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8 results on '"Hiraga, Junko S"'

1. Radiation hardness of a p-channel notch CCD developed for the X-ray CCD camera onboard the XRISM satellite

Author

Nishioka, Y., Takeda, A., Iwagaki, J., Okon, H., Shimoi, T., Hamano, T., Kanemaru, Y., Sato, J., Mori, Koji, Nakajima, Hiroshi, Hayashida, Kiyoshi, Matsumoto, Hironori, Okazaki, K., Asakura, K., Yoneyama, T., Uchida, Hiroyuki, Tanaka, Takaaki, Tsuru, Takeshi G., Tomida, Hiroshi, Kohmura, Takayoshi, Hagino, Kouichi, Murakami, Hiroshi, Kobayashi, Shogo B., Yamauchi, Makoto, Hatsukade, Isamu, Nobukawa, Masayoshi, Nobukawa, Kumiko K., Hiraga, Junko S., Uchiyama, Hideki, Yamaoka, Kazutaka, Ozaki, Masanobu, Dotani, Tadayasu, and Tsunemi, Hiroshi

Subjects
Materials science, Physics - Instrumentation and Detectors, Proton, Channel (digital image), FOS: Physical sciences, Radiation, 01 natural sciences, Fluence, Signal, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Optics, 0103 physical sciences, Instrumentation, Radiation hardening, Instrumentation and Methods for Astrophysics (astro-ph.IM), Mathematical Physics, Radiation damage to detector materials (solid state), 010308 nuclear & particles physics, business.industry, X-ray, Instrumentation and Detectors (physics.ins-det), X-ray detectors and telescopes, Satellite, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

著者人数: 33名, Accepted: 2019-03-26, 資料番号: SA1190034000

Published
2019
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2. Hitomi Observation of Radio Galaxy NGC 1275: The First X-ray Microcalorimeter Spectroscopy of Fe-K�� Line Emission from an Active Galactic Nucleus

Author

Hitomi Collaboration, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger, Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P., 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 M., Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S., Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L., Kilbourne, Caroline A., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier O., Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, 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, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, St��phane, Petre, Robert, Pinto, Ciro, Porter, Frederick S., Pottschmidt, Katja, Reynolds, Christopher S., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, 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, ��ukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin'ichiro, Urry, C. Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, 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, Zhuravleva, Irina, Zoghbi, Abderahmen, and Kawamuro, Taiki

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

The origin of the narrow Fe-K�� fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In February-March 2016, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) onboard the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high energy resolution of ~5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-K�� line with ~5.4 �� significance. The velocity width is constrained to be 500-1600 km s$^{-1}$ (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to ~20 keV, giving an equivalent width ~20 eV of the 6.4 keV line. Because the velocity width is narrower than that of broad H�� line of ~2750 km s$^{-1}$, we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-K�� line comes from a region within ~1.6 kpc from the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-K�� line from NGC 1275 is likely a low-covering fraction molecular torus or a rotating molecular disk which probably extends from a pc to hundreds pc scale in the active galactic nucleus system., 20 pages, 8 figures, 6 tables, accepted for publication in PASJ

Published
2017
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3. X-Ray Spectroscopy of SN 1006 with Suzaku

Author

Hughes, John P., Yamaguchi, Hiroya, Koyama, Katsuji, Katsuda, Satoru, Nakajima, Hiroshi, Bamba, Aya, Hiraga, Junko S., Mori, Koji, Ozaki, Masanobu, and Tsuru, Takeshi Go

Subjects
Physics, X-ray spectroscopy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Shock (mechanics), Interstellar medium, Space and Planetary Science, Ionization, Thermal, Electron temperature, Ejecta, Astrophysics::Galaxy Astrophysics
Abstract

We report on observations of SN 1006 with the X-ray Imaging Spectrometers (XIS) on board Suzaku. We firmly detected K-shell emission from Fe, for the first time, and find that the Fe ionization state is quite low. The broad band spectrum extracted from the southeast of the remnant is well fitted with a model consisting of three optically thin thermal non-equilibrium ionization plasmas and a power-law component. Two of the thermal models are highly overabundant in heavy elements and, hence, are likely due to ejecta. These components have different ionization parameters: $n_et \sim 1.4\times 10^{10}$ cm$^{-3}$ s and $n_et \sim 7.7\times 10^8$ cm$^{-3}$ s and it is the later one that produces the Fe-K emission. This suggests that Fe has been heated by the reverse shock more recently than the other elements, consistent with a picture where the ejecta are stratified by composition with Fe in the interior. On the other hand, the third thermal component is assumed to be solar abundance, and we associate it with emission from the interstellar medium (ISM). The electron temperature and ionization parameter are $kT_e \sim $0.5 keV and $n_et \sim 5.8\times 10^9$ cm$^{-3}$ s. The electron temperature is lower than that expected from the shock velocity which suggests a lack of collisionless electron heating at the forward shock. The extremely low ionization parameter and extreme non-equilibrium state are due to the low density of the ambient medium., 12 pages, 9 figures (14 figure files), accepted for publication in PASJ

Published
2008
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4. Suzaku Observations of the old pulsar wind nebula candidate HESS J1356-645

Author

Izawa, Masaharu, Dotani, Tadayasu, Fujinaga, Takahisa, Bamba, Aya, Ozaki, Masanobu, and Hiraga, Junko S.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: individual objects (HESS J1356-645, PSR J1357-6429), Pulsar wind nebula, X-rays: ISM, Pulsar, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

A largely extended X-ray emission was discovered around the pulsar PSR J1357-6429 with the Suzaku deep observations. The pulsar, whose characteristic age is 7.3 kyr, is located within the TeV gamma-ray source HESS J1356-645. The extended emission is found to have a 1sigma X-ray size of ~4 arcmin, or ~3 pc at 2.4 kpc, with a small offset from the pulsar. Its X-ray spectrum is well reproduced by a simple power-law model with a photon index of 1.70+0.07-0.06. No significant spatial variation was found for the X-ray photon index as a function of distance from the pulsar. We conclude that the extended emission is associated to the pulsar wind nebula of PSR J1357-6429. This is a new sample of largely extended nebulae around middle-aged pulsars. We discuss the evolution of this PWN according to the relic PWN scenario., Comment: 13 pages, 7 figures, PASJ, accepted

Published
2015
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5. A Study of Active Shielding Optimized for 1-80 keV Wide-Band X-ray Detector in Space

Author

Furuta, Yoshihiro, Murota, Yuki, Hiraga, Junko S., Sasano, Makoto, Murakami, Hiroaki, and Nakazawa, Kazuhiro

Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Active shielding is an effective technique to reduce background signals in hard X-ray detectors and to enable observing darker sources with high sensitivity in space. Usually the main detector is covered with some shield detectors made of scintillator crystals such as BGO (Bi$_4$Ge$_3$O$_{12}$), and the background signals are filtered out using anti-coincidence among them. Japanese X-ray observing satellites "Suzaku" and "ASTRO-H" employed this technique in their hard X-ray instruments observing at > 10 keV. In the next generation X-ray satellites, such as the NGHXT proposal, a single hybrid detector is expected to cover both soft (1-10 keV) and hard (> 10 keV) X-rays for effectiveness. However, present active shielding is not optimized for the soft X-ray band, 1-10 keV. For example, Bi and Ge, which are contained in BGO, have their fluorescence emission lines around 10 keV. These lines appear in the background spectra obtained by ASTRO-H Hard X-ray Imager, which are non-negligible in its observation energy band of 5-80 keV. We are now optimizing the design of active shields for both soft and hard X-rays at the same time. As a first step, we utilized a BGO crystal as a default material, and measured the L lines of Bi and K lines of Ge from it using the X-ray SOIPIX, "XRPIX"., 6 pages, 6 figures, Proceedings of International Workshop on SOI Pixel Detector (SOIPIX2015), Tohoku University, Sendai, Japan, 3-6, June, 2015. C15-06-03

Published
2015
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6. Spectral properties of nonthermal X-ray emission from the shell-type SNR RX J1713.7-3946 as revealed by XMM-Newton

Author

Aharonian, F. A., Hiraga, Junko S., Uchiyama, Yasunobu, and Takahashi, Tadayuki

Subjects
Physics, Photon, Molecular cloud, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Shell (structure), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, law.invention, Telescope, Space and Planetary Science, law, Electron temperature, Supernova remnant, Astrophysics::Galaxy Astrophysics
Abstract

We present the results of our morphological and spectral study of properties of the supernova remnant RX J1713.7-3946 based on data obtained with XMM-Newton. Highly inhomogeneous structures, such as the bright spots, filaments and dark voids, noted by Uchiyama et al. (2003), appear in the entire bright western portion of the shell. In addition two narrow rims are found which run parallel to each other from north to south in the western part of the remnant. No complex structures are seen in the interior region of the remnant. The X-ray spectra everywhere can be well represented with a power-law function of photon index ranging within Gamma = 2.0-2.8. A clear difference of spectra between the central dim region and the bright western portion is seen at lower energies. This differences can be ascribed either to an additional thermal component with electron temperature, kTe= 0.56keV from the center or, alternatively, to an increase in column density of Delta NH ~ 0.3 x 10^22 cm^-2 in the western region. In the context of the recent discovery by the NANTEN telescope of a molecular cloud apparently interacting with the western part of the supernova remnant, the second possibility seems to be the more likely scenario., Comment: 10 pages, 9 figures. Accepted for publication in Astronomy and Astrophysics

Published
2004
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7. The X-ray observatory Suzaku

Author

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

Subjects
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

8. Suzaku wide-band observations of SN 1006

Author

Hughes, John P., Petre, Rob, Bamba, Aya, Fukazawa, Yasushi, Hiraga, Junko S., Katagiri, Hideaki, Kokubun, Motohide, Koyama, Katsuji, Miyata, Emi, Mizuno, Tsunefumi, Mori, Koji, Nakajima, Hiroshi, Ozaki, Masanobu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Tanaka, Takaaki, Terada, Yukikatsu, Uchiyama, Yasunobu, Watanabe, Shin, and Yamaguchi, Hiroya

Subjects
Physics, Space and Planetary Science, Detector, Thermal, Astrophysics (astro-ph), Flux, Spectral response, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Wide band, Spectral line
Abstract

著者人数: 20名, Accepted: 2007-07-27, 資料番号: SA1000037000

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