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68 results on '"Kubota, Aya"'

1. Evaluation of the initial pointing accuracy of XRISM

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Kanemaru, Yoshiaki, Iizuka, Ryo, Maeda, Yoshitomo, Okajima, Takashi, Hayashi, Takayuki, Kiyokane, Kazuhiro, Nihei, Yuto, Kominato, Takashi, Ishida, Manabu, Natsukari, Chikara, Watanabe, Shin, Sato, Kosuke, Terada, Yukikatsu, Hayashi, Katsuhiro, Baluta, Chris, Yoshida, Tessei, Hoshino, Akio, Ogawa, Shoji, Fukushima, Kotaro, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kubota, Aya, Ota, Naomi, Shidatsu, Megumi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Tomokage, Yoneyama, Yamada, Satoshi, Uchida, Nagomi, Sato, Rie, Holland, Matt, Loewenstein, Michael, Miller, Eric, Yaqoob, Tahir, Hill, Robert, Doyle, Trisha, Perez-Solis, Efrain, Waddy, Morgan, Mekosh, Mark, Fox, Joseph, Tashiro, Makoto, Toda, Kenichi, and Maejima, Hironori

Published
2024
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2. Detail design of the XRISM timing system and its verification in the nominal operation mode

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Terada, Yukikatsu, Shidatsu, Megumi, Sawada, Makoto, Kominato, Takashi, Kato, So, Sato, Ryohei, Sakama, Minami, Shioiri, Takumi, Niida, Yuki, Natsukari, Chikara, Tashiro, Makoto S., Toda, Kenichi, Maejima, Hironori, Hayashi, Katsuhiro, Yoshida, Tessei, Ogawa, Shoji, Kanemaru, Yoshiaki, Hoshino, Akio, Fukushima, Kotaro, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kubota, Aya, Ota, Naomi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Yoneyama, Tomokage, Yamada, Satoshi, Uchida, Nagomi, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Baluta, Chris, Holland, Matt, Loewenstein, Michael, Miller, Eric D., Yaqoob, Tahir, Hill, Robert S., Doyle, Trisha F., Perez-Solis, Efrain, Waddy, Morgan D., Mekosh, Mark, Fox, Joseph B., Takagi, Toshihiro, Motogami, Yugo, Pottschmidt, Katja, Enoto, Teruaki, and Tanaka, Takaaki

Published
2024
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3. The in-orbit XRISM science operations

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Hayashi, Katsuhiro, Tashiro, Makoto, Terada, Yukikatsu, Yoshida, Tessei, Ogawa, Shoji, Kanemaru, Yoshiaki, Fukushima, Kotaro, Hoshino, Akio, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kitaguchi, Takao, Kubota, Aya, Ota, Naomi, Shidatsu, Megumi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Yoneyama, Tomokage, Yamada, Satoshi, Uchida, Nagomi, Sakurai, Seiko, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Baluta, Chris, Tamura, Takayuki, Fukazawa, Yasushi, Odaka, Hirokazu, Tamba, Tsubasa, Sato, Ryohei, Kato, Sou, Sakama, Minami, Shioiri, Takumi, Niida, Yuki, Sakamoto, Natsuki, Nemoto, Noboru, Omiya, Yuki, Suzuki, Nari, Takagi, Toshihiro, Motogami, Yugo, Holland, Matt, Loewenstein, Michael, Miller, Eric, Yaqoob, Tahir, Hill, Robert, Doyle, Trisha, Perez-Solis, Efrain, Waddy, Morgan, Mekosh, Mark, Fox, Joseph, Guainazzi, Matteo, Ness, Jan-Uwe, Maejima, Hironori, Toda, Ken'ichi, and Natsukari, Chikara

Published
2024
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4. Development and operation status of X-Ray Imaging and Spectroscopy Mission (XRISM)

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Tashiro, Makoto, Watanabe, Shin, Maejima, Hironori, Toda, Kenichi, Matsushita, Kyoko, Yamaguchi, Hiroya, Kelley, Richard, Reichenthal, Lillian, Hartz, Leslie, Petre, Robert, Williams, Brian, Guainazzi, Matteo, Santovincenzo, Andrea, Costantini, Elisa, Takei, Yoh, Ishisaki, Yoshitaka, Fujimoto, Ryuichi, Henegar-Leon, Joy, Sneiderman, Gary, Tomida, Hiroshi, Mori, Koji, Nakajima, Hiroshi, Terada, Yukikatsu, Holland, Matt, Loewenstein, Micheal, Kallman, Timothy, Kaastra, Jelle, Miller, Eric, Sawada, Makoto, Done, Chris, Enoto, Teruaki, Bamba, Aya, Plucinsky, Paul, Ueda, Yoshihiro, Kara, Erin, Zhuravleva, Irina, Fujita, Yutaka, Querro, Jose Antonio, Arai, Yoshitaka, Audard, Marc, Awaki, Hisamitsu, Baluta, Chris, Bando, Nobutaka, Behar, Ehud, Bialas, Thomas, Boissay-Malaquin, Rozenn, Brenneman, Laura, Brown, Gregory V., Chiao, Meng, Corrales, Lia, Cumbee, Renata, de Vries, Cor, den Herder, Jan-Willem, Diaz-Trigo, Maria, DiPirro, Michael, Dotani, Tadayasu, Ebrero Carrero, Jacobo, Ebisawa, Ken, Eckart, Megan, Eckart, Dominique, Eguchi, Satoshi, Ezoe, Yuichiro, Ferrigno, Carlo, Foster, Adam, Fukazawa, Yasushi, Fukushima, Kotaro, Furuzawa, Akihiro, Gallo, Luigi, Gorter, Nathalie, Grim, Martin, Gu, Liyi, Hagino, Koichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hell, Natalie, Hodges-Kluck, Edmund, Horiuchi, Takafumi, Hornschemeier, Ann, Hoshino, Akio, Ichinohe, Yuto, Ikuta, Chisato, Iizuka, Ryo, Ishi, Daiki, Ishida, Manabu, Ishihama, Naoki, Ishikawa, Kumi, Ishimura, Kosei, Jaffe, Tess, Katsuda, Satoru, Kanemaru, Yoshiaki, Kenyon, Steven, Kilbourne, Caroline, Kimball, Mark, Kitamoto, Shunji, Kobayashi, Shogo, Kobayashi, Akihide, Kohmura, Takayoshi, Kubota, Aya, Leutenegger, Maurice, Li, Muzi, Maeda, Yoshitomo, Markevitch, Maxim, Matsumoto, Hironori, Matsuzaki, Keiichi, McCammon, Dan, McLaughlin, Brian, McNamara, Brian, Miko, Joseph, Miller, Jon, Minesugi, Kenji, Mitani, Shinji, Mitsuishi, Ikuyuki, Mizumoto, Misaki, Mizuno, Tsunefumi, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakazawa, Kazuhiro, Natsukari, Chikara, Ness, Jan-Uwe, Nigo, Kenichiro, Nishiyama, Mari, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Mina, Ogawa, Shoji, Okajima, Takashi, Okamoto, Atsushi, Ota, Naomi, Ozaki, Masanobu, Paltani, Stephane, Porter, F. Scott, Pottschmidt, Katja, Sasaki, Takahiro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sato, Yoichi, Seta, Hiromi, Shida, Maki, Shidatsu, Megumi, Shigeto, Shuhei, Shipman, Russel, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Smith, Randall, Soong, Yang, Suzuki, Hiromasa, Szymkowiak, Andy, Takahashi, Hiromitsu, Takeo, Mai, Tamagawa, Toru, Tamura, Keisuke, Tanaka, Takaaki, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Uno, Shinichiro, Van der Meer, Erik, Vink, Jacco, Wittheof, Michael, Wolfs, Rob, Yamada, Satoshi, Yamada, Shinya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yanagase, Keiichi, Yaqoob, Tahir, Yasuda, Susumu, Yoneyama, Tomokage, and Yoshida, Tessei

Published
2024
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5. X-ray iron absorption line in Swift J1858.6−0814

Author

Asai, Kazumi, Mihara, Tatehiro, Sakai, Kento, and Kubota, Aya

Abstract

We present the spectral analysis of bright steady states in an outburst of the transient neutron star low-mass X-ray binary Swift J1858.6−0814 observed with the Neutron star Interior Composition Explorer (NICER). We detected an ionized iron K absorption line (H-like Fe) at 6.97 keV in the spectrum. We estimate the photoionization parameter using the ratio of the equivalent widths of the Fe xxvi(H-like) (17 ± 5 eV) and Fe xxv(He-like) (<3 eV) and discuss the origin of the iron absorption line. The irradiated gas producing the absorption line would locate within (3–6) × 109cm of the X-ray source. We suggest that the observed H-like Fe absorption line originates from the highly ionized gas in the inner accretion disk in Swift J1858.6−0814.

Published
2024
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6. Verification of the XRISM timing system in the GPS unsynchronized mode

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Shidatsu, Megumi, Terada, Yukikatsu, Kominato, Takashi, Kato, So, Sato, Ryohei, Sakama, Minami, Shioiri, Takumi, Motogami, Yugo, Niida, Yuki, Takagi, Toshihiro, Natsukari, Chikara, Tashiro, Makoto S., Toda, Kenichi, Maejima, Hironori, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Baluta, Chris, Hayashi, Katsuhiro, Yoshida, Tessei, Ogawa, Shoji, Kanemaru, Yoshiaki, Fukushima, Kotaro, Hoshino, Akio, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Nakazawa, Kazuhiro, Uno, Shin'ichiro, Ebisawa, Ken, Eguchi, Satoshi, Katsuda, Satoru, Kubota, Aya, Ota, Naomi, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Yoneyama, Tomokage, Yamada, Satoshi, Uchida, Nagomi, Holland, Matt, Loewenstein, Michael, Miller, Eric D., Yaqoob, Tahir, Hill, Robert S., Doyle, Trisha F., Perez-Solis, Efrain, Waddy, Morgan D., Mekosh, Mark, and Fox, Joseph B.

Published
2024
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8. The ASTRO-H (Hitomi) x-ray astronomy satellite

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Takahashi, Tadayuki, Kokubun, Motohide, Mitsuda, Kazuhisa, Kelley, Richard, Ohashi, Takaya, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall, Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura, Brown, Greg, Bulbul, Esra, Cackett, Edward, Canavan, Edgar, Chernyakova, Maria, Chiao, Meng, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, den Herder, Jan-Willem, 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, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gilmore, Kirk, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harayama, Atsushi, Harrus, Ilana, Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Yoshiyuki, Inoue, Hajime, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline, Kimball, Mark, King, Ashley, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, François, Lee, Shiu-Huang, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McGuinness, Daniel, McNamara, Brian, Mehdipour, Missagh, Miko, Joseph, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Moroso, Franco, Moseley, Harvey, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Nobukawa, Kumiko, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve, Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frederik, Paltani, Stéphane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Pontius, James, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Shin-ichiro, Sakai, Kazuhiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Yoichi, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shidatsu, Megumi, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Łukasz, 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, 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, Shin'ichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, Wik, Daniel, Wilkins, Dan, Williams, Brian, 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, and Zoghbi, Abderahmen

Published
2016
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9. Xappl: software framework for the XRISM pre-pipeline

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Eguchi, Satoshi, Tashiro, Makoto, Terada, Yukikatsu, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Uno, Shin'ichiro, Kubota, Aya, Nakazawa, Kazuhiro, Watanabe, Shin, Iizuka, Ryo, Sato, Rie, Yoneyama, Tomokage, Baluta, Chris, Ebisawa, Ken, Fukazawa, Yasushi, Hayashi, Katsuhiro, Kato, So, Katsuda, Satoru, Kitaguchi, Takao, Odaka, Hirokazu, Ohno, Masanori, Ota, Naomi, Sakama, Minami, Sato, Ryohei, Shidatsu, Megumi, Sugawara, Yasuharu, Tamba, Tsubasa, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Nagomi, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, Sakano, Masaaki, Yoshida, Tessei, and Yamada, Satoshi

Published
2022
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10. A broadband x-ray imaging spectroscopy in the 2030s: the FORCE mission

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Mori, Koji, Tsuru, Takeshi G., Nakazawa, Kazuhiro, Ueda, Yoshihiro, Watanabe, Shin, Tanaka, Takaaki, Ishida, Manabu, Matsumoto, Hironori, Awaki, Hisamitsu, Murakami, Hiroshi, Nobukawa, Masayoshi, Takeda, Ayaki, Fukazawa, Yasushi, Tsunemi, Hiroshi, Takahashi, Tadayuki, Hornschemeier, Ann, Okajima, Takashi, Zhang, William W., Williams, Brian J., Venters, Tonia, Madsen, Kristin, Yukita, Mihoko, Akamatsu, Hiroki, Bamba, Aya, Enoto, Teruaki, Fujita, Yutaka, Furuzawa, Akihiro, Hagino, Kouichi, Ishimura, Kosei, Itoh, Masayuki, Kitayama, Tetsu, Kobayashi, Shogo, Kohmura, Takayoshi, Kubota, Aya, Mizumoto, Misaki, Mizuno, Tsunefumi, Nakajima, Hiroshi, Nobukawa, Kumiko K., Noda, Hirofumi, Odaka, Hirokazu, Ota, Naomi, Sato, Toshiki, Shidatsu, Megumi, Suzuki, Hiromasa, Takahashi, Hiromitsu, Tanimoto, Atsushi, Terada, Yukikatsu, Terashima, Yuichi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Yamaguchi, Hiroya, and Yatsu, Yoichi

Published
2022
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11. The Roles of Cultural Spaces in Malaysia's Historic Towns: The Case of Kuala Dungun and Taiping

Author

Lai, Lee Yoke, Said, Ismail, and Kubota, Aya

Abstract

Cultural space constitutes the physical, cultural and perceptual attributes of a place that creates social phenomenon and place meaning. Nevertheless, cultural spaces in Malaysia's historic town were facing alteration which resulted to place declining and placelessness. Thus, this paper discusses the roles of cultural spaces that characterised the historic town's identity of Kuala Dungun and Taiping. A case study method was conducted involving site observation and questionnaire survey to collect residents’ cultural experiences. Results indicated that cultural spaces generated from routine activity, sociocultural and economic vitality contributed to identity of the historic towns.

Published
2013
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12. Memory Association in Place Making: A review

Author

Othman, Sumaiyah, Nishimura, Yukio, and Kubota, Aya

Abstract

People experience present world that is causally connected physically and mentally with past events and objects. This study is to present a synthesis of literature studies from 1990 to 2010 with relation to memory association in place making. Aspects taken into consideration include methodological issue and factor used within the city centre from the person memory and perceptions, followed by the associations between place and memory. In summary, one's memory and perception of the environment are shaped by three components; role of event, history and monument remembrance of a place that enables us to perceive a place through memory association.

Published
2013
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13. X-Ray and Near-Infrared Observations of GX 339−4 in the Low/Hard State with Suzaku and IRSF

Author

Shidatsu, Megumi, Ueda, Yoshihiro, Tazaki, Fumie, Yoshikawa, Tatsuhito, Nagayama, Takahiro, Nagata, Tetsuya, Oi, Nagisa, Yamaoka, Kazutaka, Takahashi, Hiromitsu, Kubota, Aya, Cottam, Jean, Remillard, Ronald, and Negoro, Hitoshi

Abstract

X-ray and near-infrared ( $J$– $H$– $K_{\rm s}$) observations of the galactic black-hole binary GX 339 $-$4 in the low/hard state were performed with Suzaku and IRSF in 2009 March. The spectrum in the 0.5–300 keV band is dominated by thermal Comptonization of multicolor disk photons, with a small contribution from a direct disk component, indicating that the inner disk is almost fully covered by hot corona with an electron temperature of $\approx$175 keV. The Comptonizing corona has at least two optical depths, $\tau$$\approx$1, 0.4. Analysis of the iron-K line profile yields an inner-disk radius of (13.3 $^{+6.4}_{-6.0}$) $\ R_{\rm g}$( $\ R_{\rm g}$represents the gravitational radius $GM/c^2$), with the best-fit inclination angle of $\approx$50 $^\circ$. This radius is consistent with that estimated from the continuum fit by assuming the conservation of photon numbers in Comptonization. Our results suggest that the standard disk of GX 339 $-$4 is likely truncated before reaching the innermost stable circular orbit (for a non-rotating black hole) in the low/hard states at $\sim\ $1% of the Eddington luminosity. The one-day averaged near-infrared light curves are found to be correlated with hard X-ray flux with $F_{\rm Ks}$$\propto$$F_{\rm X}^{0.45}$. The flatter near-infrared $\nu F_{\nu}$spectrum than the radio one suggests that the optically thin synchrotron radiation from the compact jets dominates the near-infrared flux. Based on a simple analysis, we estimate the magnetic field and size of the jet base to be 5 $\times$10 $^{4}\ $G and 6 $\times$10 $^{8}\ $cm, respectively. The synchrotron self Compton component is estimated to be approximately 0.4% of the total X-ray flux.

Published
2011
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14. TESTING ACCRETION DISK STRUCTURE WITH SUZAKU DATA OF LMC X-3

Author

Kubota, Aya, Done, Chris, Davis, Shane W., Dotani, Tadayasu, Mizuno, Tsunefumi, and Ueda, Yoshihiro

Abstract

The Suzaku observation of LMC X-3 gives the best data to date on the shape of the accretion disk spectrum. This is due to the combination of very low absorbing column density along this line of sight, which allows the shape of the disk emission to be constrained at low energies by the CCDs while the tail can be simultaneously determined up to 30 keV by the high-energy detectors. These data clearly demonstrate that the observed disk spectrum is broader than a simple "sum of blackbodies," and relativistic smearing of the emission is strongly required. However, the intrinsic emission should be more complex than a (color-corrected) sum of blackbodies as it should also contain photoelectric absorption edges from the partially ionized disk photosphere. These are broadened by the relativistic smearing, but the models predict [?]3%-5% deviations for 1/3-1 solar abundance around the edge energies, significantly stronger than observed. This indicates that the models need to include more physical processes such as self-irradiation, bound-bound (line) absorption, and/or emission from recombination continua and/or lines. Alternatively, if none of these match the data, it may instead require that the accretion disk density and/or emissivity profile with height is different to that assumed. Thus, these data demonstrate the feasibility of observational tests of our fundamental understanding of the vertical structure of accretion disks.

Published
2010

15. Spectral Transitions of an Ultraluminous X-Ray Source, NGC 2403 Source 3

Author

Isobe, Naoki, Makishima, Kazuo, Takahashi, Hiromitsu, Mizuno, Tsunefumi, Miyawaki, Ryouhei, Gandhi, Poshak, Kawaharada, Madoka, Senda, Atsushi, Yoshida, Tessei, Kubota, Aya, and Kobori, Hiroshi

Abstract

A Suzaku observation of an ultraluminous X-ray source, NGC 2403 Source 3, performed on 2006 March 16–17, is reported. The Suzaku XIS spectrum of Source 3 was described as multi-color black-body-like emission from an optically thick accretion disk. The innermost disk temperature and radius were measured to be $T_{\rm in}$$=$1.08$_{-0.03}^{+0.02}$keV and $R_{\rm in}$$=$122.1$_{-6.8}^{+7.7} \ \alpha^{1/2}$km, respectively, where $\alpha$$=$(cos 60$^\circ /$cos $i$) with $i$being the disk inclination. Its bolometric luminosity was estimated to be $L_{\rm bol}$$=$1.82 $\times$10$^{39}\alpha $ergs$^{-1}$. Archival Chandra and XMM-Newton data of the source were analyzed. In almost all observations, the source showed multi-color black-body-like X-ray spectra with parameters similar to those of the Suzaku observation. In only one Chandra observation, however, Source 3 exhibited a power-law-like spectrum, with a photon index of $\Gamma$$=$2.37$\pm$0.08, when it was fainter by $\sim$15% than in the Suzaku observation. This behavior is explained in terms of a transition between a slim-disk state and “very high” states, both found in Galactic black hole binaries, when their luminosity apporached the Eddington limit. These results are utilized to argue that ultraluminous X-ray sources generally have significantly higher masses than ordinary stellar-mass black holes.

Published
2009
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16. X-Ray Spectral Variability of the Seyfert Galaxy NGC 4051 Observed with Suzaku

Author

Terashima, Yuichi, Gallo, Luigi C., Inoue, Hirohiko, Markowitz, Alex G., Reeves, James N., Anabuki, Naohisa, Fabian, Andrew C., Griffiths, Richard E., Hayashida, Kiyoshi, Itoh, Takeshi, Kokubun, Norihide, Kubota, Aya, Miniutti, Giovanni, Takahashi, Tadayuki, Yamauchi, Makoto, and Yonetoku, Daisuke

Abstract

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

Published
2009
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17. Suzaku Observations of M 82 X-1 : Detection of a Curved Hard X-Ray Spectrum

Author

Miyawaki, Ryohei, Makishima, Kazuo, Yamada, Shin’ya, Gandhi, Poshak, Mizuno, Tsunefumi, Kubota, Aya, Tsuru, Takeshi G., and Matsumoto, Hironori

Abstract

A report is presented on Suzaku observations of the ultra-luminous X-ray source X-1 in the starburst galaxy M 82, made three times in 2005 October for an exposure of $\sim$30 ks each. The XIS signals from a region of radius 3$^\prime$around the nucleus defined a 2–10 keV flux of 2.1$\times$10$^{-11}$ergs$^{-1}$cm$^{-2}$attributable to point sources. The 3.2–10 keV spectrum was slightly more convex than a power-law with a photon index of 1.7. In all observations, the HXD also detected signals from M 82 up to $\sim$20 keV, at a 12-20 keV flux of 4.4$\times$10$^{-12}$ergs$^{-1}$cm$^{-2}$. The HXD spectrum was steeper than that of the XIS. The XIS and HXD spectra can be jointly reproduced by a cutoff power-law model, or similar curved models. Of the detected wide-band signals, 1$/$3 to 2$/$3 are attributable to X-1, while the remainder to other discrete sources in M 82. Regardless of the modeling of these contaminants, the spectrum attributable to X-1 is more curved than a power-law, with a bolometric luminosity of (1.5–3)$\times$10$^{40}$ergs$^{-1}$. These results are interpreted as Comptonized emission from a black hole of 100–200 solar masses, radiating roughly at the Eddington luminosity.

Published
2009
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18. Suzaku Results on Cygnus X-1 in the Low/Hard State

Author

Makishima, Kazuo, Takahashi, Hiromitsu, Yamada, Shin’ya, Done, Chris, Kubota, Aya, Dotani, Tadayasu, Ebisawa, Ken, Itoh, Takeshi, Kitamoto, Shunji, Negoro, Hitoshi, Ueda, Yoshihiro, and Yamaoka, Kazutaka

Abstract

The black-hole binary Cygnus X-1 was observed for 17ks with the Suzaku X-ray observatory in 2005 October, while it was in a low/hard state with a 0.7-300keV luminosity of $4.6\times 10^{37}$ergs $^{-1}$. The XIS and HXD spectra, spanning 0.7-400keV, were reproduced successfully, incorporating a cool accretion disk and a hot Comptonizing corona. The corona is characterized by an electron temperature of $ \sim$100keV, and two optical depths of $ \sim$0.4 and $ \sim$1.5, which account for the softer and harder continua, respectively. The disk has an innermost temperature of $ \sim$0.2keV, and is thought to protrude half way into the corona. The disk not only provides seed photons to the Compton cloud, but also produces a soft spectral excess, a mild reflection hump, and a weakly broadened iron line. A comparison with the Suzaku data on GRO J1655 $-$40 reveals several interesting spectral differences, which can mostly be attributed to inclination effects, assuming that the disk has a flat geometry while the corona is grossly spherical. An intensity-sorted spectroscopy indicates that the continuum becomes less Comptonized when the source flares up on time scales of 1-200s, while the underlying disk remains unchanged.

Published
2008
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19. Low/Hard State Spectra of GRO J1655$-$40 Observed with Suzaku

Author

Takahashi, Hiromitsu, Fukazawa, Yasushi, Mizuno, Tsunefumi, Hirasawa, Ayumi, Kitamoto, Shunji, Sudoh, Keisuke, Ogita, Takayuki, Kubota, Aya, Makishima, Kazuo, Itoh, Takeshi, Parmar, Arvind N., Ebisawa, Ken, Naik, Sachindra, Dotani, Tadayasu, Kokubun, Motohide, Ohnuki, Kousuke, Takahashi, Tadayuki, Yaqoob, Tahir, Angelini, Lorella, Ueda, Yoshihiro, Yamaoka, Kazutaka, Kotani, Taro, Kawai, Nobuyuki, Namiki, Masaaki, Kohmura, Takayoshi, and Negoro, Hitoshi

Abstract

The Galactic black-hole binary GROJ1655$-$40, a source harboring superluminal jets, was observed with Suzaku on 2005 September 22-23. The source was detected over a broad and continuous energy range of 0.7-300keV, with an intensity of $\sim$50mCrab at 20keV. At a distance of 3.2kpc, the 0.7-300keV luminosity was $\sim$5.2$\times$10$^{36}$ergs$^{-1}$($\sim$0.7% of the Eddington luminosity for a 6 $M_{\odot}$black hole). The source was in a typical low/hard state, exhibiting a power-law shaped continuum with a photon index of $\sim$1.6. During the observation, the source intensity gradually decreased by 25% at energies above $\sim$3keV, and by 35% below 2keV. This, together with the soft X-ray spectra taken with the X-ray Imaging Spectrometer (XIS), suggests the presence of an independent soft component that can be represented by emission from a cool ($\sim$0.2keV) disk. The hard X-ray spectra obtained with the Hard X-ray Detector reveal a high-energy spectral cutoff, with an $e$-folding energy of $\sim$200keV. The entire 0.7-300keV spectrum cannot be reproduced by a single thermal Comptonization model, even when considering reflection effects. Instead, the spectrum (except the soft excess) can be successfully explained by invoking two thermal-Comptonization components with different $y$-parameters. In contrast to the high/soft state spectra of this object, in which narrow iron absorption lines are detected with equivalent widths of 60-100eV, the present XIS spectra bear no such features beyond an upper-limit equivalent width of 23eV.

Published
2008
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20. Discovery of a Bright Transient Ultraluminous X-Ray Source, Suzaku J1305–4931 in NGC4945

Author

Isobe, Naoki, Kubota, Aya, Makishima, Kazuo, Gandhi, Poshak, Griffiths, Richard E., Dewangan, Gulab C., Itoh, Takeshi, and Mizuno, Tsunefumi

Abstract

An X-ray source, Suzaku J1305$-$4931, was discovered in the south-west arm of a nearby Seyfert II galaxy, NGC4945, at 0.5-10keV flux of $2.2 \times 10^{-12}$ergcm$^{-2}$s$^{-1}$during a Suzaku observation conducted on 2006 January 15-17. It was undetectable in a shorter observation on 2005 August 22-23, with an upper limit of $1.7 \times 10^{-14}$ergcm$^{-2}$s$^{-1}$. At a distance of 3.7Mpc, the bolometric luminosity of the source became $L_{\rm bol} = 4.4 \times 10^{39} \alpha$ergs$^{-1}$, where $\alpha = ({\rm\cos} 60^\circ \!/ \cos i)$and $i$is the disk inclination. The time-averaged X-ray spectrum of the source is described by a multi-color disk model, with an innermost disk temperature of $T_{\rm in} = 1.69_{-0.05}^{+0.06}$keV. It varied by a factor of $2$in intensity, following a clear correlation of $L_{\rm bol} \propto T_{\rm in}^4$. The innermost disk radius is inferred to stay constant at $R_{\rm in} = 79_{-3.9}^{+4.0} \alpha^{1/2}$km, suggesting the presence of a standard accretion disk. Relating $R_{\rm in}$with the last stable orbit around a non-rotating black hole yields a rather low black-hole mass, $\sim 9 \alpha^{1/2}$solar masses, which would imply that the source is shining at a considerable super-Eddington luminosity. These results can be better interpreted by invoking sub-Eddington emission from a rapidly spinning black hole with 20-130 solar masses.

Published
2008
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21. In-Orbit Performance of the Hard X-Ray Detector on Board Suzaku

Author

Kokubun, Motohide, Makishima, Kazuo, Takahashi, Tadayuki, Murakami, Toshio, Tashiro, Makoto, Fukazawa, Yasushi, Kamae, Tuneyoshi, Madejski, Greg M., Nakazawa, Kazuhiro, Yamaoka, Kazutaka, Terada, Yukikatsu, Yonetoku, Daisuke, Watanabe, Shin, Tamagawa, Toru, Mizuno, Tsunefumi, Kubota, Aya, Isobe, Naoki, Takahashi, Isao, Sato, Goro, Takahashi, Hiromitsu, Hong, Soojing, Kawaharada, Madoka, Kawano, Naomi, Mitani, Takefumi, Murashima, Mio, Suzuki, Masaya, Abe, Keiichi, Miyawaki, Ryouhei, Ohno, Masanori, Tanaka, Takaaki, Yanagida, Takayuki, Itoh, Takeshi, Ohnuki, Kousuke, Tamura, Ken-ichi, Endo, Yasuhiko, Hirakuri, Shinya, Hiruta, Tatsuro, Kitaguchi, Takao, Kishishita, Tetsuichi, Sugita, Satoshi, Takahashi, Takuya, Takeda, Shin’ichiro, Enoto, Teruaki, Hirasawa, Ayumi, Katsuta, Jun’ichiro, Matsumura, Satoshi, Onda, Kaori, Sato, Mitsuhiro, Ushio, Masayoshi, Ishikawa, Shin-nosuke, Murase, Koichi, Odaka, Hirokazu, Suzuki, Masanobu, Yaji, Yuichi, Yamada, Shinya, Yamasaki, Tomonori, and Yuasa, Takayuki

Abstract

The in-orbit performance and calibration of the Hard X-ray Detector (HXD) on board the X-ray astronomy satellite Suzaku are described. Its basic performances, including a wide energy bandpass of 10–600 keV, energy resolutions of $\sim 4 \,\mathrm{keV}$(FWHM) at 40 keV and $\sim 11\%$at 511 keV, and a high background rejection efficiency, have been confirmed by extensive in-orbit calibrations. The long-term gains of PIN-Si diodes have been stable within 1% for half a year, and those of scintillators have decreased by 5–20%. The residual non-X-ray background of the HXD is the lowest among past non-imaging hard X-ray instruments in energy ranges of 15–70 and 150–500 keV. We provide accurate calibrations of energy responses, angular responses, timing accuracy of the HXD, and relative normalizations to the X-ray CCD cameras using multiple observations of the Crab Nebula.

Published
2007
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22. Hard X-Ray Detector (HXD) on Board Suzaku

Author

Takahashi, Tadayuki, Abe, Keiichi, Endo, Manabu, Endo, Yasuhiko, Ezoe, Yuuichiro, Fukazawa, Yasushi, Hamaya, Masahito, Hirakuri, Shinya, Hong, Soojing, Horii, Michihiro, Inoue, Hokuto, Isobe, Naoki, Itoh, Takeshi, Iyomoto, Naoko, Kamae, Tuneyoshi, Kasama, Daisuke, Kataoka, Jun, Kato, Hiroshi, Kawaharada, Madoka, Kawano, Naomi, Kawashima, Kengo, Kawasoe, Satoshi, Kishishita, Tetsuichi, Kitaguchi, Takao, Kobayashi, Yoshihito, Kokubun, Motohide, Kotoku, Jun’ichi, Kouda, Manabu, Kubota, Aya, Kuroda, Yoshikatsu, Madejski, Greg, Makishima, Kazuo, Masukawa, Kazunori, Matsumoto, Yukari, Mitani, Takefumi, Miyawaki, Ryohei, Mizuno, Tsunefumi, Mori, Kunishiro, Mori, Masanori, Murashima, Mio, Murakami, Toshio, Nakazawa, Kazuhiro, Niko, Hisako, Nomachi, Masaharu, Okada, Yuu, Ohno, Masanori, Oonuki, Kousuke, Ota, Naomi, Ozawa, Hideki, Sato, Goro, Shinoda, Shingo, Sugiho, Masahiko, Suzuki, Masaya, Taguchi, Koji, Takahashi, Hiromitsu, Takahashi, Isao, Takeda, Shin’ichiro, Tamura, Ken-ichi, Tamura, Takayuki, Tanaka, Takaaki, Tanihata, Chiharu, Tashiro, Makoto, Terada, Yukikatsu, Tominaga, Shin’ya, Uchiyama, Yasunobu, Watanabe, Shin, Yamaoka, Kazutaka, Yanagida, Takayuki, and Yonetoku, Daisuke

Abstract

The Hard X-ray Detector (HXD) on board Suzaku covers a wide energy range from 10 keV to 600 keV by the combination of silicon PIN diodes and GSO scintillators. The HXD is designed to achieve an extremely low in-orbit background based on a combination of new techniques, including the concept of a well-type active shield counter. With an effective area of $142 \,\mathrm{cm}^{2}$at 20 keV and $273 \,\mathrm{cm}^{2}$at 150 keV, the background level at sea level reached $\sim 1 \times 10^{-5} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$at 30 keV for the PIN diodes, and $\sim 2 \times 10^{-5} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$at 100 keV, and $\sim 7 \times 10^{-6} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$at 200 keV for the phoswich counter. Tight active shielding of the HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of $\sim 4 \,\mathrm{cm}$thick BGO crystals, have a large effective area for sub-MeV to MeV $\gamma$-rays. They work as an excellent $\gamma$-ray burst monitor with limited angular resolution ($\sim 5^{\circ}$). The on-board signal-processing system and the data transmitted to the ground are also described.

Published
2007
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23. Suzaku Observation of Two Ultraluminous X-Ray Sources in NGC 1313

Author

Mizuno, Tsunefumi, Miyawaki, Ryohei, Ebisawa, Ken, Kubota, Aya, Miyamoto, Masao, Winter, Lisa M., Ueda, Yoshihiro, Isobe, Naoki, Dewangan, Gulab C., Done, Chris, Griffiths, Richard E., Haba, Yoshito, Kokubun, Motohide, Kotoku, Jun’ichi, Makishima, Kazuo, Matsushita, Kyoko, Mushotzky, Ricard F., Namiki, Masaaki, Petre, Robert, Takahashi, Hiromitsu, Tamagawa, Toru, and Terashima, Yuichi

Abstract

Two ultraluminous X-ray sources (ULXs) in the nearby Sb galaxy NGC 1313, named X-1 and X-2, were observed with Suzaku on 2005 September 15. During the observation for a net exposure of 28 ks (but over a gross time span of 90 ks), both objects varied in intensity by about 50%. The 0.4–10 keV X-ray luminosities of X-1 and X-2 were measured as $2.5 \times 10^{40} \,\mathrm{erg} \,\mathrm{s}^{-1}$and $5.8 \times 10^{39} \,\mathrm{erg} \,\mathrm{s}^{-1}$, respectively, with the former exhibiting the highest ever reported for this ULX. The spectrum of X-1 can be explained by the sum of a strong and variable power-law component with a high-energy cutoff, and a stable multicolor blackbody with an innermost disk temperature of $\sim 0.2 \,\mathrm{keV}$. These results suggest that X-1 was in a “very high” state, where disk emission is strongly Comptonized. The absorber within NGC 1313 toward X-1 is suggested to have a subsolar oxygen abundance. The spectrum of X-2 is best represented, in its fainter phase, by a multicolor blackbody model with an innermost disk temperature of 1.2–1.3 keV, and becomes flatter as the source becomes brighter. Hence, X-2 is interpreted to be in a slim-disk state. These results suggest that the two ULXs have black hole masses of some dozens to a few hundred of solar masses.

Published
2007
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24. Suzaku Discovery of Iron Absorption Lines in Outburst Spectra of the X-Ray Transient 4U 1630—472

Author

Kubota, Aya, Dotani, Tadayasu, Cottam, Jean, Kotani, Taro, Done, Chris, Ueda, Yoshihiro, Fabian, Andrew C., Yasuda, Tomonori, Takahashi, Hiromitsu, Fukazawa, Yasushi, Yamaoka, Kazutaka, Makishima, Kazuo, Yamada, Shinya, Kohmura, Takayoshi, and Angelini, Lorella

Abstract

We present the results of six Suzaku observations of the recurrent black hole transient 4U 1630$-$472 during its decline from outburst from February 8 to March 23 in 2006. All observations show the typical high/soft state spectral shape in the 2–50 keV band, roughly described by an optically thick-disk spectrum in the soft energy band plus a weak power-law tail that becomes dominant only above $\sim 20 \,\mathrm{keV}$. The disk temperature decreases from 1.4 keV to 1.2 keV as the flux decreases by a factor of 2, consistent with a constant radius, as expected for disk-dominated spectra. All of the observations reveal significant absorption lines from highly ionized (H-like and He-like) iron $\mathrm{K}\alpha$’s at 7.0 keV and 6.7 keV. The energies of these absorption lines suggest a blue shift with an outflow velocity of $\sim 1000 \,\mathrm{km} \,\mathrm{s}^{-1}$. The H-like iron $\mathrm{K}\alpha$equivalent width remains approximately constant at $\sim 30 \,\mathrm{eV}$over all of the observations, while that of the He-like $\mathrm{K}\alpha$line increases from 7 eV to 20 eV. Thus, the ionization state of the material decreases, as expected from the decline in flux. By fitting the profile with Voigt functions (curve of growth) together with detailed photo-ionization calculations, the total absorbing column, and the ionization parameter were estimated to be $(1.0 \hbox{--} 0.7) \times 10^{23} \,\mathrm{cm}^{-2}$and $(6 \hbox{--} 4) \times 10^4$, respectively, for a velocity dispersion of $500 \,\mathrm{km} \,\mathrm{s}^{-1}$. This in turn constrains the size of the plasma to be $\sim 10^{10} \,\mathrm{cm}$, assuming a source distance of 10 kpc.

Published
2007
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25. The X-Ray Observatory Suzaku

Author

Mitsuda, Kazuhisa, Bautz, Mark, Inoue, Hajime, Kelley, Richard L., Koyama, Katsuji, Kunieda, Hideyo, Makishima, Kazuo, Ogawara, Yoshiaki, Petre, Robert, Takahashi, Tadayuki, Tsunemi, Hiroshi, White, Nicholas E., Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Awaki, Hisamitsu, Bamba, Aya, Boyce, Kevin, Brown, Gregory V., Chan, Kai-Wing, Cottam, Jean, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Ezoe, Yuichiro, Fabian, Andrew C., Figueroa, Enectali, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furusho, Tae, Furuzawa, Akihiro, Gendreau, Keith, Griffiths, Richard E., Haba, Yoshito, Hamaguchi, Kenji, Harrus, Ilana, Hasinger, Günther, Hatsukade, Isamu, Hayashida, Kiyoshi, Henry, Patrick J., Hiraga, Junko S., Holt, Stephen S., Hornschemeier, Ann, Hughes, John P., Hwang, Una, Ishida, Manabu, Ishisaki, Yoshitaka, Isobe, Naoki, Itoh, Masayuki, Iyomoto, Naoko, Kahn, Steven M., Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Katayama, Haruyoshi, Kawai, Nobuyuki, Kilbourne, Caroline, Kinugasa, Kenzo, Kissel, Steve, Kitamoto, Shunji, Kohama, Mitsuhiro, Kohmura, Takayoshi, Kokubun, Motohide, Kotani, Taro, Kotoku, Jun’ichi, Kubota, Aya, Madejski, Greg M., Maeda, Yoshitomo, Makino, Fumiyoshi, Markowitz, Alex, Matsumoto, Chiho, Matsumoto, Hironori, Matsuoka, Masaru, Matsushita, Kyoko, McCammon, Dan, Mihara, Tatehiko, Misaki, Kazutami, Miyata, Emi, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Morii, Mikio, Moseley, Harvey, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagase, Fumiaki, Namiki, Masaaki, Negoro, Hitoshi, Nakazawa, Kazuhiro, Nousek, John A., Okajima, Takashi, ogasaka, yasushi, Ohashi, Takaya, Oshima, Tai, Ota, Naomi, Ozaki, Masanobu, Ozawa, Hideki, Parmar, Arvind N., Pence, William D., Porter, F. Scott, Reeves, James N., Ricker, George R., Sakurai, Ikuya, Sanders, Wilton T., Senda, Atsushi, Serlemitsos, Peter, Shibata, Ryo, Soong, Yang, Smith, Randall, Suzuki, Motoko, Szymkowiak, Andrew E., Takahashi, Hiromitsu, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, Tanaka, Yasuo, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tomida, Hiroshi, Torii, Ken’ichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsuru, Takeshi Go, Turner, Martin J. L., Ueda, Yoshihiro, Ueno, Shiro, Ueno, Masaru, Uno, Shin’ichiro, Urata, Yuji, Watanabe, Shin, Yamamoto, Norimasa, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamashita, Koujun, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yonetoku, Daisuke, and Yoshida, Atsumasa

Abstract

High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described.

Published
2007
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26. Detailed Spectral Study of an Ultra-Luminous Compact X-Ray Source, M81 X-9, in the Disk-Dominated State

Author

Tsunoda, Naoko, Kubota, Aya, Namiki, Masaaki, Sugiho, Masahiko, Kawabata, Kiyoshi, and Makishima, Kazuo

Abstract

We report on the results of detailed spectral studies of an ultra-luminous X-ray source (ULX), M81 X-9 (Holmberg IX X-1), conducted with XMM-Newton on 2001 April 22 and with ASCA on 1999 April 6. On both occasions, the source showed an unabsorbed 0.5–10 keV luminosity of $\sim 2 \times 10^{40} \,\mathrm{erg} \,\mathrm{s}^{-1}$(assuming a distance of 3.4 Mpc) and a soft spectrum, apparently represented by a multi-color disk model with an innermost disk temperature of 1.3–1.5 keV. Adding a power-law model further improved the fit. However, as previously reported, the high luminosity cannot be reconciled with the high disk temperature within the framework of the standard accretion disk radiating at a sub-Eddington luminosity. Therefore, we modified the multi-color disk model, and allowed the local disk temperature to scale as $\propto r^{-p}$on the distance $r$from the black hole, with $p$being a free parameter. We then found that the XMM-Newton and the ASCA spectra can be both successfully reproduced with $p \sim 0.6$and the innermost disk temperature of 1.4–1.8 keV. These flatter temperature profiles suggest a deviation from the standard Shakura-Sunyaev disk, and are consistent with predictions of a slim-disk model.

Published
2006
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27. On the Temperature Profile of Radiatively Efficient Geometrically Thin Disks in Black Hole Binaries with the ASCA GIS

Author

Kubota, Aya, Ebisawa, Ken, Makishima, Kazuo, and Nakazawa, Kazuhiro

Abstract

X-ray spectra of black hole binaries in the standard high/soft state were studied comprehensively using ASCA GIS data and, partially, RXTE PCA data. A mathematical disk model was applied to several black hole binaries to see whether the observed accretion disk temperature profile was consistent with that expected from the standard accretion disk model. This model is called a p-free disk and assumes that the spectrum is composed of multitemperature blackbody emission, where the local temperature T(r) at radius r is given by T(r) [?] r-p, with p being a positive free parameter. The standard disk, where the gravitational energy of the accreted matter is effectively released as blackbody radiation, roughly requires p [?] 3/4, while a small deviation is expected depending on the inner boundary conditions, general relativistic effects, and disk vertical structures. Our sample objects included LMC X-1, LMC X-3, XTE J2012+381, and GRO J1655-40. During the ASCA observations, these black hole binaries showed characteristics of the standard high/soft state. Under the standard modeling of high-state black hole binaries, the sources show disk inner temperatures of 0.76-1.17 keV, a disk fraction of the total 0.7-10 keV flux of 54%-98%, and absorption columns of (0.7-12) x 1021 cm-2. The best-fit values of p were found in the range 0.6-0.8, and the standard value of p = 3/4 was accepted for all the sources. The obtained values of p are also compared with those expected for the standard accretion disk in the Schwarzschild metric using the so-called GRAD model. The observed p-values were indeed found to be consistent with those expected from the standard accretion disk in the Schwarzschild metric.

Published
2005

28. Three Spectral States of the Disk X-Ray Emission of the Black-Hole Candidate 4U 1630−47

Author

Abe, Yukiko, Fukazawa, Yasushi, Kubota, Aya, Kasama, Daisuke, and Makishima, Kazuo

Abstract

We studied a time history of X-ray spectral states of a black-hole candidate, 4U 1630$-$47, utilizing data from a number of monitoring observations with the Rossi X-Ray Timing Explorer over 1996–2004. These observations covered five outbursts of 4U 1630$-$47, and recorded typical features of the high/soft states. The spectra in the high/soft states can be classified into three states. The first state is explained by a concept of the standard accretion disk picture. The second appears in the very high state, where a dominant hard component is seen and the disk radius apparently becomes too small. These phenomena are explained by the effect of inverse Compton scattering of disk photons, as shown by Kubota, Makishima, and Ebisawa (2001, ApJ, 560, L147) for GRO J1655$-$40. The third shows that the disk luminosity varies in proportion to $T_{\mathrm{in}}^2$, rather than $T_{\mathrm{in}}^4$, where $T_{\mathrm{in}}$is the inner-disk temperature. This state suggests an optically-thick and advection-dominated slim disk, as given by Kubota and Makishima (2004, ApJ, 601, 428) for XTE J1550$-$564. The second and third states appear, with good reproducibility, when $T_{\mathrm{in}}$and the total X-ray luminosity are higher than 1.2 keV and $\sim 2.5 \times 10^{38} (D/10 \,\mathrm{kpc})^2 [\cos \theta / (1/\sqrt{3})]^{-1} \,\mathrm{erg} \,\mathrm{s}^{-1}$, respectively, where $D$is the distance to the object and $\theta$is the inclination angle to the disk. The results suggest that these spectral states commonly appear among black-hole binaries under high accretion rates.

Published
2005
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29. Spectral Evolution of a Luminous Compact X-Ray Source in NGC 253 with Chandra and XMM-Newton Observatories*

Author

Tanaka, Takaaki, Sugiho, Masahiko, Kubota, Aya, Makishima, Kazuo, and Takahashi, Tadayuki

Abstract

Spectral studies of a luminous X-ray source, NGC 253 X21, are presented based on archival Chandra and XMM-Newton data. The Chandra observation on 1999 December 16 detected the source at a bolometric luminosity of $0.3 \times 10^{39} \,\mathrm{erg} \,\mathrm{s}^{-1}$(assuming isotropic emission), while an XMM-Newton observation on 2000 June 3 revealed a short-term source variation in the range of $(0.6 \hbox{--} 1.3) \times 10^{39} \,\mathrm{erg} \,\mathrm{s}^{-1}$. All spectra from these observations were successfully modeled by emission from an optically thick accretion disk. The average inner disk radius was kept constant at $63 \cdot (\cos60^\circ/\cos i)^{1/2} \,\mathrm{km}$, where $i$is the disk inclination, and did not vary significantly, while the disk inner temperature changed in the range of 0.9–1.4 keV. Assuming that this object is an accreting Schwarzschild black hole, and that the disk inner radius coincides with its last stable orbit, the mass of the black hole is estimated to be $\sim 7\,{{{M}_{\odot}}}$. The disk luminosity corresponds to $(30 \hbox{--} 120) \cdot(\cos60^\circ/\cos i)\%$of the Eddington limit of this black hole. Therefore, this luminous X-ray source, NGC 253 X21, is understood consistently to be an accreting stellar mass black hole in the standard disk state.

Published
2005
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30. X-Ray Spectra of the Narrow-Line Seyfert 1 Galaxy Ton S180 in Comparison with Galactic Black Holes

Author

Mio, MURASHIMA, Kubota, Aya, Makishima, Kazuo, Kokubun, Motohide, Hong, Soojing, and Negoro, Hitoshi

Abstract

An analysis was made of 0.3–15 keV X-ray spectra of a Narrow-Line Seyfert 1 Galaxy, Ton S180, using archival data from ASCA, RXTE, and XMM-Newton. At energies above 2.5 keV, a power-law with a photon index of $\sim 2.3$successfully and consistently reproduced the spectra from all of these observatories. Assuming this power-law component to extend toward lower energies, a soft excess, which is one of the most remarkable features of Narrow-Line Seyfert 1 Galaxies, is explained by another power-law multiplied by a thermal cutoff at $\sim 0.4 \,\mathrm{keV}$. Some similarities have been observed between this object and Galactic black hole binaries in very high state, the latter being realized under high accretion rates. Attempts have been made to interpret the soft excess in terms of Comptonization of the disk photons by an electron cloud surrounding the accretion disk, like BHBs in a very high state.

Published
2005
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31. The Three Spectral Regimes Found in the Stellar Black Hole XTE J1550-564 in Its High/Soft State

Author

Kubota, Aya and Makishima, Kazuo

Abstract

The present paper describes the analysis of multiple RXTE PCA data of the black hole binary with superluminal jet, XTE J1550-564, acquired during its 1998-1999 outburst. The X-ray spectra show features typical of the high/soft spectral state and can approximately be described by an optically thick disk spectrum plus a power-law tail. Three distinct spectral regimes, which we call the "standard regime," the "anomalous regime," and the "apparently standard regime," have been found from the entire set of the observed spectra. When the X-ray luminosity is well below ~6 x 1038 ergs s-1 (assuming a distance of 5 kpc), XTE J1550-564 resides in the standard regime, in which the soft spectral component dominates the power-law component and the observed disk inner radius is kept constant. When the luminosity exceeds the critical luminosity, the apparently standard regime is realized, in which the luminosity of the optically thick disk rises less steeply with the temperature, and the spectral shape is moderately distorted from that of the standard accretion disk. In this regime, the radial temperature gradient of the disk has been found to be flatter than that of the standard accretion disk. The results of the apparently standard regime suggest a slim disk, which is a solution predicted for a high mass accretion rate. In the intermediate anomalous regime (or very high state in the literature), the spectrum becomes much harder, and the disk inner radius derived using a simple disk model spectrum apparently varies significantly with time. These properties can be explained as a result of significant thermal inverse Comptonization of the disk photons, as was found from GRO J1655-40 in its anomalous regime by Kubota and coworkers.

Published
2004

32. Accretion Disk Spectra of Ultraluminous X-Ray Sources in Nearby Spiral Galaxies and Galactic Superluminal Jet Sources

Author

Ebisawa, Ken, Zycki, Piotr, Kubota, Aya, Mizuno, Tsunefumi, and Watarai, ya

Abstract

Ultraluminous compact X-ray sources (ULXs) in nearby spiral galaxies and Galactic superluminal jet sources share the common spectral characteristic that they have unusually high disk temperatures that cannot be explained in the framework of the standard optically thick accretion disk in the Schwarzschild metric. On the other hand, the standard accretion disk around the Kerr black hole might explain the observed high disk temperature, since the inner radius of the Kerr disk becomes smaller and the disk temperature can consequently be higher. However, we point out that the observable Kerr disk spectra become significantly harder than Schwarzschild disk spectra only when the disk is highly inclined. This is because the emission from the innermost part of the accretion disk is Doppler boosted for an edge-on Kerr disk while hardly seen for a face-on disk. The Galactic superluminal jet sources are known to be highly inclined systems; thus, their energy spectra may be explained with the standard Kerr disk with known black hole masses. For ULXs, on the other hand, the standard Kerr disk model seems implausible, since it is highly unlikely that their accretion disks are preferentially inclined, and if the edge-on Kerr disk model is applied, the black hole mass becomes unreasonably large ([?]300 M). Instead, the slim-disk (advection-dominated optically thick disk) model is likely to explain the observed super-Eddington luminosities, hard energy spectra, and spectral variations of ULXs. We suggest that ULXs are accreting black holes with a few tens of solar masses, which is not unexpected from the standard stellar evolution scenario, and that their X-ray emission is from the slim disk shining at super-Eddington luminosities.

Published
2003

33. Observational Evidence for a High-Energy Compton Cloud in GRO J1655-40 under a High Accretion Rate

Author

Kobayashi, Yoshihito, Kubota, Aya, Nakazawa, Kazuhiro, Takahashi, Tadayuki, and Makishima, Kazuo

Abstract

Observational results on GRO J1655$-$40 are reported, based on the X-ray spectra obtained with the PCA and the HEXTE on-board RXTE during its 1996–1997 outburst. By referring to the 40–150 keV X-ray luminosity, $L_{40 \hbox{--} 150}$, six typical spectra were selected and analyzed. When $L_{40 \hbox{--} 150}$is sufficiently below $\sim 5 \times 10^{36} \mathrm{erg} \,\mathrm{s}^{-1}$(assuming a distance of 3.2 kpc and an isotropic emission), the 3–150 keV PCA/HEXTE spectra are well described by a standard spectral model consisting of an optically-thick disk spectrum and a power-law tail. When $L_{40 \hbox{--} 150}$exceeds $5 \times 10^{36} \,\mathrm{erg} \,\mathrm{s}^{-1}$, the standard model fails to reproduce the joint spectrum, due to a mild turn-over in the HEXTE spectrum. Successful fits are recovered when the power-law component is replaced by a broken power-law model with the break energy at $\sim 40 \,\mathrm{keV}$, or by an exponentially cutoff power-law model with the cutoff energy at 190–300 keV. The fits are further improved by employing a thermal Comptonization component, wherein the electron temperature and optical depth of the Compton cloud are estimated to be 70–85 keV and 0.45–0.65, respectively. These results provide strong evidence for the existence of thermal high-energy electrons, and reconfirm the picture of strong disk Comptonization.

Published
2003
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34. Accretion disk spectra of super-luminal jet sources and ultra-luminous compact X-ray sources in nearby spiral galaxies

Author

Ebisawa, Ken, Kubota, Aya, Mizuno, Tsunefumi, and Życki, Piotr

Abstract

The Ultra-luminous Compact X-ray Sources (ULXs)in nearby spiral galaxies and the Galactic super-luminaljet sources sharethe common spectral characteristic that they haveextremely high disk temperatures which cannot be explainedin the framework of the standard accretion disk modelin the Schwarzschild metric. We have calculated an extreme Kerr disk model to examine if the Kerr disk model can instead explain the observed `too hot' accretion disk spectra.We found that the Kerr disk spectrum becomes significantly hardercompared to the Schwarzschild disk only when the disk is highlyinclined.For super-luminal jet sources, which are known to beinclined systems, the Kerr disk model may thuswork if we choose proper values for the black hole angular momentum. For the ULXs, however, the Kerr disk interpretation will be problematic,as is is highly unlikely that their accretion disks are preferentiallyinclined.

Published
2001
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35. ASCA Observation of Ultra-Luminous X-Ray Sources in the Nearby Spiral Galaxy NGC 2403

Author

Kotoku, Jun'ichi, Mizuno, Tsunefumi, Kubota, Aya, and Makishima, Kazuo

Abstract

The spiral galaxy NGC 2403 was observed with ASCA, and three previously known X-ray sources (sources 3, 4, and 5) were detected. Among them, the observed 0.5-10 keV flux of source 3 is 1.4×10−12erg s−1cm−2, implying a bolometric luminosity of 3.0×1039erg s−1. Its spectrum can be explained by emission from an optically thick accretion disk with an inner-disk temperature of 1.1 keV. The spectrum and the high luminosity suggest that source 3 is a mass-accreting black hole binary. The observed properties of source 3 can be interpreted in terms of a black hole of mass ∼ 15 M⊙, accreting at near the Eddington rate.

Published
2000
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36. The Nature of Ultraluminous Compact X-Ray Sources in Nearby Spiral Galaxies

Author

Makishima, Kazuo, Kubota, Aya, Mizuno, Tsunefumi, Ohnishi, Tomohisa, Tashiro, Makoto, Aruga, Yoichi, Asai, Kazumi, Dotani, Tadayasu, Mitsuda, Kazuhisa, Ueda, Yoshihiro, Uno, ichiro, Yamaoka, Kazutaka, Ebisawa, Ken, Kohmura, Yoshiki, and Okada, Kyoko

Abstract

Studies were made of ASCA spectra of seven ultraluminous compact X-ray sources in nearby spiral galaxies: M33 X-8, M81 X-6, IC 342 source 1, Dwingeloo 1 X-1, NGC 1313 source B, and two sources in NGC 4565. With the 0.5-10 keV luminosities in the range 1039-1040 ergs s-1, they are thought to represent a class of enigmatic X-ray sources often found in spiral galaxies. For some of them, the ASCA data are newly processed or the published spectra are reanalyzed. For others, the published results are quoted. The ASCA spectra of all seven sources have been described successfully with so-called multicolor disk blackbody emission arising from optically thick standard accretion disks around black holes. Except for the case of M33 X-8, the spectra do not exhibit hard tails. For the source luminosities not to exceed the Eddington limits, the black holes are inferred to have rather high masses, up to ~100 M. However, the observed innermost disk temperatures of these objects, Tin = 1.1-1.8 keV, are too high to be compatible with the required high black hole masses, as long as the standard accretion disks around Schwarzschild black holes are assumed. Similarly high disk temperatures are also observed from two Galactic transients with superluminal motions, GRO 1655-40 and GRS 1915+105. The issue of unusually high disk temperature may be explained by the black hole rotation, which makes the disk get closer to the black hole and hence hotter.

Published
2000

37. Detailed design of the science operations for the XRISM mission

Author

Terada, Yukikatsu, Holland, Matt, Loewenstein, Michael, Tashiro, Makoto, Takahashi, Hiromitsu, Nobukawa, Masayoshi, Mizuno, Tsunefumi, Tamura, Takayuki, Uno, Shin’ichiro, Watanabe, Shin, Baluta, Chris, Burns, Laura, Ebisawa, Ken, Eguchi, Satoshi, Fukazawa, Yasushi, Hayashi, Katsuhiro, Iizuka, Ryo, Katsuda, Satoru, Kitaguchi, Takao, Kubota, Aya, Miller, Eric, Mukai, Koji, Nakashima, Shinya, Nakazawa, Kazuhiro, Odaka, Hirokazu, Ohno, Masanori, Ota, Naomi, Sato, Rie, Sawada, Makoto, Sugawara, Yasuharu, Shidatsu, Megumi, Tamba, Tsubasa, Tanimoto, Atsushi, Terashima, Yuichi, Tsuboi, Yohko, Uchida, Yuusuke, Uchiyama, Hideki, Yamauchi, Shigeo, and Yaqoob, Tahir

Published
2021
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38. Evidence for a Black Hole in the X-Ray Transient GRS 1009–45

Author

Kubota, Aya, Tanaka, Yasuo, Makishima, Kazuo, Ueda, Yoshihiro, Dotani, Tadayasu, Inoue, Hajime, and Yamaoka, Kazutaka

Abstract

We report on the result of an X-ray observation of the X-ray Nova Velorum 1993 (GRS 1009–45), made with ASCA on 1993 November 10-11. The energy spectrum was extremely soft and accompanied by a hard tail, characteristics of the Galactic black-hole binaries in the soft state. It is well represented by a two-component model consisting of a multicolor disk model or a general relativistic accretion disk model, both describing emission from an optically thick accretion disk, and a power-law component with a photon index of ∼ 2.5. A spectral analysis of the soft component allows an estimation of the mass of the central object. For the optically-estimated distance (> 1 kpc) and inclination (> 37°), the mass is estimated to be $\gt 3.1 M_\odot$. These results strongly support that the compact object is a black hole.

Published
1998
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39. ASCA Observations of Two Ultra-Luminous Compact X-Ray Sources in the Edge-On Spiral Galaxy NGC 4565

Author

Mizuno, Tsunefumi, Ohnishi, Tomohisa, Kubota, Aya, Makishima, Kazuo, and Tashiro, Makoto

Abstract

The edge-on spiral galaxy NGC 4565 was observed for ∼ 35 ks with ASCA in the 0.5–10 keV energy band. The X-ray emission was dominated by two bright sources, which could be identified with two point-like X-ray sources seen in the ROSAT HRI image. The observed 0.5–10 keV fluxes of these sources, 1.7 × 10−12erg s−1cm−2and 0.7 × 10−12erg s−1cm−2, imply bolometric luminosities of 1.2 × 1040erg s−1and 4.6 × 1039erg s−1, respectively. They exhibit similar spectra, which can be explained by emission from optically thick accretion disks with inner-disk temperature of 1.4–1.6 keV. One of them, coincident in position with the nucleus, shows too low absorption to be the active nucleus seen through the galaxy disk. Their spectra and high luminosities suggest that they are both mass-accreting black-hole binaries. However, the black-hole mass required by the Eddington limit is rather high (≥ 50 M⊙), and the observed disk temperature is too high to be compatible with the high black-hole mass. Several attempts have been made to solve these problems.

Published
1999
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40. Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector†

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, and Uchida, Yuusuke

Abstract

We present the results from the Hitomi Soft Gamma-ray Detector (SGD) observation of the Crab nebula. The main part of SGD is a Compton camera, which in addition to being a spectrometer, is capable of measuring polarization of gamma-ray photons. The Crab nebula is one of the brightest X-ray/gamma-ray sources on the sky, and the only source from which polarized X-ray photons have been detected. SGD observed the Crab nebula during the initial test observation phase of Hitomi. We performed data analysis of the SGD observation, SGD background estimation, and SGD Monte Carlo simulations, and successfully detected polarized gamma-ray emission from the Crab nebula with only about 5 ks exposure time. The obtained polarization fraction of the phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1% ± 10.6%), and the polarization angle is ${110{^{\circ}_{.}}7}$+${13{^{\circ}_{.}}2}$/−${13{^{\circ}_{.}}0}$in the energy range of 60–160 keV (the errors correspond to the 1 σ deviation). The confidence level of the polarization detection was 99.3%. The polarization angle measured by SGD is about one sigma deviation with the projected spin axis of the pulsar, ${124{^{\circ}_{.}}0}$± ${0{^{\circ}_{.}}1}$.

Published
2018
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41. State transitions of GRS 1739−278 in the 2014 outburst

Author

Wang, Sili, Kawai, Nobuyuki, Shidatsu, Megumi, Tachibana, Yutaro, Yoshii, Taketoshi, Sudo, Masayuki, and Kubota, Aya

Abstract

We report on the X-ray spectral analysis and time evolution of GRS 1739−278 during its 2014 outburst, based on MAXI/GSC and Swift/XRT observations. Over the course of the outburst, a transition from the low/hard state to the high/soft state and then back to the low/hard state was seen. During the high/soft state, the innermost disk temperature mildly decreased, while the innermost radius estimated with the multi-color disk model remained constant at ∼18 (D/8.5 kpc)(cos i/cos 30°)−1/2km, where Dis the source distance and iis the inclination of observation. This small innermost radius of the accretion disk suggests that the central object is more likely to be a Kerr black hole rather than a Schwardzschild black hole. Applying a relativistic disk emission model to the high/soft state spectra, a mass upper limit of 18.3 M⊙was obtained based on the inclination limit i< 60° for an assumed distance of 8.5 kpc. Using the empirical relation of the transition luminosity to the Eddington limit, the mass is constrained to 4.0–18.3 M⊙for the same distance. The mass can be further constrained to be no larger than 9.5 M⊙by adopting the constraints based on the fits to the NuSTAR spectra with relativistically blurred disk reflection models (Miller et al. 2015, ApJ, 799, L6).

Published
2018
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42. Concept of the X-ray Astronomy Recovery Mission

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Tashiro, Makoto, Maejima, Hironori, Toda, Kenichi, Kelley, Richard, Reichenthal, Lillian, Lobell, James, Petre, Robert, Guainazzi, Matteo, Costantini, Elisa, Edison, Mark, Fujimoto, Ryuichi, Grim, Martin, Hayashida, Kiyoshi, den Herder, Jan-Willem, Ishisaki, Yoshitaka, Paltani, Stéphane, Matsushita, Kyoko, Mori, Koji, Sneiderman, Gary, Takei, Yoh, Terada, Yukikatsu, Tomida, Hiroshi, Akamatsu, Hiroki, Angelini, Lorella, Arai, Yoshitaka, Awaki, Hisamitsu, Babyk, Lurli, Bamba, Aya, Barfknecht, Peter, Barnstable, Kim, Bialas, Thomas, Blagojevic, Branimir, Bonafede, Joseph, Brambora, Clifford, Brenneman, Laura, Brown, Greg, Brown, Kimberly, Burns, Laura, Canavan, Edgar, Carnahan, Tim, Chiao, Meng, Comber, Brian, Corrales, Lia, de Vries, Cor, Dercksen, Johannes, Diaz-Trigo, Maria, Dillard, Tyrone, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Ferrigno, Carlo, Fukazawa, Yasushi, Fujita, Yutaka, Furuzawa, Akihiro, Gallo, Luigi, Graham, Steve, Gu, Liyi, Hagino, Kohichi, Hamaguchi, Kenji, Hatsukade, Isamu, Hawes, Dean, Hayashi, Takayuki, Hegarty, Cailey, Hell, Natalie, Hiraga, Junko, Hodges-Kluck, Edmund, Holland, Matt, Hornschemeier, Ann, Hoshino, Akio, Ichinohe, Yuto, Iizuka, Ryo, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, James, Bryan, Kallman, Timothy, Kara, Erin, Katsuda, Satoru, Kenyon, Steven, Kilbourne, Caroline, Kimball, Mark, Kitaguti, Takao, Kitamoto, Shunji, Kobayashi, Shogo, Kohmura, Takayoshi, Koyama, Shu, Kubota, Aya, Leutenegger, Maurice, Lockard, Tom, Loewenstein, Mike, Maeda, Yoshitomo, Marbley, Lynette, Markevitch, Maxim, Matsumoto, Hironori, Matsuzaki, Keiichi, McCammon, Dan, McNamara, Brian, Miko, Joseph, Miller, Eric, Miller, Jon, Minesugi, Kenji, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Mori, Hideyuki, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard, Nakajima, Hiroshi, Nakamura, Hideto, Nakashima, Shinya, Nakazawa, Kazuhiro, Natsukari, Chikara, Nigo, Kenichiro, Nishioka, Yusuke, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogawa, Mina, Ohashi, Takaya, Ohno, Masahiro, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Onizuka, Michitaka, Ota, Naomi, Ozaki, Masanobu, Plucinsky, Paul, Porter, F. Scott, Pottschmidt, Katja, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Seta, Hiromi, Shelton, Ken, Shibano, Yasuko, Shida, Maki, Shidatsu, Megumi, Shirron, Peter, Simionescu, Aurora, Smith, Randall, Someya, Kazunori, Soong, Yang, Suagawara, Yasuharu, Szymkowiak, Andy, Takahashi, Hiromitsu, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Terashima, Yuichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Ueda, Yoshihiro, Uno, Shinichiro, Walsh, Thomas, Watanabe, Shin, Williams, Brian, Wolfs, Rob, Wright, Michael, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Shigeo, Yamauchi, Makoto, Yanagase, Keiichi, Yaqoob, Tahir, Yasuda, Susumu, Yoshioka, Nasa, Zabala, Jaime, and Irina, Zhuravleva

Published
2018
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43. Hitomi (ASTRO-H) X-ray Astronomy Satellite

Author

Takahashi, Tadayuki, Kokubun, Motohide, Mitsuda, Kazuhisa, Kelley, Richard L., Ohashi, Takaya, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall W., Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Canavan, Edgar, Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, O’ Dell, Steve, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Gilmore, Kirk, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, den Herder, Jan-Willem, Hiraga, Junko S., Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwai, Masachika, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline A., Kimball, Mark, King, Ashley, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Konami, Saori, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Mcguinness, Daniel, McNamara, Brian R., Mehdipour, Missagh, Miko, Joseph, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Moroso, Franco, Moseley, Harvey, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard F., Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, de Plaa, Jelle, Pohl, Martin, Pontius, James, Porter, Frederick S., Pottschmidt, Katja, Ramsey, Brian, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Yoichi, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shidatsu, Megumi, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall K., Sneiderman, Gary, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Sugita, Hiroyuki, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shin’ichiro, Urry, C. Megan, Ursino, Eugenio, de Vries, Cor P., Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamada, Takahiro, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, and Zoghbi, Abderahmen

Published
2018
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44. Hitomi X-ray observation of the pulsar wind nebula G21.5−0.9

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Sato, Toshiki, Nakaniwa, Nozomu, Murakami, Hiroaki, and Guest, Benson

Abstract

We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5−0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8–80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of Γ1= 1.74 ± 0.02 and Γ2= 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833−1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 σ. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.

Published
2018
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46. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi*

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Canning, Rebecca E A, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashi, Tasuku, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Shota, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Keigo, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Wang, Qian H S, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen

Abstract

Extending the earlier measurements reported in Hitomi collaboration (2016, Nature, 535, 117), we examine the atmospheric gas motions within the central 100 kpc of the Perseus cluster using observations obtained with the Hitomi satellite. After correcting for the point spread function of the telescope and using optically thin emission lines, we find that the line-of-sight velocity dispersion of the hot gas is remarkably low and mostly uniform. The velocity dispersion reaches a maxima of approximately 200 km s−1toward the central active galactic nucleus (AGN) and toward the AGN inflated northwestern “ghost” bubble. Elsewhere within the observed region, the velocity dispersion appears constant around 100 km s−1. We also detect a velocity gradient with a 100 km s−1amplitude across the cluster core, consistent with large-scale sloshing of the core gas. If the observed gas motions are isotropic, the kinetic pressure support is less than 10% of the thermal pressure support in the cluster core. The well-resolved, optically thin emission lines have Gaussian shapes, indicating that the turbulent driving scale is likely below 100 kpc, which is consistent with the size of the AGN jet inflated bubbles. We also report the first measurement of the ion temperature in the intracluster medium, which we find to be consistent with the electron temperature. In addition, we present a new measurement of the redshift of the brightest cluster galaxy NGC 1275.

Published
2018
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47. Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS*

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furukawa, Maki, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier O, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ogorzalek, Anna, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shiníchiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shiníchiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen

Abstract

Thanks to its high spectral resolution (∼5 eV at 6 keV), the Soft X-ray Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure of spatially resolved emission lines from highly ionized ions in galaxy clusters for the first time. In this series of papers, using the SXS we have measured the velocities of gas motions, metallicities and the multi-temperature structure of the gas in the core of the Perseus Cluster. Here, we show that when inferring physical properties from line emissivities in systems like Perseus, the resonant scattering effect should be taken into account. In the Hitomi waveband, resonant scattering mostly affects the Fe xxvHeα line (w)—the strongest line in the spectrum. The flux measured by Hitomi in this line is suppressed by a factor of ∼1.3 in the inner ∼30 kpc, compared to predictions for an optically thin plasma; the suppression decreases with the distance from the center. The wline also appears slightly broader than other lines from the same ion. The observed distortions of the wline flux, shape, and distance dependence are all consistent with the expected effect of the resonant scattering in the Perseus core. By measuring the ratio of fluxes in optically thick (w) and thin (Fe xxvforbidden, Heβ, Lyα) lines, and comparing these ratios with predictions from Monte Carlo radiative transfer simulations, the velocities of gas motions have been obtained. The results are consistent with the direct measurements of gas velocities from line broadening described elsewhere in this series, although the systematic and statistical uncertainties remain significant. Further improvements in the predictions of line emissivities in plasma models, and deeper observations with future X-ray missions offering similar or better capabilities to the Hitomi SXS, will enable resonant scattering measurements to provide powerful constraints on the amplitude and anisotropy of cluster gas motions.

Published
2018
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48. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hell, Natalie, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, and Raassen, A J J

Abstract

The Hitomi Soft X-ray Spectrometer spectrum of the Perseus cluster, with ∼5 eV resolution in the 2–9 keV band, offers an unprecedented benchmark of the atomic modeling and database for hot collisional plasmas. It reveals both successes and challenges of the current atomic data and models. The latest versions of AtomDB/APEC (3.0.8), SPEX (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band spectrum, and are in close agreement on best-fit temperature, emission measure, and abundances of a few elements such as Ni. For the Fe abundance, the APEC and SPEX measurements differ by 16%, which is 17 times higher than the statistical uncertainty. This is mostly attributed to the differences in adopted collisional excitation and dielectronic recombination rates of the strongest emission lines. We further investigate and compare the sensitivity of the derived physical parameters to the astrophysical source modeling and instrumental effects. The Hitomi results show that accurate atomic data and models are as important as the astrophysical modeling and instrumental calibration aspects. Substantial updates of atomic databases and targeted laboratory measurements are needed to get the current data and models ready for the data from the next Hitomi-level mission.

Published
2018
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49. Temperature structure in the Perseus cluster core observed with Hitomi*

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furukawa, Maki, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Kato, Yuichi, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shiníchiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shiníchiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen

Abstract

The present paper explains the temperature structure of X-ray emitting plasma in the core of the Perseus cluster based on 1.8–20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) on board the Hitomi Observatory. A series of four observations was carried out, with a total effective exposure time of 338 ks that covered a central region of ∼7΄ in diameter. SXS was operated with an energy resolution of ∼5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions, but also transitions from higher principal quantum numbers were clearly resolved from Si through Fe. That enabled us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single-temperature thermal plasma model in collisional ionization equilibrium, but detailed line-ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with the atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures could be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single-temperature approximation are due to the effects of projecting the known radial temperature gradient in the cluster core along the line of sight. A comparison with the Chandra/ACIS and the XMM-Newton/RGS results, on the other hand, suggests that additional lower-temperature components are present in the intracluster medium (ICM), but not detectable with Hitomi/SXS giving its 1.8–20 keV energy band.

Published
2018
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50. Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin΄ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin΄ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Tominaga, Nozomu, and Moriya, Takashi J

Abstract

The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 ad. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core-collapse SN. Intensive searches have been made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that SN 1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core-collapse SNe. X-ray imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit on the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter on board the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from as yet undetected thermal plasma in the 2–12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of ≲ 1 M⊙for a wide range of assumed shell radius, size, and plasma temperature values both in and out of collisional equilibrium. To compare with the observation, we further performed hydrodynamic simulations of the Crab SNR for two SN models (Fe-core versus EC) under two SN environments (uniform interstellar medium versus progenitor wind). We found that the observed mass limit can be compatible with both SN models if the SN environment has a low density of ≲ 0.03 cm−3(Fe core) or ≲ 0.1 cm−3(EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10−5M⊙yr−1at 20 km s−1for the wind environment.

Published
2018
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