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1. The β-decay of 70Kr into 70Br: Restoration of the pseudo-SU(4) symmetry

Author

Vitéz-Sveiczer, A., Algora, A., Morales, A.I., Rubio, B., Kiss, G.G., Sarriguren, P., van Isacker, P., de Angelis, G., Recchia, F., Nishimura, S., Agramunt, J., Guadilla, V., Montaner-Pizá, A., Orrigo, S.E.A., Horváth, A., Napoli, D., Lenzi, S., Boso, A., Phong, V.H., Wu, J., Söderström, P.-A., Sumikama, T., Suzuki, H., Takeda, H., Ahn, D.S., Baba, H., Doornebal, P., Fukuda, N., Inabe, N., Isobe, T., Kubo, T., Kubono, S., Sakurai, H., Shimizu, Y., Sidong, C., Blank, B., Ascher, P., Gerbaux, M., Goigoux, T., Giovinazzo, J., Grévy, S., Kurtukián Nieto, T., Magron, C., Gelletly, W., Dombrádi, Zs., Fujita, Y., Tanaka, M., Aguilera, P., Molina, F., Eberth, J., Diel, F., Lubos, D., Borcea, C., Ganioglu, E., Nishimura, D., Oikawa, H., Takei, Y., Yagi, S., Korten, W., de France, G., Davies, P., Liu, J., Lee, J., Lokotko, T., Kojouharov, I., Kurz, N., Shaffner, H., Petrovici, A., Ministry of Innovation and Technology (Hungary), Agencia Nacional de Investigación y Desarrollo (Chile), RIKEN Nishina Center for Accelerator-Based Science, University of Tokyo, Ministerio de Ciencia e Innovación (España), Ministerio de Ciencia, Innovación y Universidades (España), Consejo Superior de Investigaciones Científicas (España), Science and Technology Facilities Council (UK), Ministry of Human Capacities (Hungary), Japan Society for the Promotion of Science, Hungarian Academy of Sciences, Grand Accélérateur National d'Ions Lourds (GANIL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Nuclear and High Energy Physics, QRPA calculations, Kr, Pseudo-SU(4) symmetry, pn pairing, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], Beta decay of, 70, GT strength distribution, Beta decay of Kr 70 | GT strength distribution | pn pairing | Pseudo-SU(4) symmetry | QRPA calculations
Abstract

8 pags., 4 figs., 1 tab., The β-decay of the even-even nucleus 70Kr with Z=N+2, has been investigated at the Radioactive Ion Beam Factory (RIBF) of the RIKEN Nishina Center using the BigRIPS fragment separator, the ZeroDegree Spectrometer, the WAS3ABI implantation station and the EURICA HPGe cluster array. Fifteen γ-rays associated with the β-decay of 70Kr into 70Br have been identified for the first time, defining ten populated states below Eexc=3300 keV. The half-life of 70Kr was derived with increased precision and found to be t1/2=45.19±0.14 ms. The β-delayed proton emission probability has also been determined as εp=0.545(23)%. An increase in the β-strength to the yrast 1+ state in comparison with the heaviest Z=N+2 system studied so far (62Ge decay) is observed that may indicate increased np correlations in the T=0 channel. The β-decay strength deduced from the results is interpreted in terms of the proton-neutron quasiparticle random-phase approximation (pnQRPA) and also with a schematic model that includes isoscalar and isovector pairing in addition to quadrupole deformation. The application of this last model indicates an approximate realization of pseudo-SU(4) symmetry in this system., This work was supported by the National Research, Development and Innovation Fund of the Ministry for Innovation and Technology, Hungary with project no. TKP2021-NKTA-42 under the TKP2021 funding scheme. FM acknowledges the support of ANID/FONDECYT Regular 1171467 and ANID/FONDECYT Regular 1221364 national projects. This work was carried out at the RIBF operated by RIKEN Nishina Center and CNS, University of Tokyo. We acknowledge the EUROBALL Owners Committee for the loan of germanium detectors and the PreSpec Collaboration for the readout electronics of the cluster detectors. This work was supported by the Spanish MICINN grants FPA2014-52823-C2-1-P, FPA2017- 83946-C2-1-P (MCIU/AEI/FEDER); Ministerio de Ciencia e Innovación grant PID2019-104714GB-C21; Centro de Excelencia Severo Ochoa del IFIC SEV-2014-0398; Junta para la Ampliación de Estudios Programme (CSIC JAE-Doc contract) co-financed by FSE, by NKFIH (NN128072), the National Research, Development and Innovation Fund of Hungary Project No. K 128729 the STFC (UK) through Grant No. ST/P005314/, the PROMETEO/2019/007 project and by the ÚNKP-20-5-DE-02 New National Excellence Program of the Ministry of Human Capacities of Hungary and by the JSPS KAKENHI of Japan (Grant No. 25247045). G.G. Kiss acknowledges support from the János Bolyai research fellowship of the Hungarian Academy of Sciences. A. A. acknowledges partial support of the JSPS Invitational Fellowships for Research in Japan (ID: L1955) P. S. acknowledges support from MCI/AEI/FEDER,UE (Spain) under grant PGC2018-093636-B-I00.

Published
2022

2. Photometric behavior of Ryugu’s NIR spectral parameters

Author

Longobardo, Andrea, Palomba, E., Galiano, Anna, Dirri, Fabrizio, Zinzi, Angelo, D'Amore, Mario, Domingue, Deborah L., Kitazato, K., Yokota, Y., Schroeder, Stephan, Iwata, T., Matsuoka, M., Hiroi, T., Takir, D., Nakamura, T., Abe, M., Ohtake, M., Matsuura, S., Watanabe, S, Yoshikawa, M., Saiki, T., Okada, T., Tanaka, S., Yamamoto, Y., Takei, Y., Shirai, K., Hirata, N., Matsumoto, K., and Tsuda, T.

Subjects
Photometry, parameters, Space and Planetary Science, spectral, Ryugu, Astronomy and Astrophysics, NIR
Abstract

Context. JAXA’s Hayabusa2 mission rendezvoused the Ryugu asteroid for 1.5 years to clarify the carbonaceous asteroids’ record for Solar System origin and evolution. Aims. We studied the photometric behavior of the spectral parameters characterizing the near-infrared (NIR) spectra of Ryugu provided by the Hayabusa2/NIRS3 instrument, that is to say 1.9 µm reflectance, 2.7 and 2.8 µm band depths (ascribed to phyllosilicates), and NIR slope. Methods. For each parameter, we applied the following empirical approach: (1) retrieval of the equigonal albedo by applying the Akimov disk function (this step was only performed for the reflectance photometric correction); (2) retrieval of the median spectral parameter value at each phase angle bin; and (3) retrieval of the phase function by a linear fit. Results. Ryugu’s phase function shows a steepness similar to Ceres, according to the same taxonomy of the two asteroids. Band depths decrease with increasing phase angle: this trend is opposite to that observed on other asteroids explored by space missions and is ascribed to the very dark albedo. NIR and visible phase reddening are similar, contrary to other asteroids, where visible phase reddening is larger: this could be due to surface darkness or to particle smoothness. Albedo and band depths are globally uncorrelated, but locally anticorrelated. A correlation between darkening and reddening is observed.

Published
2022

3. Hayabusa2 Extended Mission: New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period

Author

Hirabayashi, M., Mimasu, Y., Sakatani, N., Watanabe, S., Tsuda, Y., Saiki, T., Kikuchi, S., Kouyama, T., Yoshikawa, M., Tanaka, S., Nakazawa, S., Takei, Y., Terui, F., Takeuchi, H., Fujii, A., Iwata, T., Tsumura, K., Matsuura, S., Shimaki, Y., Urakawa, S., Ishibashi, Y., Hasegawa, S., Ishiguro, M., Kuroda, D., Okumura, S., Sugita, S., Okada, T., Kameda, S., Kamata, S., Higuchi, A., Senshu, H., Noda, H., Matsumoto, K., Suetsugu, R., Hirai, T., Kitazato, K., Farnocchia, D., Naidu, S. P., Tholen, D. J., Hergenrother, C. W., Whiteley, R. J., Moskovitz, N. A., Abell, P. A., and group, the Hayabusa2 extended mission study

Subjects
Atmospheric Science, Solar System, 010504 meteorology & atmospheric sciences, Computer science, Cruise, Aerospace Engineering, FOS: Physical sciences, Sample (statistics), 01 natural sciences, Phase (combat), 0103 physical sciences, Aerospace engineering, Aerospace, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Spacecraft, business.industry, Rendezvous, Astronomy and Astrophysics, Geophysics, Space and Planetary Science, Asteroid, General Earth and Planetary Sciences, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Hayabusa2 is the Japanese Asteroid Return Mission and targeted the carbonaceous asteroid Ryugu, conducted by the Japan Aerospace Exploration Agency (JAXA). The goal of this mission was to conduct proximity operations including remote sensing observations, material sampling, and a Small Carry-On Impact experiment, as well as sample analyses. As of September 2020, the spacecraft is on the way back to Earth with samples from Ryugu with no critical issues after the successful departure in November 2019. Here, we propose an extended mission in which the spacecraft will rendezvous with a small asteroid with ~30 m - ~40 m in diameter that is rotating at a spin period of ~10 min after an additional ~10-year cruise phase. We introduce that two scenarios are suitable for the extended mission. In the first scenario, the spacecraft will perform swing-by maneuvers at Venus once and Earth twice to arrive at asteroid 2001 AV43. In the second scenario, it will perform swing-by maneuvers at Earth twice to reach asteroid 1998 KY26. In both scenarios, the mission will continue until the early 2030s. JAXA recently released the decision that the spacecraft will rendezvous with 1998 KY26. This paper focuses on our scientific assessments of the two scenarios but leaves the decision process to go to 1998 KY26 for future reports. Rendezvous operations will be planned to detail the physical properties and surrounding environments of the target, one of the smallest elements of small planetary bodies. By achieving the planned operations, the mission will provide critical hints on the violent histories of collisions and accumulations of small bodies in the solar system. Furthermore, the established scientific knowledge and techniques will advance key technologies for planetary defense., Comment: 51 pages, 9 figures, and 10 tables. The article is in press in Advances in Space Research

Published
2021
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4. Dysfunction of a Peripheral Lipid Sensor Gpr120 Causes Pgd2-microglia-provoked Neuroinflammation

Author

Keisuke Yoshikawa, Sakemoto C, Takei Y, Yagishita-kyo N, Hirasawa A, Shinji Yamamoto, Yamashina K, Kensuke Iwasa, Awaji T, and Kei Maruyama

Subjects
medicine.anatomical_structure, Microglia, business.industry, Medicine, GPR120, lipids (amino acids, peptides, and proteins), business, Neuroscience, Neuroinflammation, Peripheral
Abstract

Background Neuroinflammation is a key pathological component of neurodegenerative disease and is characterized by microglial activation and the secretion of proinflammatory mediators. We previously reported that a surge in prostaglandin D2 (PGD2) production and PGD2-induced microglial activation could provoke neuroinflammation. We also reported that a lipid sensor GPR120 (free fatty acid receptor 4), which is expressed in enteroendocrine cells in the intestine, could be activated by polyunsaturated fatty acids (PUFA), thereby mediating secretion of glucagon-like peptide-1 (GLP-1). Dysfunction of GPR120 results in obesity in both mice and humans. To reveal the relationship between PGD2-microglia-provoked neuroinflammation and intestinal PUFA/GPR120 signaling, we investigated neuroinflammation and neuronal function in GPR120 knockout (KO) mice. Results In the current study, we discovered notable PGD2-microglia-provoked neuroinflammation (increased PGD2 production and microglial activation) and neurodegeneration (declines in neurogenesis, hippocampal volume, and cognitive function) in GPR120 KO mice. We also found that Hematopoietic-prostaglandin D synthase (H-PGDS) was expressed in microglia, microglia were activated by PGD2, H-PGDS expression was upregulated in GPR120 KO hippocampus, and inhibition of PGD2 production attenuated this neuroinflammatory pathway, suggesting that PGD2-microglia-provoked neuroinflammation was constantly occurring in the hippocampus of GPR120 KO mice. GPR120 mRNA was detected in the intestinal tissues, but not in the brain tissue of WT mice. GPR120 KO mice exhibited reduced intestinal, plasma, and intracerebral GLP-1 levels. Peripheral administration of a GLP-1 analogue, liraglutide, reduced PGD2-microglia-provoked neuroinflammation and further neurodegeneration in GPR120 KO mice. Conclusions Our results suggest that PGD2-microglia-provoked neuroinflammation and neurodegeneration observed in GPR120 KO mice are probably caused by defects in intestinal GPR120 function, and not in the CNS. Our results also suggest that GLP-1 secretion, stimulated by intestinal GPR120, may remotely contribute to suppression of PGD2-microglia-provoked neuroinflammation and further neurodegeneration in the hippocampus.

Published
2020

5. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi*

Author

Aharonia, F., Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M. W., Blandford, R., Brenneman, L. W., Brown, G. V., Bulbul, E., Cackett, E. M., Canning, R. E. A., Chernyakova, M., Chiao, M. P., Coppi, P. S., Costantini, E., Plaa, J., Vries, C. P., Den Herder, J. -W, Done, C., Dotani, T., Ebisawa, K., Eckart, M. E., Enoto, T., Ezoe, Y., Fabian, A. C., Ferrigno, C., Foster, A. R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L. C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I. M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J. S., Hornschemeier, A., Hoshino, A., Hughes, J. P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, S., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R. L., Kilbourne, C. A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H. A., Kubota, A., Kunieda, H., Laurent, P., Lee, S. -H, Leutenegger, M. A., Limousin, O., Loewenstein, M., Long, K. S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Kyoko Matsushita, Mccammon, D., Mcnamara, B. R., Mehdipour, M., Miller, E. D., Miller, J. M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R. F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K. K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F. S., Pottschmidt, K., Reynolds, C. S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P. J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R. K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Amagawa, T. T., Tamura, T., Tanaka, K., Tanaka, T., Tanaka, Y., Tanaka, Y. T., Tashiro, M. S., Tawara, Y., Terada, Y., Erashima, Y. T., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T. G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C. M., Ursino, E., Wang, Q. H. S., Watanabe, S., Werner, N., Wilkins, D. R., Williams, B. J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N. Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
galaxies: clusters: individual, galaxies: clusters: intracluster medium, Active galactic nucleus, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], individual (NGC 1275) [galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: individual, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: individual (Perseus) [galaxies], 01 natural sciences, Intracluster medium, 0103 physical sciences, Emission spectrum, Brightest cluster galaxy, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Settore FIS/05, 010308 nuclear & particles physics, Velocity gradient, RCUK, Velocity dispersion, Astronomy and Astrophysics, Redshift, ST/J003697/2, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, Electron temperature, galaxies: clusters [X-rays], ST/L00075X/1, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: Hitomi Collaboration 197名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 林, 佑; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 197 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hayashi, Tasuku; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 201710-31, 資料番号: SA1170334000

Published
2018

6. Simultaneous investigation of the $\mathbf{T=1~ (J^��=0^+)}$ and $\mathbf{T=0 ~ (J^��=9^+)}$ $��$ decays in $^{70}$Br

Author

Morales, A. I., Algora, A., Rubio, B., Kaneko, K., Nishimura, S., Aguilera, P., Orrigo, S. E. A., Molina, F., de Angelis, G., Recchia, F., Kiss, G., Phong, V. H., Wu, J., Nishimura, D., Oikawa, H., Goigoux, T., Giovinazzo, J., Ascher, P., Agramunt, J., Ahn, D. S., Baba, H., Blank, B., Borcea, C., Boso, A., Davies, P., Diel, F., Dombr��di, Zs., Doornenbal, P., Eberth, J., de France, G., Fujita, Y., Fukuda, N., Ganioglu, E., Gelletly, W., Gerbaux, M., Gr��vy, S., Guadilla, V., Inabe, N., Isobe, T., Korten, W., Kubo, T., Kubono, S., Nieto, T. Kurtuki��n, Lenzi, S., Lubos, D., Magron, C., Montaner-Piz��, A., Napoli, D. R., Sakurai, H., Shimizu, Y., Sidong, C., S��derstr��m, P. -A., Sumikama, T., Suzuki, H., Takeda, H., Takei, Y., Tanaka, M., and Yagi, S.

Subjects
FOS: Physical sciences, Nuclear Experiment (nucl-ex)
Abstract

The $��$ decay of the odd-odd nucleus $^{70}$Br has been investigated with the BigRIPS and EURICA setups at the Radioactive Ion Beam Factory (RIBF) of the RIKEN Nishina Center. The $T=0$ ($J^��=9^+$) and $T=1$ ($J^��=0^+$) isomers have both been produced in in-flight fragmentation of $^{78}$Kr with ratios of 41.6(8)\% and 58.4(8)\%, respectively. A half-life of $t_{1/2}=2157^{+53}_{-49}$ ms has been measured for the $J^��=9^+$ isomer from $��$-ray time decay analysis. Based on this result, we provide a new value of the half-life for the $J^��=0^+$ ground state of $^{70}$Br, $t_{1/2}=78.42\pm0.51$ ms, which is slightly more precise, and in excellent agreement, with the best measurement reported hitherto in the literature. For this decay, we provide the first estimate of the total branching fraction decaying through the $2^+_1$ state in the daughter nucleus $^{70}$Se, $R(2^+_1)=1.3\pm1.1\%$. We also report four new low-intensity $��$-ray transitions at 661, 1103, 1561, and 1749 keV following the $��$ decay of the $J^��=9^+$ isomer. Based on their coincidence relationships, we tentatively propose two new excited states at 3945 and 4752 keV in $^{70}$Se with most probable spins and parities of $J^��=(6^+)$ and $(8^+)$, respectively. The observed structure is interpreted with the help of shell-model calculations, which predict a complex interplay between oblate and prolate configurations at low excitation energies.

Published
2017
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7. Oral Contraceptive Progestin and Estrogen Use and Increases in Breast, Ovarian, and Endometrial Cancers

Author

Blackhall K, Grant Ec, Deval B, Rafii A, Ö Tunçalp, Harrison P, Taneichi A, Slinger G, Olufemi T Oladapo, Yaldo A, Widmer M, Warren Ce, Nwala E, Levardon M, Roberts I, Thouimy M, Hiroyuki Fujiwara, Narumi R, Maurice Bucagu, Liao L, Torloni Mr, Lin J, Browning A, Shakur H, Sripad P, Trautvetter L, Keya Kt, Amy Law, Lynen R, Trabert B, Gulmezoglu Am, Ferrer P, Rane A, Morisawa H, Takei Y, Michels Ka, Samain E, Sydenham E, and Matsubara S

Subjects
Program evaluation, Cancer Research, medicine.medical_specialty, Population, 03 medical and health sciences, 0302 clinical medicine, medicine, Humans, 030212 general & internal medicine, education, Socioeconomic status, education.field_of_study, Public health, Estrogens, medicine.disease, Endometrial Neoplasms, Oncology, Family planning, 030220 oncology & carcinogenesis, Female, Medical emergency, Progestins, Rural area, Colorectal Neoplasms, On-the-job training, Contraceptives, Oral, First aid
Abstract

The Peoples Health Center located in Savar Bangladesh makes extensive use of barefoot doctors and permits them to perform many functions generally reserved for medical personnel including minor surgery. The center was established in 1972 by Dr. Chowdhury who believed that paramedics were capable of providing effective medical care and that their services could help compensate for the dearth of trained medical personnel in the rural areas of Bangladesh. The center is run by a staff of 114 and has 3 structural levels. The main center at Savar serves a population of over 100000 and has a 15 bed hospital operating facilities a pathology laboratory a pharmacy and a handful of trained doctors. A number of sub-centers are strategically located to serve approximately 15000-20000 rural residents. The sub-centers are equipped to perform routine pathological examinations tubectomies and other forms of minor surgery. Paramedics at each sub-center are expected to make home visits to approximately 3000 residents in a 5 mile area. The paramedics are trained to provide many services including: 1) family planning; 2) immunization; 3) instruction in nutritional and sanitation matters; 4) first aid; 5) routine pathological examinations; 6) mini-laparotomy tubectomies; 7) menstrual regulation; and 8) abortion. Individuals recruited for the paramedic program have from 6-10 years of basic education and received 6 months of paramedical training. Practical experience and on the job training are stressed in the program. The Center recognizes that the economic situation of the residents of the area must be improved before any real inroads can be made toward improving their health status. The Center actively attempts to alter economic conditions by: 1) sponsoring programs which provide employment opportunities for women; 2) providing low cost loans to landless residents to enable them to break their pattern of cyclical indebtedness to their landlords; and 3) running a school for local children. These activities are frequently attacked by landlords by Moslem priests who oppose the attempt to improve the status of women and by doctors who feel threatened by the paramedics.

Published
2018

8. The quiescent intracluster medium in the core of the Perseus cluster

Author

Aharonian, F, Akamatsu, H, Akimoto, F, Allen, S.~W., Anabuki, N, Angelini, L, Arnaud, K, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, M, Blandford, R, Brenneman, L, Brown, G.~V., Bulbul, E, Cackett, E, Chernyakova, M, Chiao, M, Coppi, P, Costantini, E, de Plaa, J, den Herder, J.-W., Done, C, Dotani, T, Ebisawa, K, Eckart, M, Enoto, T, Ezoe, Y, Fabian, A.~C., Ferrigno, C, Foster, A, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, L, Gandhi, P, Giustini, M, Goldwurm, A, Gu, L, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, I, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, J, Hornschemeier, A, Hoshino, A, Hughes, J, Iizuka, R, Inoue, H, Inoue, Y, Ishibashi, K, Ishida, M, Ishikawa, K, Ishisaki, Y, Itoh, M, Iyomoto, N, Kaastra, J, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, Nobuyuki, Kelley, R, Khangulyan, D, Kilbourne, C, King, A, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, H, Kubota, A, Kunieda, H, Laurent, P, Lebrun, F, Lee, S.-H., Leutenegger, M, Limousin, O, Loewenstein, M, Long, K.~S., Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, McCammon, D, McNamara, B, Mehdipour, M, Miller, E, Miller, J, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Moseley, H, Mukai, K, Murakami, H, Murakami, T, Mushotzky, R, Nagino, R, Nakagawa, T, Nakajima, H, Nakamori, T, Nakano, T, Nakashima, S, Nakazawa, K, Nobukawa, M, Noda, H, Nomachi, M, O'Dell, S, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Parmar, A, Petre, R, Pinto, C, Pohl, M, Porter, F.~S., Pottschmidt, K, Ramsey, B, Reynolds, C, Russell, H, Safi-Harb, S, Saito, S, Sakai, K, Sameshima, H, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemitsos, P, Seta, H, Shidatsu, M, Simionescu, A, Smith, R, Soong, Y, Stawarz, L, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, K, Tamura, T, Tanaka, T, Tanaka, Y, Tashiro, M, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, T, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Ueno, S, Uno, S, Urry, M, Ursino, E, de Vries, C, Watanabe, S, Werner, N, Wik, D, Wilkins, D, Williams, B, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, N.~Y., Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Yoichi, Yonetoku, D, Yoshida, A, Yuasa, T, Zhuravleva, I, and Zoghbi, A

Subjects
galaxies and clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High-energy astronomy, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, 010309 optics, Computational astrophysics, Settore FIS/05 - Astronomia e Astrofisica, Intracluster medium, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, high-energy astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Multidisciplinary, Astronomy, Velocity dispersion, Astrophysics - Astrophysics of Galaxies, Galaxy, Sky, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 215名(Hitomi Collaboration), Accepted: 2016-06-04, 資料番号: SA1160094000

Published
2016

9. Supplementary Material for: Familial Influences on Mismatch Negativity and Its Association with Plasma Glutamate Level: A Magnetoencephalographic Study in Twins

Author

Nishimura, Y., Kawakubo, Y., Suga, M., Hashimoto, K., Takei, Y., Takei, K., Inoue, H., Yumoto, M., Takizawa, R., and Kasai, K.

Abstract

Mismatch negativity (MMN) or its magnetic counterpart (magnetic mismatch negativity; MMNm) is regarded as a promising biomarker for schizophrenia. Previous electroencephalographic studies of MMN have demonstrated a moderate-to-high heritability for MMN amplitudes. N-methyl-D-aspartate receptor-dependent glutamatergic neurotransmission is implicated in MMN generation. We hypothesized that the differences between identical twins in MMNm variables might be associated with differences in plasma levels of amino acids involved in glutamatergic neurotransmission. Thirty-three pairs of monozygotic (MZ) and 10 pairs of dizygotic (DZ) twins underwent MMNm recording. The MMNm in response to tone duration changes, tone frequency changes, and phonemic changes was recorded using 204-channel magnetoencephalography. Of these, 26 MZ and 7 DZ twin pairs underwent blood sampling for determination of plasma amino acid levels. MMNm peak strength showed relatively high correlations in both MZ and DZ twin pairs. The differences in MMNm latencies tended to correlate with the differences in plasma amino acid levels within MZ pairs, while no significant correlation was observed after the Bonferroni correction. We observed a familial trait in MMNm strength. The differences in MMN latency in MZ twins might be influenced by changes in glutamate levels and glutamate-glutamine cycling; however, the results need to be replicated.

Published
2016
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10. Expected properties of the two-point autocorrelation function of the intergalactic medium

Author

Ursino, E., Branchini, ENZO FRANCO, Galeazzi, M., Marulli, F., Moscardini, L., Piro, L., Roncarelli, M., Takei, Y., Ursino, E., Branchini, ENZO FRANCO, Galeazzi, M., Marulli, F., Moscardini, L., Piro, L., Roncarelli, M., Takei, Y., E. Ursino, E. Branchini, M. Galeazzi, F. Marulli, L. Moscardini, L. Piro, M. Roncarelli, and Y. Takei

Subjects
large-scale structure of Universe, X-rays: diffuse background, diffuse radiation
Abstract

Recent analyses of the fluctuations of the soft diffuse X-ray background (DXB) have provided indirect detection of a component consistent with the elusive warm-hot intergalactic medium (WHIM). In this work we use theoretical predictions obtained from hydrodynamical simulations to investigate the angular correlation properties of the WHIM in emission and assess the possibility of indirect detection with next-generation X-ray missions. Our results indicate that the angular correlation signal of the WHIM is generally weak but dominates the angular correlation function of the DXB outside virialized regions. Its indirect detection is possible but requires rather long exposure times [0.1-1] Ms, large (similar to 1 degrees x 1 degrees) fields of view and accurate subtraction of isotropic fore/background contributions, mostly contributed by Galactic emission. The angular correlation function of the WHIM, which turns out to be positive for theta < 5 arcmin, provides limited information on its spatial distribution. A satisfactory characterization of the WHIM in 3D can be obtained through spatially resolved spectroscopy. 1Ms long exposures with next generation detectors will allow to detect similar to 400 OVII+OVIII X-ray emission systems that could be used to trace the spatial distribution of the WHIM. We predict that these observations will allow us to estimate the WHIM correlation function with high statistical significance out to similar to 10 Mpc h(-1) and characterize its dynamical state through the analysis of redshift-space distortions. The detectable WHIM, which is typically associated with the outskirts of virialized regions rather than the filaments, has a non-zero correlation function with slope gamma = -1.7 +/- 0.1 and correlation length r(0) = 4.0 +/- 0.1 Mpc h(-1) in the range r =[4.5, 12] Mpc h(-1). Redshift-space distances can be measured to assess the dynamical properties of the gas that we predict to be typically infalling on to large virialized structures.

Published
2011

11. EDGE: Explorer of diffuse emission and gamma-ray burst explosions RID C-2252-2008

Author

Piro L, den Herder J, Ohashi T, Amati L, Atteia JL, Barthelmy S, Barbera M, Barret D, Basso S, Boer M, Borgani S, Boyarskiy O, BRANCHINI, ENZO FRANCO, Branduardi Raymont G, Briggs M, Brunetti G, Budtz Jorgensen C, Burrows D, Campana S, Caroli E, Chincarini G, Christensen F, Cocchi M, Comastri A, Corsi A, Cotroneo V, Conconi P, Colasanti L, Cusumano G, de Rosa A, Del Santo M, Ettori S, Ezoe Y, Ferrari L, Feroci M, Finger M, Fishman G, Fujimoto R, Galeazzi M, Galli A, Gatti F, Gehrels N, Gendre B, Ghirlanda G, Ghisellini G, Giommi P, Girardi M, Guzzo L, Haardt F, Hepburn I, Hermsen W, Hoevers H, Holland A, in't Zand J, Ishisaki Y, Kawahara H, Kawai N, Kaastra J, Kippen M, de Korte PAJ, Kouveliotou C, Kusenko A, Labanti C, Lieu R, Macculi C, Makishima K, Mazzotta P, McCammon D, Mendez M, Mineo T, Mitchell S, Mitsuda K, Molendi S, Moscardini L, Mushotzky R, Natalucci L, Nicastro F, O'Brien P, Osborne J, Paerels F, Page M, Paltani S, Pareschi G, Perinati E, Perola C, Ponman T, Rasmussen A, Roncarelli M, Rosati P, Ruchayskiy O, Quadrini E, Sakurai I, Salvaterra R, Sasaki S, Sato G, Schaye J, Schmitt J, Sciortino S, Shaposhnikov M, Shinozaki K, Spiga D, Suto Y, Tagliaferri G, Takahashi T, Takei Y, Tawara Y, Tozzi P, Tsunemi H, Tsuru T, Ubertini P, Ursino E, Viel M, Vink J, White N, Willingale R, Wijers R, Yoshikawa K, Yamasaki N., MATT, Giorgio, Piro, L, den Herder, J, Ohashi, T, Amati, L, Atteia, Jl, Barthelmy, S, Barbera, M, Barret, D, Basso, S, Boer, M, Borgani, S, Boyarskiy, O, Branchini, ENZO FRANCO, Branduardi Raymont, G, Briggs, M, Brunetti, G, Budtz Jorgensen, C, Burrows, D, Campana, S, Caroli, E, Chincarini, G, Christensen, F, Cocchi, M, Comastri, A, Corsi, A, Cotroneo, V, Conconi, P, Colasanti, L, Cusumano, G, de Rosa, A, Del Santo, M, Ettori, S, Ezoe, Y, Ferrari, L, Feroci, M, Finger, M, Fishman, G, Fujimoto, R, Galeazzi, M, Galli, A, Gatti, F, Gehrels, N, Gendre, B, Ghirlanda, G, Ghisellini, G, Giommi, P, Girardi, M, Guzzo, L, Haardt, F, Hepburn, I, Hermsen, W, Hoevers, H, Holland, A, in't Zand, J, Ishisaki, Y, Kawahara, H, Kawai, N, Kaastra, J, Kippen, M, de Korte, Paj, Kouveliotou, C, Kusenko, A, Labanti, C, Lieu, R, Macculi, C, Makishima, K, Matt, Giorgio, Mazzotta, P, Mccammon, D, Mendez, M, Mineo, T, Mitchell, S, Mitsuda, K, Molendi, S, Moscardini, L, Mushotzky, R, Natalucci, L, Nicastro, F, O'Brien, P, Osborne, J, Paerels, F, Page, M, Paltani, S, Pareschi, G, Perinati, E, Perola, C, Ponman, T, Rasmussen, A, Roncarelli, M, Rosati, P, Ruchayskiy, O, Quadrini, E, Sakurai, I, Salvaterra, R, Sasaki, S, Sato, G, Schaye, J, Schmitt, J, Sciortino, S, Shaposhnikov, M, Shinozaki, K, Spiga, D, Suto, Y, Tagliaferri, G, Takahashi, T, Takei, Y, Tawara, Y, Tozzi, P, Tsunemi, H, Tsuru, T, Ubertini, P, Ursino, E, Viel, M, Vink, J, White, N, Willingale, R, Wijers, R, Yoshikawa, K, and Yamasaki, N.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

How structures of various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE (Piro et al., 2007) will trace the cosmic history of the baryons from the early generations of massive stars by Gamma-Ray Burst (GRB) explosions, through the period of galaxy cluster formation, down to the very low redshift Universe, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (the so-called warm hot intragalactic medium). In addition EDGE, with its unprecedented capabilities, will provide key results in many important fields. These scientific goals are feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities by: (a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution. This enables the study of their star-forming and host galaxy environments and the use of GRBs as back lights of large scale cosmological structures; (b) observing and surveying extended sources (galaxy clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution). The mission concept includes four main instruments: a Wide-field Spectrometer (0.1-2.2 eV) with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager (0.3-6 keV) with high angular resolution (HPD = 15") constant over the full 1.4 degree field of view, and a Wide Field Monitor (8-200 keV) with a FOV of A1/4 of the sky, which will trigger the fast repointing to the GRB. Extension of its energy response up to 1 MeV will be achieved with a GRB detector with no imaging capability. This mission is proposed to ESA as part of the Cosmic Vision call. We will outline the science drivers and describe in more detail the payload of this mission.

Published
2009

12. ASTRO-H White Paper - High Resolution Spectroscopy of Interstellar and Circumgalactic Gas in the Milky Way and Other Galaxies

Author

Paerels, F., Yamasaki, N., Anabuki, N., Costantini, E., de Vries, C., Fujimoto, R., Hornschemeier, A., Iizuka, R., Kilbourne, C., Konami, S., LaMassa, S., Loewenstein, M., McCammon, D., Matsushita, K., McNamara, B., Mitsuishi, I., Nagino, R., Nakagawa, T., Porter, S., Sakai, K., Smith, R. K., Takei, Y., Tsuru, T., Uchiyama, H., Yamaguchi, H., and Yamauchi, S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

We describe the potential of high resolution imaging spectroscopy with the SXS on ASTRO-H to advance our understanding of the interstellar- and circumgalactic media of our own Galaxy, and other galaxies. Topics to be addressed range from absorption spectroscopy of dust in the Galactic interstellar medium, to observations to constrain the total mass-, metal-, and energy flow out of starburst galaxies., Comment: 21 pages, 13 figures, ASTRO-H White Paper

Published
2014
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13. EDGE: Explorer of diffuse emission and gamma-ray burst explosions - art. no. 668805

Author

den Herder J. W., Piro L., Ohashi T., Amati L., Atteia J., Barthelmy S., Barbera M., Barret D., Basso S., Boer M., Borgani S., Boyarskiy O., BRANCHINI, ENZO FRANCO, Branduardi Raymont G., Briggs M., Brunetti G., Budtz Jorgensenf C., Burrows D., Campana S., Caroli E., Chincarini G., Christensen F., Cocchi M., Comastri A., Corsi A., Cotroneo V., Conconi P., Colasanti L., Cusumano G., de Rosa A., Del Santo M., Ettori S., Ezoe Y., Ferrari L., Feroci M., Finger M., Fishman G., Fujimoto R., Galeazzi M., Galli A., Gatti F., Gehrels N., Gendre B., Ghirlanda G., Ghisellini G., Giommi P., Girardi M., Guzzo L., Haardt F., Hepburn I., Hermsen W., Hoevers H., Holland A., Zand J. In't, Ishisaki Y., Kawahara H., Kawai N., Kaastra J., Kippen M., de Korte P. A. J., Kouveliotou C., Kusenko A., Labanti C., Lieu R., Macculi C., Makishima K., Matt G., Mazotta P., McCammon D., Mendez M., Mineo T., Mitchell S., Mitsuda K., Molendi S., Moscardini L., Mushotzky R., Natalucci L., Nicastro F., O'Brien P., Osborne J., Paerels F., Page M., Paltani S., Pareschi G., Perinati E., Perola C., Ponman T., Rasmussen A., Roncarelli M., Rosati P., Ruchayskiy O., Quadrini E., Sakurai I., Salvaterra R., Sasaki S., Sato G., Schaye J., Schmidtt J., Scioritino S., Shaposhnikov M., Shinozaki K., Spiga D., Suto Y., Tagliaferri G., Takahashi T., Takei Y., Tawara Y., Tozzi P., Tsunemi H., Tsuru T., Ubertini P., Ursino E., Viel M., Vink J., White N., Willingale R., Wijers R., Yoshikawa K., Yamasaki N., BE ODell SL, Pareschi G, RI White Nicholas/B 6428 2012 Barthelmy Scott/D 2943 2012 Gehrels Neil/D 2971 2012, den Herder, J. W., Piro, L., Ohashi, T., Amati, L., Atteia, J., Barthelmy, S., Barbera, M., Barret, D., Basso, S., Boer, M., Borgani, S., Boyarskiy, O., Branchini, ENZO FRANCO, Branduardi Raymont, G., Briggs, M., Brunetti, G., Budtz Jorgensenf, C., Burrows, D., Campana, S., Caroli, E., Chincarini, G., Christensen, F., Cocchi, M., Comastri, A., Corsi, A., Cotroneo, V., Conconi, P., Colasanti, L., Cusumano, G., de Rosa, A., Del Santo, M., Ettori, S., Ezoe, Y., Ferrari, L., Feroci, M., Finger, M., Fishman, G., Fujimoto, R., Galeazzi, M., Galli, A., Gatti, F., Gehrels, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Giommi, P., Girardi, M., Guzzo, L., Haardt, F., Hepburn, I., Hermsen, W., Hoevers, H., Holland, A., Zand J., In'T, Ishisaki, Y., Kawahara, H., Kawai, N., Kaastra, J., Kippen, M., de Korte, P. A. J., Kouveliotou, C., Kusenko, A., Labanti, C., Lieu, R., Macculi, C., Makishima, K., Matt, G., Mazotta, P., Mccammon, D., Mendez, M., Mineo, T., Mitchell, S., Mitsuda, K., Molendi, S., Moscardini, L., Mushotzky, R., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pareschi, G., Perinati, E., Perola, C., Ponman, T., Rasmussen, A., Roncarelli, M., Rosati, P., Ruchayskiy, O., Quadrini, E., Sakurai, I., Salvaterra, R., Sasaki, S., Sato, G., Schaye, J., Schmidtt, J., Scioritino, S., Shaposhnikov, M., Shinozaki, K., Spiga, D., Suto, Y., Tagliaferri, G., Takahashi, T., Takei, Y., Tawara, Y., Tozzi, P., Tsunemi, H., Tsuru, T., Ubertini, P., Ursino, E., Viel, M., Vink, J., White, N., Willingale, R., Wijers, R., Yoshikawa, K., Yamasaki, N., BE ODell, Sl, Pareschi, G, and RI White Nicholas/B 6428 2012 Barthelmy Scott/D 2943 2012 Gehrels Neil/D 2971, 2012

Published
2007

14. Possible non-thermal nature of the soft-excess emission in the cluster of galaxies Sersic 159-03

Author

Werner, N., Kaastra, J.S., Takei, Y., Lieu, R., Vink, J., Tamura, T., Astrophysics, Omgevingsrecht (t/m 2009), Dep Natuurkunde, Afdeling ISEP, and Sub High energy Astrophysics begr 1/1/15

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an analysis of new Suzaku data and archival data from XMM-Newton of the cluster of galaxies Sérsic 159-03, which has a strong soft X-ray excess emission component. The Suzaku observation confirms the presence of the soft excess emission, but it does not confirm the presence of redshifted Ovii lines in the cluster. Radial profiles and 2D maps derived from XMM-Newton observations show that the soft excess emission has a strong peak at the position of the central cD galaxy and the maps do not show any significant azimuthal variations. Although the soft excess emission can be fitted equally well with both thermal and nonthermal models, its spatial distribution is neither consistent with the models of intercluster warm-hot filaments, nor with models of clumpy warm intracluster gas associated with infalling groups. Using the data obtained by the XMM-Newton Reflection Grating Spectrometers we do not confirm the presence of the warm gas in the cluster centre with the expected properties assuming the soft excess is of thermal origin. The observed properties of the soft excess emission are consistent with the non-thermal interpretation. While the high density of relativistic electrons associated with the peak of the soft emission in the cluster centre might have been provided by an active galactic nucleus in the central cD galaxy, the underlying population might have been accelerated in diffuse shocks.

Published
2007

15. Pale-cell acanthosis

Author

Takei Y, Fukushiro S, and Ackerman Ab

Subjects
Adult, Male, endocrine system, Follicular mucinosis, Pathology, medicine.medical_specialty, Skin Neoplasms, Cell, Acanthosis, Dermatology, Epidermolytic hyperkeratosis, Epithelium, Pathology and Forensic Medicine, medicine, Humans, Nevus, Aged, Papilloma, integumentary system, business.industry, Keratosis, General Medicine, Middle Aged, medicine.disease, Acantholysis, medicine.anatomical_structure, Female, Acantholytic dyskeratosis, Epidermis, Warts, business, Clear cell
Abstract

Pale-cell acanthosis is a distinctive reaction of epidermal epithelium and is analogous to other epithelial reaction patterns such as epidermolytic hyperkeratosis, focal acantholytic dyskeratosis, cornoid lamellation, and follicular mucinosis.

Published
1985

17. Ionizing radiation sensor utilizing radiophotoluminescence in Ag +-activated phosphate glass and its application to environmental radiation monitoring

Author

Miyamoto, Y., Kinoshita, K., Kobayashi, H., Fujiwara, A., Koyama, S., Takei, Y., Nanto, H., Yamamoto, T., Kurobori, T., Takayuki Yanagida, Yoshikawa, A., Sakakura, M., Shimotsuma, Y., Miura, K., and Hirao, K.

Subjects
environmental radiation, glass dosemeter, Ag+-activated phosphate glass, femtosecond laser pulse, radiophotoluminescence, photoreduction

18. Search for Thermal X-ray Features from the Crab nebula with Hitomi Soft X-ray Spectrometer

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sato, T, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Tominaga, N, Moriya, Tj, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Hitomi, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], observational [methods], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kinetic energy, 01 natural sciences, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, ISM: individual (Crab nebula), 14. Life underwater, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, instrumentation: spectrographs, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectrometer, supernova remnants [ISM], Astronomy and Astrophysics, Plasma, Radius, Astrophysics - Astrophysics of Galaxies, Supernova, Crab Nebula, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), individual (Crab nebula) [ISM], methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 194名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 萩野, 浩一; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; 佐藤, 寿紀; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 194 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Sato, Toshiki; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-06-30, 資料番号: SA1170339000

19. Development of the multi-pixel x-ray microcalorimeters

Author

Kudo, H., Nakamura, T., Takahiro Arakawa, Ohtsuka, S., Izumi, T., Shoji, S., Sato, H., Kobayashi, H., Mori, K., Homma, T., Osaka, T., Mitsuda, K., Yamasaki, N. Y., Fujimoto, R., Iyomoto, N., Oshima, T., Futamoto, K., Takei, Y., Ichitsubo, T., Fujimori, T., Ishisaki, Y., Morita, U., Koga, T., Sato, K., Ohashi, T., Kuroda, Y., Onishi, M., and Otake, K.

20. Recent progress and future plan of heavy-ion radiotherapy facility, HIMAC

Author

Noda, K., Furukawa, T., Hara, Y., Inaniwa, T., Iwata, Y., Katagiri, K., Kanematsu, N., Kitagawa, A., Kota Mizushima, Mori, S., Murakami, T., Muramatsu, M., Nakao, M., Noda, A., Sato, S., Shirai, T., Takada, E., and Takei, Y.

Abstract

The carbon-ion radiotherapy (RT) with HIMAC has been conducted since 1994, and the accumulated treatment number exceeded 9,000 in May 2014. During the last two decades, NIRS has developed both the accelerator and beam-delivery technologies related to the carbon-ion RT, which has brought several carbon-ion RT facilities in Japan. At present, NIRS has developed a carbon-ion rotating gantry with the superconducting technology to be operated from 2016. As the future plan, NIRS has developed a direct acceleration system of positron-emission beams for verification on an irradiation field, and NIRS also just starts a design study of a superconducting synchrotron ring for carbon-ion RT.

26. Fast raster scanning system for HIMAC new treatment facility

Author

Furukawa, T., Inaniwa, T., Sato, S., Shirai, T., Takei, Y., Takeshita, E., Kota Mizushima, Iwata, Y., Himukai, T., Mori, S., Fukuda, S., Minohara, S., Murakami, T., and Noda, K.

Abstract

A new treatment facility project, as an extension of the existing HIMAC facility, has been initiated for the further development of carbon-ion therapy in NIRS. The challenge of this project is to realize treatment of a moving target by scanning irradiation. In order to realize this by rescanning with gating within an acceptable irradiation time, the development of a fast scanning system is required. To test the fast rescanning irradiation and to verify the design, a new scanning irradiation system was installed into existing HIMAC experiment course. The beam test of the fast scanning system was successfully carried out. In this paper, the performance of the fast scanning was demonstrated.

27. Clinical utility of transarterial infusion chemotherapy using cisplatin-lipiodol emulsion for unresectable hepatocellular carcinoma

Author

Beppu, T., Sugimoto, K., Shiraki, K., Tameda, M., Inagaki, Y., Ogura, S., Kasai, C., Kusagawa, S., Nojiri, K., Yoneda, M., Fuke, H., Yamamoto, N., Takei, Y., Masashi Fujimori, Hasegawa, T., Yamanaka, T., Uraki, J., Kashima, M., Takaki, H., Nakatsuka, A., Yamakado, K., and Takeda, K.

Subjects
Adult, Male, Carcinoma, Hepatocellular, Liver Neoplasms, Kaplan-Meier Estimate, Middle Aged, Ethiodized Oil, Treatment Outcome, Humans, Infusions, Intra-Arterial, Emulsions, Female, Cisplatin, Neoplasm Staging, Retrospective Studies
Abstract

We evaluated the clinical efficacy of transarterial infusion chemotherapy using a cisplatin-lipiodol emulsion for unresectable hepatocellular carcinoma (HCC).Fifty-seven patients with advanced HCC, with no indications for surgical resection or local ablative therapy, such as percutaneous ethanol injection and radiofrequency ablation, were enrolled in this retrospective study.Twelve patients were treated with cisplatin-alone at a dose of 65 mg/m(2) by infusion into the artery. Forty-two patients were treated with the same dose of cisplatin suspended in 1-10 ml of lipiodol (C/LPD). Cumulative survival rates in the cisplatin-treated group were 46.2% at one year, and 18.5% at two years, whereas these in the C/LPD group were 81.6% and 44.4%, respectively, with a significant difference between the two groups (p0.01). In the cisplatin-treated group (n=13), no (0%) patients had a complete response (CR), two (15%) a partial response (PR), three (23%) no change (NC), and eight (62%) progressive disease (PD). In the C/LPD group (n=44), four (9%) patients had CR, 16 (35%) PR, 12 (26%) NC, and 12 (26%) PD. CR and PR were seen in 15% of the cisplatin-treated group and in 44% of the C/LPD group. C/LPD was significantly more effective than cisplatin-alone (p=0.039). Some patients showed tumor response to C/LPD after intra-arterial infusion of low-dose 5-fluorouracil.C/LPD produced superior effects compared to cisplatin-alone for unresectable HCC, causing no major side-effects, and increasing the survival rate.

28. X-ray Spectroscopy of the Warm-Hot Intergalactic Medium

Author

Paerels, F., Den Herder, J. -W, Ohashi, T., Bautz, M., Bryan, G., Buote, D., Bykov, A., Canizares, C., Fang, T., Galeazzi, M., Kaastra, J., Nicastro, F., Putman, M., Rasmussen, A., Schattenburg, M., Joop Schaye, Schiminovich, D., Takei, Y., and Werner, N.

30. In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background

Author

Kilbourne, C. A., Sawada, M., Tsujimoto, M., Angellini, L., Boyce, K. R., Megan Eckart, Fujimoto, R., Ishisaki, Y., Kelley, R. L., Koyama, S., Leutenegger, M. A., Loewenstein, M., Mccammon, D., Mitsuda, K., Nakashima, S., Porter, F. S., Seta, H., Takei, Y., Tashiro, M. S., Terada, Y., Yamada, S., and Yamasaki, N. Y.

32. STUDYING THE WARM-HOT INTERGALACTIC MEDIUM IN EMISSION

Author

Ursino, E., Branchini, E., Piro, L., Corsi, A., Amati, L., Herder, J. W. den, Galeazzi, M., Kaastra, J., Moscardini, L., Nicastro, F., Paerels, F., Roncarelli, M., Viel, M., Takei, Yoh, Ohashi, Takaya, Kawahara, H., Mitsuda, Kazuhisa, Takei, Y., Ursino, E., Branchini, ENZO FRANCO, Ohashi, T., Kawahara, H., Mitsuda, K., Piro, L., Corsi, A., Amati, L., den Herder, J. W., Galeazzi, M., Kaastra, J., Moscardini, L., Nicastro, F., Paerels, F., Roncarelli, M., Viel, M., Takei Y., Ursino E., Branchini F., Ohashi T., Kawahara H., Mitsuda K., Piro L., Corsi A., Amati L., den Herder J.W., Galeazzi M., Kaastra J., Moscardini L., Nicastro F., Paerels F., Roncarelli M., Viel M., Astrophysics, Dep Natuurkunde, and Afd Astrophysics begr 1/1/17

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Warm–hot intergalactic medium, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, Spectral line, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, large-scale structure of universe, Physics, cosmology: observation, COSMIC cancer database, 010308 nuclear & particles physics, Detector, Astronomy and Astrophysics, cosmology: observations, intergalactic medium, X-rays: diffuse background, Space and Planetary Science, K-alpha, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 17名, Accepted: 2011-03-31, 資料番号: SA1002994000

Published
2011

33. Chandra View of the Warm-hot Intergalactic Medium toward 1ES 1553+113: Absorption-line Detections and Identifications. I

Author

Nicastro, F., Elvis, M., Krongold, Y., Mathur, S., Gupta, A., Danforth, C., Barcons, X., Borgani, S., Branchini, E., Cen, R., Dave, R., Kaastra, J., Paerels, F., Piro, L., Shull, J. M., Zappacosta, L., Takei, Yoh, Universidad de Cantabria, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, University of Colorado, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Nicastro, F., Elvis, M., Krongold, Y., Mathur, S., Gupta, A., Danforth, C., Barcons, X., Borgani, S., Branchini, ENZO FRANCO, Cen, R., Dave, R., Kaastra, J., Paerels, F., Piro, L., Shull, J. M., Takei, Y., Zappacosta, L., F., Nicastro, M., Elvi, Y., Krongold, S., Mathur, A., Gupta, C., Danforth, X., Barcon, Borgani, Stefano, E., Branchini, R., Cen, R., Davé, J., Kaastra, F., Paerel, L., Piro, J. M., Shull, Y., Takei, and L., Zappacosta

Subjects
Opacity, Absorption spectroscopy, media_common.quotation_subject, atomic processes, Astrophysics, X-rays: general, 01 natural sciences, Spectral line, general [X-rays], 0103 physical sciences, identification [Line], atomic processe, 010306 general physics, Blazar, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, media_common, Intergalactic medium, Physics, Sigma, intergalactic medium, line: identification, opacity, Astronomy and Astrophysics, opacity - X-rays: general, Atomic processes, Redshift, Baryon, Space and Planetary Science, Sky
Abstract

Nicastro et al., We present the first results from our pilot 500 ks Chandra Low Energy Transmission Grating Large Program observation of the soft X-ray brightest source in the z ≳ 0.4 sky, the blazar 1ES 1553+113, aimed to secure the first uncontroversial detections of the missing baryons in the X-rays. We identify a total of 11 possible absorption lines, with single-line statistical significances between 2.2σ and 4.1σ. Six of these lines are detected at high single-line statistical significance (3.6 ≤ σ ≤ 4.1), while the remaining five are regarded as marginal detections in association with either other X-ray lines detected at higher significance and/or far-ultraviolet (FUV) signposts. Three of these lines are consistent with metal absorption at z ≃ 0, and we identify them with Galactic O I and C II. The remaining eight lines may be imprinted by intervening absorbers and are all consistent with being high-ionization counterparts of FUV H I and/or O VI intergalactic medium signposts. In particular, five of these eight possible intervening absorption lines (single-line statistical significances of 4.1σ, 4.1σ, 3.9σ, 3.8σ, and 2.7σ), are identified as C V and C VI Kα absorbers belonging to three WHIM systems at zX = 0.312, z X = 0.237, and 〈zX 〉 = 0.133, which also produce broad H I (and O VI for the zX = 0.312 system) absorption in the FUV. For two of these systems (zX = 0.312 and 0.237), the Chandra X-ray data led the a posteriori discovery of physically consistent broad H I associations in the FUV (for the third system the opposite applies), so confirming the power of the X-ray-FUV synergy for WHIM studies. The true statistical significances of these three X-ray absorption systems, after properly accounting for the number of redshift trials, are 5.8σ (z X = 0.312; 6.3σ if the low-significance O V and C V Kβ associations are considered), 3.9σ (zX = 0.237), and 3.8σ (zX 〉 = 0.133), respectively. © 2013. The American Astronomical Society. All rights reserved., F.N. acknowledges support from Chandra Grant GO1-12174X, and from INAF-ASI ADAE Grant 1.05.04.13.15. M.S. and C.D. acknowledge support from COS Grant NNX08AC14G to the University of Colorado, from NASA. X.B. acknowledges support by the Spanish Ministry of Economy and Competitiveness through grant AYA2010-21490-C02-01.

Published
2013

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