat.) \pm 0.19\,\mathrm{(syst.)}}) \times 10^{-4}\,\mu^{-1} \mathrm{g^{-1} cm^{2}}$ at 259 GeV of average muon energy at the Super-Kamiokande detector., Comment: 10 pages, 10 figures, 3 tables
Published: 2022

8. Searching for neutrinos from solar flares across solar cycles 23 and 24 with the Super-Kamiokande detector

Author: Okamoto, K., Abe, K., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, Y., Kataoka, Y., Kashiwagi, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nagao, Y., Nakahata, M., Nakano, Y., Nakayama, S., Noguchi, Y., Sato, K., Sekiya, H., Shimizu, K., Shiozawa, M., Shiba, H., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Watanabe, S., Yano, T., Han, S., Kajita, T., Okumura, K., Tashiro, T., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Kim, J. Y., Lee, S. H., Lim, I. T., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchene, A., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., 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., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., 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., Bhuiyan, N., Boschi, T., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Yamamoto, S., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarrant, A., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Vilela, C., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Piplani, N., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, J. Y., Fannon, J. E. P., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Walker, J., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Sasaki, R., Suzuki, S., and Wada, K.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Space Physics
Abstract: Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we searched for neutrino interactions within narrow time windows coincident with $\gamma$-rays and soft X-rays recorded by satellites. In addition, we performed the first attempt to search for solar-flare neutrinos from solar flares on the invisible side of the Sun by using the emission time of coronal mass ejections (CMEs). By selecting twenty powerful solar flares above X5.0 on the visible side and eight CMEs whose emission speed exceeds $2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, we found two (six) neutrino events coincident with solar flares occurring on the visible (invisible) side of the Sun, with a typical background rate of $0.10$ ($0.62$) events per flare in the MeV-GeV energy range. No significant solar-flare neutrino signal above the estimated background rate was observed. As a result we set the following upper limit on neutrino fluence at the Earth $\mathit{\Phi}<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidence level for the largest solar flare. The resulting fluence limits allow us to constrain some of the theoretical models for solar-flare neutrino emission., Comment: 36 pages, 18 figures, 9 tables (Figure 12 was replaced because it was incorrect in version 1.)
Published: 2022

9. Search for Cosmic-ray Boosted Sub-GeV Dark Matter using Recoil Protons at Super-Kamiokande

Author: Collaboration, The Super-Kamiokande, Abe, K., Hayato, Y., Hiraide, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., 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., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., 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., Goldsack, A., Katori, T., Migenda, J., Taani, M., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Nova, F., Yang, J. Y., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Iwamoto, K., Nakagiri, K., Nakajima, Y., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment
Abstract: We report a search for cosmic-ray boosted dark matter with protons using the 0.37 megaton$\times$years data collected at Super-Kamiokande experiment during the 1996-2018 period (SKI-IV phase). We searched for an excess of proton recoils above the atmospheric neutrino background from the vicinity of the Galactic Center. No such excess is observed, and limits are calculated for two reference models of dark matter with either a constant interaction cross-section or through a scalar mediator. This is the first experimental search for boosted dark matter with hadrons using directional information. The results present the most stringent limits on cosmic-ray boosted dark matter and exclude the dark matter-nucleon elastic scattering cross-section between $10^{-33}\text{ cm}^{2}$ and $10^{-27}\text{ cm}^{2}$ for dark matter mass from 10 MeV/$c^2$ to 1 GeV/$c^2$., Comment: With 1-page appendix. A bug was found in July 2023. This version is updated to match the erratum
Published: 2022
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10. Search for proton decay via $p\rightarrow \mu^+K^0$ in 0.37 megaton-years exposure of Super-Kamiokande

Author: Collaboration, Super-Kamiokande, Matsumoto, R., Abe, K., Hayato, Y., Hiraide, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., 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., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Kim, J. Y., Lim, I. T., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., 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., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., 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., Goldsack, A., Katori, T., Migenda, J., Taani, M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Yamamoto, S., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tsui, K. M., Tarrant, A., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jiang, M. Jia J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, J. Y., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment
Abstract: We searched for proton decay via $p\to\mu^+K^0$ in 0.37\,Mton$\cdot$years of data collected between 1996 and 2018 from the Super-Kamiokande water Cherenkov experiment. The selection criteria were defined separately for $K^0_S$ and $K^0_L$ channels. No significant event excess has been observed. As a result of this analysis, which extends the previous search by an additional 0.2\,Mton$\cdot$years of exposure and uses an improved event reconstruction, we set a lower limit of $3.6\times10^{33}$ years on the proton lifetime., Comment: 13 pages, 11 figures
Published: 2022

11. Effect of projectile shape and interior structure on crater size in strength regime

Author: Kadono, T., Arakawa, M., Tsujido, S., Yasui, M., Hasegawa, S., Kurosawa, K., Shirai, K., Okamoto, C., Ogawa, K., Iijima, Y., Shimaki, Y., and Wada, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Geophysics
Abstract: Experiments on crater formation in the strength regime were conducted using projectiles of various shapes with an aspect ratio of ~1, including both solid and hollow interiors. The surface diameter, inner (pit) diameter, and depth of the craters on basalt and porous gypsum targets were measured. Using the bulk density of the projectile, the surface diameter and depth for basalt and the pit diameter and depth for porous gypsum were scaled using the pi-scaling law for crater formation in the strength regime. The numerical code iSALE was used to simulate the impact of projectiles of various shapes and interior structure with similar bulk densities. Results show that the distributions of the maximum (peak) pressure experienced and particle velocity in the targets were similar regardless of projectile shape and interior structure, implying that the dimensions of the final craters were almost identical. This is consistent with the experimental results. Thus, we conclude that the size of the craters formed by the impact of projectiles with different shape and interior structure can be scaled using a conventional scaling law in the strength regime, using bulk density as projectile density., Comment: 38 pages, 9 figures, 4 tables, 1 supporting information, accepted for publication in Earth, Planets and Space
Published: 2022
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12. Three-dimensional constraint-based void-growth model for high temperature hydrogen attack

Author: Vijayvargia, K., Dadfarnia, M., Sofronis, P., Kubota, M., Staykov, A., Wada, K., Pugh, J. A., and Eason, T. J.
Published: 2023
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13. Search for supernova bursts in Super-Kamiokande IV

Author: collaboration, The Super-Kamiokande, Mori, M., Abe, K., Hayato, Y., Hiraide, K., Ieki, K., Ikeda, M., Imaizumi, S., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nagao, Y., Nakahata, M., Nakano, Y., Nakayama, S., Noguchi, Y., Okada, T., Okamoto, K., Orii, A., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., Shiozawa, M., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Tomiya, T., Watanabe, S., Yano, T., Yoshida, S., Han, S., Kajita, T., Okumura, K., Tashiro, T., Wang, X., Xia, J., Megias, G. D., Bravo-Berguno, D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Zsoldos, S., Pointon, B. W., Blaszczyk, F. d. M., Kearns, E., Raaf, J. L., Stone, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, Hill, J., Kim, J. Y., Lim, I. T., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Paganini, P., Quilain, B., Santos, A. D., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., 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., Ludovici, L., Gonin, M., Pronost, G., Maekawa, Y., Nishimura, Y., Fujisawa, C., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Ozaki, H., Shiozawa, T., Suzuki, A. T., Takeuchi, Y., Yamamoto, S., Kotsar, Y., Ashida, Y., Bronner, C., Feng, J., Hirota, S., Kikawa, T., Nakaya, T., Wendell, R. A., Yasutome, K., McCauley, N., Mehta, P., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Niwa, T., Tsukada, M., Lagoda, J., Lakshmi, S. M., Mijakowski, P., Zalipska, J., Mandal, M., Prabhu, Y. S., Jiang, J., Jung, C. K., Vilela, C., Wilking, M. J., Yanagisawa, C., Jia, M., Hagiwara, K., Harada, M., Horai, T., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Piplani, N., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Nova, F., Boschi, T., Gao, J., Goldsack, A., Katori, T., Di Lodovico, F., Migenda, J., Taani, M., Yang, J. Y., Jenkins, S. J., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Seo, J. W., Yu, I., Nishijima, K., Koshiba, M., Nakagiri, K., Nakajima, Y., Iwamoto, K., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Yoshida, T., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ohta, K., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Hadley, D., Nicholson, M., Flaherty, M. O', Richards, B., Ali, A., Jamieson, B., Walker, J., Marti, Ll., Minamino, A., Pintaudi, G., Sasaki, R., Sano, S., Suzuki, S., Wada, K., Cao, S., Ichikawa, A., Nakamura, K. D., and Tairafun, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: Super-Kamiokande has been searching for neutrino bursts characteristic of core-collapse supernovae continuously, in real time, since the start of operations in 1996. The present work focuses on detecting more distant supernovae whose event rate may be too small to trigger in real time, but may be identified using an offline approach. The analysis of data collected from 2008 to 2018 found no evidence of distant supernovae bursts. This establishes an upper limit of 0.29 year$^{-1}$ on the rate of core-collapse supernovae out to 100 kpc at 90% C.L.. For supernovae that fail to explode and collapse directly to black holes the limit reaches to 300 kpc.
Published: 2022
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14. Pre-Supernova Alert System for Super-Kamiokande

Author: Collaboration, Super-Kamiokande, Machado, L. N., Abe, K., Hayato, Y., Hiraide, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., Shiozawa, M., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Watanabe, S., Yano, T., de Perio, P., Martens, K., Vagins, M. R., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Han, S., Kajita, T., Okumura, K., Tashiro, T., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Akutsu, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Prouse, N. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Hill, J., Kim, J. Y., Lim, I. T., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Cao, S., Choi, K., Anthony, L. H. V., Martin, D., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Catanesi, M. G., Radicioni, E., Calabria, N. F., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Sasaki, R., Friend, M., Hasegawa, T., Ishida, T., Jakkapu, M., Kobayashi, T., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Boschi, T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Yaamoto, S., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Nova, F., Yang, J. Y., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Iwamoto, K., Nakagiri, K., Nakajima, Y., Taniuchi, N., Yokoyama, M., Izumiyama, S., Kuze, M., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yonenaga, M., Martin, J. F., Tanaka, H. A., Towstego, T., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.
Subjects: High Energy Physics - Experiment, Astrophysics - High Energy Astrophysical Phenomena, Physics - Instrumentation and Detectors
Abstract: In 2020, the Super-Kamiokande (SK) experiment moved to a new stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate was added to the water in the detector, enhancing the efficiency to detect thermal neutrons and consequently improving the sensitivity to low energy electron anti-neutrinos from inverse beta decay (IBD) interactions. SK-Gd has the potential to provide early alerts of incipient core-collapse supernovae through detection of electron anti-neutrinos from thermal and nuclear processes responsible for the cooling of massive stars before the gravitational collapse of their cores. These pre-supernova neutrinos emitted during the silicon burning phase can exceed the energy threshold for IBD reactions. We present the sensitivity of SK-Gd to pre-supernova stars and the techniques used for the development of a pre-supernova alarm based on the detection of these neutrinos in SK, as well as prospects for future SK-Gd phases with higher concentrations of Gd. For the current SK-Gd phase, high-confidence alerts for Betelgeuse could be issued up to nine hours in advance of the core-collapse itself., Comment: 20 pages
Published: 2022
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15. Testing Non-Standard Interactions Between Solar Neutrinos and Quarks with Super-Kamiokande

Author: Collaboration, Super-Kamiokande, Weatherly, P., Abe, K., Bronner, C., Hayato, Y., Hiraide, K., Ikeda, M., Iyogi, K., Kameda, J., Kanemura, Y., Kataoka, Y., Kato, Y., Kishimoto, Y., Miki, S., Miura, M., Moriyama, S., Mochizuki, T., Nakahata, M., Nakano, Y., Nakayama, S., Okada, T., Okamoto, K., Orii, A., Pronost, G., Sato, K., Sekiya, H., Shiozawa, M., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Tasaka, S., Wang, X., Watanabe, S., Yano, T., Han, S., Kajita, T., Kaneyuki, K., Okumura, K., Tashiro, T., Wang, R., Xia, J., Megias, G. D., Labarga, L., Zaldivar, B., Pointon, B. W., Blaszczyk, F. d. M., Kachulis, C., Kearns, E., Raaf, J. L., Stone, J. L., Sulak, L. R., Sussman, S., Wan, L., Wester, T., Berkman, S., Tobayama, S., Bian, J., Elnimr, M., Griskevich, N. J., Kropp, W. R., Locke, S., Mine, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Ganezer, K. S., Hill, J., Kim, J. Y., Lim, I. T., Park, R. G., Bodur, B., Li, Z., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Giampaolo, A., Hedri, S. El, Imber, J., Mueller, Th. A., Paganini, P., Quilain, B., Santos, A. D., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Matsuno, S., Cao, S., Amey, J., Anthony, L. H. V., Litchfield, R. P., Ma, W. Y., Martin, D., Scott, M., Sztuc, A. A., Uchida, Y., Wascko, M. O., Berardi, V., Catanesi, M. G., Intonti, R. A., Radicioni, E., Calabria, N. F., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ospina, N., Ludovici, L., Gonin, M., Maekawa, Y., Nishimura, Y., Friend, M., Hasegawa, T., Ishida, T., Jakkapu, M., Kobayashi, T., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Boschi, T., Di Lodovico, F., Gao, J., Katori, T., Migenda, J., Taani, M., Zsoldos, S., Abe, KE., Hasegawa, M., Isobe, Y., Kotsar, Y., Miyabe, H., Ozaki, H., Sugimoto, T., Suzuki, A. T., Takeuchi, Y., Yamamoto, S., Ashida, Y., Feng, J., Hayashino, T., Hirota, S., Jiang, M., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Fernandez, P., McCauley, N., Mehta, P., Pritchard, A., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Murase, M., Frankiewicz, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Li, X., Palomino, J. L., Santucci, G., Vilela, C., Wilking, M. J., Yanagisawa, C., Fukuda, D., Hagiwara, K., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Sakai, S., Sakuda, M., Takahira, Y., Xu, C., Kuno, Y., Barr, G., Barrow, D., Cook, L., Goldsack, A., Samani, S., Simpson, C., Wark, D., Sedgwick, S. Molina, Tacik, R., Nova, F., Yang, J. Y., Jenkins, S. J., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Choi, Y., Kim, S. B., Seo, J. W., Yu, I., Ichikawa, A., Nakamura, K. D., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Suda, Y., Taniuchi, N., Yokoyama, M., Martens, K., Murdoch, M., Vagins, M. R., Hamabe, D., Izumiyama, S., Kuze, M., Okajima, Y., Yoshida, T., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Shinoki, M., Suganuma, T., Yonenaga, M., Martin, J. F., Nantais, C. M., Tanaka, H. A., Towstego, T., Akutsu, R., de Perio, P., Gousy-Leblanc, V., Hartz, M., Konaka, A., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Giorgio, P., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Sasaki, R., and Wada, K.
Subjects: High Energy Physics - Experiment, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Non-Standard Interactions (NSI) between neutrinos and matter affect the neutrino flavor oscillations. Due to the high matter density in the core of the Sun, solar neutrinos are suited to probe these interactions. Using the $277$ kton-yr exposure of Super-Kamiokande to $^{8}$B solar neutrinos, we search for the presence of NSI. Our data favors the presence of NSI with down quarks at 1.8$\sigma$, and with up quarks at 1.6$\sigma$, with the best fit NSI parameters being ($\epsilon_{11}^{d},\epsilon_{12}^{d}$) = (-3.3, -3.1) for $d$-quarks and ($\epsilon_{11}^{u},\epsilon_{12}^{u}$) = (-2.5, -3.1) for $u$-quarks. After combining with data from the Sudbury Neutrino Observatory and Borexino, the significance increases by 0.1$\sigma$., Comment: Author: Pierce Weatherly 25 pages. To be submitted to Physical Review D
Published: 2022

16. Asynchronous Gathering Algorithms for Autonomous Mobile Robots with Lights

Author: Nakai, R., Sudo, Y., and Wada, K.
Subjects: Computer Science - Distributed, Parallel, and Cluster Computing
Abstract: We consider a Gathering problem for n autonomous mobile robots with persistent memory called light in an asynchronous scheduler (ASYNC). It is well known that Gathering is impossible when robots have no lights in basic common models, if the system is semi-synchronous (SSYNC) or even centralized (only one robot is active in each time). It is known that Gathering can be solved by robots with 10 colors of lights in ASYNC. This result is obtained by combining the following results. (1) The simulation of SSYNC robots with k colors by ASYNC robots with 5k colors, and (2) Gathering is solved by SSYNC robots with 2 colors. In this paper, we improve the result by reducing the number of colors and show that Gathering can be solved by ASYNC robots with 3 colors of lights. We also show that we can construct a simulation algorithm of any unfair SSYNC algorithm using k colors by ASYNC robots with 3k colors, where unfairness does not guarantee that every robot is activated infinitely often. Combining this simulation and the Gathering algorithm by SSYNC robots with 2 colors, we obtain a Gathering algorithm by ASYNC robots with 6 colors. Our main result can be obtained by reducing the number of colors from 6 to 3.
Published: 2021

17. The Galaxy Activity, Torus and Outflow Survey (GATOS): II. Torus and polar dust emission in nearby Seyfert galaxies

Author: Alonso-Herrero, A., García-Burillo, S., Hoenig, S. F., García-Bernete, I., Almeida, C. Ramos, González-Martín, O., López-Rodríguez, E., Boorman, P. G., Bunker, A. J., Burtscher, L., Combes, F., Davies, R., Díaz-Santos, T., Gandhi, P., García-Lorenzo, B., Hicks, E. K. S., Hunt, L. K., Ichikawa, K., Imanishi, M., Izumi, T., Labiano, A., Levenson, N. A., Packham, C., Pereira-Santaella, M., Ricci, C., Rigopoulou, D., Roche, P., Rosario, D. J., Rouan, D., Shimizu, T., Stalevski, M., Wada, K., and Williamson, D.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We compare mid-IR and ALMA far-IR images of 12 nearby Seyferts selected from GATOS. The mid-IR unresolved emission contributes more than 60% of the nuclear emission in most galaxies. By contrast, the ALMA 870micron continuum emission is mostly resolved and typically along the torus equatorial direction (Paper I, Garcia-Burillo et al. 2021). The Eddington ratios and nuclear hydrogen column densities NH of half the sample are favorable to launching polar and/or equatorial dusty winds, according to simulations. Six show mid-IR extended emission in the polar direction as traced by the NLR and perpendicular to the ALMA emission. In a few, the nuclear NH might be too high to uplift large quantities of dusty material along the polar direction. Five galaxies have low NH and/or Eddington ratios and thus polar dusty winds are not likely. We generate new CAT3D-WIND disk-wind model images. At low wind-to-disk cloud ratios the far-IR model images have disk- and ring-like morphologies. The X-shape associated with dusty winds is seen better in the far-IR at intermediate-high inclinations for the extended-wind configurations. In most models, the mid-IR emission comes from the inner part of the disk/cone. Extended bi-conical and one-sided polar mid-IR emission is seen in extended-wind configurations and high wind-to-disk cloud ratios. When convolved to our resolution, the model images reproduce qualitative aspects of the observed morphologies. Low-intermediate wind-to-disk ratios are required to account for the large fractions of unresolved mid-IR emission. This work and Paper I provide observational support for the torus+wind scenario. The wind component is more relevant at high Eddington ratios and/or AGN luminosities, and polar dust emission is predicted at NH of up to $10^{24}$cm$^{-2}$. The torus/disk component, on the other hand, prevails at low luminosities and/or Eddington ratios. (Abridged), Comment: 27 pages, 27 figures. Accepted for publication in A&A
Published: 2021
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18. Publisher Correction: Granular flow experiment using artificial gravity generator at International Space Station

Author: Ozaki, S., Ishigami, G., Otsuki, M., Miyamoto, H., Wada, K., Watanabe, Y., Nishino, T., Kojima, H., Soda, K., Nakao, Y., Sutoh, M., Maeda, T., and Kobayashi, T.
Published: 2023
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19. Granular flow experiment using artificial gravity generator at International Space Station

Author: Ozaki, S., Ishigami, G., Otsuki, M., Miyamoto, H., Wada, K., Watanabe, Y., Nishino, T., Kojima, H., Soda, K., Nakao, Y., Sutoh, M., Maeda, T., and Kobayashi, T.
Published: 2023
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20. The Galaxy Activity, Torus and Outflow Survey (GATOS) I. ALMA images of dusty molecular tori in Seyfert galaxies

Author: García-Burillo, S., Alonso-Herrero, A., Almeida, C. Ramos, González-Martín, O., Combes, F., Usero, A., Hönig, S., Querejeta, M., Hicks, E. K. S., Hunt, L. K., Rosario, D., Davies, R., Boorman, P. G., Bunker, A. J., Burtscher, L., Colina, L., Díaz-Santos, T., Gandhi, P., García-Bernete, I., García-Lorenzo, B., Ichikawa, K., Imanishi, M., Izumi, T., Labiano, A., Levenson, N. A., López-Rodríguez, E., Packham, C., Pereira-Santaella, M., Ricci, C., Rigopoulou, D., Rouan, D., Shimizu, T., Stalevski, M., Wada, K., and Williamson, D.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present the first results of the Galaxy Activity, Torus and Outflow Survey (GATOS), a project aimed at understanding the properties of the dusty molecular tori and their connection to the host galaxy in nearby Seyfert galaxies. Our project expands the range of AGN luminosities and Eddington ratios covered by previous surveys of Seyferts conducted by ALMA and allows us to study the gas feeding and feedback cycle in a combined sample of 19 Seyferts. We used ALMA to obtain new images of the emission of molecular gas and dust using the CO(3-2) and HCO+(4-3) lines as well as their underlying continuum emission at 870 microns with high spatial resolutions (0.1'' ~ 7 - 13 pc) in the CND of 10 nearby (D < 28 Mpc) Seyfert galaxies. Our new ALMA observations detect 870 micron continuum and CO line emission from spatially resolved disks located around the AGN in all the sources. The bulk of the continuum flux can be accounted for by thermal emission from dust in the majority of the targets. For most of the sources the disks show a preponderant orientation perpendicular to the AGN wind axes, as expected for dusty molecular tori. The median diameters and molecular gas masses of the tori are ~ 42 pc, and ~ 6 x 10**5 Msun, respectively. We find a positive correlation between the line-of-sight gas column densities responsible for the absorption of X-rays and the molecular gas column densities derived from CO towards the AGN in our sources. The radial distributions of molecular gas in the CND of our combined sample show signs of nuclear-scale molecular gas deficits. We also detect molecular outflows in the sources that show the most extreme nuclear-scale gas deficits in our sample. These observations find for the first time supporting evidence that the imprint of AGN feedback is more extreme in higher luminosity and/or higher Eddington ratio Seyfert galaxies., Comment: 41 pages, new version revised and accepted by A&A on the 22nd of June 2021
Published: 2021
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21. Associations Between Adult Attention-Deficit/Hyperactivity Disorder (ADHD) Traits and Sociodemographic Characteristics in Japanese Workers

Author: Suzuki T, Wada K, Nakazato M, Ohtani T, Yamazaki M, and Ikeda S
Subjects: adhd traits, eating habits, income, lifestyle habits, sleep, socioeconomic status., Neurosciences. Biological psychiatry. Neuropsychiatry, RC321-571, Neurology. Diseases of the nervous system, RC346-429
Abstract: Tomoko Suzuki,1 Koji Wada,1,2 Michiko Nakazato,3 Toshiyuki Ohtani,4 Michiko Yamazaki,2 Shunya Ikeda1,2 1Department of Public Health, School of Medicine, International University of Health and Welfare, Narita, Japan; 2Department of Social Medical Sciences, Graduate School of Medicine, International University of Health and Welfare, Tokyo, Japan; 3Department of Psychiatry, School of Medicine, International University of Health and Welfare, Narita, Japan; 4Safety and Health Organization, Chiba University, Chiba, JapanCorrespondence: Tomoko Suzuki, Department of Public Health, School of Medicine, International University of Health and Welfare, 4-3 Kozunomori, Narita, Chiba, 286-8686, Japan, Tel +81-476-20-7701, Fax +81-476- 28-1188, Email tsuzuki7@iuhw.ac.jp; tsuzuki2992@gmail.comPurpose: Most previous studies that described associations between adult attention-deficit/hyperactivity disorder (ADHD) and sociodemographic characteristics were focused on individuals diagnosed with ADHD, and few studies investigated ADHD traits in the general population. Additionally, some workers, who experienced no problems while at university and successfully graduated from university, developed ADHD traits after finding employment. This study described associations between ADHD traits and sociodemographic characteristics among Japanese workers who were university graduates.Patients and Methods: Participants were randomly selected workers (n=1240) from across Japan who completed a self-administered online survey. ADHD traits were measured using an adult ADHD Self-report Scale, with scoring rules applied to reflect the Diagnostic and Statistical Manual of Mental Disorders, Fifth Edition criteria. Information was collected on sociodemographic characteristics including sex, age, socioeconomic status, working time, and health-related behaviors. We performed partial correlation analysis to estimate trend associations and used analysis of covariance to compare adjusted averages. This model was adjusted for all variables.Results: Males had higher levels of ADHD traits than females (p = 0.001), and younger age was associated with higher levels of ADHD traits (p < 0.001). Workers with low incomes had higher levels of ADHD traits than workers with high incomes (p = 0.009). More frequent consumption of midnight meals was associated with higher levels of ADHD traits (p < 0.001), although there were no differences for breakfast, lunch, and dinner. Those who did not get enough rest from sleep had higher levels of ADHD traits (p = 0.007).Conclusion: Results for high levels of ADHD traits among workers were consistent with previous studies for adults diagnosed with ADHD, even though all participants had successfully graduated from university. Assessment of these ADHD traits may support prevention of health deterioration related to these ADHD traits.Keywords: ADHD traits, eating habits, income, lifestyle habits, sleep, socioeconomic status
Published: 2023

22. ALMA resolves the remarkable molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377

Author: Aalto, S., Falstad, N., Muller, S., Wada, K., Gallagher, J. S., König, S., Sakamoto, K., Vlemmings, W., Ceccobello, C., Dasyra, K., Combes, F., García-Burillo, S., Oya, Y., Martín, S., van der Werf, P., Evans, A. S., and Kotilainen, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Submillimetre and millimetre observations are important in probing the properties of the molecular gas and dust around obscured active galactic nuclei (AGNs) and their feedback. With very high-resolution (0."02x0."03 (2x3 pc)) ALMA 345 GHz observations of CO 3-2, HCO$^+$ 4-3, HCN 4-3 $\nu_2$=1$f$, and continuum we have studied the molecular outflow and nucleus of the extremely radio-quiet lenticular galaxy NGC1377. The outflow is resolved, revealing a 150 pc long, clumpy, high-velocity, collimated molecular jet. The molecular emission is emerging from the spine of the jet with an average diameter of 3-7 pc. A narrow-angle, rotating molecular wind surrounds the jet and is enveloped by a larger-scale, slower CO-emitting structure. The jet and narrow wind are turbulent ($\sigma>$40 kms$^{-1}$) and have steep radial gas excitation gradients. The jet shows velocity reversals that we propose are caused by precession, or episodic directional changes. We suggest that an important process powering the outflow is magneto-centrifugal driving. In contrast, the large-scale CO-envelope may be a slow wind, or cocoon that stems from jet-wind interactions. An asymmetric, nuclear r$\sim$2 pc and hot (>180 K) dust structure with a high molecular column density, N(H$_2$)$\sim1.8 \times 10^{24}$ cm$^{-2}$, is detected in continuum and vibrationally excited HCN. Its luminosity is likely powered by a buried AGN. The mass of the supermassive black hole (SMBH) is estimated to $\sim9\times10^6$ M$_\odot$ and the SMBH of NGC1377 appears to be at the end of an intense phase of accretion. The nuclear growth may be fuelled by low-angular momentum gas inflowing from gas ejected in the molecular jet and wind. Such a feedback-loop of cyclic accretion and outflows would be an effective process in growing the nuclear SMBH. This result invites new questions as to SMBH growth processes in obscured, dusty galaxies., Comment: 16 pages, 12 figures, accepted for publication in Astronomy and Astrophysics. Updated affiliations, added reference
Published: 2020
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23. Association Between Oral Health and Swallowing Function in the Elderly

Author: Yamano T, Nishi K, Omori F, Wada K, and Naito T
Subjects: dysphagia, oral health assessment tool, video endoscopy, video fluorography, Geriatrics, RC952-954.6
Abstract: Takafumi Yamano,1 Kensuke Nishi,1 Fumitaka Omori,2 Kaori Wada,2 Toru Naito3 1Section of Otorhinolaryngology, Department of Medicine, Fukuoka Dental College, Fukuoka, 814-0193, Japan; 2Department of Otorhinolaryngology, Fukuoka Dental College Hospital, Fukuoka, 814-0193, Japan; 3Section of Gerodontology, Department of General Dentistry Fukuoka Dental College, Fukuoka, 814-0193, JapanCorrespondence: Takafumi Yamano, Section of Otorhinolaryngology, Department of Medicine, Fukuoka Dental College, 2-15-1 Tamura,Sawara-ku, Fukuoka, 814-0193, Japan, Fax +81 928013678, Email yamano@fdcnet.ac.jpObjective: Although the oral environment significantly affects the risk of pneumonia, there have been few studies regarding its relation with swallowing. There is no doubt that there is a significant link between the oral environment and the development of pneumonia; however, there have been few comparative studies of swallowing using video endoscopy (VE) and video fluorography (VF) as indicators to determine the actual availability of oral intake and the choice of food form. This study was performed to examine whether the oral environment or swallowing function contributes more to the development of pneumonia in the elderly.Methods: The study population consisted of 24 patients (7 men and 17 women; age range: 64– 97 years; average age: 86 years) assessed using the Oral Health Assessment Tool (OHAT), VE and VF at Fukuoka Dental College Hospital. The most common disease was pneumonia (17 patients), followed by cerebral infarction (5 patients), pyelonephritis (4 patients), bronchitis (2 patients), Parkinson’s disease (2 patients), scleroderma (1 patient), diabetes (1 patient), eosophageal cancer (1 patient) and Parkinson’s syndrome> (1 patient). Some patients had multiple diseases. Oral intake was possible in 20 patients (80%), whereas tube feeding and gastric banding were required in 4 patients.Results: The OHAT score was not correlated with either the VE or VF score. Furthermore, the OHAT score was not significantly different between the multiple- and no/single-pneumonia episode groups. The group with multiple episodes of pneumonia had lower VE and VF scores than those with no or only a single episode of pneumonia.Conclusion: Oral assessment, VE and VF are necessary to evaluate swallowing in patients with suspected dysphagia. Swallowing function, especially as assessed by VE and VF, is more important than examination of the oral environment for evaluating risk of recurrent aspiration pneumonia in the elderly. In addition, multiple factors contribute to recurrent pneumonia in patients with a good oral environment, including subclinical aspiration, pharyngeal clearance and delayed activation of the gag reflex.Keywords: dysphagia, Oral Health Assessment Tool, video endoscopy, video fluorography
Published: 2023

24. Hydrogen-induced intergranular cracking of pure nickel under various strain rates and temperatures in gaseous hydrogen environment

Author: Wada, K., Shibata, C., Enoki, H., Iijima, T., and Yamabe, J.
Published: 2023
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25. Effect of the duration of previous osteoporosis treatment on the effect of romosozumab treatment

Author: Tominaga, A., Wada, K., Okazaki, K., Nishi, H., Terayama, Y., Kodama, Y., and Kato, Y.
Published: 2022
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26. An Online Survey About Electroconvulsive Therapy in Japan During the COVID-19 Pandemic: Comparison of Early and Recent Stages

Author: Hirata R, Kawashima H, Tsuboi T, Wada K, Takebayashi M, and Suwa T
Subjects: electroconvulsive therapy, coronavirus disease 2019, pandemic, personal protective equipment, clinical decision-making, Neurosciences. Biological psychiatry. Neuropsychiatry, RC321-571, Neurology. Diseases of the nervous system, RC346-429
Abstract: Risa Hirata,1 Hirotsugu Kawashima,1,5 Takashi Tsuboi,2,5 Ken Wada,3,5 Minoru Takebayashi,4,5 Taro Suwa1,5 1Department of Psychiatry, Kyoto University Hospital, Kyoto, Japan; 2Department of Neuropsychiatry, Kyorin University School of Medicine, Tokyo, Japan; 3Department of Psychiatry, Hiroshima Citizens Hospital, Hiroshima City Hospital Organization, Hiroshima, Japan; 4Department of Neuropsychiatry, Faculty of Life Sciences, Kumamoto University, Kumamoto, Japan; 5ECT Committee, Japanese Society of General Hospital Psychiatry (JSGHP), Tokyo, JapanCorrespondence: Taro Suwa, Department of Psychiatry, Kyoto University Hospital, 54, Shogoin Kawahara-cho, Sakyo-ku, Kyoto-shi, Kyoto, Japan, Tel +81-75-751-3386, Fax +81-75-751-3246, Email tarosuwa@kuhp.kyoto-u.ac.jpPurpose: To provide an overview of how electroconvulsive therapy (ECT) practice in Japan has changed as the coronavirus disease 2019 (COVID-19) pandemic continues.Patients and Methods: We surveyed healthcare institutions, primarily university and general hospitals, regarding changes in the number of patients undergoing ECT and infection control measures in the early (August 2020) and recent (August 2021) stages of the COVID-19 pandemic. Data for the early and recent stages were also compared between urban and non-urban areas.Results: Among 32 facilities, the number of patients undergoing ECT decreased in 11 facilities (34.4%) from April 2020 to March 2021 compared with the previous year, whereas the number increased in 12 (37.5%) from April to June 2021 compared with the previous year. As of August 2021, some facilities had ongoing restrictions. Compared with non-urban facilities, the number of patients undergoing ECT decreased more in urban facilities, which also had more ECT restrictions. Maintenance ECT was used at the same rate as before the pandemic for 23 (82.1%) of 28 institutions. Regarding infection control measures, many facilities considered polymerase chain reaction testing before ECT and required all staff to wear surgical masks and eye shields during ECT.Conclusion: The COVID-19 pandemic in Japan greatly affected the use of ECT in 2020; however, by the summer of 2021, infection control measures were relatively well established, the number of ECT cases stabilized and increased, and the decision to use ECT was again possible.Keywords: electroconvulsive therapy, coronavirus disease 2019, pandemic, personal protective equipment, clinical decision making
Published: 2022

27. Particle size distributions inside and around the artificial crater produced by the Hayabusa2 impact experiment on Ryugu

Author: Ogawa, K., Sakatani, N., Kadono, T., Arakawa, M., Honda, R., Wada, K., Shirai, K., Shimaki, Y., Ishibashi, K., Yokota, Y., Saiki, T., Imamura, H., Tsuda, Y., Nakazawa, S., Takagi, Y., Hayakawa, M., Yano, H., Okamoto, C., Iijima, Y., Morota, T., Kameda, S., Tatsumi, E., Cho, Y., Yoshioka, K., Sawada, H., Matsuoka, M., Yamada, M., Kouyama, T., Suzuki, H., Honda, C., and Sugita, S.
Published: 2022
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28. High power experiment and heat load evaluation of transmission line for the ECH/CD system in JT-60SA

Author: Kobayashi, T., Yamazaki, H., Hiranai, S., Sawahata, M., Terakado, M., Ishita, K., Hinata, J., Sato, F., Wada, K., Ikeda, R., Shinya, T., Yajima, S., Kajiwara, K., Takahashi, K., and Moriyama, S.
Published: 2022
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29. The life cycle of starbursting circumnuclear gas discs

Author: Schartmann, M., Mould, J., Wada, K., Burkert, A., Durré, M., Behrendt, M., Davies, R. I., and Burtscher, L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: High-resolution observations from the sub-mm to the optical wavelength regime resolve the central few 100pc region of nearby galaxies in great detail. They reveal a large diversity of features: thick gas and stellar discs, nuclear starbursts, in- and outflows, central activity, jet interaction, etc. Concentrating on the role circumnuclear discs play in the life cycles of galactic nuclei, we employ 3D adaptive mesh refinement hydrodynamical simulations with the RAMSES code to self-consistently trace the evolution from a quasi-stable gas disc, undergoing gravitational (Toomre) instability, the formation of clumps and stars and the disc's subsequent, partial dispersal via stellar feedback. Our approach builds upon the observational finding that many nearby Seyfert galaxies have undergone intense nuclear starbursts in their recent past and in many nearby sources star formation is concentrated in a handful of clumps on a few 100pc distant from the galactic centre. We show that such observations can be understood as the result of gravitational instabilities in dense circumnuclear discs. By comparing these simulations to available integral field unit observations of a sample of nearby galactic nuclei, we find consistent gas and stellar masses, kinematics, star formation and outflow properties. Important ingredients in the simulations are the self-consistent treatment of star formation and the dynamical evolution of the stellar distribution as well as the modelling of a delay time distribution for the supernova feedback. The knowledge of the resulting simulated density structure and kinematics on pc scale is vital for understanding inflow and feedback processes towards galactic scales., Comment: accepted by MNRAS
Published: 2017
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30. On the disappearance of a cold molecular torus around the low-luminosity active galactic nucleus of NGC 1097

Author: Izumi, T., Kohno, K., Fathi, K., Hatziminaoglou, E., Davies, R. I., Martín, S., Matsushita, S., Schinnerer, E., Espada, D., Aalto, S., Onishi, K., Turner, J. L., Imanishi, M., Nakanishi, K., Meier, D. S., Wada, K., Kawakatu, N., and Nakajima, T.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We used the Atacama Large Millimeter/submillimeter Array (ALMA) to map the CO(3-2) and the underlying continuum emissions around the type 1 low-luminosity active galactic nucleus (LLAGN; bolometric luminosity $\lesssim 10^{42}$ erg~s$^{-1}$) of NGC 1097 at $\sim 10$ pc resolution. These observations revealed a detailed cold gas distribution within a $\sim 100$ pc of this LLAGN. In contrast to the luminous Seyfert galaxy NGC 1068, where a $\sim 7$ pc cold molecular torus was recently revealed, a distinctively dense and compact torus is missing in our CO(3-2) integrated intensity map of NGC 1097. Based on the CO(3-2) flux, the gas mass of the torus of NGC 1097 would be a factor of $\gtrsim 2-3$ less than that found for NGC 1068 by using the same CO-to-H$_2$ conversion factor, which implies less active nuclear star formation and/or inflows in NGC 1097. Our dynamical modeling of the CO(3-2) velocity field implies that the cold molecular gas is concentrated in a thin layer as compared to the hot gas traced by the 2.12 $\mu$m H$_2$ emission in and around the torus. Furthermore, we suggest that NGC 1097 hosts a geometrically thinner torus than NGC 1068. Although the physical origin of the torus thickness remains unclear, our observations support a theoretical prediction that geometrically thick tori with high opacity will become deficient as AGNs evolve from luminous Seyferts to LLAGNs., Comment: 9 pages, 5 figures. Accepted for publication in ApJL
Published: 2017
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31. Luminous, pc-scale CO 6-5 emission in the obscured nucleus of NGC1377

Author: Aalto, S., Muller, S., Costagliola, F., Sakamoto, K., Gallagher, J. S., Falstad, N., König, S., Dasyra, K., Wada, K., Combes, F., García-Burillo, S., Kristensen, L. E., Martín, S., van der Werf, P., Evans, A. S., and Kotilainen, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: High resolution submm observations are important in probing the morphology, column density and dynamics of obscured active galactic nuclei (AGNs). With high resolution (0.06 x 0.05) ALMA 690 GHz observations we have found bright (TB >80 K) and compact (FWHM 10x7 pc) CO 6-5 line emission in the nucleus of the extremely radio-quiet galaxy NGC1377. The integrated CO 6-5 intensity is aligned with the previously discovered jet/outflow of NGC1377 and is tracing the dense (n>1e4 cm-3), hot gas at the base of the outflow. The velocity structure is complex and shifts across the jet/outflow are discussed in terms of jet-rotation or separate, overlapping kinematical components. High velocity gas (deltaV +-145 km/s) is detected inside r<2-3 pc and we suggest that it is emerging from an inclined rotating disk or torus of position angle PA=140+-20 deg with a dynamical mass of approx 3e6 Msun. This mass is consistent with that of a supermassive black hole (SMBH), as inferred from the M-sigma relation. The gas mass of the proposed disk/torus constitutes <3% of the nuclear dynamical mass. In contrast to the intense CO 6-5 line emission, we do not detect dust continuum with an upper limit of S(690GHz)<2mJy. The corresponding, 5 pc, H2 column density is estimated to N(H2)<3e23 cm-2, which is inconsistent with a Compton Thick (CT) source. We discuss the possibility that CT obscuration may be occuring on small (subparsec) or larger scales. From SED fitting we suggest that half of the IR emission of NGC1377 is nuclear and the rest (mostly the far-infrared (FIR)) is more extended. The extreme radio quietness, and the lack of emission from other star formation tracers, raise questions on the origin of the FIR emission. We discuss the possibility that it is arising from the dissipation of shocks in the molecular jet/outflow or from irradiation by the nuclear source along the poles., Comment: 7 pages, 5 figures, submitted to Astronomy and Astrophysics
Published: 2017
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32. Early clinical effects, safety, and predictors of the effects of romosozumab treatment in osteoporosis patients: one-year study

Author: Tominaga, A., Wada, K., Okazaki, K., Nishi, H., Terayama, Y., and Kato, Y.
Published: 2021
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33. “All-seeing puncture” and micro-PCNL using HDIG scope provide more safety

Author: Nakajima, H., primary, Wada, K., additional, Koike, C., additional, Ogawa, K., additional, Nagami, T., additional, Kobayashi, Y., additional, Tsuboi, I., additional, Yokoyama, S., additional, Yoshioka, S., additional, Mitani, K., additional, Tanaka, G., additional, and Hara, T., additional
Published: 2024
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34. High detectivity PbSxSe1-x films for mid-wavelength infrared detectors

Author: Maksimov, O., Su, P., Bhattacharya, P., Stoll, K.E., Wada, K., Kimerling, L.C., Agarwal, A., and Bhandari, H.B.
Published: 2021
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35. Anomalously porous boulders on (162173) Ryugu as primordial materials from its parent body

Author: Sakatani, N., Tanaka, S., Okada, T., Fukuhara, T., Riu, L., Sugita, S., Honda, R., Morota, T., Kameda, S., Yokota, Y., Tatsumi, E., Yumoto, K., Hirata, N., Miura, A., Kouyama, T., Senshu, H., Shimaki, Y., Arai, T., Takita, J., Demura, H., Sekiguchi, T., Müller, T. G., Hagermann, A., Biele, J., Grott, M., Hamm, M., Delbo, M., Neumann, W., Taguchi, M., Ogawa, Y., Matsunaga, T., Wada, T., Hasegawa, S., Helbert, J., Hirata, N., Noguchi, R., Yamada, M., Suzuki, H., Honda, C., Ogawa, K., Hayakawa, M., Yoshioka, K., Matsuoka, M., Cho, Y., Sawada, H., Kitazato, K., Iwata, T., Abe, M., Ohtake, M., Matsuura, S., Matsumoto, K., Noda, H., Ishihara, Y., Yamamoto, K., Higuchi, A., Namiki, N., Ono, G., Saiki, T., Imamura, H., Takagi, Y., Yano, H., Shirai, K., Okamoto, C., Nakazawa, S., Iijima, Y., Arakawa, M., Wada, K., Kadono, T., Ishibashi, K., Terui, F., Kikuchi, S., Yamaguchi, T., Ogawa, N., Mimasu, Y., Yoshikawa, K., Takahashi, T., Takei, Y., Fujii, A., Takeuchi, H., Yamamoto, Y., Hirose, C., Hosoda, S., Mori, O., Shimada, T., Soldini, S., Tsukizaki, R., Ozaki, M., Tachibana, S., Ikeda, H., Ishiguro, M., Yabuta, H., Yoshikawa, M., Watanabe, S., and Tsuda, Y.
Published: 2021
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36. A precessing molecular jet signaling an obscured, growing supermassive black hole in NGC1377?

Author: Aalto, S., Costagliola, F., Muller, S., Sakamoto, K., Gallagher, J. S., Dasyra, K., Wada, K., Combes, F., García-Burillo, S., Kristensen, L., Martín, S., van der Werf, P., Evans, A. S., and Kotilainen, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: With high resolution (0."25 x 0."18) ALMA CO 3-2 observations of the nearby (D=21 Mpc, 1"=102 pc), extremely radio-quiet galaxy NGC1377, we have discovered a high-velocity, very collimated nuclear outflow which we interpret as a molecular jet with a projected length of +-150 pc. Along the jet axis we find strong velocity reversals where the projected velocity swings from -150 km/s to +150 km/s. A simple model of a molecular jet precessing around an axis close to the plane of the sky can reproduce the observations. The velocity of the outflowing gas is difficult to constrain due to the velocity reversals but we estimate it to be between 240 and 850 km/s and the jet to precess with a period P=0.3-1.1 Myr. The CO emission is clumpy along the jet and the total molecular mass in the high-velocity (+-(60 to 150 km/s)) gas lies between 2e6 Msun (light jet) and 2e7 Msun (massive jet). There is also CO emission extending along the minor axis of NGC1377. It holds >40% of the flux in NGC1377 and may be a slower, wide-angle molecular outflow which is partially entrained by the molecular jet. We discuss the driving mechanism of the molecular jet and suggest that it is either powered by a very faint radio jet or by an accretion disk-wind similar to those found towards protostars. The nucleus of NGC1377 harbours intense embedded activity and we detect emission from vibrationally excited HCN J=4-3 v_2=1f which is consistent with hot gas and dust. We find large columns of H2 in the centre of NGC1377 which may be a sign of a high rate of recent gas infall. The dynamical age of the molecular jet is short (<1 Myr), which could imply that it is young and consistent with the notion that NGC1377 is caught in a transient phase of its evolution. However, further studies are required to determine the age of the molecular jet, its mass and the role it is playing in the growth of the nucleus of NGC1377., Comment: This is a revised and expanded version of a previous submission which now has 13 pages, 6 figures (+ 4 in the Appendix) and is accepted for publication in Astronomy & Astrophysics
Published: 2015
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37. On the Disappearance of a Cold Molecular Torus around the Low-luminosity Active Galactic Nucleus of NGC 1097

Author: Izumi, T, Kohno, K, Fathi, K, Hatziminaoglou, E, Davies, RI, Martin, S, Matsushita, S, Schinnerer, E, Espada, D, Aalto, S, Onishi, K, Turner, JL, Imanishi, M, Nakanishi, K, Meier, DS, Wada, K, Kawakatu, N, and Nakajima, T
Subjects: galaxies: active, galaxies: individual, galaxies: ISM, galaxies: Seyfert, Astronomy & Astrophysics, Astronomical and Space Sciences
Published: 2017

38. Early clinical effects, safety, and appropriate selection of bone markers in romosozumab treatment for osteoporosis patients: a 6-month study

Author: Tominaga, A., Wada, K., Kato, Y., Nishi, H., Terayama, Y., and Okazaki, K.
Published: 2021
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39. Reanalyses of Anomalous Gravitational Microlensing Events in the OGLE-III Early Warning System Database with Combined Data

Author: Jeong, J., Park, H., Han, C., Gould, A., Udalski, A., Szymański, M. K., Pietrzyński, G., Soszyński, I., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sweatman, W. L., Sumi, T., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Albrow, M. D., Batista, V., Beaulieu, J. -P., Caldwell, J. A. R., Cassan, A., Cole, A., Coutures, C., Dieters, S., Dominik, M., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Hoffman, M., Huber, M., Jørgensen, U. G., Kane, S. R., Kubas, D., Martin, R., Marquette, J. -B., Menzies, J., Pitrou, C., Pollard, K., Sahu, K. C., Vinter, C., Wambsganss, J., Williams, A., Allen, W., Bolt, G., Choi, J. -Y., Christie, G. W., DePoy, D. L., Drummond, J., Gaudi, B. S., Hwang, K. -H., Jung, Y. K., Lee, C. -U., Mallia, F., Maoz, D., Maury, A., McCormick, J., Monard, L. A. G., Moorhouse, D., Natusch, T., Ofek, E. O., Park, B. -G., Pogge, R. W., Santallo, R., Shin, I. -G., Thornley, G., Yee, J. C., Allan, A., Bramich, D. M., Burgdorf, M. J., Horne, K., Hundertmark, M., Kains, N., Snodgrass, C., Steele, I., Street, R., and Tsapras, Y.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We reanalyze microlensing events in the published list of anomalous events that were observed from the OGLE lensing survey conducted during 2004-2008 period. In order to check the existence of possible degenerate solutions and extract extra information, we conduct analyses based on combined data from other survey and follow-up observation and consider higher-order effects. Among the analyzed events, we present analyses of 8 events for which either new solutions are identified or additional information is obtained. We find that the previous binary-source interpretations of 5 events are better interpreted by binary-lens models. These events include OGLE-2006-BLG-238, OGLE-2007-BLG-159, OGLE-2007-BLG-491, OGLE-2008-BLG-143, and OGLE-2008-BLG-210. With additional data covering caustic crossings, we detect finite-source effects for 6 events including OGLE-2006-BLG-215, OGLE-2006-BLG-238, OGLE-2006-BLG-450, OGLE-2008-BLG-143, OGLE-2008-BLG-210, and OGLE-2008-BLG-513. Among them, we are able to measure the Einstein radii of 3 events for which multi-band data are available. These events are OGLE-2006-BLG-238, OGLE-2008-BLG-210, and OGLE-2008-BLG-513. For OGLE-2008-BLG-143, we detect higher-order effect induced by the changes of the observer's position caused by the orbital motion of the Earth around the Sun. In addition, we present degenerate solutions resulting from the known close/wide or ecliptic degeneracy. Finally, we note that the masses of the binary companions of the lenses of OGLE-2006-BLG-450 and OGLE-2008-BLG-210 are in the brown-dwarf regime., Comment: 10 pages, 4 tables, 9 figures. Accepted in ApJ, Author list updated
Published: 2015
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40. Thermally altered subsurface material of asteroid (162173) Ryugu

Author: Kitazato, K., Milliken, R. E., Iwata, T., Abe, M., Ohtake, M., Matsuura, S., Takagi, Y., Nakamura, T., Hiroi, T., Matsuoka, M., Riu, L., Nakauchi, Y., Tsumura, K., Arai, T., Senshu, H., Hirata, N., Barucci, M. A., Brunetto, R., Pilorget, C., Poulet, F., Bibring, J.-P., Domingue, D. L., Vilas, F., Takir, D., Palomba, E., Galiano, A., Perna, D., Osawa, T., Komatsu, M., Nakato, A., Arai, T., Takato, N., Matsunaga, T., Arakawa, M., Saiki, T., Wada, K., Kadono, T., Imamura, H., Yano, H., Shirai, K., Hayakawa, M., Okamoto, C., Sawada, H., Ogawa, K., Iijima, Y., Sugita, S., Honda, R., Morota, T., Kameda, S., Tatsumi, E., Cho, Y., Yoshioka, K., Yokota, Y., Sakatani, N., Yamada, M., Kouyama, T., Suzuki, H., Honda, C., Namiki, N., Mizuno, T., Matsumoto, K., Noda, H., Ishihara, Y., Yamada, R., Yamamoto, K., Yoshida, F., Abe, S., Higuchi, A., Yamamoto, Y., Okada, T., Shimaki, Y., Noguchi, R., Miura, A., Hirata, N., Tachibana, S., Yabuta, H., Ishiguro, M., Ikeda, H., Takeuchi, H., Shimada, T., Mori, O., Hosoda, S., Tsukizaki, R., Soldini, S., Ozaki, M., Terui, F., Ogawa, N., Mimasu, Y., Ono, G., Yoshikawa, K., Hirose, C., Fujii, A., Takahashi, T., Kikuchi, S., Takei, Y., Yamaguchi, T., Nakazawa, S., Tanaka, S., Yoshikawa, M., Watanabe, S., and Tsuda, Y.
Published: 2021
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41. Collisional history of Ryugu’s parent body from bright surface boulders

Author: Tatsumi, E., Sugimoto, C., Riu, L., Sugita, S., Nakamura, T., Hiroi, T., Morota, T., Popescu, M., Michikami, T., Kitazato, K., Matsuoka, M., Kameda, S., Honda, R., Yamada, M., Sakatani, N., Kouyama, T., Yokota, Y., Honda, C., Suzuki, H., Cho, Y., Ogawa, K., Hayakawa, M., Sawada, H., Yoshioka, K., Pilorget, C., Ishida, M., Domingue, D., Hirata, N., Sasaki, S., de León, J., Barucci, M. A., Michel, P., Suemitsu, M., Saiki, T., Tanaka, S., Terui, F., Nakazawa, S., Kikuchi, S., Yamaguchi, T., Ogawa, N., Ono, G., Mimasu, Y., Yoshikawa, K., Takahashi, T., Takei, Y., Fujii, A., Yamamoto, Y., Okada, T., Hirose, C., Hosoda, S., Mori, O., Shimada, T., Soldini, S., Tsukizaki, R., Mizuno, T., Iwata, T., Yano, H., Ozaki, M., Abe, M., Ohtake, M., Namiki, N., Tachibana, S., Arakawa, M., Ikeda, H., Ishiguro, M., Wada, K., Yabuta, H., Takeuchi, H., Shimaki, Y., Shirai, K., Hirata, N., Iijima, Y., Tsuda, Y., Watanabe, S., and Yoshikawa, M.
Published: 2021
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42. Impact of Oscillating Positive Expiratory Pressure Device Use on Post-Discharge Hospitalizations: A Retrospective Cohort Study Comparing Patients with COPD or Chronic Bronchitis Using the Aerobika® and Acapella® Devices

Author: Tse J, Wada K, Wang Y, Coppolo D, Kushnarev V, and Suggett J
Subjects: database, exacerbations, re-hospitalization, sputum clearance, opep, Diseases of the respiratory system, RC705-779
Abstract: Jenny Tse,1 Keiko Wada,1 Yi Wang,1 Dominic Coppolo,2 Vladimir Kushnarev,3 Jason Suggett3 1IQVIA, Medical and Scientific Services, Real World Solutions, Cambridge, MA, USA; 2Monaghan Medical Corporation, Clinical Strategy and Development, Plattsburgh, NY, USA; 3Trudell Medical International, Science and Technology, London, ON, CanadaCorrespondence: Jenny TseIQVIA, 201 Broadway, 5th Fl, Cambridge, MA 02139, USATel +1 617-583-0627Email Jenny.Tse@iqvia.comPurpose: Managing and preventing disease exacerbations are key goals of COPD care. Oscillating positive expiratory pressure (OPEP) devices have been shown to improve clinical outcomes when added to COPD standard of care. This retrospective database study compared real-world resource use and disease exacerbation among patients with COPD or chronic bronchitis prescribed either of two commonly used OPEP devices.Patients and methods: Patients using the Aerobika® (Trudell Medical International, London, ON, Canada) or Acapella® (Smiths Medical, Wampsville, New York, USA) OPEP device for COPD or chronic bronchitis were identified from hospital claims linked to medical and prescription claims between September 2013 and April 2018; the index date was the first hospital visit with an OPEP device. Severe disease exacerbation, defined as an inpatient visit with a COPD or chronic bronchitis diagnosis, and all-cause healthcare resource utilization over 30 days and 12 months post-discharge were compared in propensity score (PS)-matched Aerobika device and Acapella device users.Results: In total, 619 Aerobika device and 1857 Acapella device users remained after PS matching. After discharge from the index visit, Aerobika device users were less likely to have ≥ 1 severe exacerbation within 30 days (12.0% vs 17.4%, p=0.01) and/or 12 months (39.6% vs 45.3%, p=0.01) and had fewer 12-month severe exacerbations (mean, 0.7 vs 0.9 per patient per year, p=0.01), with significantly longer time to first severe exacerbation than Acapella users (log-rank p=0.01). Aerobika device users were also less likely to have ≥ 1 all-cause inpatient visit within 30 days (13.9% vs 20.3%, p< 0.001) and 12 months (44.9% vs 51.8%, p=0.003) than Acapella users.Conclusion: Patients receiving the Aerobika OPEP device, compared to the Acapella device, had lower rates of subsequent severe disease exacerbation and all-cause inpatient admission. This suggests that Aerobika OPEP device may be a beneficial add-on to usual care and that OPEP devices may vary in clinical effectiveness.Keywords: database, exacerbations, re-hospitalization, sputum clearance, OPEP
Published: 2020

43. A pulse stretcher for a LINAC-based pulsed slow-positron beam providing a quasi-continuous beam with an energy of 5.2 keV

Author: Wada, K., Maekawa, M., Mochizuki, I., Shidara, T., Kawasuso, A., Kimura, M., and Hyodo, T.
Published: 2020
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44. Study on seismic behavior of circular steel pier subjected to three dimensional ground acceleration

Author: Wada, K., primary, Mori, M., additional, and Shirahata, H., additional
Published: 2021
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45. Pathogenetic role of neutrophil extracellular traps in coronary flow impairment following percutaneous coronary intervention in acute myocardial infarction patients -A multicenter study-

Author: Takeuchi, S, primary, Nishimiya, K, additional, Wada, K, additional, Adachi, A, additional, Oyama, K, additional, Shindo, T, additional, Godo, S, additional, Hao, K, additional, Shiroto, T, additional, Namiuchi, S, additional, Takahashi, J, additional, and Yasuda, S, additional
Published: 2023
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46. Time-resolved infrared emission from radiation-driven central obscuring structures in Active Galactic Nuclei

Author: Schartmann, M., Wada, K., Prieto, M. A., Burkert, A., and Tristram, K. R. W.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The central engines of Seyfert galaxies are thought to be enshrouded by geometrically thick gas and dust structures. In this article, we derive observable properties for a self-consistent model of such toroidal gas and dust distributions, where the geometrical thickness is achieved and maintained with the help of X-ray heating and radiation pressure due to the central engine. Spectral energy distributions (SEDs) and images are obtained with the help of dust continuum radiative transfer calculations with RADMC-3D. For the first time, we are able to present time-resolved SEDs and images for a physical model of the central obscurer. Temporal changes are mostly visible at shorter wavelengths, close to the combined peak of the dust opacity as well as the central source spectrum and are caused by variations in the column densities of the generated outflow. Due to the three-component morphology of the hydrodynamical models -- a thin disc with high density filaments, a surrounding fluffy component (the obscurer) and a low density outflow along the rotation axis -- we find dramatic differences depending on wavelength: whereas the mid-infrared images are dominated by the elongated appearance of the outflow cone, the long wavelength emission is mainly given by the cold and dense disc component. Overall, we find good agreement with observed characteristics, especially for those models, which show clear outflow cones in combination with a geometrically thick distribution of gas and dust, as well as a geometrically thin, but high column density disc in the equatorial plane., Comment: 16 pages, 12 figures, accepted for publication in MNRAS
Published: 2014
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47. Hydrogen embrittlement susceptibility of additively manufactured 316L stainless steel: Influence of post-processing, printing direction, temperature and pre-straining

Author: Álvarez, G., primary, Harris, Z., additional, Wada, K., additional, Rodríguez, C., additional, and Martínez-Pañeda, E., additional
Published: 2023
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48. OGLE-2013-BLG-0102LA,B: Microlensing binary with components at star/brown-dwarf and brown-dwarf/planet boundaries

Author: Jung, Y. K., Udalski, A., Sumi, T., Han, C., Gould, A., Skowron, J., Kozłowski, S., Poleski, R., Wyrzykowski, Ł., Szymański, M. K., Pietrzyński, G., Soszyński, I., Ulaczyk, K., Pietrukowicz, P., Mróz, P., Kubiak, M., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Larsen, P., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Albrow, M., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Hwang, K. -H., Lee, C. -U., Park, H., Owen, S., Pogge, R. W., Shin, I. -G., and Yee, J. C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the analysis of the gravitational microlensing event OGLE-2013-BLG-0102. The light curve of the event is characterized by a strong short-term anomaly superposed on a smoothly varying lensing curve with a moderate magnification $A_{\rm max}\sim 1.5$. It is found that the event was produced by a binary lens with a mass ratio between the components of $q = 0.13$ and the anomaly was caused by the passage of the source trajectory over a caustic located away from the barycenter of the binary. From the analysis of the effects on the light curve due to the finite size of the source and the parallactic motion of the Earth, the physical parameters of the lens system are determined. The measured masses of the lens components are $M_{1} = 0.096 \pm 0.013~M_{\odot}$ and $M_{2} = 0.012 \pm 0.002~M_{\odot}$, which correspond to near the hydrogen-burning and deuterium-burning mass limits, respectively. The distance to the lens is $3.04 \pm 0.31~{\rm kpc}$ and the projected separation between the lens components is $0.80 \pm 0.08~{\rm AU}$., Comment: 6 figures, 2 tables, ApJ submitted
Published: 2014
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49. A Terrestrial Planet in a ~1 AU Orbit Around One Member of a ~15 AU Binary

Author: Gould, A., Udalski, A., Shin, I. -G., Porritt, I., Skowron, J., Han, C., Yee, J. C., Kozłowski, S., Choi, J. -Y., Poleski, R., Wyrzykowski, Ł., Ulaczyk, K., Pietrukowicz, P., Mróz, P., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Gaudi, B. S., Christie, G. W., Drummond, J., McCormick, J., Natusch, T., Ngan, H., Tan, T. -G., Albrow, M., DePoy, D. L., Hwang, K. -H., Jung, Y. K., Lee, C. -U., Park, H., Pogge, R. W., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Koshimoto, N., Larsen, P., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L., Rattenbury, N. J., Saito, To., Sullivan, D. J., Sumi, T., Suzuki, D., Tristram, P. J., Tsurumi, N., Wada, K., Yamai, N., Yock, P. C. M., Yonehara, A., Shvartzvald, Y., Maoz, D., Kaspi, S., and Friedmann, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We detect a cold, terrestrial planet in a binary-star system using gravitational microlensing. The planet has low mass (2 Earth masses) and lies projected at $a_{\perp,ph}$ ~ 0.8 astronomical units (AU) from its host star, similar to the Earth-Sun distance. However, the planet temperature is much lower, T<60 Kelvin, because the host star is only 0.10--0.15 solar masses and therefore more than 400 times less luminous than the Sun. The host is itself orbiting a slightly more massive companion with projected separation $a_{\perp,ch}=$10--15 AU. Straightforward modification of current microlensing search strategies could increase their sensitivity to planets in binary systems. With more detections, such binary-star/planetary systems could place constraints on models of planet formation and evolution. This detection is consistent with such systems being very common., Comment: Published in Science, Main and supplementary material combined
Published: 2014
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50. OGLE-2008-BLG-355Lb: A Massive Planet around A Late type Star

Author: Koshimoto, N., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Rattenbury, N., Abe, F., Botzler, C. S., Freeman, M., Fukagawa, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Muraki, Y., Ohnishi, K., Saito, To., Shibai, H., Sullivan, D. J., Suzuki, K., Suzuki, D., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Soszyński, I, Pietrzyński, G., Poleski, R., Ulaczyk, K., and Wyrzykowski, Ł.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a massive planet OGLE-2008-BLG-355Lb. The light curve analysis indicates a planet:host mass ratio of q = 0.0118 +/- 0.0006 at a separation of 0.877 +/- 0.010 Einstein radii. We do not measure a significant microlensing parallax signal and do not have high angular resolution images that could detect the planetary host star. Therefore, we do not have a direct measurement of the host star mass. A Bayesian analysis, assuming that all host stars have equal probability to host a planet with the measured mass ratio implies a host star mass of M_h = 0.37_{-0.17}^{+0.30} M_Sun and a companion of mass M_P = 4.6^{+3.7}_{-2.2} M_Jup, at a projected separation of r_proj = 1.70^{+0.29}_{-0.30} AU. The implied distance to the planetary system is D_L = 6.8 +/- 1.1 kpc. A planetary system with the properties preferred by the Bayesian analysis would be a challenge to the core-accretion model of planet formation, as the core-accretion model predicts that massive planets are far more likely to form around more massive host stars. This core accretion model prediction is not consistent with our Bayesian prior of an equal probability of host stars of all masses to host a planet with the measured mass ratio. So, if the core accretion model prediction is right, we should expect that follow-up high angular resolution observations will detect a host star with a mass in the upper part of the range allowed by the Bayesian analysis. That is, the host would probably be a K or G dwarf., Comment: 42 pages, 12 figures, submitted for publication in ApJ
Published: 2014
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