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669 results on '"Terashima, Yuichi"'

201. X-ray study of Compton-thick AGNs with Suzaku

Author

粟木, 久光, Awaki, Hisamitsu, 寺島, 雄一, Terashima, Yuichi, 檜垣, 裕介, Higaki, Yusuke, 米谷, 哲明, Yonetani, Tetsuaki, 上田, 佳宏, Ueda, Yoshihiro, 粟木, 久光, Awaki, Hisamitsu, 寺島, 雄一, Terashima, Yuichi, 檜垣, 裕介, Higaki, Yusuke, 米谷, 哲明, Yonetani, Tetsuaki, 上田, 佳宏, and Ueda, Yoshihiro

Abstract

We have obtained broad-band spectra of 11 Compton-thick Seyfert 2 galaxies with Suzaku. The spectra are well represented by a three component model, consisting of a soft component, an absorbed power-law component, and a reflection component, accompanied by both a strong iron Kalpha line and several weak lines. Fixing the photon indices of the power law and the reflection components at 1.9, we obtain the column density N(sub H) and the intrinsic X-ray luminosity in the 2 - 10 keV band. We update the N(sub H) distribution of the bright [OIII] sample by Risaliti et al. (1999), and find that observed luminosities of Compton thick AGNs are only 1-10% of the intrinsic luminosities in the 2 - 10 keV band. This is consistent with small ratios of L(sub X)/L(sub [OIII]) of Compton thick AGNs., Meeting Information: The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science

Published
2015

202. Wide-Band Spectroscopy of the Compton Thick Seyfert 2 Galaxy Markarian 3 with Suzaku

Author

Awaki, Hisamitsu, Anabuki, Naohisa, Fukazawa, Yasushi, Gallo, Luigi C., Ikeda, Shinya, Isobe, Naoki, Itoh, Takeshi, Kunieda, Hideyo, Makishima, Kazuo, Markowitz, Alex, Miniutti, Giovanni, Mizuno, Tsunefumi, Okajima, Takashi, Ptak, Andrew, Reeves, James N., Takahashi, Tadayuki, Terashima, Yuichi, Yaqoob, Tahir, 粟木, 久光, 穴吹, 直久, 深沢, 泰司, 池田, 真也, 磯部, 直樹, 伊藤, 健, 國枝, 秀世, 牧島, 一夫, 水野, 恒史, 岡島, 崇, 高橋, 忠幸, 寺島, 雄一, Awaki, Hisamitsu, Anabuki, Naohisa, Fukazawa, Yasushi, Gallo, Luigi C., Ikeda, Shinya, Isobe, Naoki, Itoh, Takeshi, Kunieda, Hideyo, Makishima, Kazuo, Markowitz, Alex, Miniutti, Giovanni, Mizuno, Tsunefumi, Okajima, Takashi, Ptak, Andrew, Reeves, James N., Takahashi, Tadayuki, Terashima, Yuichi, Yaqoob, Tahir, 粟木, 久光, 穴吹, 直久, 深沢, 泰司, 池田, 真也, 磯部, 直樹, 伊藤, 健, 國枝, 秀世, 牧島, 一夫, 水野, 恒史, 岡島, 崇, 高橋, 忠幸, and 寺島, 雄一

Abstract

著者人数: 18名, Accepted: 2007-07-11

Published
2015

203. Deconstructing NGC 7130

Author

Levenson, N. A., Weaver, K. A., Heckman, T. M., 粟木, 久光, 寺島, 雄一, Awaki, Hisamitsu, Terashima, Yuichi, Levenson, N. A., Weaver, K. A., Heckman, T. M., 粟木, 久光, 寺島, 雄一, Awaki, Hisamitsu, and Terashima, Yuichi

Abstract

Accepted: 2004-09-09

Published
2015

204. Mid- and Far-Infrared Properties of a Complete Sample of Local Active Galactic Nuclei

Author

市川, 幸平, 上田, 佳宏, 寺島, 雄一, 大藪, 進喜, Gandhi, Poshak, 松田, 桂子, 中川, 貴雄, Ichikawa, Kohei, Ueda, Yoshihiro, Terashima, Yuichi, Oyabu, Shinki, Matsuta, Keiko, Nakagawa, Takao, 市川, 幸平, 上田, 佳宏, 寺島, 雄一, 大藪, 進喜, Gandhi, Poshak, 松田, 桂子, 中川, 貴雄, Ichikawa, Kohei, Ueda, Yoshihiro, Terashima, Yuichi, Oyabu, Shinki, Matsuta, Keiko, and Nakagawa, Takao

Abstract

Accepted: 2012-05-07

Published
2015

207. Submillimeter ALMA Observations of the Dense Gas in the Low-Luminosity Type-1 Active Nucleus of NGC 1097

Author

泉, 拓磨, 河野, 孝太郎, Martin, Sergio, Espada, Daniel, 原田, ななせ, 松下, 聡樹, Hsieh, Pei-Ying, Turner, Jean L., Meier, David S., Schinnerer, Eva, 今西, 昌俊, 田村, 陽一, Curran, Max T., 土居, 明広, Fathi, Kambiz, Krips, Melanie, Lundgren, Andreas A., 中井, 直正, 中島, 拓, Regan, Michael W., Sheth, Kartik, 高野, 秀路, 谷口, 暁星, 寺島, 雄一, 濤崎, 智佳, Wiklind, Tommy, Izumi, Takuma, Kohno, Kotaro, Harada, Nanase, Matsushita, Satoki, Imanishi, Masatoshi, Tamura, Yoichi, Doi, Akihiro, Nakai, Naomasa, Nakajima, Taku, Takano, Shuro, Taniguchi, Akio, Terashima, Yuichi, Tosaki, Tomoka, 泉, 拓磨, 河野, 孝太郎, Martin, Sergio, Espada, Daniel, 原田, ななせ, 松下, 聡樹, Hsieh, Pei-Ying, Turner, Jean L., Meier, David S., Schinnerer, Eva, 今西, 昌俊, 田村, 陽一, Curran, Max T., 土居, 明広, Fathi, Kambiz, Krips, Melanie, Lundgren, Andreas A., 中井, 直正, 中島, 拓, Regan, Michael W., Sheth, Kartik, 高野, 秀路, 谷口, 暁星, 寺島, 雄一, 濤崎, 智佳, Wiklind, Tommy, Izumi, Takuma, Kohno, Kotaro, Harada, Nanase, Matsushita, Satoki, Imanishi, Masatoshi, Tamura, Yoichi, Doi, Akihiro, Nakai, Naomasa, Nakajima, Taku, Takano, Shuro, Taniguchi, Akio, Terashima, Yuichi, and Tosaki, Tomoka

Abstract

著者人数: 26名, Accepted: 2013-06-01

Published
2015

208. Detection of the 'Active' Nucleus of M32

Author

Ho, Luis C., 寺島, 雄一, Ulvestad, James S., Terashima, Yuichi, Ho, Luis C., 寺島, 雄一, Ulvestad, James S., and Terashima, Yuichi

Abstract

Accepted: 2003-02-05

Published
2015

209. Reflection-Dominated Nuclear X-Ray Emission in the Early-Type Galaxy ESO 565-G019

Author

Gandhi, Poshak, 寺島, 雄一, 山田, 真也, Mushotzky, R. F., 上田, 佳宏, Baumgartner, W. H., Alexander, D. M., Malzac, J., Vaghmare, K., 高橋, 忠幸, Done, C., Terashima, Yuichi, Yamada, Shinya, Ueda, Yoshihiro, Takahashi, Tadayuki, Gandhi, Poshak, 寺島, 雄一, 山田, 真也, Mushotzky, R. F., 上田, 佳宏, Baumgartner, W. H., Alexander, D. M., Malzac, J., Vaghmare, K., 高橋, 忠幸, Done, C., Terashima, Yuichi, Yamada, Shinya, Ueda, Yoshihiro, and Takahashi, Tadayuki

Abstract

著者人数: 11名, Accepted: 2013-05-21

Published
2015

211. ALMA OBSERVATIONS OF THE SUBMILLIMETER DENSE MOLECULAR GAS TRACERS IN THE LUMINOUS TYPE-1 ACTIVE NUCLEUS OF NGC 7469

Author

Izumi, Takuma, primary, Kohno, Kotaro, additional, Aalto, Susanne, additional, Doi, Akihiro, additional, Espada, Daniel, additional, Fathi, Kambiz, additional, Harada, Nanase, additional, Hatsukade, Bunyo, additional, Hattori, Takashi, additional, Hsieh, Pei-Ying, additional, Ikarashi, Soh, additional, Imanishi, Masatoshi, additional, Iono, Daisuke, additional, Ishizuki, Sumio, additional, Krips, Melanie, additional, Martín, Sergio, additional, Matsushita, Satoki, additional, Meier, David S., additional, Nagai, Hiroshi, additional, Nakai, Naomasa, additional, Nakajima, Taku, additional, Nakanishi, Kouichiro, additional, Nomura, Hideko, additional, Regan, Michael W., additional, Schinnerer, Eva, additional, Sheth, Kartik, additional, Takano, Shuro, additional, Tamura, Yoichi, additional, Terashima, Yuichi, additional, Tosaki, Tomoka, additional, Turner, Jean L., additional, Umehata, Hideki, additional, and Wiklind, Tommy, additional

Published
2015
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212. Hyper-luminous dust-obscured galaxies discovered by the Hyper Suprime-Cam on Subaru and WISE

Author

Toba, Yoshiki, primary, Nagao, Tohru, additional, Strauss, Michael A., additional, Aoki, Kentaro, additional, Goto, Tomotsugu, additional, Imanishi, Masatoshi, additional, Kawaguchi, Toshihiro, additional, Terashima, Yuichi, additional, Ueda, Yoshihiro, additional, Bosch, James, additional, Bundy, Kevin, additional, Doi, Yoshiyuki, additional, Inami, Hanae, additional, Komiyama, Yutaka, additional, Lupton, Robert H., additional, Matsuhara, Hideo, additional, Matsuoka, Yoshiki, additional, Miyazaki, Satoshi, additional, Morokuma, Tomoki, additional, Nakata, Fumiaki, additional, Oi, Nagisa, additional, Onoue, Masafusa, additional, Oyabu, Shinki, additional, Price, Paul, additional, Tait, Philip J., additional, Takata, Tadafumi, additional, Tanaka, Manobu M., additional, Terai, Tsuyoshi, additional, Turner, Edwin L., additional, Uchida, Tomohisa, additional, Usuda, Tomonori, additional, Utsumi, Yousuke, additional, Yamada, Yoshihiko, additional, and Wang, Shiang-Yu, additional

Published
2015
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213. LOCAL INSTABILITY SIGNATURES IN ALMA OBSERVATIONS OF DENSE GAS IN NGC 7469

Author

Fathi, Kambiz, primary, Izumi, Takuma, additional, Romeo, Alessandro B., additional, Martín, Sergio, additional, Imanishi, Masatoshi, additional, Hatziminaoglou, Evanthia, additional, Aalto, Susanne, additional, Espada, Daniel, additional, Kohno, Kotaro, additional, Krips, Melanie, additional, Matsushita, Satoki, additional, Meier, David S., additional, Nakai, Naomasa, additional, and Terashima, Yuichi, additional

Published
2015
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215. X-Ray Spectral Variability of the Seyfert Galaxy NGC 4051 Observed with Suzaku

Author

Gallo, Luigi C., Markowitz, Alex G., Reeves, James N., Fabian, Andrew C., Griffiths, Richard E., Miniutti, Giovanni, Terashima, Yuichi, Inoue, Hirohiko, Anabuki, Naohisa, Hayashida, Kiyoshi, Itoh, Takeshi, Kokubun, Motohide, Kubota, Aya, Takahashi, Tadayuki, Yamauchi, Makoto, Yonetoku, Daisuke, APC - Astrophysique des Hautes Energies (APC - AHE), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Lantz, Simone, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), 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)-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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Gaussian, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Ionization, 0103 physical sciences, Black-body radiation, Emission spectrum, 010303 astronomy & astrophysics, Physics, [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galaxy, X-rays: galaxies, Amplitude, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: individual (NGC 4051), symbols, Equivalent width
Abstract

We report results from a Suzaku observation of the narrow-line Seyfert 1 NGC 4051. During our observation, large amplitude rapid variability is seen and the averaged 2--10 keV flux is 8.1x10^-12 erg s^-1 cm^-2, which is several times lower than the historical average. The X-ray spectrum hardens when the source flux becomes lower, confirming the trend of spectral variability known for many Seyfert 1 galaxies. The broad-band averaged spectrum and spectra in high and low flux intervals are analyzed. The spectra are first fitted with a model consisting of a power-law component, a reflection continuum originating in cold matter, a blackbody component, two zones of ionized absorber, and several Gaussian emission lines. The amount of reflection is rather large (R ~ 7, where R=1 corresponds to reflection by an infinite slab), while the equivalent width of the Fe-K line at 6.4 keV is modest (140 eV) for the averaged spectrum. We then model the overall spectra by introducing partial covering for the power-law component and reflection continuum independently. The column density for the former is 1x10^23 cm^-2, while it is fixed at 1x10^24 cm-2 for the latter. By comparing the spectra in different flux states, we identify the causes of spectral variability. (abridged), 19 pages, 18 figures, accepted for publication in PASJ (Suzaku 3rd special issue)

Published
2008

216. 「すざく」衛星による2型セイファート銀河の観測

Author

Awaki, Hisamitu, Terashima, Yuichi, Fukazawa, Yasushi, Ito, Takeshi, Ueda, Yoshihiro, and Suzaku, Team et al.

Abstract

第8回宇宙科学シンポジウム (2008年1月8日-9日. 宇宙航空研究開発機構宇宙科学研究本部(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 8ｔh Space Science Symposium (January 8-9, 2008. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000056131, レポート番号: P4-8

Published
2008

217. Development of command plan generation system for the Suzaku satellite

Author

Terashima, Yuichi and Suzaku Operation Team, Institute of Space and Astronautical Science, JAXA

Subjects
観測データベース, programming environment, observation, command and control, ORL, スケジューリング, 指令と制御, programming language, コマンド計画, 衛星制御, Observation Data Base, プログラミング言語, 観測, command plan, computer program, すざく, satellite control, プログラミング環境, scheduling, 計算機プログラム, Operation Request Language, Suzaku
Abstract

X線天文衛星「すざく」は公募によって選ばれた観測対象の観測を続けている。観測を進めるために必要な衛星のコマンド計画は、宇宙航空研究開発機構宇宙科学研究本部で作成し、内之浦宇宙空間観測所から衛星に対して送信する。我々はこのような日々の観測を容易かつ確実に行うための、コマンド計画作成システムを開発した。システムの詳細、これまでの衛星の運用の経緯とともに、今後のコマンド作成システムヘの展望を述べる。, The X-ray observatory Suzaku observes celestial objects according to a list of targets selected by a peer review process. Command plans to conduct the observations are made at ISAS/JAXA and sent to the satellite from the tracking station in Uchinoura Space Center (USC). We developed a command plan generation system, which allows us to prepare daily plans easily and reliably. Details of the system, status of satellite operations, and future prospects are discussed., 資料番号: AA0063227000, レポート番号: JAXA-RM-06-006

Published
2007

218. Suzaku observation of IRAS 00521-7054, a peculiar type-II AGN with a very broad feature at 6 keV

Author

Ricci, Claudio, Tazaki, Fumie, Ueda, Yoshihiro, Paltani, Stephane, Boissay, Rozenn, Terashima, Yuichi, Ricci, Claudio, Tazaki, Fumie, Ueda, Yoshihiro, Paltani, Stephane, Boissay, Rozenn, and Terashima, Yuichi

Abstract

IRAS 00521$-$7054 is the first Seyfert 2 in which the presence of an extremely large Fe K$\alpha$ line has been claimed. We report here on the analysis of a 100 ks Suzaku observation of the source. We confirm the existence of a very strong excess over the power-law X-ray continuum at $E\sim6$ keV ($EW\simeq 800$ eV), extending down to $\sim 4.5$ keV, and found that the X-ray spectrum of the source can be explained by two different models. i) An absorption scenario, in which the X-ray source is obscured by two fully-covering ionized absorbers, with a strong reflection component from neutral material ($R\sim 1.7$), a black body component and four narrow Gaussian lines (corresponding to Fe K$\alpha$, Fe K$\beta$, Fe xxv and Fe xxvi). ii) A reflection scenario, in which the X-ray spectrum is dominated by an obscured ($\log N_{\rm\,H}\sim 22.9$) blurred reflection produced in an ionized disk around a rotating supermassive black hole with a spin of $a \geq 0.73$, and affected by light-bending ($R\sim 2.7$), plus two narrow Gaussian lines (corresponding to Fe K$\alpha$ and Fe K$\beta$). The narrow Fe K$\alpha$ and K$\beta$ lines are consistent with being produced by ionized iron, and in particular by Fe xiv-Fe xvi and Fe xii-Fe xvi for the absorption and reflection scenario, respectively. While the X-ray continuum varies significantly during the observation, the intensity of the broad feature appears to be constant, in agreement with both the absorption and reflection scenarios. For both scenarios we obtained a steep power-law emission ($\Gamma\sim 2.2-2.3$), and we speculate that the source might be an obscured narrow-line Seyfert 1., Comment: Accepted for publication in ApJ. 13 pages, 7 figures, 2 tables

Published
2014
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219. Tracking the Complex Absorption in NGC 2110 with Two Suzaku Observations

Author

Rivers, Elizabeth, Markowitz, Alex, Rothschild, Richard, Bamba, Aya, Fukazawa, Yasushi, Okajima, Takashi, Reeves, James, Terashima, Yuichi, Ueda, Yoshihiro, Rivers, Elizabeth, Markowitz, Alex, Rothschild, Richard, Bamba, Aya, Fukazawa, Yasushi, Okajima, Takashi, Reeves, James, Terashima, Yuichi, and Ueda, Yoshihiro

Abstract

We present spectral analysis of two Suzaku observations of the Seyfert 2 galaxy, NGC 2110. This source has been known to show complex, variable absorption which we study in depth by analyzing these two observations set seven years apart and by comparing to previously analyzed observations with the XMM-Newton and Chandra observatories. We find that there is a relatively stable, full-covering absorber with a column density of ~3$\times 10 ^{22}$ cm$^{-2}$, with an additional patchy absorber that is likely variable in both column density and covering fraction over timescales of years, consistent with clouds in a patchy torus or in the broad line region. We model a soft emission line complex, likely arising from ionized plasma and consistent with previous studies. We find no evidence for reflection from an accretion disk in this source with no contribution from relativistically broadened Fe Ka line emission nor from a Compton reflection hump., Comment: Accepted to ApJ: March, 2014

Published
2014
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220. The ASTRO-H X-ray Astronomy Satellite

Author

Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall, Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura, Brown, Greg, Cackett, Edward, Canavan, Edgar, Chernyakova, Maria, Chiao, Meng, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gilmore, Kirk, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hamaguchi, Kenji, Harayama, Atsushi, Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Hwang, Una, Iizuka, Ryo, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Ito, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline, Kimball, Mark, Kimura, Masashi, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Konami, Saori, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, LaMassa, Stephanie, Laurent, Philippe, Lebrun, Franccois, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Mcguinness, Daniel, McNamara, Brian, Miko, Joseph, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Moroso, Franco, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, Dell, Steve O', Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, St'ephane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Pontius, James, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian, Reis, Rubens, Reynolds, Christopher, Ricci, Claudio, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sato, Goro, Sato, Yoichi, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Hiroyuki, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Hiroaki, Takeda, Shin-ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, 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, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Ueda, Shutaro, Ueno, Shiro, Uno, Shinichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, White, Nicholas, Wilkins, Dan, Yamada, Takahiro, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, Zoghbi, Abderahmen, ZuHone, John, Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall, Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura, Brown, Greg, Cackett, Edward, Canavan, Edgar, Chernyakova, Maria, Chiao, Meng, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gilmore, Kirk, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hamaguchi, Kenji, Harayama, Atsushi, Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Hwang, Una, Iizuka, Ryo, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Ito, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline, Kimball, Mark, Kimura, Masashi, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Konami, Saori, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, LaMassa, Stephanie, Laurent, Philippe, Lebrun, Franccois, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Mcguinness, Daniel, McNamara, Brian, Miko, Joseph, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Moroso, Franco, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, Dell, Steve O', Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, St'ephane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Pontius, James, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian, Reis, Rubens, Reynolds, Christopher, Ricci, Claudio, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sato, Goro, Sato, Yoichi, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Hiroyuki, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Hiroaki, Takeda, Shin-ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, 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, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Ueda, Shutaro, Ueno, Shiro, Uno, Shinichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, White, Nicholas, Wilkins, Dan, Yamada, Takahiro, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, Zoghbi, Abderahmen, and ZuHone, John

Abstract

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions developed by the Institute of Space and Astronautical Science (ISAS), with a planned launch in 2015. The ASTRO-H mission is equipped with a suite of sensitive instruments with the highest energy resolution ever achieved at E > 3 keV and a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. The simultaneous broad band pass, coupled with the high spectral resolution of Delta E < 7 eV of the micro-calorimeter, will enable a wide variety of important science themes to be pursued. ASTRO-H is expected to provide breakthrough results in scientific areas as diverse as the large-scale structure of the Universe and its evolution, the behavior of matter in the gravitational strong field regime, the physical conditions in sites of cosmic-ray acceleration, and the distribution of dark matter in galaxy clusters at different redshifts., Comment: 24 pages, 18 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray"

Published
2014
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221. The ASTRO-H X-ray astronomy satellite

Author

Takahashi, Tadayuki, additional, Mitsuda, Kazuhisa, additional, Kelley, Richard, additional, Aharonian, Felix, additional, Akamatsu, Hiroki, additional, Akimoto, Fumie, additional, Allen, Steve, additional, Anabuki, Naohisa, additional, Angelini, Lorella, additional, Arnaud, Keith, additional, Asai, Makoto, additional, Audard, Marc, additional, Awaki, Hisamitsu, additional, Azzarello, Philipp, additional, Baluta, Chris, additional, Bamba, Aya, additional, Bando, Nobutaka, additional, Bautz, Marshall, additional, Bialas, Thomas, additional, Blandford, Roger D., additional, Boyce, Kevin, additional, Brenneman, Laura, additional, Brown, Gregory, additional, Cackett, Ed, additional, Canavan, Edgar, additional, Chernyakova, Maria, additional, Chiao, Meng, additional, Coppi, Paolo, additional, Costantini, Elisa, additional, de Plaa, Jelle, additional, den Herder, Jan-Willem, additional, DiPirro, Michael, additional, Done, Chris, additional, Dotani, Tadayasu, additional, Doty, John, additional, Ebisawa, Ken, additional, Enoto, Teruaki, additional, Ezoe, Yuichiro, additional, Fabian, Andrew, additional, Ferrigno, Carlo, additional, Foster, Adam, additional, Fujimoto, Ryuichi, additional, Fukazawa, Yasushi, additional, Funk, Stefan, additional, Furuzawa, Akihiro, additional, Galeazzi, Massimiliano, additional, Gallo, Luigi, additional, Gandhi, Poshak, additional, Gilmore, Kirk, additional, Guainazzi, Matteo, additional, Haas, Daniel, additional, Haba, Yoshito, additional, Hamaguchi, Kenji, additional, Harayama, Atsushi, additional, Hatsukade, Isamu, additional, Hayashi, Katsuhiro, additional, Hayashi, Takayuki, additional, Hayashida, Kiyoshi, additional, Hiraga, Junko, additional, Hirose, Kazuyuki, additional, Hornschemeier, Ann, additional, Hoshino, Akio, additional, Hughes, John, additional, Hwang, Una, additional, Iizuka, Ryo, additional, Inoue, Yoshiyuki, additional, Ishibashi, Kazunori, additional, Ishida, Manabu, additional, Ishikawa, Kumi, additional, Ishimura, Kosei, additional, Ishisaki, Yoshitaka, additional, Itoh, Masayuki, additional, Iwata, Naoko, additional, Iyomoto, Naoko, additional, Jewell, Chris, additional, Kaastra, Jelle, additional, Kallman, Timothy, additional, Kamae, Tuneyoshi, additional, Kataoka, Jun, additional, Katsuda, Satoru, additional, Katsuta, Junichiro, additional, Kawaharada, Madoka, additional, Kawai, Nobuyuki, additional, Kawano, Taro, additional, Kawasaki, Shigeo, additional, Khangaluyan, Dmitry, additional, Kilbourne, Caroline, additional, Kimball, Mark, additional, Kimura, Masashi, additional, Kitamoto, Shunji, additional, Kitayama, Tetsu, additional, Kohmura, Takayoshi, additional, Kokubun, Motohide, additional, Konami, Saori, additional, Kosaka, Tatsuro, additional, Koujelev, Alexander, additional, Koyama, Katsuji, additional, Krimm, Hans, additional, Kubota, Aya, additional, Kunieda, Hideyo, additional, LaMassa, Stephanie, additional, Laurent, Philippe, additional, Lebrun, François, additional, Leutenegger, Maurice, additional, Limousin, Olivier, additional, Loewenstein, Michael, additional, Long, Knox, additional, Lumb, David, additional, Madejski, Grzegorz, additional, Maeda, Yoshitomo, additional, Makishima, Kazuo, additional, Markevitch, Maxim, additional, Masters, Candace, additional, Matsumoto, Hironori, additional, Matsushita, Kyoko, additional, McCammon, Dan, additional, McGuinness, Daniel, additional, McNamara, Brian, additional, Miko, Joseph, additional, Miller, Jon, additional, Miller, Eric, additional, Mineshige, Shin, additional, Minesugi, Kenji, additional, Mitsuishi, Ikuyuki, additional, Miyazawa, Takuya, additional, Mizuno, Tsunefumi, additional, Mori, Koji, additional, Mori, Hideyuki, additional, Moroso, Franco, additional, Muench, Theodore, additional, Mukai, Koji, additional, Murakami, Hiroshi, additional, Murakami, Toshio, additional, Mushotzky, Richard, additional, Nagano, Housei, additional, Nagino, Ryo, additional, Nakagawa, Takao, additional, Nakajima, Hiroshi, additional, Nakamori, Takeshi, additional, Nakashima, Shinya, additional, Nakazawa, Kazuhiro, additional, Namba, Yoshiharu, additional, Natsukari, Chikara, additional, Nishioka, Yusuke, additional, Nobukawa, Masayoshi, additional, Noda, Hirofumi, additional, Nomachi, Masaharu, additional, O'Dell, Steve, additional, Odaka, Hirokazu, additional, Ogawa, Hiroyuki, additional, Ogawa, Mina, additional, Ogi, Keiji, additional, Ohashi, Takaya, additional, Ohno, Masanori, additional, Ohta, Masayuki, additional, Okajima, Takashi, additional, Okazaki, Tsuyoshi, additional, Ota, Naomi, additional, Ozaki, Masanobu, additional, Paerels, Frits, additional, Paltani, Stéphane, additional, Parmar, Arvind, additional, Petre, Robert, additional, Pinto, Ciro, additional, Pohl, Martin, additional, Pontius, James, additional, Porter, F. S., additional, Pottschmidt, Katja, additional, Ramsey, Brian, additional, Reis, Rubens, additional, Reynolds, Christopher, additional, Ricci, Claudio, additional, Russell, Helena, additional, Safi-Harb, Samar, additional, Saito, Shinya, additional, Sakai, Shin-ichiro, additional, Sameshima, Hiroaki, additional, Sato, Kosuke, additional, Sato, Rie, additional, Sato, Goro, additional, Sawada, Makoto, additional, Serlemitsos, Peter, additional, Seta, Hiromi, additional, Shibano, Yasuko, additional, Shida, Maki, additional, Shimada, Takanobu, additional, Shirron, Peter, additional, Simionescu, Aurora, additional, Simmons, Cynthia, additional, Smith, Randall, additional, Sneiderman, Gary, additional, Soong, Yang, additional, Stawarz, Lukasz, additional, Sugawara, Yasuharu, additional, Sugita, Satoshi, additional, Szymkowiak, Andrew, additional, Tajima, Hiroyasu, additional, Takahashi, Hiroaki, additional, Takahashi, Hiromitsu, additional, Takeda, Shin-ichiro, additional, Takei, Yoh, additional, Tamagawa, Toru, additional, Tamura, Keisuke, additional, Tamura, Takayuki, additional, Tanaka, Takaaki, additional, Tanaka, Yasuyuki, additional, Tanaka, Yasuo, additional, Tashiro, Makoto, additional, Tawara, Yuzuru, additional, Terada, Yukikatsu, additional, Terashima, Yuichi, additional, Tombesi, Francesco, additional, Tomida, Hiroshi, additional, Tsuboi, Yoko, additional, Tsujimoto, Masahiro, additional, Tsunemi, Hiroshi, additional, Tsuru, Takeshi, additional, Uchida, Hiroyuki, additional, Uchiyama, Hideki, additional, Uchiyama, Yasunobu, additional, Ueda, Yoshihiro, additional, Ueda, Shutaro, additional, Ueno, Shiro, additional, Uno, Shinichiro, additional, Urry, Meg, additional, Ursino, Eugenio, additional, de Vries, Cor, additional, Wada, Atsushi, additional, Watanabe, Shin, additional, Watanabe, Tomomi, additional, Werner, Norbert, additional, White, Nicholas, additional, Wilkins, Dan, additional, Yamada, Shinya, additional, Yamada, Takahiro, additional, Yamaguchi, Hiroya, additional, Yamaoka, Kazutaka, additional, Yamasaki, Noriko, additional, Yamauchi, Makoto, additional, Yamauchi, Shigeo, additional, Yaqoob, Tahir, additional, Yatsu, Yoichi, additional, Yonetoku, Daisuke, additional, Yoshida, Atsumasa, additional, Yuasa, Takayuki, additional, Zhuravleva, Irina, additional, Zoghbi, Abderahmen, additional, and ZuHone, John, additional

Published
2014
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223. Infrared and Hard X-Ray Diagnostics of AGN Identification from the AKARI and Swift/bat All-Sky Surveys

Author

Gandhi, P., Stawarz, Lukasz, Matsuta, Keiko, Dotani, Tadayasu, Nakagawa, Takao, Isobe, Naoki, Ueda, Yoshihiro, Ichikawa, Kohei, Terashima, Yuichi, Oyabu, Shinki, and Yamamura, Issei

Subjects
Physics, Swift, Active galactic nucleus, Infrared, Point source, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, General Medicine, Astrophysics, galaxies [infrared], Galaxy, Luminosity, law.invention, Telescope, Sky, law, active [galaxies], galaxies [X-ray], computer, Astrophysics::Galaxy Astrophysics, media_common, computer.programming_language
Abstract

著者人数: 11名, Accepted: 2012-08-10, 資料番号: SA1004458000

Published
2012

224. Chandra Snapshot Observations of LINERs with a Compact Radio Core

Author

Terashima, Yuichi and Wilson, Andrew S.

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

The results of Chandra snapshot observations of 11 LINERs (Low-Ionization Nuclear Emission-line Regions), three low-luminosity Seyfert galaxies, and one HII-LINER transition object are presented. Our sample consists of all the objects with a flat or inverted spectrum compact radio core in the VLA survey of 48 low-luminosity AGN (LLAGN) by Nagar et al. (2000). An X-ray nucleus is detected in all galaxies except one and their X-ray luminosities are in the range 5x10^38 to 8x10^41 ergs s^-1. The X-ray to Halpha luminosity ratios for 11 out of 14 objects are in good agreement with the value characteristic of LLAGNs and more luminous AGNs, and indicate that their optical emission lines are predominantly powered by a LLAGN. For three objects, this ratio is less than expected. Comparing with multi-wavelength results, we find that these three galaxies are most likely to be heavily obscured AGN. We compare the radio to X-ray luminosity ratio of LLAGNs with those of more-luminous AGNs, and confirm the suggestion that a large fraction of LLAGNs are radio loud., 4 pages, To appear in the proceedings of the workshop "X-ray spectroscopy of AGN with Chandra and XMM-Newton", Eds., Th. Boller, S. Komossa, S. Kahn, and H. Kunieda

Published
2002

225. Ultraluminous X-ray Sources in M51

Author

Terashima, Yuichi and Wilson, Andrew S.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We present the results of Chandra observations of off-nuclear X-ray sources in the spiral galaxy M51 (NGC 5194). 113 X-ray sources have been detected in the field of view and 84 among them project within the disk of NGC 5194. Six and twenty eight sources have luminosities exceeding 1x10^39 ergs s^-1 and 1x10^38 ergs s^-1 in the 0.5-8 keV band, respectively. The number of luminous sources is much higher than normal spiral and elliptical galaxies and similar to galaxies experiencing starburst activity. X-ray spectra of most of the detected sources are consistent with a power law with a photon index between 1 and 2, while one source has an extremely hard spectrum and two sources have soft spectra. The spectra of three ultraluminous sources are consistent with both a power law and a multicolor disk blackbody (MCD) model, while a power law model is preferable to a MCD model in two objects. One luminous object which shows a remarkable spectrum, including emission lines, is also found and discussed., 4 pages, to appear in the Proceedings of the Symposium on ``New Visions of the Universe in the XMM-Newton and Chandra Era'', 26-30 November 2001, ESTEC, The Netherlands

Published
2002

226. Fe K Emission Lines in Low-luminosity AGNs

Author

Terashima, Yuichi, Iyomoto, Naoko, Ho, Luis C., and Ptak, Andrew F.

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

We present the results of a systematic analysis of Fe K emission lines in low-luminosity AGNs (LLAGNs) observed with ASCA. We used a sample of LLAGNs with small intrinsic absorption to compare with luminous AGNs and accretion models. Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the objects show no significant Fe K emission line. We made a composite spectrum of sources without detected Fe emission lines to search for weak lines and obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4 keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. Even in those objects with detected Fe lines, a skewed broad component, typically observed in Seyfert 1s, is not seen. The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole. Alternatively, it might be due to the ionization of a standard disk. The lack of big blue bump favors the former., 4 pages, In ``X-ray Emission from Accretion onto Black Holes'', proceedings of a workshop held by JHU and LHEA, in Baltimore, MD, June 20-23, 2001, eds. T. Yaqoob, & J. H. Krolik, published electronically

Published
2002

227. Chandra Snapshot Observations of Low-Luminosity AGNs with a Compact Radio Source

Author

Terashima, Yuichi and Wilson, Andrew S.

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

The results of Chandra snapshot observations of 11 LINERs (Low-Ionization Nuclear Emission-line Regions), three low-luminosity Seyfert galaxies, and one HII-LINER transition object are presented. Our sample consists of all the objects with a flat or inverted spectrum compact radio core in the VLA survey of 48 low-luminosity AGNs (LLAGNs) by Nagar et al. (2000). An X-ray nucleus is detected in all galaxies except one and their X-ray luminosities are in the range 5x10^38 to 8x10^41 erg/s. The X-ray spectra are generally steeper than expected from thermal bremsstrahlung emission from an advection-dominated accretion flow (ADAF). The X-ray to Halpha luminosity ratios for 11 out of 14 objects are in good agreement with the value characteristic of LLAGNs and more luminous AGNs, and indicate that their optical emission lines are predominantly powered by a LLAGN. For three objects, this ratio is less than expected. Comparing with properties in other wavelengths, we find that these three galaxies are most likely to be heavily obscured AGN. We use the ratio RX = \nu L\nu (5 GHz)/LX, where LX is the luminosity in the 2-10 keV band, as a measure of radio loudness. In contrast to the usual definition of radio loudness (RO = L\nu(5 GHz)/L\nu(B)), RX can be used for heavily obscured (NH >~ 10^23 cm^-2, AV>50 mag) nuclei. Further, with the high spatial resolution of Chandra, the nuclear X-ray emission of LLAGNs is often easier to measure than the nuclear optical emission. We investigate the values of RX for LLAGNs, luminous Seyfert galaxies, quasars and radio galaxies and confirm the suggestion that a large fraction of LLAGNs are radio loud., Comment: 15 pages, accepted for publication in ApJ

Published
2002
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228. X-ray Emission from the Type Ic Supernova 1994I Observed with Chandra

Author

Immler, Stefan, Wilson, Andrew S., and Terashima, Yuichi

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We present two high-resolution Chandra X-ray observations of supernova (SN) 1994I which show, for the first time, that the interaction of the blast wave from a Type Ic SN with its surrounding circumstellar material (CSM) can give rise to soft X-ray emission. Given a 0.3-2 keV band X-ray luminosity of L_x ~ 1 x 10^{37} ergs/s between six and seven years after the outburst of SN 1994I, and assuming the X-ray emission arises from the shock-heated CSM, we derive a pre-SN mass-loss rate of \dot{M} ~ 1 x 10^{-5} M_sun/yr (v_w/10 km/s). Combining the results with earlier ROSAT observations, we construct the X-ray lightcurve of SN 1994I. A best-fit X-ray rate of decline of L_x \propto t^{-s} with index s~1 and a CSM density profile of rho_csm \propto r^{-1.9\pm0.1} are inferred, consistent with what is expected for a constant mass-loss rate and constant wind velocity profile for the SN progenitor (rho_csm \propto r^{-2})., Comment: 5 pages, 3 figures, accepted for publication in the Astrophysical Journal Letters

Published
2002
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229. Submillimeter ALMA Observations of the Dense Gas in the Low-Luminosity Type-1 Active Nucleus of NGC 1097

Author

Izumi, Takuma, Izumi, Takuma, Kohno, Kotaro, Martin, Sergio, Espada, Daniel, Harada, Nanase, Matsushita, Satoki, Hsieh, Pei-Ying, Turner, Jean L, Meier, David S, Schinnerer, Eva, Imanishi, Masatoshi, Tamura, Yoichi, Curran, Max T, Doi, Akihiro, Fathi, Kambiz, Krips, Melanie, Lundgren, Andreas A, Nakai, Naomasa, Nakajima, Taku, Regan, Michael W, Sheth, Kartik, Takano, Shuro, Taniguchi, Akio, Terashima, Yuichi, Tosaki, Tomoka, Wiklind, Tommy, Izumi, Takuma, Izumi, Takuma, Kohno, Kotaro, Martin, Sergio, Espada, Daniel, Harada, Nanase, Matsushita, Satoki, Hsieh, Pei-Ying, Turner, Jean L, Meier, David S, Schinnerer, Eva, Imanishi, Masatoshi, Tamura, Yoichi, Curran, Max T, Doi, Akihiro, Fathi, Kambiz, Krips, Melanie, Lundgren, Andreas A, Nakai, Naomasa, Nakajima, Taku, Regan, Michael W, Sheth, Kartik, Takano, Shuro, Taniguchi, Akio, Terashima, Yuichi, Tosaki, Tomoka, and Wiklind, Tommy

Abstract

We present the first 100 pc scale view of the dense molecular gas in the central ~ 1.3 kpc region of the type-1 Seyfert NGC 1097 traced by HCN (J=4-3) and HCO+ (J=4-3) lines afforded with ALMA band 7. This galaxy shows significant HCN enhancement with respect to HCO+ and CO in the low-J transitions, which seems to be a common characteristic in AGN environments. Using the ALMA data, we study the characteristics of the dense gas around this AGN and search for the mechanism of HCN enhancement. We find a high HCN (J=4-3) to HCO+ (J=4-3) line ratio in the nucleus. The upper limit of the brightness temperature ratio of HCN (v2=1^{1f}, J=4-3) to HCN (J=4-3) is 0.08, which indicates that IR pumping does not significantly affect the pure rotational population in this nucleus. We also find a higher HCN (J=4-3) to CS (J=7-6) line ratio in NGC 1097 than in starburst galaxies, which is more than 12.7 on the brightness temperature scale. Combined from similar observations from other galaxies, we tentatively suggest that this ratio appears to be higher in AGN-host galaxies than in pure starburst ones similar to the widely used HCN to HCO+ ratio. LTE and non-LTE modeling of the observed HCN and HCO+ lines using J=4-3 and 1-0 data from ALMA, and J=3-2 data from SMA, reveals a high HCN to HCO+ abundance ratio (5 < [HCN]/[HCO+] < 20: non-LTE analysis) in the nucleus, and that the high-J lines (J=4-3 and 3-2) are emitted from dense (10^{4.5} < n_H2 [/cc] < 10^6), hot (70 < Tkin [K] < 550) regions. Finally we propose that the high temperature chemistry is more plausible to explain the observed enhanced HCN emission in NGC 1097 than the pure gas phase PDR/XDR chemistry.

Published
2013

230. Suzaku View of the Swift/BAT Active Galactic Nuclei. V. Torus Structure of Two Luminous Radio-loud AGNs (3C 206 and PKS 0707-35)

Author

Tazaki, Fumie, Ueda, Yoshihiro, Terashima, Yuichi, Mushotzky, Richard, Tombesi, Francesco, Tazaki, Fumie, Ueda, Yoshihiro, Terashima, Yuichi, Mushotzky, Richard, and Tombesi, Francesco

Abstract

We present the results from broad-band X-ray spectral analysis of 3C 206 and PKS 0707-35 with Suzaku and Swift/BAT, two of the most luminous unobscured and obscured radio-loud active galactic nuclei with hard X-ray luminosities of 10^{45.5} erg s^{-1} and 10^{44.9} erg s^{-1} (14--195 keV), respectively. Based on the radio core luminosity, we estimate that the X-ray spectrum of 3C 206 contains a significant (~ 60% in the 14--195 keV band) contribution from the jet, while it is negligible in PKS 0707-35. We can successfully model the spectra with the jet component (for 3C 206), the transmitted emission, and two reflection components from the torus and the accretion disk. The reflection strengths from the torus are found to be R_{torus} (= \Omega/2\pi) = 0.29 +- 0.18 and 0.41 +- 0.18 for 3C 206 and PKS 0707-35, respectively, which are smaller than those in typical Seyfert galaxies. Utilizing the torus model by Ikeda et al. (2009), we quantify the relation between the half opening angle of a torus (\theta_{oa}) and the equivalent width of an iron-K line. The observed equivalent width of 3C 206, < 71 eV, constrain the column density in the equatorial plane to N_{H}^{eq} < 10^{23} cm^{-2}, or the half opening angle to \theta_{oa} > 80^\circ if N_{H}^{eq} = 10^{24} cm^{-2} is assumed. That of PKS 0707-35, 72 +- 36 eV, is consistent with N_{H}^{eq} ~ 10^{23} cm^{-2}. Our results suggest that the tori in luminous radio-loud AGNs are only poorly developed. The trend is similar to that seen in radio-quiet AGNs, implying that the torus structure is not different between AGNs with jets and without jets., Comment: 12 pages, 8 figures, accepted for publication in the Astrophysical Journal

Published
2013
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231. Broad Band X-Ray Spectra of Two Low-luminosity Active Galactic Nuclei NGC 1566 and NGC 4941

Author

Kawamuro, Taiki, Ueda, Yoshihiro, Tazaki, Fumie, Terashima, Yuichi, Kawamuro, Taiki, Ueda, Yoshihiro, Tazaki, Fumie, and Terashima, Yuichi

Abstract

We report the first broad band X-ray spectra of the low luminosity active galactic nuclei (LLAGN) NGC 1566 (type 1.5) and NGC 4941 (type 2) observed with Suzaku and Swift/BAT covering the 0.5-195 keV band. Both targets have hard X-ray luminosities of ~ 10^{41-42} ergs/s in the 15-55 keV band. The spectra of the nucleus are well reproduced by a sum of partially or fully covered transmitted emission and its reflection from the accretion disk, reprocessed emission from the torus accompanied by a strong narrow iron-K\alpha line, and a scattered component (for NGC 4941). We do not significantly detect a broad iron-K\alpha line from the inner accretion disk in both targets, and obtain an upper limit on the corresponding solid angle of \Omega/2\pi < 0.3 in NGC 1566. The reflection strength from the torus is moderate, \Omega/2\pi =0.45^{+0.13}_{-0.10} in NGC 1566 and \Omega/2\pi =0.64^{+0.69}_{-0.27} in NGC 4941. Comparison of the equivalent width of the narrow iron-K\alpha line with a model prediction based on a simple torus geometry constrains its half-opening angle to be \theta_oa ~ 60-70 degree in NGC 4941. These results agree with the obscured AGN fraction obtained from hard X-ray and mid-infrared selected samples at similar luminosities. Our results support the implication that the averaged covering fraction of AGN tori is peaked at L 10^{42-43} ergs/s but decreases toward lower luminosities., Comment: 11 pages, 6 figures, accepted for publication in ApJ

Published
2013
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232. The ASTRO-H X-ray Observatory

Author

Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Henri AartsFelix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Mark, Blandford, Roger, Boyce, Kevin, Brown, Greg, Cackett, Ed, Chernyakova, Maria, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gendreau, Keith, Gilmore, Kirk, Haas, Daniel, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Hwang, Una, Iizuka, Ryo, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishimura, Kosei, Ishisaki, Yoshitaka, Ito, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawahara, Hajime, Kawaharada, Madoka, Kawai, Nobuyuki, Kawasaki, Shigeo, Khangaluyan, Dmitry, Kilbourne, Caroline, Kimura, Masashi, Kinugasa, Kenzo, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, LaMassa, Stephanie, Laurent, Philippe, Lebrun, Francois, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Marchand, Genevieve, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Toshio, Murakami, Hiroshi, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Nomachi, Masaharu, Dell, Steve O', Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Parmar, Arvind, Petre, Robert, Pohl, Martin, Porter, F. Scott, Ramsey, Brian, Reis, Rubens, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sanders, Jeremy, Sato, Goro, Sato, Rie, Sato, Yoichi, Sato, Kosuke, Sawada, Makoto, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Hiroyuki, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takeda, Shin-ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yoko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shinichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Werner, Norbert, White, Nicholas, Yamada, Takahiro, Yamada, Shinya, Yamaguchi, Hiroya, Yamasaki, Noriko, Yamauchi, Shigeo, Yamauchi, Makoto, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Henri AartsFelix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Mark, Blandford, Roger, Boyce, Kevin, Brown, Greg, Cackett, Ed, Chernyakova, Maria, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gendreau, Keith, Gilmore, Kirk, Haas, Daniel, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Hwang, Una, Iizuka, Ryo, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishimura, Kosei, Ishisaki, Yoshitaka, Ito, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawahara, Hajime, Kawaharada, Madoka, Kawai, Nobuyuki, Kawasaki, Shigeo, Khangaluyan, Dmitry, Kilbourne, Caroline, Kimura, Masashi, Kinugasa, Kenzo, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, LaMassa, Stephanie, Laurent, Philippe, Lebrun, Francois, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Marchand, Genevieve, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Toshio, Murakami, Hiroshi, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Nomachi, Masaharu, Dell, Steve O', Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Parmar, Arvind, Petre, Robert, Pohl, Martin, Porter, F. Scott, Ramsey, Brian, Reis, Rubens, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sanders, Jeremy, Sato, Goro, Sato, Rie, Sato, Yoichi, Sato, Kosuke, Sawada, Makoto, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Hiroyuki, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takeda, Shin-ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yoko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shinichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Werner, Norbert, White, Nicholas, Yamada, Takahiro, Yamada, Shinya, Yamaguchi, Hiroya, Yamasaki, Noriko, Yamauchi, Shigeo, Yamauchi, Makoto, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, and Yuasa, Takayuki

Abstract

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the high-energy universe via a suite of four instruments, covering a very wide energy range, from 0.3 keV to 600 keV. These instruments include a high-resolution, high-throughput spectrometer sensitive over 0.3-2 keV with high spectral resolution of Delta E < 7 eV, enabled by a micro-calorimeter array located in the focal plane of thin-foil X-ray optics; hard X-ray imaging spectrometers covering 5-80 keV, located in the focal plane of multilayer-coated, focusing hard X-ray mirrors; a wide-field imaging spectrometer sensitive over 0.4-12 keV, with an X-ray CCD camera in the focal plane of a soft X-ray telescope; and a non-focusing Compton-camera type soft gamma-ray detector, sensitive in the 40-600 keV band. The simultaneous broad bandpass, coupled with high spectral resolution, will enable the pursuit of a wide variety of important science themes., Comment: 22 pages, 17 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray"

Published
2012
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233. The Low-mass, Highly Accreting Black Hole Associated with the Active Galactic Nucleus 2XMM J123103.2+110648

Author

Ho, Luis C., Kim, Minjin, Terashima, Yuichi, Ho, Luis C., Kim, Minjin, and Terashima, Yuichi

Abstract

Optical spectra and images taken with the Baade 6.5 meter Magellan telescope confirm that 2XMM J123103.2+110648, a highly variable X-ray source with an unusually soft spectrum, is indeed associated with a type 2 (narrow-line) active nucleus at a redshift of z = 0.11871. The absence of broad Halpha or Hbeta emission in an otherwise X-ray unabsorbed source suggests that it intrinsically lacks a broad-line region. If, as in other active galaxies, the ionized gas and stars in J1231+1106 are in approximate virial equilibrium, and the black hole mass versus stellar velocity dispersion relation holds, the exceptionally small velocity dispersion of 33.5 km/s for [O III] 5007 implies that the black hole mass is approximately 10^5 solar masses, among the lowest ever detected. Such a low black hole mass is consistent with the general characteristics of the host, a small, low-luminosity, low-mass disk galaxy. We estimate the Eddington ratio of the black hole to be > 0.5, in good agreement with expectations based on the X-ray properties of the source., Comment: To appear in The Astrophysical Journal Letters

Published
2012
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234. Mid and Far Infrared Properties of a Complete Sample of Local AGNs

Author

Ichikawa, Kohei, Ueda, Yoshihiro, Terashima, Yuichi, Oyabu, Shinki, Gandhi, Poshak, Matsuta, Keiko, Nakagawa, Takao, Ichikawa, Kohei, Ueda, Yoshihiro, Terashima, Yuichi, Oyabu, Shinki, Gandhi, Poshak, Matsuta, Keiko, and Nakagawa, Takao

Abstract

We investigate the mid- (MIR) to far-infrared (FIR) properties of a nearly complete sample of local Active Galactic Nuclei (AGNs) detected in the Swift/BAT all sky hard X-ray (14-195 keV) survey, based on the cross correlation with the AKARI infrared survey catalogs complemented by those with IRAS and WISE. Out of 135 non-blazer AGNs in the Swift/BAT 9 month catalog, we obtain the MIR photometric data for 128 sources either in the 9, 12, 18, 22, and/or 25 um band. We find good correlation between their hard X-ray and MIR luminosities over 3 orders of magnitude (42< log lambda L_{lambda}(9, 18 um)< 45), which is tighter than that with the FIR luminosities at 90 um. This suggests that thermal emission from hot dusts irradiated by the AGN emission dominate the MIR fluxes. Both X-ray unabsorbed and absorbed AGNs follow the same correlation, implying isotropic infrared emission, as expected in clumpy dust tori rather than homogeneous ones. We find excess signals around 9 um in the averaged infrared spectral energy distribution from heavy obscured "new type" AGNs with small scattering fractions in the X-ray spectra. This could be attributed to the PAH emission feature, suggesting that their host galaxies have strong starburst activities., Comment: 14 pages, 8 figures, accepted for publication in ApJ

Published
2012
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235. A New Sample of Candidate Intermediate-Mass Black Holes Selected by X-ray Variability

Author

Kamizasa, Naoya, Terashima, Yuichi, Awaki, Hisamitsu, Kamizasa, Naoya, Terashima, Yuichi, and Awaki, Hisamitsu

Abstract

We present the results of X-ray variability and spectral analysis of a sample of 15 new candidates for active galactic nuclei with relatively low-mass black holes (BHs). They are selected from the Second XMM-Newton Serendipitous Source Catalogue based on strong variability quantified by normalized excess variances. Their BH masses are estimated to be 1.1-6.6x10^6 M_solar by using a correlation between excess variance and BH mass. Seven sources have estimated BH masses smaller than 2x10^6 M_solar, which are in the range for intermediate-mass black holes. Eddington ratios of sources with known redshifts range from 0.07 to 0.46 and the mean Eddington ratio is 0.24. These results imply that some of our sources are growing supermassive black holes, which are expected to have relatively low masses with high Eddington ratios. X-ray photon indices of the 15 sources are in the range of ~0.57-2.57, and 5 among them have steep (>2) photon indices, which are the range for narrow-line Seyfert 1s. Soft X-ray excess is seen in 12 sources, and is expressed by a blackbody model with kT~83-294 eV. We derive a correlation between X-ray photon indices and Eddington ratios, and find that the X-ray photon indices of about a half of our sources are flatter than the positive correlation suggested previously., Comment: To Appear in ApJ, 14 pages, 5 figures

Published
2012
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236. A Candidate Active Galactic Nucleus with a Pure Soft Thermal X-ray Spectrum

Author

Terashima, Yuichi, Kamizasa, Naoya, Awaki, Hisamitsu, Kubota, Aya, Ueda, Yoshihiro, Terashima, Yuichi, Kamizasa, Naoya, Awaki, Hisamitsu, Kubota, Aya, and Ueda, Yoshihiro

Abstract

We report the discovery of a candidate active galactic nucleus (AGN), 2XMM J123103.2+110648 at z = 0.13, with an X-ray spectrum represented purely by soft thermal emission reminiscent of Galactic black hole (BH) binaries in the disk-dominated state. This object was found in the second XMM serendipitous source catalogue as a highly variable X-ray source. In three separate observations, its X-ray spectrum can be represented either by a multicolor disk blackbody model with an inner temperature of kT_in~0.16-0.21 keV or a Wien spectrum Comptonized by an optically thick plasma with kT~0.14-0.18 keV. The soft X-ray luminosity in the 0.5--2 keV band is estimated to be (1.6-3.8)x10^42 erg/s. Hard emission above ~2 keV is not detected. The ratio of the soft to hard emission is the strongest among AGNs observed thus far. Spectra selected in high/low flux time intervals are examined in order to study spectral variability. In the second observation with the highest signal-to-noise ratio, the low energy (below 0.7 keV) spectral regime flattens when the flux is high, while the shape of the high energy part (1-1.7 keV) remains unchanged. This behavior is qualitatively consistent with being caused by strong Comptonization. Both the strong soft excess and spectral change consistent with Comptonization in the X-ray spectrum imply that the Eddington ratio is large, which requires a small BH mass (smaller than ~10^5M_solar., Comment: To Appear in ApJ, 8 pages, 7 figures

Published
2012
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237. Infrared and hard X-ray diagnostics of AGN identification from the Swift/BAT and AKARI all-sky surveys

Author

Matsuta, Keiko, Gandhi, Poshak, Dotani, Tadayasu, Nakagawa, Takao, Isobe, Naoki, Ueda, Yoshihiro, Ichikawa, Kohei, Terashima, Yuichi, Oyabu, Shinki, Yamamura, Issei, Stawarz, Łukasz, Matsuta, Keiko, Gandhi, Poshak, Dotani, Tadayasu, Nakagawa, Takao, Isobe, Naoki, Ueda, Yoshihiro, Ichikawa, Kohei, Terashima, Yuichi, Oyabu, Shinki, Yamamura, Issei, and Stawarz, Łukasz

Abstract

We combine data from two all-sky surveys in order to study the connection between the infrared and hard X-ray (>10keV) properties for local active galactic nuclei (AGN). The Swift/Burst Alert Telescope all-sky survey provides an unbiased, flux-limited selection of hard X-ray detected AGN. Cross-correlating the 22-month hard X-ray survey with the AKARI all-sky survey, we studied 158 AGN detected by the AKARI instruments. We find a strong correlation for most AGN between the infrared (9, 18, and 90 micron) and hard X-ray (14-195 keV) luminosities, and quantify the correlation for various subsamples of AGN. Partial correlation analysis confirms the intrinsic correlation after removing the redshift contribution. The correlation for radio galaxies has a slope and normalization identical to that for Seyfert 1s, implying similar hard X-ray/infrared emission processes in both. In contrast, Compton-thick sources show a large deficit in the hard X-ray band, because high gas column densities diminish even their hard X-ray luminosities. We propose two photometric diagnostics for source classification: one is an X-ray luminosity vs. infrared color diagram, in which type 1 radio-loud AGN are well isolated from the others in the sample. The other uses the X-ray vs. infrared color as a useful redshift-independent indicator for identifying Compton-thick AGN. Importantly, Compton-thick AGN and starburst galaxies in composite systems can also be differentiated in this plane based upon their hard X-ray fluxes and dust temperatures. This diagram may be useful as a new indicator to classify objects in new and upcoming surveys such as WISE and NuSTAR., Comment: 17 pages, 5 figures, 5 tables. Accepted for publication in the Astrophysical Journal

Published
2012
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238. Suzaku Observation of Six New Swift/BAT AGNs: Evidence for Two Types of Obscured Population

Author

Eguchi, Satoshi, Ueda, Yoshihiro, Terashima, Yuichi, Mushotzky, Richard, and Tueller, Jack

Subjects
galaxies: active - gamma rays: observations - X-rays: galaxies - X-rays: general
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We present a systematic spectral analysis with Suzaku of six AGNs detected in the Swift/BAT hard X-ray (15 - 200 keV) survey. The 0.5 - 200 keV spectra of these sources can be uniformly fit with a base model consisting of heavily absorbed (logN(sub H) > 23.5 cm(sup -2)) transmitted components, scattered lights, a reflection component, and an iron-K emission line. There are two distinct groups, three "new type" AGNs (including the two sources reported by Ueda et al. 2007) with an extremely small scattered fraction (f(sub scat) < 0.5 % ) and strong reflection component (R = Omega/2pi greater than or approximately equal to 0.8, where Omega is the solid angle of the reflector), and three "classical type" ones with f(sub scat) > 0.5 % and R greater than or approximately equal to 0.8. The spectral parameters suggest that the new type has an optically thick torus for Thomson scattering (N(sub H) approximately 10(sup 25) cm(sup -2)) with a small opening angle of theta approximately 20 deg viewed in a rather face-on geometry, while the classical type has a thin torus (logN(sub H) approximately 23 - 24 cm(sup -2)) with theta > or similar to 30 deg. We infer that a significant number of new type AGNs with an edge-on view is missing in the current all-sky hard X-ray surveys., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574140, レポート番号: JAXA-SP-09-008E

Published
2010

239. The AGN Power in Type 2 ULIRGs with a High [OIII] Luminosity Observed by Suzaku and XMM-Newton

Author

Hirata, Yoshitaka, Terashima, Yuichi, Anabuki, Naohisa, Nakagawa, Takao, and Awaki, Hisamitsu

Subjects
ULIRG, active galactic nuclei, starburst galaxy
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We present results from observations of three ultraluminous infrared galaxies(ULIRGs) with Suzaku and XMM-Newton. Their optical emission lines are classified as seyfert 2 and extinction-corrected [OIII]lambda5007 line luminosities are (3.2 - 61) x 10 (sup 43) erg s(sup -1), which are in the range for quasars. Their X-ray spectra are explained by a combination of unabsorbed and absorbed power-law components. Fe Kalpha lines are not detected. The absorption-corrected 2-10 keV luminosities L(sub (2 - 10 keV)) are in the range of (3.3 - 24) x 10(sup 42) erg s(sup -1). These results indicate that these objects are Compton-thin AGNs with Seyfert class luminosity. We compare the far infrared (FIR) luminosities L(sub FIR) with the bolometric luminosities of the AGNs and find that the contribution of AGNs to L(sub FIR) is at most a few tens of percent., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574130, レポート番号: JAXA-SP-09-008E

Published
2010

240. Fe -K line Profile and X-ray Spectral Variability of the Seyfert 1.9 Galaxy NGC 7314 Observed with Suzaku

Author

Kawahara, Hiroshi, Terashima, Yuichi, Yaqoob, Tahir, and Awaki, Hisamitsu

Subjects
Seyfert galaxy, NGC 7314, variability
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We present results from a Suzaku observation of the Seyfert 1.9 galaxy NGC 7314. The light curve in the 2-10 keV band shows rapid variability on timescales of approximately 1000 sec. The time-averaged spectrum in 0.5 - 25 keV is explained a model consisting of absorbed and unabsorbed power laws, a reflection continuum and a gaussian at 6.4 keV. The line at 6.4 keV is relatively narrow (sigma approximately 50 eV) and does not vary on a timescale of approximately 10 years. This narrow line is likely to be primarily from distant matter. We analyze spectra in the time intervals with fluxes higher/lower than the mean. The normalization of the absorbed power law varies by a factor 1.6, while the photon index, the amount of the reflection, and the intensity of the Fe line remains constant., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574125, レポート番号: JAXA-SP-09-008E

Published
2010

241. X-ray study of Compton-thick AGNs with Suzaku

Author

Awaki, Hisamitsu, Terashima, Yuichi, Higaki, Yusuke, Yonetani, Tetsuaki, and Ueda, Yoshihiro

Subjects
galaxies: active - galaxies: Seyfert - X-rays: galaxies
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We have obtained broad-band spectra of 11 Compton-thick Seyfert 2 galaxies with Suzaku. The spectra are well represented by a three component model, consisting of a soft component, an absorbed power-law component, and a reflection component, accompanied by both a strong iron Kalpha line and several weak lines. Fixing the photon indices of the power law and the reflection components at 1.9, we obtain the column density N(sub H) and the intrinsic X-ray luminosity in the 2 - 10 keV band. We update the N(sub H) distribution of the bright [OIII] sample by Risaliti et al. (1999), and find that observed luminosities of Compton thick AGNs are only 1-10% of the intrinsic luminosities in the 2 - 10 keV band. This is consistent with small ratios of L(sub X)/L(sub [OIII]) of Compton thick AGNs., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574126, レポート番号: JAXA-SP-09-008E

Published
2010

242. Multi-wavelength Properties of X-ray Selected Buried AGNs

Author

Noguchi, Kazuhisa, Terashima, Yuichi, and Awaki, Hisamitsu

Subjects
X-rays: galaxies, galaxies: active, galaxies: Seyfert
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We construct a new sample of obscured AGNs and investigate their X-ray spectra and multi-wavelength properties. Our sample is consisting of 38 AGNs selected from the XMM-Newton serendipitous source catalogue, and covers a broad range of scattering fractions (approximately 0.1 - 10%), which is the fraction of scattered emission with respect to direct emission. Their spectra obtained with XMM-Newton and/or Suzaku are analyzed to calculate scattering fractions and we find eight objects with a very small scattering fraction (, Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574128, レポート番号: JAXA-SP-09-008E

Published
2010

243. Suzaku Observation of the Radio Galaxy 4C 50.55 ( IGR J 21247+5058 )

Author

Tazaki, Fumie, Ueda, Yoshihiro, Ishino, Yukiko, Eguchi, Satoshi, Isobe, Naoki, Terashima, Yuichi, and Mushotzky, Richard F.

Subjects
galaxies: active - galaxies: individual (4C 50.55) - X-rays: galaxies
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We present preliminary results from a 100 ksec Suzaku observation of 4C 50.55 (IGR J 21247+5058). 4C 50.55 is the brightest broad line radio galaxy in the hard X-ray (>10 keV) band detected with INTEGRAL and Swift, which is located close to the Galactic plane. From a combination of the XIS and HXD, we are for the first time able to obtain simultaneous broad-band spectra of this source. A rapid flux increase by approximately 20% is found in the XIS light curve in the last 20 ksec exposure. The spectra before the flux rise can be well represented by a partially absorbed cutoff power law with a reflection component. The cutoff energy is found to be 46(sup +3)(sub -6) keV (with a photon index of 1.60(sup +0.04)(sub -0.08)), which is lower than that observed in normal AGNs. The variable component shows a softer spectrum than the averaged spectrum, which may contain the jet emission., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574129, レポート番号: JAXA-SP-09-008E

Published
2010

244. Suzaku View of the Swift/Bat Active Galactic Nuclei. IV. Nature of Two Narrow-Line Radio Galaxies (3C 403 and IC 5063)

Author

Tazaki, Fumie, Ueda, Yoshihiro, Terashima, Yuichi, Mushotzky, Richard F., Tazaki, Fumie, Ueda, Yoshihiro, Terashima, Yuichi, and Mushotzky, Richard F.

Abstract

We report the results of Suzaku broad band X-ray observations of the two narrow-line radio galaxies (NLRGs), 3C 403 and IC 5063. Combined with the Swift/BAT spectra averaged for 58 months, we are able to accurately constrain their spectral properties over the 0.5--200 keV band. The spectra of both nuclei are well represented with an absorbed cut-off power law, an absorbed reflection component from cold matter with an iron-K emission line, and an unabsorbed soft component, which gives a firm upper limit for the scattered emission. The reflection strength normalized to the averaged BAT flux is R = \Omega/2\pi ~ 0.6 in both targets, implying that their tori have a sufficiently large solid angle to produce the reprocessed emission. A numerical torus model with an opening angle of ~ 50 deg well reproduces the observed spectra. We discuss the possibility that the amount of the normal gas responsible for Thomson scattering is systematically smaller in radio galaxies compared with Seyfert galaxies., Comment: 9 pages, 3 figures

Published
2011
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245. Suzaku View of the Swift/BAT Active Galactic Nuclei. III. Application of Numerical Torus Models to Two Nearly Compton Thick AGNs (NGC 612 and NGC 3081)

Author

Eguchi, Satoshi, Ueda, Yoshihiro, Awaki, Hisamitsu, Aird, James, Terashima, Yuichi, Mushotzky, Richard, Eguchi, Satoshi, Ueda, Yoshihiro, Awaki, Hisamitsu, Aird, James, Terashima, Yuichi, and Mushotzky, Richard

Abstract

The broad band spectra of two Swift/BAT AGNs obtained from Suzaku follow-up observations are studied: NGC 612 and NGC 3081. Fitting with standard models, we find that both sources show similar spectra characterized by a heavy absorption with $N_{\rm{H}} \simeq 10^{24} \ \rm{cm}^{-2}$, the fraction of scattered light is $f_{\rm{scat}} = 0.5-0.8%$, and the solid angle of the reflection component is $\Omega/2\pi = 0.4-1.1$. To investigate the geometry of the torus, we apply numerical spectral models utilizing Monte Carlo simulations by Ikeda et al. (2009) to the Suzaku spectra. We find our data are well explained by this torus model, which has four geometrical parameters. The fit results suggest that NGC 612 has the torus half opening-angle of $\simeq 60^{\circ}-70^{\circ}$ and is observed from a nearly edge-on angle with a small amount of scattering gas, while NGC 3081 has a very small opening angle $\simeq 15^\circ$ and is observed on a face-on geometry, more like the deeply buried "new type" AGNs found by Ueda et al. (2007). We demonstrate the potential power of direct application of such numerical simulations to the high quality broad band spectra to unveil the inner structure of AGNs., Comment: 12 pages, 7 figures, 5 tables, submitted to the Astrophysical Journal, accepted on 2010 December 30

Published
2010
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246. The ASTRO-H Mission

Author

Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Felix, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Awaki, Hisamitsu, Bamba, Aya, Bando, Nobutaka, Bautz, Mark, Blandford, Roger, Boyce, Kevin, Brown, Greg, Chernyakova, Maria, Coppi, Paolo, Costantini, Elisa, Cottam, Jean, Crow, John, de Plaa, Jelle, de Vries, Cor, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gandhi, Poshak, Gendreau, Keith, Gilmore, Kirk, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hughes, John, Hwang, Una, Iizuka, Ryo, Ishibashi, Kazunori, Ishida, Manabu, Ishimura, Kosei, Ishisaki, Yoshitaka, Isobe, Naoki, Ito, Masayuki, Iwata, Naoko, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Katsuda, Satoru, Kawaharada, Madoka, Kawai, Nobuyuki, Kawasaki, Shigeo, Khangaluyan, Dmitry, Kilbourne, Caroline, Kinugasa, Kenzo, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Kosaka, Tatsuro, Kotani, Taro, Koyama, Katsuji, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, Francois, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Miller, Jon, Mineshige, Shin, Minesugi, Kenji, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nakagawa, Yujin, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakazawa, Kazuhiro, Namba, Yoshiharu, Nomachi, Masaharu, Dell, Steve O', Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Parmer, Arvind, Petre, Robert, Pohl, Martin, Porter, Scott, Ramsey, Brian, Reynolds, Christopher, Sakai, Shin-ichiro, Sambruna, Rita, Sato, Goro, Sato, Yoichi, Serlemitsos, Peter, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugita, Hiroyuki, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tozuka, Miyako, Tsuboi, Yoko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Urry, Meg, Watanabe, Shin, White, Nicholas, Yamada, Takahiro, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Felix, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Awaki, Hisamitsu, Bamba, Aya, Bando, Nobutaka, Bautz, Mark, Blandford, Roger, Boyce, Kevin, Brown, Greg, Chernyakova, Maria, Coppi, Paolo, Costantini, Elisa, Cottam, Jean, Crow, John, de Plaa, Jelle, de Vries, Cor, Herder, Jan-Willem den, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gandhi, Poshak, Gendreau, Keith, Gilmore, Kirk, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hughes, John, Hwang, Una, Iizuka, Ryo, Ishibashi, Kazunori, Ishida, Manabu, Ishimura, Kosei, Ishisaki, Yoshitaka, Isobe, Naoki, Ito, Masayuki, Iwata, Naoko, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Katsuda, Satoru, Kawaharada, Madoka, Kawai, Nobuyuki, Kawasaki, Shigeo, Khangaluyan, Dmitry, Kilbourne, Caroline, Kinugasa, Kenzo, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Kosaka, Tatsuro, Kotani, Taro, Koyama, Katsuji, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, Francois, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Miller, Jon, Mineshige, Shin, Minesugi, Kenji, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nakagawa, Yujin, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakazawa, Kazuhiro, Namba, Yoshiharu, Nomachi, Masaharu, Dell, Steve O', Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Parmer, Arvind, Petre, Robert, Pohl, Martin, Porter, Scott, Ramsey, Brian, Reynolds, Christopher, Sakai, Shin-ichiro, Sambruna, Rita, Sato, Goro, Sato, Yoichi, Serlemitsos, Peter, Shida, Maki, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugita, Hiroyuki, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tozuka, Miyako, Tsuboi, Yoko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Urry, Meg, Watanabe, Shin, White, Nicholas, Yamada, Takahiro, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yatsu, Yoichi, Yonetoku, Daisuke, and Yoshida, Atsumasa

Abstract

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the high-energy universe by performing high-resolution, high-throughput spectroscopy with moderate angular resolution. ASTRO-H covers very wide energy range from 0.3 keV to 600 keV. ASTRO-H allows a combination of wide band X-ray spectroscopy (5-80 keV) provided by multilayer coating, focusing hard X-ray mirrors and hard X-ray imaging detectors, and high energy-resolution soft X-ray spectroscopy (0.3-12 keV) provided by thin-foil X-ray optics and a micro-calorimeter array. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft X-ray telescope (0.4-12 keV) and a non-focusing soft gamma-ray detector (40-600 keV) . The micro-calorimeter system is developed by an international collaboration led by ISAS/JAXA and NASA. The simultaneous broad bandpass, coupled with high spectral resolution of Delta E ~7 eV provided by the micro-calorimeter will enable a wide variety of important science themes to be pursued., Comment: 18 pages, 12 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray"

Published
2010
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247. Scattered X-rays in Obscured Active Galactic Nuclei and their Implications for Geometrical Structure and Evolution

Author

Noguchi, Kazuhisa, Terashima, Yuichi, Ishino, Yukiko, Hashimoto, Yasuhiro, Koss, Michael, Ueda, Yoshihiro, Awaki, Hisamitsu, Noguchi, Kazuhisa, Terashima, Yuichi, Ishino, Yukiko, Hashimoto, Yasuhiro, Koss, Michael, Ueda, Yoshihiro, and Awaki, Hisamitsu

Abstract

We construct a new sample of 32 obscured active galactic nuclei (AGNs) selected from the Second XMM-Newton Serendipitous Source Catalogue to investigate their multiwavelength properties in relation to the "scattering fraction", the ratio of the soft X-ray flux to the absorption-corrected direct emission. The sample covers a broad range of the scattering fraction (0.1%-10%). A quarter of the 32 AGNs have a very low scattering fraction (smaller than 0.5%), which suggests that they are buried in a geometrically thick torus with a very small opening angle. We investigate correlations between the scattering fraction and multiwavelength properties. We find that AGNs with a small scattering fraction tend to have low [O III]lambda5007/X-ray luminosity ratios. This result agrees with the expectation that the extent of the narrow-line region is small because of the small opening angle of the torus. There is no significant correlation between scattering fraction and far-infrared luminosity. This implies that a scale height of the torus is not primarily determined by starburst activity. We also compare scattering fraction with black hole mass or Eddington ratio and find a weak anti-correlation between the Eddington ratio and scattering fraction. This implies that more rapidly growing supermassive black holes tend to have thicker tori., Comment: 13 pages, 10 figures, accepted for publication in ApJ

Published
2010
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248. Suzaku Observation of the Brightest Broad-Line Radio Galaxy 4C 50.55 (IGR J 21247+5058)

Author

Tazaki, Fumie, Ueda, Yoshihiro, Ishino, Yukiko, Eguchi, Satoshi, Isobe, Naoki, Terashima, Yuichi, Mushotzky, Richard F., Tazaki, Fumie, Ueda, Yoshihiro, Ishino, Yukiko, Eguchi, Satoshi, Isobe, Naoki, Terashima, Yuichi, and Mushotzky, Richard F.

Abstract

We report the results from a deep Suzaku observation of 4C 50.55 (IGR J 21247+5058), the brightest broad-line radio galaxy in the hard X-ray (> 10 keV) sky. The simultaneous broad band spectra over 1-60 keV can be represented by a cut-off power law with two layers of absorption and a significant reflection component from cold matter with a solid angle of \Omega/2\pi \approx 0.2. A rapid flux rise by ~ 20% over 2 \times 10^4 sec is detected in the 2-10 keV band. The spectral energy distribution suggests that there is little contribution to the total X-ray emission from jets. Applying a thermal Comptonization model, we find that corona is optically thick (\tau_e \approx 3) and has a relatively low temperature (kT_e \approx 30 keV). The narrow iron-K emission line is consistent with a picture where the standard disk is truncated and/or its inner part is covered by optically thick Comptonizing corona smearing out relativistic broad line features. The inferred disk structure may be a common feature of accretion flows onto black holes that produce powerful jets., Comment: 8 pages, 7 figures

Published
2010
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249. A New Sample of Buried Active Galactic Nuclei Selected from the Second XMM-Newton Serendipitous Source Catalogue

Author

Noguchi, Kazuhisa, Terashima, Yuichi, Awaki, Hisamitsu, Noguchi, Kazuhisa, Terashima, Yuichi, and Awaki, Hisamitsu

Abstract

We present the results of X-ray spectral analysis of 22 active galactic nuclei (AGNs) with a small scattering fraction selected from the Second XMM-Newton Serendipitous Source Catalogue using hardness ratios. They are candidates of buried AGNs, since a scattering fraction, which is a fraction of scattered emission by the circumnuclear photoionized gas with respect to direct emission, can be used to estimate the size of the opening part of an obscuring torus. Their X-ray spectra are modeled by a combination of a power law with a photon index of 1.5-2 absorbed by a column density of 10^23-24 cm^-2, an unabsorbed power law, narrow Gaussian lines, and some additional soft components. We find that scattering fractions of 20 among 22 objects are less than a typical value (3%) for Seyfert2s observed so far. In particular, those of eight objects are smaller than 0.5%, which are in the range for buried AGNs found in recent hard X-ray surveys. Moreover, [O III] lambda5007 luminosities at given X-ray luminosities for some objects are smaller than those for Seyfert2s previously known. This fact could be interpreted as a smaller size of optical narrow emission line regions produced in the opening direction of the obscuring torus. These results indicate that they are strong candidates for the AGN buried in a very geometrically thick torus., Comment: To appear in ApJ, 14 pages, 6 figures

Published
2009
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250. Spectral Variation of the Seyfert 1 Galaxy MCG-6-30-15 observed with Suzaku

Author

Miyakawa, Takehiro, Ebisawa, Ken, Terashima, Yuichi, Tsuchihashi, Fuminori, Inoue, Hajime, Zycki, Piotr, Miyakawa, Takehiro, Ebisawa, Ken, Terashima, Yuichi, Tsuchihashi, Fuminori, Inoue, Hajime, and Zycki, Piotr

Abstract

We have investigated spectral variation of the Seyfert 1 galaxy MCG-6-30-15 observed with Suzaku in January 2006 for three separate periods spreading over fourteen days. We found that the time-averaged continuum energy spectrum between 1 keV and 40 keV can be approximated with a spectral model composed of the direct power-law component, its reflection component, two warm absorbers with different ionization states, and neutral absorption. We have taken two approaches to study its spectral variation at various timescales: The first approach is to make intensity-sliced spectra and study correlation between the intensity and spectral shape. The second approach is to study spectral changes between the intervals when the source flux is above ("bright state") and below ("faint state") the average for fixed time-intervals. In both approaches, we found a clear correlation between the intensity in the 6 -- 10 keV band and the spectral ratio of 0.5 -- 3.0 keV/6.0-- 10 keV. Such a spectral variation requires change of the apparent slope of the direct component, whereas the shape and intensity of the reflection component being invariable. The observed apparent spectral change is explained by variation of the ionization degree of one of the two warm absorbers due to intrinsic source luminosity variation. Current results suggest that the warm absorber has a critical role to explain the observed continuum spectral shape and variation of MCG-6-30-15, which is essential to constrain parameters of the putatively broadened iron line emission feature., Comment: 11 pages, accepted for publication in PASJ

Published
2009
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