9 results on '"Matsumoto, Hironori"'
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2. Inverse First Ionization Potential Effects in Giant Solar Flares Found from Earth X-Ray Albedo with Suzaku/XIS
- Author
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Beppu, Tatsuhiko, Kanemaru, Yoshiaki, Sato, Kosuke, Morita, Kae, Sagara, Hikari, Ogawa, Futa, Takahashi, Haruya, Nobukawa, Masayoshi, Matsumoto, Hironori, Nakajima, Hiroshi, Yokoyama, Takaaki, Katsuda, Satoru, Ohno, Masanori, Mori, Koji, Tashiro, Makoto S., Terada, Yukikatsu, Murakami, Hiroshi, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Noda, Hirofumi, Ezoe, Yuichiro, Tsuboi, Yohko, Maeda, Yoshitomo, and Narukage, Noriyuki
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Physics ,Solar x-ray emission (1536) ,Solar flare ,Solar abundances (1474) ,X-ray ,Inverse ,Astronomy and Astrophysics ,Astrophysics ,Albedo ,Solar flares (1496) ,Solar corona (1483) ,Space and Planetary Science ,Ionization energy ,Earth (classical element) ,Solar x-ray flares (1816) - Abstract
著者人数: 24名, Accepted: 2020-01-28, 資料番号: SA1190237000
- Published
- 2020
- Full Text
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3. $Hitomi$ constraints on the 3.5 keV line in the Perseus galaxy cluster
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Hitomi Collaboration, Aharonian, Felix A., Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Arnaud, Keith A., Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger D., Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hornschemeier, Ann E., Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Shota, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwai, Masachika, Iyomoto, Naoko, Kaastra, Jelle S., Kallman, Timothy, Kamae, Tuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kelley, Richard L., Khangulyan, Dmitry, Kilbourne, Caroline A., King, Ashley L., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Shu, Koyama, Katsuji, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, Francois, Lee, Shiu-Hang, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Grzegorz M., Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Moseley, Harvey, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve L., Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian D., Reynolds, Christopher S., Russell, Helen R., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew E., Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shin'ichiro, Urry, C. Meg, Ursino, Eugenio, de Vries, Cor P., Watanabe, Shin, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Zhuravleva, Irina, Zoghbi, Abderahmen, Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Hitomi, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
galaxies: clusters: individual ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,galaxies: clusters: intracluster medium ,clusters: individual: A426 [galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Dark matter ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,galaxies: clusters: individual (A426) ,01 natural sciences ,dark matter ,X-ray ,Settore FIS/05 - Astronomia e Astrofisica ,gas ,0103 physical sciences ,calorimeter ,Emission spectrum ,Spectroscopy ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,Line (formation) ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Nebula ,010308 nuclear & particles physics ,dark matter: decay ,Astronomy and Astrophysics ,charge exchange ,Astrophysics - Astrophysics of Galaxies ,K-line ,Galaxy ,flux ,Space and Planetary Science ,clusters: intracluster medium [galaxies] ,Astrophysics of Galaxies (astro-ph.GA) ,X-rays: galaxies: clusters ,galaxy: cluster ,galaxies: clusters [X-rays] ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,signature ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E=3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark-matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of Sxvi (E=3.44 keV rest-frame) -- a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment., Discussion of systematics significantly expanded. 9 pages, 5 figures; ApJ Lett. in press
- Published
- 2017
- Full Text
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4. Performance of the Charge-Injection Capability of Suzaku XIS
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Bautz, Mark W., Kissel, Steve E, Lamarr, Beverly, Prigozhin, Gregory Y., Nakajima, Hiroshi, Yamaguchi, Hiroya, Matsumoto, Hironori, Tsuru, Takeshi Go, Koyama, Katsuji, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Torii, Kenichi, Namiki, Masaaki, Katsuda, Satoru, Shoji, Masayuki, Matsuura, Daisuke, Miyauchi, Tomofumi, Dotani, Tadayasu, Ozaki, Masanobu, and Murakami, Hiroshi
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Physics ,business.industry ,Astrophysics (astro-ph) ,Astrophysics::Instrumentation and Methods for Astrophysics ,Imaging spectrometer ,FOS: Physical sciences ,Astronomy and Astrophysics ,Charge (physics) ,Astrophysics ,Radiation ,Spectral line ,Full width at half maximum ,Optics ,Space and Planetary Science ,Dispersion (optics) ,Calibration ,business ,Line (formation) - Abstract
著者人数：20名, Accepted: 2007-03-08, 資料番号: SA1000299000
- Published
- 2008
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5. X-ray Imaging Spectrometers (XIS) of Astro-E2
- Author
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Bautz, M. W., Doty, J. P., Ricker, G. R., Foster, R. F., Prigozhin, G. Y., Kissel, S. E., Burke, B. E., Pillsbury, A. D., LaMarr, B., Matsumoto, Hironori, Koyama, Katsuji, Tsuru, Takeshi G., Nakajima, Hiroshi, Yamaguchi, Hiroya, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Miyata, Emi, Torii, Ken'ichi, Namiki, Masaaki, Dotani, Tadayasu, Ozaki, Masanobu, Murakami, Hiroshi, Anabuki, Naohisa, Kitamoto, Shunji, Awaki, Hisamitsu, Kohmura, Takayoshi, Katayama, Haruyoshi, and Bamba, Aya
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Physics ,Nuclear and High Energy Physics ,Spectrometer ,Pixel ,business.industry ,X-ray ,Cosmic ray ,law.invention ,Telescope ,Optics ,law ,Calibration ,Optoelectronics ,Satellite ,Quantum efficiency ,business ,Instrumentation - Abstract
著者人数: 28名, 資料番号: SA1004000000
- Published
- 2005
6. Suzaku Reveals Helium-burning Products in the X-ray Emitting Planetary Nebula BD+303639
- Author
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Arnaud, K., Murashima, Mio, Kokubun, Motohide, Makishima, Kazuo, Kotoku, Junichi, Murakami, Hiroshi, Matsushita, Kyoko, Hayashida, Kiyoshi, Hamaguchi, Kenji, and Matsumoto, Hironori
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Physics ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,X-ray ,Imaging spectrometer ,FOS: Physical sciences ,chemistry.chemical_element ,Astronomy and Astrophysics ,Astrophysics ,Planetary nebula ,chemistry ,Space and Planetary Science ,Observatory ,Astrophysics::Solar and Stellar Astrophysics ,Helium ,Astrophysics::Galaxy Astrophysics - Abstract
BD+303639, the brightest planetary nebula at X-ray energies, was observed with Suzaku, an X-ray observatory launched on 2005 July 10. Using the X-ray Imaging Spectrometer, the K-lines from C VI, O VII, and O VIII were resolved for the first time, and C/O, N/O, and Ne/O abundance ratios determined. The C/O and Ne/O abundance ratios exceed the solar value by a factor of at least 30 and 5, respectively. These results indicate that the X-rays are emitted mainly by helium shell-burning products., 12 pages, 4 figures, accepted for publication in The Astrophysical Journal Letters
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- 2006
7. ASCA observation of M 87.
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Beig, R., Ehlers, J., Frisch, U., Hepp, K., Jaffe, R. L., Kippenhahn, R., Ojima, I., Weidenmüller, H. A., Wess, J., Zittartz, J., Beiglböck, W., Röser, Hermann-Josef, Meisenheimer, Klaus, and Matsumoto, Hironori
- Abstract
We present the ASCA results of spatially resolved X-ray spectra in the central regions of the Virgo cluster, near to the central elliptical galaxy M 87 and 40′ northwest of M 87 (M 87 NW). Since the spectra of the M 87 region is complex, an adequate fit requires at least two thin thermal-plasma components. The temperatures of the hot and cool components are approximately 3.0 and 1.3 keV, respectively, and the temperature of these components are both nearly constant over the central 10′ radius from the center of M 87. The spectrum of M 87NW, on the other hand, can be well fitted by a single thin thermal-plasma model of ∼ 2.7 keV temperature. The abundances of Fe, Si, and S rise towards the center of M 87, though the ratios of Si/Fe and S/Si remain constant. We also found, contrary to the Einstein results, that the abundance ratio of oxygen to iron (O/Fe) is smaller than the solar value. We found no strong nuclear activity from M 87. [ABSTRACT FROM AUTHOR]
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- 1999
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8. The X-ray observatory Suzaku
- Author
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Bautz, Mark, Kelley, Richard L., Petre, Robert, Figueroa, Enectali, Soong, Yang, Gendreau, Keith, Griffiths, Richard E., Harrus, Ilana, White, Nicholas E., Hasinger, Gunther, Henry, Patrick J., Holt, Stephen S., Hornschemeier, Ann, Hughes, John P., Hwang, Una, Smith, Randall, Kahn, Steven M., Kilbourne, Caroline, Kissel, Steve, Szymkowiak, Andrew E., Madejski, Greg M., Markowitz, Alex, Matsumoto, Chiho, Matsumoto, Hironori, Mccammon, Dan, Moseley, Harvey, Mushotzky, Richard, Nousek, John A., Chan, Kai-Wing, Ozawa, Hideki, Parmer, Arvind N., Pence, William D., Turner, Martin J. L., Angelini, Lorella, Arnaud, Keith, Boyce, Kevin, Brown, Gregory V., Porter, F. Scott, Cottam, Jean, Reeves, James N., Ricker, George R., Doty, John, Sanders, Wilton T., Fabian, Andrew C., Serlemitsos, Peter, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tomida, Hiroshi, Torii, Ken'ichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsuru, Takeshi Go, Ueda, Yoshihiro, Ueno, Shiro, Ueno, Masaru, Uno, Shin'ichiro, Urata, Yuji, Watanabe, Shin, Yamamoto, Norimasa, Ishida, Manabu, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Ishisaki, Yoshitaka, Isobe, Naoki, Itoh, Masayuki, Iyomoto, Naoko, Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Mitsuda, Kazuhisa, Inoue, Hajime, Katayama, Haruyoshi, Koyama, Katsuji, Kunieda, Hideyo, Makishima, Kazuo, Ogawara, Yoshiaki, Takahashi, Tadayuki, Tsunemi, Hiroshi, Anabuki, Naohisa, Kawai, Nobuyuki, Awaki, Hisamitsu, Bamba, Aya, Dotani, Tadayasu, Ebisawa, Ken, Ezoe, Yuichiro, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furusho, Tae, Furuzawa, Akihiro, Kinugasa, Kenzo, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashida, Kiyoshi, Hiraga, Junko S., Kitamoto, Shunji, Kohama, Mitsuhiro, Kohmura, Takayoshi, Kokubun, Motohide, Kotani, Taro, Kotoku, Jun'ichi, Kubota, Aya, Maeda, Yoshitomo, Makino, Fumiyoshi, Matsuoka, Masaru, Matsushita, Kyoko, Mihara, Tatehiko, Misaki, Kazutami, Miyata, Emi, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Morii, Mikio, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Nagase, Fumiaki, Namiki, Masaaki, Negoro, Hitoshi, Nakazawa, Kazuhiro, Okajima, Takashi, Ogasaka, Yasushi, Ohashi, Takaya, Oshima, Tai, Ota, Naomi, Ozaki, Masanobu, Sakurai, Ikuya, Senda, Atsushi, Shibata, Ryo, Suzuki, Motoko, Takahashi, Hiromitsu, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, and Tanaka, Yasuo
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Physics ,Scientific instrument ,instrumentation ,Spacecraft ,business.industry ,Astrophysics::High Energy Astrophysical Phenomena ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,X-rays: general ,Space and Planetary Science ,Observatory ,space vehicles ,space vehicles: instruments ,business - Abstract
著者人数: 143名, Accepted: 2006-09-27, 資料番号: SA1000631000
9. X-Ray Evidence of an AGN in the Starburst Galaxy M82.
- Author
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Kaper, Lex, Heuvel, Edward P. J. van den, Woudt, Patrick A., Tsuru, Takeshi G., and Matsumoto, Hironori
- Abstract
The X-ray spectrum of the famous starburst galaxy M82 consists of three components: soft, medium, and hard (Tsuru et al. 1997). We conducted a monitoring observation with ASCA in 1996. Although the X-ray flux of the soft and medium components remained constant, a significant time variability of the hard component was found between 3 x 1040 erg s-1 and 1 x 1041 erg s-1 at various time scales from 3 ks to one month. The spectrum of the variable source obtained by subtracting the spectrum of the lowest state from the highest state suggests strong absorption of $N_H \sim 10^{22}$ cm2, which means a variable source is embedded in the center of M82. These observations suggest existence of a LLAGN in M82. [ABSTRACT FROM AUTHOR]
- Published
- 2001
- Full Text
- View/download PDF
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