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151 results on '"Lorella Angelini"'

1. Soft X-Ray Energy Spectra in the Wide-field Galactic Disk Area Revealed with HaloSat

Author: Kazuki Ampuku, Ikuyuki Mitsuishi, Koki Sakuta, Philip Kaaret, Daniel M. LaRocca, and Lorella Angelini
Subjects: X-ray astronomy, Diffuse x-ray background, Galaxy disks, Galaxy stellar disks, the Milky Way, Astrophysics, QB460-466
Abstract: We analyzed data from HaloSat observations for five fields in the Galactic disk located far away from the Galactic center (135° < l < 254°) to understand the nature of soft X-ray energy emission in the Galactic disk. The fields have 14° diameter and were selected to contain no significant high-flux X-ray sources. All five HaloSat soft X-ray energy spectra (0.4–7 keV with energy resolution of < 100 eV below 1 keV) show a possibility of the presence of unresolved high-temperature plasma in the Galactic disk (UHTPGD) with a temperature of 0.8–1.0 keV and an emission measure of (8–11) × 10 ^−4 cm ^−6 pc in addition to the soft X-ray diffuse background components mainly studied at higher Galactic latitudes (solar wind charge exchange emission, Local Hot Bubble, Milky Way halo emission, and the cosmic X-ray background). This suggests that the UHTPGD is present across the whole Galactic disk. We also observed UHTPGD emission in a region with no bright sources in an XMM-Newton field contained within one of the HaloSat fields. The temperature and emission measure are consistent with those measured with HaloSat. Moreover, the stacked spectra of the X-ray pointlike sources and near-infrared-identified point sources such as stars in the XMM-Newton field also show a spectral feature similar to the UHTPGD emission. This suggests that the UHTPGD may partly originate from pointlike sources such as stars.
Published: 2024
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2. Research Campaign: Lunar Gravitational-wave Antenna

Author: Lorella Angelini, Francesca Badaracco, Stefano Benetti, Alessandro Bertolini, Xing Bian, Alessandro Bonforte, Enrico Bozzo, Marcel ter Brake, Marica Branchesi, Enrico Cappellaro, Christophe Collette, Michael Coughlin, Stefano Covino, Roberto Della Ceca, Riccardo De Salvo, Gianluca Di Rico, Alessandro Frigeri, Carlo Giunchi, Joris van Heijningen, Vuk Mandic, Szabolcs Marka, Andrea Maselli, Daniele Melini, Ana Carolina Silva Oliveira, Marco Olivieri, Andrea Perali, Roberto Serafinelli, and Paola Severgnini
Subjects: Communications And Radar
Abstract: The Lunar Gravitational-wave Antenna (LGWA) is a mission conceived as a network of stations to measure the vibrations of the Moon caused by gravitational waves (GWs). The long-term vision is to accomplish ground-breaking, paradigm shifting science in the coming decades on the Moon. LGWA will lead to the first observation of GW signals in the decihertz band greatly expanding our understanding of the universe and laying out a path to eventually probe the moment of its creation. LGWA stations will also be unique contributions to a lunar geophysical network shedding light on the Moon’s formation history. LGWA is a project of inclusion and international collaboration, where space-faring and space-aspiring nations can contribute to the LGWA network with their own stations whose cost depends on the targeted station lifetime and deployment location. With respect to the baseline concept proposed here, different sensor technologies can be implemented over time with the goal to continually increase the performance of the LGWA network. The broader context of lunar GW detection and its long-term vision are outlined in an accompanying topical white paper.
Published: 2022

3. Lunar Gravitational-wave Detection

Author: Jan Harms, Lorella Angelini, Michael Coughlin, Douglas Currie, Simone Dell'Agnello, Karan Jani, Stavros Katsanevas, Taichi Kawamura, Abraham Loeb, and Philippe Lognone
Subjects: Lunar and Planetary Science and Exploration
Abstract: Lunar gravitational-wave (GW) detection has been under consideration since Apollo 17 when the Lunar Surface Gravimeter developed under the coordination of Joseph Weber was deployed on the Moon with the goal to observe lunar surface vibrations generated by passing GWs [1]. The experiment did not run with its targeted performance, but even if it had, we know today that it would not have been sensitive enough to detect GW signals. Vibrations caused by GWs are expected to be several orders of magnitude weaker than what the instrument was designed to observe. The main motivation to bring such an experiment to the Moon was that with the extremely low level of seismicity observed with previously deployed Apollo seismometers [2] (see �figure 1), Weber suspected that GW signals could be detected.
Published: 2021

4. HILIGT, Upper Limit Servers II - Implementing the Data Servers

Author: Ole Konig, Richard D. Saxton, Peter Kretschmar, Lorella Angelini, Guillaume Belanger, Phil A. Evans, Michael J. Freyberg, Volodymyr Savchenko, Iris Traulsen, and Jorn Wilms
Subjects: Astronomy, Computer Programming And Software
Abstract: The High-Energy Light curve Generator(HILIGT) is a new web-based tool which allows the user to generate long-term light curves of X-ray sources. It provides historical data and calculates upper limits from image data in real-time. HILIGT utilizes data from twelve satellites, both modern missions such as XMM-Newton and Swift, and earlier facilities such as ROSAT, EXOSAT, Einstein or Ariel V. Together, this enables the user to query 50 years of X-ray data and, for instance, study outburst behavior of transient sources. In this paper we focus on the individual back-end servers for each satellite, detailing the software layout, database design, catalog calls, and image footprints. We compile all relevant calibration information of these missions and provide an in-depth summary of the details of X-ray astronomical instrumentation and data.
Published: 2021
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5. Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector

Author: Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, and Yuusuke Uchida
Published: 2018
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6. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi

Author: Hitomi Collaboration, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Natalie Hell, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, and A J J Raassen
Published: 2018
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7. Hitomi X-ray observation of the pulsar wind nebula G21.5−0.9

Author: Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shin’ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shin’ichiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, Toshiki Sato, Nozomu Nakaniwa, Hiroaki Murakami, and Benson Guest
Published: 2018
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8. The Neil Gehrels Swift Observatory

Author: Lorella Angelini, S. Bradley Cenko, Jamie A. Kennea, Michael H. Siegel, and Scott D. Barthelmy
Published: 2022

9. A Search for the 3.5 keV Line from the Milky Way's Dark Matter Halo with HaloSat

Author: E. M. Silich, P. Kaaret, Keith Jahoda, J. Richardson, Anna Zajczyk, R. Ringuette, D. M. LaRocca, and Lorella Angelini
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, Sterile neutrino, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Dark matter halo, Space and Planetary Science, Neutrino astronomy, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: Previous detections of an X-ray emission line near 3.5 keV in galaxy clusters and other dark matter-dominated objects have been interpreted as observational evidence for the decay of sterile neutrino dark matter. Motivated by this, we report on a search for a 3.5 keV emission line from the Milky Way's galactic dark matter halo with HaloSat. As a single pixel, collimated instrument, HaloSat observations are impervious to potential systematic effects due to grazing incidence reflection and CCD pixelization, and thus may offer a check on possible instrumental systematic errors in previous analyses. We report non-detections of a $\sim$3.5 keV emission line in four HaloSat observations near the Galactic Center. In the context of the sterile neutrino decay interpretation of the putative line feature, we provide 90% confidence level upper limits on the 3.5 keV line flux and 7.1 keV sterile neutrino mixing angle: $F \leq 0.077$ ph cm$^{-2}$ s$^{-1}$ sr$^{-1}$ and $\sin^2(2\theta) \leq 4.25 \times 10^{-11}$. The HaloSat mixing angle upper limit was calculated using a modern parameterization of the Milky Way's dark matter distribution, and in order to compare with previous limits, we also report the limit calculated using a common historical model. The HaloSat mixing angle upper limit places constraints on a number of previous mixing angle estimates derived from observations of the Milky Way's dark matter halo and galaxy clusters, and excludes several previous detections of the line. The upper limits cannot, however, entirely rule out the sterile neutrino decay interpretation of the 3.5 keV line feature., Comment: accepted for publication in The Astrophysical Journal, 14 pages, 7 figures
Published: 2021

10. Lunar Gravitational-wave Antenna

Author: Maila Agostini, Marta Civitani, Marica Branchesi, Paola Severgnini, Costanzo Federico, Mauro Focardi, Giovanni Pareschi, Ashish Sharma, Stefano Covino, Alessandro Bertolini, Roberto Della Ceca, Christophe Collette, Marco Pallavicini, Nandita Khetan, Lorella Angelini, Jan Harms, Claudio Pernechele, Ho Jung Paik, Gianpiero Tagliaferri, F. Badaracco, Alessandro Pajewski, Aniello Grado, R. Serafinelli, Lorenzo Betti, Matteo Di Giovanni, Massimo Della Valle, Raffaele Votta, S. Ronchini, Luca Izzo, Joris van Heijningen, Andrea Possenti, E. Coccia, Carlo Giunchi, Gor Oganesyan, Giorgio Spada, Vladimiro Noce, Simone Dall'Osso, Riccardo Pozzobon, Marco Olivieri, Alessandro Frigeri, C. M. Mow-Lowry, Riccardo DeSalvo, Daniele Melini, Augusto Marcelli, Michael W. Coughlin, Enzo Brocato, Enrico Cappellaro, Emanuele Pace, Michelangelo Formisano, Ruggero Stanga, Giuseppe Mitri, Filippo Ambrosino, Andrea Maselli, Luca Naponiello, Cesare Dionisio, Valentina Braito, P. D'Avanzo, Eliana Palazzi, Harms, Jan, Ambrosino, Filippo, Angelini, Lorella, Braito, Valentina, Branchesi, Marica, Brocato, Enzo, Cappellaro, Enrico, Coccia, Eugenio, Coughlin, Michael, Ceca, Roberto Della, Valle, Massimo Della, Dionisio, Cesare, Federico, Costanzo, Formisano, Michelangelo, Frigeri, Alessandro, Grado, Aniello, Izzo, Luca, Marcelli, Augusto, Maselli, Andrea, Olivieri, Marco, Pernechele, Claudio, Possenti, Andrea, Ronchini, Samuele, Serafinelli, Roberto, Severgnini, Paola, Agostini, Maila, Badaracco, Francesca, Bertolini, Alessandro, Betti, Lorenzo, Civitani, Marta Maria, Collette, Christophe, Covino, Stefano, Dall’Osso, Simone, D’Avanzo, Paolo, DeSalvo, Riccardo, Giovanni, Matteo Di, Focardi, Mauro, Giunchi, Carlo, Heijningen, Joris van, Khetan, Nandita, Melini, Daniele, Mitri, Giuseppe, Mow-Lowry, Conor, Naponiello, Luca, Noce, Vladimiro, Oganesyan, Gor, Pace, Emanuele, Paik, Ho Jung, Pajewski, Alessandro, Palazzi, Eliana, Pallavicini, Marco, Pareschi, Giovanni, Pozzobon, Riccardo, Sharma, Ashish, Spada, Giorgio, Stanga, Ruggero, Tagliaferri, Gianpiero, Votta, Raffaele, and (Astro)-Particles Physics
Subjects: Inertial frame of reference, 010504 meteorology & atmospheric sciences, Bar (music), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational waves, Lunar science, Observatory, 0103 physical sciences, Gravitational waves, moon, gravitational waves antenna, gravitational waves detection, Aerospace engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Unified Astronomy Thesaurus concepts: Gravitational waves (678), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Gravitational wave, business.industry, Gravimeter, Detector, Astronomy and Astrophysics, Lunar science (972), Vibration, Space and Planetary Science, Physics::Space Physics, Antenna (radio), Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract: Monitoring of vibrational eigenmodes of an elastic body excited by gravitational waves was one of the first concepts proposed for the detection of gravitational waves. At laboratory scale, these experiments became known as resonant-bar detectors first developed by Joseph Weber in the 1960s. Due to the dimensions of these bars, the targeted signal frequencies were in the kHz range. Weber also pointed out that monitoring of vibrations of Earth or Moon could reveal gravitational waves in the mHz band. His Lunar Surface Gravimeter experiment deployed on the Moon by the Apollo 17 crew had a technical failure rendering the data useless. In this article, we revisit the idea and propose a Lunar Gravitational-Wave Antenna (LGWA). We find that LGWA could become an important partner observatory for joint observations with the space-borne, laser-interferometric detector LISA, and at the same time contribute an independent science case due to LGWA's unique features. Technical challenges need to be overcome for the deployment of the experiment, and development of inertial vibration sensor technology lays out a future path for this exciting detector concept., 29 pages, 17 figures
Published: 2021

11. Detection of polarized gamma-ray emission from the Crab nebula with Hitomi Soft Gamma-ray Detector

Author: Akio Hoshino, Katsuhiro Hayashi, Manabu Ishida, Hideki Uchiyama, Takayuki Tamura, Shunji Kitamoto, Shin'ichiro Takeda, Shinya Saito, Daisuke Yonetoku, Peter J. Serlemtsos, Yoshitaka Ishisaki, Masachika Iwai, Hiroshi Nakajima, Megumi Shidatsu, Kumi Ishikawa, Hans A. Krimm, Ken Ebisawa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Andrew C. Fabian, Brian R. McNamara, Shu Koyama, Samar Safi-Harb, Jan-Willem den Herder, R. Sato, Isamu Hatsukade, Hironori Matsumoto, Yoshitomo Maeda, Missagh Mehdipour, Teruaki Enoto, Hirokazu Odaka, Jelle de Plaa, Hiroshi Tsunemi, Maurice A. Leutenegger, Francesco Tombesi, Jelle Kaastra, Richard L. Kelley, Kazuhiro Nakazawa, Ikuyuki Mitsuishi, Takuya Miyazawa, G. Sato, Yohko Tsuboi, Frederick S. Porter, Norbert Werner, Fumie Akimoto, Junko S. Hiraga, Magnus Axelsson, Shinya Yamada, Ciro Pinto, David H. Lumb, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Takeshi Go Tsuru, Kosuke Sato, Koji Mori, Caroline A. Kilbourne, Yuichi Terashima, Kyoko Matsushita, Timothy R. Kallman, Philippe Laurent, Olivier Limousin, Toru Tamagawa, Luigi C. Gallo, Aya Bamba, Roger Blandford, Kiyoshi Hayashida, Yasunobu Uchiyama, Cor P. de Vries, Tsuneyoshi Kamae, Hirofumi Noda, Gregory V. Brown, Carlo Ferrigno, Yoshihiro Ueda, Yuusuke Uchida, Eric D. Miller, Yuichiro Ezoe, Andrea Goldwurm, Hiromi Seta, Frits Paerels, Katja Pottschmidt, Kazuhiro Sakai, Shin'ichiro Uno, Yoshito Haba, Stéphane Paltani, Hiromitsu Takahashi, Kazuhisa Mitsuda, Masanori Ohno, Satoshi Sugita, Masahiro Tsujimoto, Christopher S. Reynolds, Shin Mineshige, Ryuichi Fujimoto, Peter Kretschmar, Masayoshi Nobukawa, Yoh Takei, Tahir Yaqoob, Jon M. Miller, Dan R. Wilkins, Meng P. Chiao, Matteo Guainazzi, Aurora Simionescu, Hisamitsu Awaki, Paolo De Coppi, Katsuji Koyama, Masanobu Ozaki, Kumiko K. Nobukawa, Yasuharu Sugawara, Daniel Maier, Tadayuki Takahashi, Jun Kataoka, Aya Kubota, Hiroyuki Uchida, Laura Brenneman, John P. Hughes, Takayoshi Kohmura, Takaaki Tanaka, Hajime Inoue, Lorella Angelini, Toru Sasaki, Greg Madejski, Shutaro Ueda, Takao Nakagawa, Tadayasu Dotani, Maria Chernyakova, Motohide Kokubun, Takao Kitaguchi, Irina Zhuravleva, Shin Watanabe, Dan McCammon, Hideyuki Mori, Randall K. Smith, Edward M. Cackett, Norbert Schartel, Margherita Giustini, Megan E. Eckart, Tsunefumi Mizuno, Liyi Gu, Chris Done, Takeshi Nakamori, Takaya Ohashi, Shiu-Hang Lee, Michael Loewenstein, Adam R. Foster, Poshak Gandhi, Yasushi Fukazawa, Kenji Hamaguchi, Satoru Katsuda, Knox S. Long, Ilana M. Harrus, Yuzuru Tawara, Hideyo Kunieda, Lukasz Stawarz, C. Megan Urry, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Tetsu Kitayama, Felix Aharonian, Yoshiyuki Inoue, Noriko Y. Yamasaki, Eugenio Ursino, Takayuki Hayashi, Yukikatsu Terada, Makoto Yamauchi, Yasuo Tanaka, Steven W. Allen, Kazuo Makishima, Marc Audard, Shinya Nakashima, Naomi Ota, Hiroyasu Tajima, Hiroshi Murakami, Hiroshi Tomida, Hiroya Yamaguchi, Ryo Iizuka, Kouichi Hagino, Yoichi Yatsu, Kazutaka Yamaoka, Koji Mukai, Abderahmen Zoghbi, Makoto Tashiro, Ann Hornschemeier, Makoto Sawada, Marshall W. Bautz, Takashi Okajima, Esra Bulbul, Yang Soong, Akihiro Furuzawa, Hiroki Akamatsu, Andrew Szymkowiak, Robert Petre, Elisa Costantini, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, polarimeters [instrumentation], X-rays: individual (Crab), symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, polarization, Brewster's angle, Spectrometer, 010308 nuclear & particles physics, Gamma ray, instrumentation: polarimeters, Astronomy and Astrophysics, Polarization (waves), Crab Nebula, individual (Crab) [X-rays], Space and Planetary Science, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: 著者人数: 193名(所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子; 内田, 悠介), Accepted: 2018-09-30, 資料番号: SA1180351000
Published: 2018

12. Concept of the X-ray Astronomy Recovery Mission

Author: Shinya Yamada, Laura Brenneman, Yang Soong, Eric J. Miller, Kyoko Matsushita, Katja Pottschmidt, Johannes Dercksen, Hiromi Seta, Toru Tamagawa, Keiichi Matsuzaki, Yukikatsu Terada, Edgar Canavan, Rie Sato, F. Scott Porter, Hiroshi Murakami, Yoh Takei, Kimberly D. Brown, Michael J. DiPirro, Steven Kenyon, Hiroshi Tomida, Timothy R. Kallman, Richard L. Kelley, Atsushi Okamoto, Rob Wolfs, Matteo Guainazzi, Shinya Nakashima, Kenji Hamaguchi, Shin Watanabe, Lorella Angelini, Takayoshi Kohmura, Brian R. McNamara, Thomas G. Bialas, Megumi Shidatsu, Kumi Ishikawa, Aya Kubota, Takayuki Tamura, Jon M. Miller, Mark O. Kimball, Gary A. Sneiderman, Joseph Bonafede, Yoshitaka Arai, Kosei Ishimura, Mina Ogawa, A. E. Szymkowiak, Hiroshi Nakajima, Kenichi Toda, Steve Graham, Takao Kitaguchi, Makoto Sawada, Tom Lockard, Erin Kara, Yutaka Fujita, Dean Hawes, Shin'ichiro Uno, Hideyuki Mori, Kenichiro Nigo, Jan-Willem den Herder, Randall K. Smith, Luigi C. Gallo, Chikara Natsukari, Hideto Nakamura, Makoto Yamauchi, Michitaka Onizuka, Yoshitaka Ishisaki, Thomas Walsh, Koji Mori, Peter Barfknecht, Kazuhiro Nakazawa, Maria Diaz-Trigo, Manabu Ishida, Makoto Tashiro, Hiromitsu Takahashi, Satoru Katsuda, Cor P. de Vries, M. Ohno, Zhuravleva Irina, Meng P. Chiao, Aurora Simionescu, Kim Barnstable, Cailey Hegarty, Aya Bamba, Naomi Ota, Joseph Miko, M. Loewenstein, Connor Martz, Hirokazu Odaka, Ann Hornschemeier, Carlo Ferrigno, Edmund Hodges-Kluck, B. Blagojević, Liyi Gu, Masanobu Ozaki, Kenji Minesugi, Kazunori Someya, Kumiko K. Nobukawa, Junko S. Hiraga, Hiroya Yamaguchi, Shogo B. Kobayashi, Greg Brown, C. Brambora, Hiroyuki Uchida, Richard F. Mushotzky, Peter Shirron, Chris Done, Dan McCammon, Natalie Hell, Laura A. Burns, Kazunori Ishibashi, Brian J. Williams, Jaime Zabala, Brian Comber, Hironori Matsumoto, Matthew Holland, Teruaki Enoto, Stéphane Paltani, Yusuke Nishioka, Tim Carnahan, Masahiro Tsujimoto, Takayuki Hayashi, Lurli Babyk, Maki Shida, Ken Shelton, Isamu Hatsukade, Takeshi Go Tsuru, Kosuke Sato, Yoshihiro Ueda, Caroline A. Kilbourne, Yasuharu Suagawara, Tsunefumi Mizuno, Susumu Yasuda, S. Koyama, Hironori Maejima, Lia Corrales, Masayoshi Nobukawa, Yoshitomo Maeda, Yasushi Fukazawa, Hisamitsu Awaki, Takaaki Tanaka, Tadayasu Dotani, Megan E. Eckart, Takaya Ohashi, J. V. Lobell, Hiroshi Tsunemi, Ikuyuki Mitsuishi, Noriko Y. Yamasaki, Hirofumi Noda, Lillian Reichenthal, Yuichi Terashima, Kiyoshi Hayashida, Lynette Marbley, Tahir Yaqoob, Ryuichi Fujimoto, Ken Ebisawa, Kohichi Hagino, Martin Grim, Bryan L. James, Yohko Tsuboi, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Tyrone DIllard, Nasa Yoshioka, Akio Hoshino, Hideki Uchiyama, Shunji Kitamoto, Paul P. Plucinsky, Mark Edison, Yuichiro Ezoe, Yasuko Shibano, Koji Mukai, Michael R. Wright, Ryo Iizuka, Masayuki Ohta, Keiichi Yanagase, Hiroki Akamatsu, Robert Petre, Elisa Costantini, Kazutaka Yamaoka, Maurice A. Leutenegger, Takashi Okajima, and Akihiro Furuzawa
Subjects: X-ray astronomy, Attitude control system, COSMIC cancer database, 010308 nuclear & particles physics, business.industry, Computer science, Energy transfer, media_common.quotation_subject, High resolution, Field of view, 01 natural sciences, Universe, 0103 physical sciences, Aerospace engineering, business, 010303 astronomy & astrophysics, Event (particle physics), media_common
Abstract: The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi,“Resolving astrophysical problems by precise high-resolution X-ray spectroscopy”.1 This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission’s initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020’s and 2030’s. Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: “Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects”. To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 × 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.
Published: 2018

13. Hitomi (ASTRO-H) X-ray Astronomy Satellite

Author: Laura Brenneman, Hironori Matsumoto, Kirk Gilmore, Takayuki Yuasa, D. Lumb, Manabu Ishida, Aurora Simionescu, Takao Nakagawa, Junichiro Katsuta, Esra Bulbul, Meng P. Chiao, Philippe Laurent, Jelle de Plaa, Hiroyuki Ogawa, Keith Arnaud, Keiji Ogi, John P. Doty, B. Ramsey, Yuzuru Tawara, C. Megan Urry, Eric D. Miller, Peter Shirron, Gregory V. Brown, Dan R. Wilkins, Hiroshi Tsunemi, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Steven W. Allen, Naoko Iyomoto, Taro Kawano, Katja Pottschmidt, Yang Soong, Tadayuki Takahashi, Yasuharu Sugawara, Ikuyuki Mitsuishi, Margherita Giustini, Greg Madejski, Tetsu Kitayama, Megumi Shidatsu, Hideyuki Mori, Łukasz Stawarz, Randall K. Smith, Satoshi Sugita, Norbert Schartel, James Pontius, Kazuhiro Nakazawa, Eugenio Ursino, Katsuhiro Hayashi, Toshio Nakano, Satoru Katsuda, Cor P. de Vries, Adam R. Foster, Masanobu Ozaki, Kenji Minesugi, Tomomi Watanabe, Yuichi Terashima, Christopher S. Reynolds, Hiroaki Sameshima, Alex Koujelev, Naohisa Anabuki, Isamu Hatsukade, Masaharu Nomachi, Yoichi Yatsu, Yasunobu Uchiyama, Steve O' Dell, Ann Hornschemeier, Akio Hoshino, Yasuo Tanaka, M. Pohl, Kyoko Matsushita, Masahiro Tsujimoto, Hideki Uchiyama, Mark O. Kimball, Arvind Parmar, Gary A. Sneiderman, Yoshiyuki Inoue, Toru Tamagawa, Yukikatsu Terada, Shinya Nakashima, Tsuneyoshi Kamae, Dmitry Khangulyan, Kiyoshi Hayashida, Rie Sato, Aya Bamba, Roger Blandford, Kazunori Ishibashi, Shinya Saito, Caroline A. Kilbourne, Toshio Murakami, Takeda Shin'ichiro, Missagh Mehdipour, Motohide Kokubun, Masachika Iwai, Dan McCammon, Michael J. DiPirro, Marshall W. Bautz, Shunji Kitamoto, Naomi Ota, Brian R. McNamara, Frits Paerels, Stéphane Paltani, Magnus Axelsson, Edgar Canavan, Nobutaka Bando, Peter J. Serlemitsos, Shu Koyama, Felix Aharonian, Matteo Guainazzi, Joseph Miko, Masayoshi Nobukawa, Thomas G. Bialas, Koji Mori, Makoto Yamauchi, Uno Shin'ichiro, Hirokazu Odaka, Toru Sasaki, Mina Ogawa, Philipp Azzarello, Atsushi Wada, Tsuyoshi Okazaki, Ken Ebisawa, Takeshi Go Tsuru, Yoshitomo Maeda, Jon M. Miller, A. L. King, Cynthia Simmons, Hirofumi Noda, Hiromitsu Takahashi, Kazuhisa Mitsuda, Carlo Ferrigno, Hiroyasu Tajima, Kazuo Makishima, Erin Kara, Fumie Akimoto, Shigeo Kawasaki, Kumi Ishikawa, Kosuke Sato, Hiroshi Nakajima, Knox S. Long, Jun Kataoka, Keisuke Shinozaki, Kazuyuki Hirose, Keisuke Tamura, Teruaki Enoto, Yoh Takei, Yoshito Haba, Shinya Yamada, Richard L. Kelley, Yoshihiro Ueda, Megan E. Eckart, Takaya Ohashi, Shin-ichiro Sakai, Kevin R. Boyce, D. Haas, Atsushi Okamoto, Kazuhiro Sakai, Ryo Nagino, Makoto Asai, Maurice A. Leutenegger, Michael Loewenstein, Daniel R. Wik, Yohko Tsuboi, Maria Chernyakova, Shiro Ueno, Koji Mukai, Hiroshi Murakami, Takeshi Nakamori, Hiroshi Tomida, Tahir Yaqoob, Norbert Werner, Paolo Coppi, Abderahmen Zoghbi, Shin Watanabe, Kosei Ishimura, Hideyo Kunieda, Candace Masters, Yusuke Nishioka, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Andrew C. Fabian, Ryuichi Fujimoto, Kenji Hamaguchi, Liyi Gu, Edward M. Cackett, Chris Done, Junko S. Hiraga, Chris Baluta, Noriko Y. Yamasaki, Maki Shida, Makoto Tashiro, Takanobu Shimada, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Ilana M. Harrus, Naoko Iwata, Timothy R. Kallman, Takuya Miyazawa, Kumiko K. Nobukawa, Madoka Kawaharada, Hisamitsu Awaki, Takaaki Tanaka, Tadayasu Dotani, Goro Sato, Ciro Pinto, Hiroya Yamaguchi, Harvey Moseley, Yoshiharu Namba, Shutaro Ueda, Masayuki Itoh, Takayoshi Kohmura, Daisuke Yonetoku, Yoshitaka Ishisaki, Hans A. Krimm, Hiromi Seta, Atsumasa Yoshida, Kouichi Hagino, Yuichiro Ezoe, Samar Safi-Harb, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Yasuko Shibano, Frederick S. Porter, Saori Konami, Takayuki Tamura, Shin Mineshige, Peter Kretschmar, Yoichi Sato, Helen Russell, Hiroyuki Uchida, Elisa Costantini, Chikara Natsukari, Housei Nagano, Jan-Willem den Herder, Francesco Tombesi, Jelle Kaastra, Daniel S. McGuinness, Masanori Ohno, Hiroyuki Sugita, Katsuji Koyama, Tsunefumi Mizuno, Theodore Muench, Shiu-Hang Lee, Poshak Gandhi, Yasushi Fukazawa, Stefan Funk, Luigi C. Gallo, Tatsuro Kosaka, Andrea Goldwurm, Ryo Iizuka, Masayuki Ohta, Kazutaka Yamaoka, Marc Audard, Makoto Sawada, Takashi Okajima, Franco Moroso, Akihiro Furuzawa, Aya Kubota, Chris Jewell, Olivier Limousin, Takayuki Hayashi, Takao Kitaguchi, Takahiro Yamada, Hiroki Akamatsu, Andrew Szymkowiak, Robert Petre, Irina Zhuravleva, Dublin Institute for Advanced Studies (DIAS), SRON Netherlands Institute for Space Research (SRON), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern]-Universität Bern [Bern], Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Stockholm University, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University [Stanford], AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Stanford University, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Space operations, X-ray telescope, microcalorimeter, 01 natural sciences, x-ray astronomy, 010309 optics, gamma-ray astronomy, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation, ComputingMilieux_MISCELLANEOUS, Remote sensing, [PHYS]Physics [physics], X-ray astronomy, Spacecraft, business.industry, Mechanical Engineering, Astronomy and Astrophysics, hard x-ray, Gamma-ray astronomy, First light, Electronic, Optical and Magnetic Materials, Spacecraft system, x-ray, Space and Planetary Science, Control and Systems Engineering, gamma ray, Satellite, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: 270名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 高橋, 忠幸; 国分, 紀秀; 満田, 和久; Baluta, Chris; 坂東, 信尚; 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 廣瀬, 和之; 飯塚, 亮; 石田, 学; 石川, 久美; 石村, 康生; 岩井, 将親; 岩田, 直子; 河野, 太郎; 川崎, 繁男; 小山, 志勇; 前田, 良知; 峯杉, 賢治; 中川, 貴雄; 夏苅, 権; 小川, 博之; 小川, 美奈; 太田, 方之; 岡崎, 健; 尾崎, 正伸; 坂井, 真一郎; 鮫島, 寛明; 佐藤, 悟郎; 佐藤, 理江; 柴野, 靖子; 志田, 真樹; 嶋田, 貴信; Simionescu, Aurora; 菅原, 泰晴; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 田代, 信; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 上野, 史郎; 和田, 篤始; 渡辺, 伸; 山田, 隆弘; 山崎, 典子）, Number of authors: 270 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Takahashi, Tadayuki; Kokubun, Motohide; Mitsuda, Kazuhisa; Baluta, Chris; Bando, Nobutaka; Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hirose, Kazuyuki; Iizuka, Ryo; Ishida, Manabu; Ishikawa, Kumi; Ishimura, Kosei; Iwai, Masachika; Iwata, Naoko; Kawano, Taro; Kawasaki, Shigeo; Koyama, Shu; Maeda, Yoshitomo; Minesugi, Kenji; Nakagawa, Takao; Natsukari, Chikara; Ogawa, Hiroyuki; Ogawa, Mina; Ohta, Masayuki; Okazaki, Tsuyoshi; Ozaki, Masanobu; Sakai, Shinichiro; Sameshima, Hiroaki; Sato, Goro; Sato, Rie; Shibano, Yasuko; Shida, Maki; Shimada, Takanobu; Simionescu, Aurora; Sugawara, Yasuharu; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tashiro, Makoto; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Ueno, Shiro; Wada, Atsushi; Watanabe, Shin; Yamada, Takahiro; Yamasaki, Noriko Y.), Accepted: 2018-02-05, 資料番号: SA1170333000
Published: 2018

14. Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS

Author: Randall Smith, Hirokazu Odaka, Kumiko K. Nobukawa, Shin Watanabe, Hiroki Akamatsu, Goro Sato, Robert Petre, Ciro Pinto, G. U. Liyi, Shinya Yamada, Michael Loewenstein, Shutaro Ueda, Chris Done, Kazuhiro Sakai, Koji Mori, Kenji Hamaguchi, Elisa Costantini, Ilana M. Harrus, Carlo Ferrigno, Norbert Schartel, Yang Soong, Takayoshi Kohmura, Satoru Katsuda, Knox S. Long, Hiroshi Tsunemi, Ikuyuki Mitsuishi, Isamu Hatsukade, Ryo Iizuka, Kazutaka Yamaoka, Kouichi Hagino, Yuichiro Ezoe, Hironori Matsumoto, Makoto Sawada, Takashi Okajima, Akihiro Furuzawa, Francesco Tombesi, Kazuo Makishima, Yasuyuki T. Tanaka, Caroline A. Kilbourne, H. Tomida, Eugenio Ursino, Kumi Ishikawa, Yoshiyuki Inoue, Jon M. Miller, Jun Kataoka, Cor P. de Vries, Hiromi Seta, Yuichi Terashima, Hiromitsu Takahashi, Kazuhisa Mitsuda, Takao Nakagawa, L. E.E. Shiu-Hang, Marshall W. Bautz, Yukikatsu Terada, Christopher S. Reynolds, Teruaki Enoto, Missagh Mehdipour, Motohide Kokubun, Andrew E. Szymkowiak, Maurice A. Leutenegger, Meng P. Chiao, John P. Hughes, Yohko Tsuboi, Norbert Werner, Takeshi Go Tsuru, Peter J. Serlemtsos, Yoshitaka Ishisaki, Katsuji Koyama, Kiyoshi Hayashida, Daniel Maier, Hajime Inoue, Lorella Angelini, Aurora Simionescu, Hiroshi Nakajima, Kosuke Sato, Yoshitomo Maeda, David H. Lumb, Fumie Akimoto, Margherita Giustini, Manabu Ishida, Esra Bulbul, Shigeo Yamauchi, Maxim Markevitch, Tsuneyoshi Kamae, Yuto Ichinohe, Makoto Yamauchi, Hans A. Krimm, Masanori Ohno, Anna Ogorzalek, Yoshihiro Ueda, Yoshito Haba, Steven W. Allen, Maki Furukawa, Kyoko Matsushita, Samar Safi-Harb, B. J. Williams, Stéphane Paltani, Masayoshi Nobukawa, Yuzuru Tawara, Timothy R. Kallman, Hiroya Yamaguchi, Junko S. Hiraga, Magnus Axelsson, O. T.A. Naomi, Toru Tamagawa, Katsuhiro Hayashi, Rie Sato, Takuya Miyazawa, Maria Chernyakova, Akio Hoshino, Hirofumi Noda, Yasunobu Uchiyama, Frits Paerels, Hisamitsu Awaki, Jan-Willem den Herder, Yasuo Tanaka, Yasuharu Sugawara, U. N.O. Shiníchiro, Łukasz Stawarz, Takaaki Tanaka, Matteo Guainazzi, Tadayasu Dotani, Hideki Uchiyama, Toru Sasaki, Jelle Kaastra, Koji Mukai, Abderahmen Zoghbi, Luigi C. Gallo, Edward M. Cackett, Shunji Kitamoto, Shinya Saito, Laura Brenneman, Takao Kitaguchi, Paolo De Coppi, Yoichi Yatsu, Masachika Iwai, Megan E. Eckart, Takaya Ohashi, Richard F. Mushotzky, Andrew C. Fabian, Kazuhiro Nakazawa, Tahir Yaqoob, Daisuke Yonetoku, Hideyo Kunieda, Nobuyuki Kawai, Megumi Shidatsu, Brian R. McNamara, Ryuichi Fujimoto, Tetsu Kitayama, Shu Koyama, Noriko Y. Yamasaki, Ken Ebisawa, Massimiliano Galeazzi, Takeshi Nakamori, Felix Aharonian, Aya Bamba, Ann Hornschemeier, Roger Blandford, Adam R. Foster, Takayuki Hayashi, Philippe Laurent, Makoto Tashiro, Shin'ichiro Takeda, Gregory V. Brown, Masahiro Tsujimoto, Jelle de Plaa, Dan R. Wilkins, Tadayuki Takahashi, Marc Audard, Hiroshi Murakami, Greg Madejski, Hideyuki Mori, Shinya Nakashima, Hiroyasu Tajima, Satoshi Sugita, Masanobu Ozaki, Katja Pottschmidt, C. Megan Urry, Tsunefumi Mizuno, Dan McCammon, Shin Mineshige, Peter Kretschmar, Richard L. Kelley, Yoh Takei, Poshak Gandhi, Yasushi Fukazawa, Eric D. Miller, Takayuki Tamura, Aya Kubota, Irina Zhuravleva, Andrea Goldwurm, Frederick S. Porter, Hiroyuki Uchida, Olivier Limousin, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: galaxies: clusters: individual, galaxies: clusters: intracluster medium, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, clusters: individual (Perseus Cluster) [galaxies], 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Ionization, 0103 physical sciences, Radiative transfer, Emission spectrum, Spectral resolution, 010306 general physics, Anisotropy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astronomy and Astrophysics, Computational physics, Amplitude, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, galaxies: clusters [X-rays], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: Hitomi Collaboration 194名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 194 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-10-08, 資料番号: SA1170335000
Published: 2018

15. Temperature structure in the Perseus cluster core observed with Hitomi

Author: Laura Brenneman, Missagh Mehdipour, Motohide Kokubun, Manabu Ishida, Shinya Yamada, Kazuhiro Sakai, Kyoko Matsushita, Timothy R. Kallman, Toru Tamagawa, Hiroya Yamaguchi, Kouichi Hagino, Yuichiro Ezoe, Marc Audard, Frits Paerels, Ciro Pinto, Shin'ichiro Uno, Olivier Limousin, Matteo Guainazzi, Koji Mukai, Abderahmen Zoghbi, Toru Sasaki, Daisuke Yonetoku, Satoshi Sugita, Hiroki Akamatsu, Kumiko K. Norukawa, Yoshitaka Ishisaki, Andrew Szymkowiak, Dan R. Wilkins, Hans A. Krimm, Marshall W. Bautz, Samar Safi-Harb, Katsuhiro Hayashi, Tadayuki Takahashi, Masanobu Ozaki, Robert Petre, Takayoshi Kohmura, Aya Kubota, Elisa Costantini, Yoichi Yatsu, Kazutaka Yamaoka, Hirokazu Odaka, Frederick S. Porter, Satoru Katsuda, Greg Madejski, Hironori Matsumoto, Yoshiyuki Inoue, Knox S. Long, Takao Nakagawa, Irina Zhuravleva, Dan McCammon, Chris Done, Takeshi Nakamori, Yukikatsu Terada, Hiroshi Murakami, Hideyuki Mori, Shinya Saito, Makoto Sawada, Takashi Okajima, Randall K. Smith, Paolo De Coppi, Masachika Iwai, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Hiroshi Tomida, Yuzuru Tawara, C. Megan Urry, Richard F. Mushotzky, Teruaki Enoto, Maurice A. Leutenegger, Nobuyuki Kawai, Norbert Schartel, Brian J. Williams, Meng P. Chiao, Kumi Ishikawa, G. Sato, Takao Kitaguchi, Maki Furukawa, Shiu-Hang Lee, Michael Loewenstein, Akihiro Furuzawa, Masayoshi Nobukawa, Tahir Yaqoob, Yasuharu Sugawara, Margherita Giustini, Jan-Willem den Herder, Tetsu Kitayama, Kenji Hamaguchi, Megumi Shidatsu, Felix Aharonian, Yasuo Tanaka, Luigi C. Gallo, Shinya Nakashima, Ann Hornschemeier, Aurora Simionescu, Andrea Goldwurm, Naomi Ota, Steven W. Allen, Eugenio Ursino, Richard L. Kelley, Takuya Miyazawa, Hiroshi Nakajima, Ilana M. Harrus, Takayuki Hayashi, David H. Lumb, Katja Pottschmidt, Ryo Iizuka, Liyi Gu, Hiroyasu Tajima, Takeshi Go Tsuru, Kosuke Sato, Shin Mineshige, P. J. Serlemitsos, Peter Kretschmar, Jon M. Miller, Yoshihiro Ueda, Tsunefumi Mizuno, Tsuneyoshi Kamae, Philippe Laurent, Ryuichi Fujimoto, Shin'ichiro Takeda, Gregory V. Brown, Koji Mori, Eric D. Miller, Hiromi Seta, Hirofumi Noda, Adam R. Foster, Poshak Gandhi, Yasushi Fukazawa, Cor P. de Vries, Ken Ebisawa, Yasuyuki T. Tanaka, Masanori Ohno, Christopher S. Reynolds, Massimiliano Galeazzi, Carlo Ferrigno, Masahiro Tsujimoto, Hiroyuki Uchida, Jelle de Plaa, John P. Hughes, Francesco Tombesi, Jelle Kaastra, Katsuji Koyama, Hiroshi Tsunemi, Yasunobu Uchiyama, Daniel Maier, Hajime Inoue, Lorella Angelini, Andrew C. Fabian, Shutaro Ueda, Ikuyuki Mitsuishi, Brian R. McNamara, Shu Koyama, Yuichi Terashima, Stéphane Paltani, Kiyoshi Hayashida, Yoshitomo Maeda, Isamu Hatsukade, Makoto Tashiro, Caroline A. Kilbourne, Esra Bulbul, Hisamitsu Awaki, Yang Soong, Takaaki Tanaka, Tadayasu Dotani, Kazuo Makishima, Megan E. Eckart, Takaya Ohashi, Jun Kataoka, R. Sato, Hideyo Kunieda, Lukasz Stawarz, Junko S. Hiraga, Magnus Axelsson, Noriko Y. Yamasaki, Yohko Tsuboi, Norbert Werner, Fumie Akimoto, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Akio Hoshino, Hideki Uchiyama, Takayuki Tamura, Shunji Kitamoto, Kazuhiro Nakazawa, Yuichi Kato, Aya Bamba, Roger Blandford, Yoh Takei, Yoshito Haba, Maria Chernyakova, Shin Watanabe, Edward M. Cackett, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )
Subjects: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, observational [methods], energy resolution, FOS: Physical sciences, Excitation temperature, helium, quantum number, clusters: individual (Perseus) [galaxies], 01 natural sciences, plasma: model, Ion, iron, Settore FIS/05 - Astronomia e Astrofisica, Ionization, Intracluster medium, gas, 0103 physical sciences, excited state, ionization, X-ray: emission, structure, plasma: thermal, cluster, 010303 astronomy & astrophysics, fine structure, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, galaxies: clusters: individual (Perseus), central region, temperature, Astronomy and Astrophysics, Plasma, observatory, Temperature gradient, Space and Planetary Science, X-rays: galaxies: clusters, Excited state, galaxies: clusters [X-rays], ion, spectrometer, methods: observational, Atomic physics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: Hitomi Collaboration 194名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 194 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-14, 資料番号: SA1170336000
Published: 2018

16. Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi

Author: Hitomi Collaboration, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steven W Allen, Lorella Angelini, Marc Audard, Hisamitsu Awaki, Magnus Axelsson, Aya Bamba, Marshall W Bautz, Roger Blandford, Laura W Brenneman, Gregory V Brown, Esra Bulbul, Edward M Cackett, Maria Chernyakova, Meng P Chiao, Paolo S Coppi, Elisa Costantini, Jelle de Plaa, Cor P de Vries, Jan-Willem den Herder, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew C Fabian, Carlo Ferrigno, Adam R Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi C Gallo, Poshak Gandhi, Margherita Giustini, Andrea Goldwurm, Liyi Gu, Matteo Guainazzi, Yoshito Haba, Kouichi Hagino, Kenji Hamaguchi, Ilana M Harrus, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Kiyoshi Hayashida, Junko S Hiraga, Ann Hornschemeier, Akio Hoshino, John P Hughes, Yuto Ichinohe, Ryo Iizuka, Hajime Inoue, Yoshiyuki Inoue, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Masachika Iwai, Jelle Kaastra, Tim Kallman, Tsuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Nobuyuki Kawai, Richard L Kelley, Caroline A Kilbourne, Takao Kitaguchi, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Katsuji Koyama, Shu Koyama, Peter Kretschmar, Hans A Krimm, Aya Kubota, Hideyo Kunieda, Philippe Laurent, Shiu-Hang Lee, Maurice A Leutenegger, Olivier O Limousin, Michael Loewenstein, Knox S Long, David Lumb, Greg Madejski, Yoshitomo Maeda, Daniel Maier, Kazuo Makishima, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian R McNamara, Missagh Mehdipour, Eric D Miller, Jon M Miller, Shin Mineshige, Kazuhisa Mitsuda, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard F Mushotzky, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Shinya Nakashima, Kazuhiro Nakazawa, Kumiko K Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Takaya Ohashi, Masanori Ohno, Takashi Okajima, Naomi Ota, Masanobu Ozaki, Frits Paerels, Stéphane Paltani, Robert Petre, Ciro Pinto, Frederick S Porter, Katja Pottschmidt, Christopher S Reynolds, Samar Safi-Harb, Shinya Saito, Kazuhiro Sakai, Toru Sasaki, Goro Sato, Kosuke Sato, Rie Sato, Makoto Sawada, Norbert Schartel, Peter J Serlemtsos, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall K Smith, Yang Soong, Łukasz Stawarz, Yasuharu Sugawara, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Tadayuki Takahashi, Shiníchiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Takaaki Tanaka, Yasuo Tanaka, Yasuyuki T Tanaka, Makoto S Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Hideki Uchiyama, Yasunobu Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shiníchiro Uno, C Megan Urry, Eugenio Ursino, Shin Watanabe, Norbert Werner, Dan R Wilkins, Brian J Williams, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Yoichi Yatsu, Daisuke Yonetoku, Irina Zhuravleva, Abderahmen Zoghbi, Nozomi Nakaniwa, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, X-rays: binaries, general [binaries], Settore FIS/05 - Astronomia e Astrofisica, individual (IGR J16318-4848) [stars], Ionization, 0103 physical sciences, Continuum (set theory), 010306 general physics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Scattering, stars: individual (IGR J16318-4848), Astronomy and Astrophysics, binaries: general, Space and Planetary Science, binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Doppler broadening
Abstract: 著者人数: Hitomi Collaboration 193名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 萩野, 浩一; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子; 中庭, 望）, Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.; Nakaniwa, Nozomi), Accepted: 2017-11-02, 資料番号: SA1170342000
Published: 2018

17. Hitomi X-ray observation of the pulsar wind nebula G21.5$−$0.9

Author: Tsuneyoshi Kamae, Chris Done, Takeshi Nakamori, Hirofumi Noda, Philippe Laurent, Gregory V. Brown, Masahiro Tsujimoto, Luigi C. Gallo, Andrea Goldwurm, Akio Hoshino, Edward M. Cackett, Makoto Tashiro, Yoichi Yatsu, Kazutaka Yamaoka, Makoto Yamauchi, Makoto Sawada, Esra Bulbul, Yasuo Tanaka, Katsuji Koyama, Hiromitsu Takahashi, Kazuhisa Mitsuda, Tsunefumi Mizuno, Jon M. Miller, Takashi Okajima, Katsuhiro Hayashi, Yang Soong, Daisuke Yonetoku, Peter J. Serlemtsos, Yoshitaka Ishisaki, Hans A. Krimm, Akihiro Furuzawa, Olivier Limousin, Shiu-Hang Lee, Takao Kitaguchi, Laura Brenneman, Hideki Uchiyama, Samar Safi-Harb, Koji Mukai, Poshak Gandhi, Yasushi Fukazawa, Abderahmen Zoghbi, Ann Hornschemeier, Marc Audard, Hiroki Akamatsu, Andrew Szymkowiak, D. Lumb, Koji Mori, Hiroshi Tsunemi, Kazuhiro Nakazawa, Jan-Willem den Herder, Robert Petre, Shinya Saito, Aya Kubota, Takayuki Hayashi, Shinya Nakashima, Carlo Ferrigno, Eric D. Miller, Shin'ichiro Uno, Masachika Iwai, Dan McCammon, Takao Nakagawa, Irina Zhuravleva, Satoshi Sugita, Naomi Ota, Nozomu Nakaniwa, Ikuyuki Mitsuishi, Richard L. Kelley, Missagh Mehdipour, Motohide Kokubun, Dan R. Wilkins, Tadayuki Takahashi, Marshall W. Bautz, Francesco Tombesi, Jelle Kaastra, Katja Pottschmidt, Shunji Kitamoto, Masanobu Ozaki, Yuzuru Tawara, Margherita Giustini, Ken Ebisawa, Ryo Iizuka, Greg Madejski, Takeshi Go Tsuru, Shin Mineshige, Toshiki Sato, Liyi Gu, Hiroyasu Tajima, Aya Bamba, Roger Blandford, Yuichi Terashima, C. Megan Urry, Richard F. Mushotzky, Peter Kretschmar, Kosuke Sato, Knox S. Long, Steven W. Allen, Hideyuki Mori, Hiroyuki Uchida, Yoshihiro Ueda, Kyoko Matsushita, Nobuyuki Kawai, Brian J. Williams, Hiroshi Murakami, Tetsu Kitayama, Randall K. Smith, Hiroshi Tomida, Norbert Schartel, Toru Tamagawa, Łukasz Stawarz, Rie Sato, Hiroya Yamaguchi, Hisamitsu Awaki, Takaaki Tanaka, Frits Paerels, Tadayasu Dotani, Yasuharu Sugawara, Ciro Pinto, Paolo Coppi, Kiyoshi Hayashida, Frederick S. Porter, Matteo Guainazzi, Isamu Hatsukade, Toru Sasaki, Megan E. Eckart, Takaya Ohashi, Yasunobu Uchiyama, Kouichi Hagino, Yuichiro Ezoe, Megumi Shidatsu, Kumi Ishikawa, Takayuki Tamura, Stéphane Paltani, Hideyo Kunieda, Eugenio Ursino, Adam R. Foster, Ryuichi Fujimoto, Caroline A. Kilbourne, Yoh Takei, Yoshito Haba, Noriko Y. Yamasaki, Elisa Costantini, Shin'ichiro Takeda, Takayoshi Kohmura, Maria Chernyakova, Shin Watanabe, Aurora Simionescu, Hiroshi Nakajima, Satoru Katsuda, Magnus Axelsson, Meng P. Chiao, Jelle de Plaa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Yohko Tsuboi, Norbert Werner, Andrew C. Fabian, Kazuo Makishima, Fumie Akimoto, Jun Kataoka, Brian R. McNamara, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Shu Koyama, Masayoshi Nobukawa, Tahir Yaqoob, Hironori Matsumoto, Yoshitomo Maeda, Cor P. de Vries, Benson Guest, Masanori Ohno, Christopher S. Reynolds, Hirokazu Odaka, Michael Loewenstein, Kenji Hamaguchi, Ilana M. Harrus, Manabu Ishida, Yoshiyuki Inoue, Yukikatsu Terada, Hiroaki Murakami, Timothy R. Kallman, Takuya Miyazawa, Shinya Yamada, Kazuhiro Sakai, Felix Aharonian, Junko S. Hiraga, Hiromi Seta, Teruaki Enoto, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Maurice A. Leutenegger, Kumiko K. Nobukawa, Goro Sato, Shutaro Ueda, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Photon, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, pulsars: individual (PSRJ1833-1034), 01 natural sciences, Pulsar wind nebula, Power law, Spectral line, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, Pulsar, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectrometer, supernova remnants [ISM], individual (PSR J1833-1034) [pulsars], Astronomy and Astrophysics, ISM: individual objects (G21.5-0.9), Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, individual objects (G21.5-0.9) [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: 196名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子; 佐藤, 寿紀; 中庭, 望), Number of authors: Hitomi Collaboration 197 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hayashi, Tasuku; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.; Sato, Toshiki; Nakaniwa, Nozomu), Accepted: 2018-02-14, 資料番号: SA1180104000
Published: 2018

18. Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-K$\alpha$ line emission from an active galactic nucleus

Author: Yasuo Tanaka, Hideki Uchiyama, Takao Nakagawa, Margherita Giustini, Shunji Kitamoto, Peter J. Serlemitsos, Marc Audard, Jon M. Miller, Kumi Ishikawa, Hirokazu Odaka, Yuzuru Tawara, Takeshi Go Tsuru, Kosuke Sato, Koji Mukai, Abderahmen Zoghbi, Kazuhiro Nakazawa, Yasuharu Sugawara, Yoshihiro Ueda, C. Megan Urry, Richard F. Mushotzky, Nobuyuki Kawai, Ann Hornschemeier, Katja Pottschmidt, Aya Kubota, Hironori Matsumoto, Richard L. Kelley, Brian J. Williams, Luigi C. Gallo, Tetsu Kitayama, Megumi Shidatsu, Felix Aharonian, Shin'ichiro Takeda, Paolo De Coppi, Teruaki Enoto, David H. Lumb, Shin Mineshige, Kyoko Matsushita, Maurice A. Leutenegger, Masayoshi Nobukawa, Tahir Yaqoob, Irina Zhuravleva, Olivier Limousin, Steven W. Allen, Eugenio Ursino, Toru Tamagawa, Missagh Mehdipour, Adam R. Foster, Jan-Willem den Herder, Takayuki Hayashi, Rie Sato, Peter Kretschmar, Taiki Kawamuro, Aurora Simionescu, Makoto Yamauchi, Hiromitsu Takahashi, Manabu Ishida, Kazuhisa Mitsuda, Shiu-Hang Lee, Michael Loewenstein, Frits Paerels, Tsuneyoshi Kamae, Meng P. Chiao, Takao Kitaguchi, Kenji Hamaguchi, Aya Bamba, Matteo Guainazzi, Kouichi Hagino, Philippe Laurent, Jelle de Plaa, Hiroshi Tsunemi, Kazuo Makishima, Toru Sasaki, Roger Blandford, Koji Mori, Timothy R. Kallman, Ilana M. Harrus, Ikuyuki Mitsuishi, Laura Brenneman, Hiroki Akamatsu, Francesco Tombesi, Daisuke Yonetoku, Jelle Kaastra, Yoshitaka Ishisaki, Makoto Tashiro, Andrew Szymkowiak, Satoru Katsuda, Esra Bulbul, Hans A. Krimm, Eric D. Miller, Shin'ichiro Uno, Andrea Goldwurm, Hirofumi Noda, Knox S. Long, Samar Safi-Harb, Yoshitomo Maeda, Stephane Ṕaltani, Carlo Ferrigno, Yang Soong, Liyi Gu, Satoshi Sugita, Hiroshi Nakajima, Cor P. de Vries, Marshall W. Bautz, Robert Petre, Yuichi Terashima, Masanori Ohno, Christopher S. Reynolds, Shinya Nakashima, Shinya Saito, Hisamitsu Awaki, Yoh Takei, Yoshito Haba, Tsunefumi Mizuno, Masanobu Ozaki, Katsuji Koyama, Kiyoshi Hayashida, Takaaki Tanaka, Yuichiro Ezoe, Masachika Iwai, Tadayasu Dotani, Jun Kataoka, Naomi Ota, Hiroya Yamaguchi, Yohko Tsuboi, Takuya Miyazawa, Dan R. Wilkins, Norbert Werner, Fumie Akimoto, Motohide Kokubun, Kumiko K. Nobukawa, Gregory V. Brown, Elisa Costantini, Megan E. Eckart, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Tadayuki Takahashi, Goro Sato, Takaya Ohashi, Poshak Gandhi, Katsuhiro Hayashi, Yasushi Fukazawa, Hiroyasu Tajima, Maria Chernyakova, Shin Watanabe, Hideyo Kunieda, Greg Madejski, Dan McCammon, Shutaro Ueda, Masahiro Tsujimoto, Ryuichi Fujimoto, Junko S. Hiraga, Magnus Axelsson, Lukasz Stawarz, Hiroshi Murakami, Noriko Y. Yamasaki, Frederick S. Porter, Hiromi Seta, Ken Ebisawa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Hideyuki Mori, Hiroshi Tomida, Randall K. Smith, Edward M. Cackett, Hiroyuki Uchida, Chris Done, Takayuki Tamura, Norbert Schartel, John P. Hughes, Daniel Maier, Hajime Inoue, Lorella Angelini, Takeshi Nakamori, Ryo Iizuka, Andrew C. Fabian, Yoichi Yatsu, Kazutaka Yamaoka, Brian R. McNamara, Ciro Pinto, Shu Koyama, Makoto Sawada, Yasunobu Uchiyama, Takashi Okajima, Akihiro Furuzawa, Takayoshi Kohmura, Isamu Hatsukade, Caroline A. Kilbourne, Shinya Yamada, Kazuhiro Sakai, Yoshiyuki Inoue, Yukikatsu Terada, Akio Hoshino, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, individual (NGC 1275) [galaxies], [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], galaxies: active, observational [methods], galaxies: radio galaxy, radio galaxy [galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, galaxies: individual (NGC 1275), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Astronomy and Astrophysics, Torus, Galaxy, galaxies [X-rays], Full width at half maximum, X-rays: galaxies, Space and Planetary Science, active [galaxies], H-alpha, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width
Abstract: 著者人数: Hitomi Collaboration 193名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 萩野, 浩一; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; Lee, Shiu-Hang; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Lee, Shiu-Hang; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-11-16, 資料番号: SA1170338000
Published: 2018

19. Solar abundance ratios of the iron-peak elements in the Perseus cluster

Author: Yasuo Tanaka, Hideki Uchiyama, Hironori Matsumoto, T. Hayashi, Cor P. de Vries, Shin'ichiro Uno, Shinya Nakashima, Ann Hornschemeier, Satoshi Sugita, Naomi Ota, Masanori Ohno, Christopher S. Reynolds, Megumi Shidatsu, Kumi Ishikawa, Lukasz Stawarz, Hiroshi Murakami, Shunji Kitamoto, Hiroshi Tomida, Masanobu Ozaki, Katsuji Koyama, Kenji Hamaguchi, Kazuhiro Nakazawa, Hiroyasu Tajima, Katja Pottschmidt, Marshall W. Bautz, Daisuke Yonetoku, Yoshitaka Ishisaki, Shin Mineshige, Hans A. Krimm, Marc Audard, Motohide Kokubun, Chris Done, Peter Kretschmar, Katsuhiro Hayashi, Jon M. Miller, Samar Safi-Harb, Hiroshi Tsunemi, Aya Bamba, Ikuyuki Mitsuishi, Takeshi Nakamori, Dan McCammon, Hiromi Seta, Olivier Limousine, Roger Blandford, Hirokazu Odaka, Andrew C. Fabian, Yohko Tsuboi, Norbert Werner, Fumie Akimoto, Shigeo Yamauchi, Hiroya Yamaguchi, Daniel R. Wik, David H. Lumb, Yuichi Terashima, Richard L. Kelley, Hiroyuki Uchida, Kiyoshi Hayashida, Shinya Yamada, Brian R. McNamara, Kyoko Matsushita, Shu Koyama, John P. Hughes, Maxim Markevitch, Yuto Ichinohe, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Shinya Saito, Yasunobu Uchiyama, Kouichi Hagino, C. Megan Urry, Shiu-Hang Lee, Missagh Mehdipour, Kazuhiro Sakai, Michael Loewenstein, Yuichiro Ezoe, Masachika Iwai, Hajime Inoue, Yoh Takei, Abderahmen Zoghbi, Ciro Pinto, Yoshito Haba, Jun Kataoka, Richard F. Mushotzky, Toru Tamagawa, Gregory V. Brown, Hiroshi Nakajima, Steven W. Allen, Lorella Angelini, Kumiko K. Nobukawa, Junko S. Hiraga, Magnus Axelsson, Takuya Miyazawa, Tsunefumi Mizuno, Meng P. Chiao, Stéphane Paltani, Rie Sato, Ryuichi Fujimoto, Peter J. Serlemitsos, Ryo Iizuka, Goro Sato, Nobuyuki Kawai, Yoichi Yatsu, Brian J. Williams, Kazutaka Yamaoka, Maria Chernyakova, Eric D. Miller, Ilana M. Harrus, Frits Paerels, Poshak Gandhi, Yasushi Fukazawa, Shin Watanabe, Ken Ebisawa, Yasuyuki T. Tanaka, Shutaro Ueda, Tetsu Kitayama, P. Laurent, Massimiliano Galeazzi, Koji Mukai, Makoto Tashiro, Masahiro Tsujimoto, Edward M. Cackett, Matteo Guainazzi, Frederick S. Porter, Takeshi Go Tsuru, Kosuke Sato, Aya Kubota, Timothy R. Kallman, Makoto Sawada, Esra Bulbul, Paolo De Coppi, Felix Aharonian, Takao Kitaguchi, Teruaki Enoto, Kazuo Makishima, Toru Sasaki, Maurice A. Leutenegger, Takao Nakagawa, Masayoshi Nobukawa, Takayoshi Kohmura, Laura Brenneman, Takayuki Tamura, Irina Zhuravleva, Tahir Yaqoob, Yang Soong, Tsuneyoshi Kamae, Takashi Okajima, Yoshihiro Ueda, Yasuharu Sugawara, Eugenio Ursino, Adam R. Foster, Manabu Ishida, Isamu Hatsukade, Satoru Katsuda, Knox S. Long, Yoshiyuki Inoue, Luigi C. Gallo, Akihiro Furuzawa, Hirofumi Noda, Koji Mori, Caroline A. Kilbourne, Yukikatsu Terada, Carlo Ferrigno, Hiroki Akamatsu, Andrew Szymkowiak, Dan R. Wilkins, Daniel Maier, Tadayuki Takahashi, Robert Petre, Margherita Giustini, Elisa Costantini, Jan-Willem den Herder, Greg Madejski, Francesco Tombesi, Jelle Kaastra, Hideyuki Mori, Randall K. Smith, Norbert Schartel, Shin'ichiro Takeda, Aurora Simionescu, Jelle de Plaa, Andrea Goldwurm, Megan E. Eckart, Takaya Ohashi, Hideyo Kunieda, Noriko Y. Yamasaki, Y. Tawara, Yoshitomo Maeda, Hisamitsu Awaki, Takaaki Tanaka, Tadayasu Dotani, Liyi Gu, Akio Hoshino, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Apollo - University of Cambridge Repository
Subjects: Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Nucleosynthesis, Intracluster medium, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, Multidisciplinary, White dwarf, Astronomy, Iron peak, Hitomi Collaboration, Supernova, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: 著者人数: Hitomi Collaboration 193名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 將親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子), Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida. Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-09-21, 資料番号: SA1170128000
Published: 2017

20. Inflight Calibration of the Hitomi Soft X-ray Spectrometer (2) Point Spread Function

Author: Nozomi Nakaniwa, Richard Kelley, Peter J. Serlemitsos, Tahir Yaqoob, Manabu Ishida, Sho Kurashima, Masahiro Tsujimoto, Ryota Asai, Takayuki Hayashi, Lorella Angelini, Hideyuki Mori, Yoshitomo Maeda, Takashi Okajima, Akihiro Furuzawa, Ryo Iizuka, Toshiki Sato, and Shu Koyama
Subjects: Point spread function, Physics, Soft x ray, Spectrometer, business.industry, Calibration (statistics), FOS: Physical sciences, telescopes, Astronomy and Astrophysics, 01 natural sciences, 010309 optics, Optics, techniques: imaging spectroscopy, Space and Planetary Science, 0103 physical sciences, space vehicles: instruments, Astrophysics - Instrumentation and Methods for Astrophysics, business, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: 著者人数: 17名, Accepted: 2017-11-11, 資料番号: SA1170316000
Published: 2017
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21. Spectral response and effective area functions of the Hitomi imaging instruments

Author: Lorella Angelini, Hiromitsu Takahashi, M. C. Witthoeft, Robert S. Hill, Kristin Rutkowski, Tahir Yaqoob, H. A. Krimm, Michael S. Dutka, Eric D. Miller, Hiroya Yamaguchi, and Michael Loewenstein
Subjects: Physics, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Mechanical Engineering, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, X-ray telescope, 01 natural sciences, Spectral line, Electronic, Optical and Magnetic Materials, law.invention, 010309 optics, Telescope, Space and Planetary Science, Control and Systems Engineering, law, 0103 physical sciences, Calibration, Ray tracing (graphics), Satellite, 010303 astronomy & astrophysics, Instrumentation, Remote sensing
Abstract: We describe the tools and the underlying methods and principles for generating the spectral response functions for the four imaging instruments that were flown on the Hitomi x-ray astronomy satellite [Soft X-ray Spectrometer, or SXS; Soft X-ray Imager, or SXI, and two Hard X-ray Imagers, or HXI]. In essence, the spectral response function is a temporally and spatially averaged effective area and line-spread-function. For model-fitting x-ray spectra from an instrument, the spectral response function encapsulates the end-to-end physics of the entire system from telescope to detector, and also includes satellite attitude drift, exposure corrections, and in the case of the HXIs, drift in the telescope/detector alignment system. Accuracy in the construction of the spectral response functions is, therefore, critical to maximize the science return from the data.
Published: 2018

22. Heasim and skyback simulation tools and their application to the Hitomi mission

Author: Tahir Yaqoob, Michael S. Dutka, Lorella Angelini, M. C. Witthoeft, Michael Loewenstein, Robert S. Hill, and David A. Riethmiller
Subjects: Vignetting, Spectrometer, Computer science, Event (computing), Mechanical Engineering, Monte Carlo method, Astronomy and Astrophysics, Construct (python library), 01 natural sciences, Electronic, Optical and Magnetic Materials, 010309 optics, Range (mathematics), Computer engineering, Space and Planetary Science, Control and Systems Engineering, 0103 physical sciences, Calibration, Relevance (information retrieval), 010303 astronomy & astrophysics, Instrumentation
Abstract: We present an introduction to the heasim multimission observation and skyback background, high-energy pseudo Monte Carlo astrophysical simulation tools. Heasim may be used to accurately and efficiently construct flexible image transport system (FITS) event files for simple or composite sources with a wide range of standard and user-defined spatial, spectral, and temporal characteristics. Skyback is designed to enable users to assess the impact of background discrete and diffuse emission on prospective observations, and skyback output may be directly input into heasim. We present a brief overview of heasim and skyback input, algorithms, usage, and output. We also introduce the sxsbranch tool that computes Hitomi soft X-ray spectrometer resolution grade branching ratios, emphasizing its application to simulations. We include several examples of particular relevance to the Hitomi mission.
Published: 2018

23. The Polarimeter for Relativistic Astrophysical X-ray Sources

Author: Chryssa Kouveliotou, Timothy R. Kallman, Craig B. Markwardt, Robert Petre, Jeremy D. Schnittman, Yang Soong, Takashi Okajima, Tod E. Strohmayer, Yuzuru Tawara, P. Kaaret, Joanne E. Hill, J. Kevin Black, Keith Jahoda, Toru Tamagawa, Lorella Angelini, and Theodore Jaeger
Subjects: Physics, COSMIC cancer database, Time projection chamber, Spacecraft, 010308 nuclear & particles physics, business.industry, Linear polarization, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Astronomy, Polarimeter, 01 natural sciences, Neutron star, Observatory, 0103 physical sciences, business, 010303 astronomy & astrophysics
Abstract: The Polarimeter for Relativistic Astrophysical X-ray Sources (PRAXyS) is one of three Small Explorer (SMEX) missions selected by NASA for Phase A study, with a launch date in 2020. The PRAXyS Observatory exploits grazing incidence X-ray mirrors and Time Projection Chamber Polarimeters capable of measuring the linear polarization of cosmic X-ray sources in the 2-10 keV band. PRAXyS combines well-characterized instruments with spacecraft rotation to ensure low systematic errors. The PRAXyS payload is developed at the Goddard Space Flight Center with the Johns Hopkins University Applied Physics Laboratory, University of Iowa, and RIKEN (JAXA) collaborating on the Polarimeter Assembly. The LEOStar-2 spacecraft bus is developed by Orbital ATK, which also supplies the extendable optical bench that enables the Observatory to be compatible with a Pegasus class launch vehicle. A nine month primary mission will provide sensitive observations of multiple black hole and neutron star sources, where theory predicts polarization is a strong diagnostic, as well as exploratory observations of other high energy sources. The primary mission data will be released to the community rapidly and a Guest Observer extended mission will be vigorously proposed.
Published: 2016

24. DISCOVERY OF HOT GAS IN OUTFLOW IN NGC 3379

Author: Andrew J. King, Roger R. Fu, Nicola Brassington, Dong-Woo Kim, J. C. Gallagher, G. Fabbiano, Silvia Pellegrini, V. Kalogera, Andreas Zezas, Ginevra Trinchieri, Steve Zepf, Roger L. Davies, Lorella Angelini, TRINCHIERI G., PELLEGRINI S., FABBIANO G., FU R., BRASSINGTON N. J., ZEZAS A., KIM D.-W., GALLAGHER J., ANGELINI L., DAVIES R. L., KALOGERA V., KING A. R., ZEPF S., Brassington N., Trinchieri G., Pellegrini S., Fabbiano G., Fu R., Kim D.W., Zezas A., Gallagher J., Angelini L., Davies R., Kalogera V., King A., and Zepf S.
Subjects: Physics, Solar mass, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radial distribution, Radius, Astrophysics, Galaxy, Early type, Luminosity, Interstellar medium, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Outflow, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report the discovery of a faint (L_x ~ 4 10^37 erg/s, 0.5-2 keV), out-flowing gaseous hot interstellar medium (ISM) in NGC 3379. This represents the lowest X-ray luminosity ever measured from a hot phase of the ISM in a nearby early type galaxy. The discovery of the hot ISM in a very deep Chandra observation was possible thanks to its unique spectral and spatial signatures, which distinguish it from the integrated stellar X-ray emission, responsible for most of the unresolved emission in the Chandra data. This hot component is found in a region of about 800 pc in radius at the center of the galaxy and has a total mass M~ 3 10^5 solar masses. Independent theoretical prediction of the characteristics of an ISM in this galaxy, based on the intrinsic properti es of NGC 3379, reproduce well the observed luminosity, temperature, and radial distribution and mass of the hot gas, and indicate that the gas is in an outflowing phase, predicted by models but not observed in any system so far., Comment: Accepted for publication in The Astrophysical Journal
Published: 2016

25. DEEP CHANDRA MONITORING OBSERVATIONS OF NGC 3379: CATALOG OF SOURCE PROPERTIES

Author: Roger L. Davies, Andreas Zezas, Ar King, Giuseppina Fabbiano, Kalogera, Silvia Pellegrini, Ginevra Trinchieri, J. C. Gallagher, A. Kundu, S. E. Zepf, Tassos Fragos, Lorella Angelini, D. W. Kim, Nicola Brassington, Brassington N. J., Fabbiano G., Kim D.-W., Zezas A., Zepf S., Kundu A., Angelini L., Davies R. L., Gallagher J., Kalogera V., Fragos T., King A. R., Pellegrini S., and Trinchieri G.
Subjects: Physics, X-rays: galaxies, Space and Planetary Science, Astrophysics (astro-ph), Galaxies: individual (NGC 3379), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, X-rays: binarie
Abstract: We present the properties of the discrete X-ray sources detected in our monitoring program of the `typical' elliptical galaxy, NGC 3379, observed with Chandra ACIS-S in five separate pointings, resulting in a co-added exposure of 324-ks. From this deep observation, 132 sources have been detected within the region overlapped by all observations, 98 of which lie within the D25 ellipse of the galaxy. These 132 sources range in Lx from 6E35 erg/s (with 3sigma upper limit 1E39 erg/s, which has been classified as a ULX. From optical data, 10 X-ray sources have been determined to be coincident with a globular cluster, these sources tend to have high X-ray luminosity, with three of these sources exhibiting Lx> 1E38 erg/s. From X-ray source photometry, it has been determined that the majority of the 132 sources that have well constrained colors, have values that are consistent with typical LMXB spectra. Additionally to this, a sub-population of 10 sources has been found to exhibit very hard spectra and it is expected that most of these sources are absorbed background AGN. There are 64 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Five of these sources have been identified as transient candidates, with a further 3 possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy., Accepted for publication in ApJS, 120 pages, with 14 figures. No changes from previous revision
Published: 2016

26. Astro-H data analysis, processing and archive

Author: Hiromitsu Takahashi, Hans A. Krimm, Joseph Eggen, Yukitatsu Terada, Robert S. Hill, Lorella Angelini, Michael Loewenstein, Andrew Sargent, Ilana M. Harrus, Eric D. Miller, Masayoshi Nobukawa, Tahir Yaqoob, Kristin Rutkowski, M. C. Witthoeft, Makoto Sawada, Michael S. Dutka, and Hiroya Yamaguchi
Subjects: Engineering, Data processing, Operations research, business.industry, Payload, Plan (drawing), 01 natural sciences, Pipeline (software), 010309 optics, Software, 0103 physical sciences, Systems engineering, Analysis software, business, 010303 astronomy & astrophysics
Abstract: Astro-H (Hitomi) is an X-ray/Gamma-ray mission led by Japan with international participation, launched on February 17, 2016. The payload consists of four different instruments (SXS, SXI, HXI and SGD) that operate simultaneously to cover the energy range from 0.3 keV up to 600 keV. This paper presents the analysis software and the data processing pipeline created to calibrate and analyze the Hitomi science data along with the plan for the archive and user support. These activities have been a collaborative effort shared between scientists and software engineers working in several institutes in Japan and USA.
Published: 2016

27. Discovery of X-Ray Emission from the Galactic Supernova Remnant G32.8-0.1 with Suzaku

Author: Robert Petre, Lorella Angelini, John W. Hewitt, Ping Zhou, Aya Bamba, Yukikatsu Terada, Samar Safi-Harb, Fabrizio Bocchino, and Makoto Sawada
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), X-ray astronomy, 010308 nuclear & particles physics, Molecular cloud, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Gamma-ray astronomy, Astrophysics, 01 natural sciences, Space and Planetary Science, Ionization, 0103 physical sciences, High Energy Stereoscopic System, Supergiant, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the first dedicated X-ray study of the supernova remnant (SNR) G32.8-0.1 (Kes 78) with Suzaku. X-ray emission from the whole SNR shell has been detected for the first time. The X-ray morphology is well correlated with the emission from the radio shell, while anti-correlated with the molecular cloud found in the SNR field. The X-ray spectrum shows not only conventional low-temperature (kT ~ 0.6 keV) thermal emission in a non-equilibrium ionization state, but also a very high temperature (kT ~ 3.4 keV) component with a very low ionization timescale (~ 2.7e9 cm^{-3}s), or a hard non-thermal component with a photon index Gamma~2.3. The average density of the low-temperature plasma is rather low, of the order of 10^{-3}--10^{-2} cm^{-3}, implying that this SNR is expanding into a low-density cavity. We discuss the X-ray emission of the SNR, also detected in TeV with H.E.S.S., together with multi-wavelength studies of the remnant and other gamma-ray emitting SNRs, such as W28 and RCW 86. Analysis of a time-variable source, 2XMM J185114.3-000004, found in the northern part of the SNR, is also reported for the first time. Rapid time variability and a heavily absorbed hard X-ray spectrum suggest that this source could be a new supergiant fast X-ray transient., Comment: 20 pages, 14 figures, ApJ, in press
Published: 2016

28. The ASTRO-H (Hitomi) x-ray astronomy satellite

Author: Yasuharu Sugawara, Luigi C. Gallo, Manabu Ishida, Hiroya Yamaguchi, Makoto Yamauchi, Hiromitsu Takahashi, Kazuhisa Mitsuda, Eric J. Miller, Ciro Pinto, Grzegorz Madejski, Meng P. Chiao, Yoshiharu Namba, Kumiko K. Nobukawa, Goro Sato, Harvey Moseley, Takayoshi Kohmura, Mina Ogawa, Greg Brown, Kevin R. Boyce, Missagh Mehdipour, Shutaro Ueda, Satoru Katsuda, Philipp Azzarello, Shin'ichiro Uno, Atsushi Wada, Takao Kitaguchi, Knox S. Long, Yohko Tsuboi, Nobutaka Bando, Shin-ichiro Sakai, Hajime Inoue, Masayuki Itoh, Kazuyuki Hirose, Norbert Werner, Fumie Akimoto, Timothy R. Kallman, Shigeo Yamauchi, Maxim Markevitch, Yuto Ichinohe, Naohisa Anabuki, Satoshi Sugita, Yoshiyuki Inoue, Olivier Limousin, Meg Urry, Kouichi Hagino, Akio Hoshino, Kumi Ishikawa, Cor P. de Vries, Teruaki Enoto, Yasuo Tanaka, M. Pohl, Masanobu Ozaki, Kenji Minesugi, Peter Shirron, Maurice A. Leutenegger, Koji Mori, Hideki Uchiyama, Yukikatsu Terada, D. Haas, Keith A. Arnaud, Masanori Ohno, Christopher S. Reynolds, Hiromi Seta, Yusuke Nishioka, Carlo Ferrigno, Edgar Canavan, Katsuji Koyama, Daniel R. Wik, Shunji Kitamoto, Keisuke Shinozaki, Katsuhiro Hayashi, Dan McCammon, David H. Lumb, Kyoko Matsushita, Hiroyuki Uchida, John P. Hughes, Daniel Maier, Lorella Angelini, Taro Kawano, Cynthia Simmons, Shiro Ueno, Koji Mukai, Abderahmen Zoghbi, Makoto Asai, Toru Tamagawa, Rie Sato, Keisuke Tamura, Yuzuru Tawara, Łukasz Stawarz, Motohide Kokubun, Hiroshi Murakami, Hiroshi Tomida, F. Scott Porter, Hiroshi Tsunemi, Ikuyuki Mitsuishi, Michael J. DiPirro, Richard F. Mushotzky, Nobuyuki Kawai, Brian J. Williams, Richard L. Kelley, Hirokazu Odaka, Matteo Guainazzi, Kazuo Makishima, Yuichiro Ezoe, Takahiro Yamada, Hiroki Akamatsu, Andrew Szymkowiak, Philippe Laurent, James Pontius, Yasunobu Uchiyama, Tetsu Kitayama, Megumi Shidatsu, Felix Aharonian, Shigeo Kawasaki, Takanobu Shimada, Laura Brenneman, Toru Sasaki, Isamu Hatsukade, A. L. King, Takuya Miyazawa, Toshio Nakano, Atsumasa Yoshida, Robert Petre, Shinya Yamada, Stéphane Paltani, Eugenio Ursino, Adam R. Foster, Takayuki Hayashi, Shiu-Hang Lee, Toshio Murakami, Chris Done, Takeshi Nakamori, Kazuhiro Sakai, Ryo Nagino, Yuichi Terashima, Caroline A. Kilbourne, Michael Loewenstein, Shin Mineshige, Peter Kretschmar, John P. Doty, Candace Masters, Yoichi Sato, Junko S. Hiraga, Magnus Axelsson, Kenji Hamaguchi, Marshall W. Bautz, Junichiro Katsuta, Hiroaki Sameshima, Ilana M. Harrus, Thomas G. Bialas, Elisa Costantini, Daniel S. McGuinness, Yoichi Yatsu, Kazutaka Yamaoka, Naoko Iwata, Mark O. Kimball, Arvind Parmar, Yasuko Shibano, Norbert Schartel, Helen Russell, Gary A. Sneiderman, Steve Allen, Kiyoshi Hayashida, Makoto Sawada, Megan E. Eckart, Takaya Ohashi, Dmitry Khangulyan, Kosei Ishimura, Tatsuro Kosaka, Andrea Goldwurm, Takashi Okajima, Hirofumi Noda, Franco Moroso, F. B. S. Paerels, Hiroyuki Sugita, Alex Koujelev, Masaharu Nomachi, Tomomi Watanabe, Marc Audard, Tsunefumi Mizuno, Hideyo Kunieda, Keiji Ogi, Akihiro Furuzawa, Brian D. Ramsey, Masayoshi Nobukawa, Shinya Saito, Poshak Gandhi, Yasushi Fukazawa, Liyi Gu, Peter J. Serlemitsos, Noriko Y. Yamasaki, Tsuyoshi Okazaki, Takeshi Go Tsuru, Kosuke Sato, Aya Kubota, Chris Jewell, Yoshitomo Maeda, Yoshihiro Ueda, Shinya Nakashima, Irina Zhuravleva, Andrew C. Fabian, Tahir Yaqoob, Housei Nagano, Erin Kara, Brian R. McNamara, Naomi Ota, Shu Koyama, Joseph Miko, Madoka Kawaharada, Hisamitsu Awaki, Steve O'Dell, Takaaki Tanaka, Hironori Matsumoto, Tadayasu Dotani, Ken Ebisawa, Dan R. Wilkins, Hiroyasu Tajima, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Chikara Natsukari, Jan-Willem den Herder, Tadayuki Takahashi, Francois Lebrun, Hiroshi Nakajima, Yoh Takei, Hideyuki Mori, Yoshito Haba, Jun Kataoka, Randall K. Smith, Atsushi Okamoto, Maria Chernyakova, Shin Watanabe, Edward M. Cackett, Shin'ichiro Takeda, Takayuki Tamura, Francesco Tombesi, Jelle Kaastra, Maki Shida, Chris Baluta, Kirk Gilmore, Aurora Simionescu, Ann Hornschemeier, Kazuhiro Nakazawa, Jelle de Plaa, Naoko Iyomoto, Atsushi Harayama, Aya Bamba, Katja Pottschmidt, Roger Blandford, Kazunori Ishibashi, Makoto Tashiro, Esra Bulbul, Yang Soong, Paolo De Coppi, Daisuke Yonetoku, Yoshitaka Ishisaki, Hans A. Krimm, Samar Safi-Harb, Masahiro Tsujimoto, Ryuichi Fujimoto, Takao Nakagawa, Hiroyuki Ogawa, Margherita Giustini, Tuneyoshi Kamae, Takayuki Yuasa, Ryo Iizuka, Masayuki Ohta, Jon M. Miller, and Theodore Muench
Subjects: Physics, X-ray astronomy, Spacecraft, business.industry, Astronomy, High resolution, First light, Gamma-ray astronomy, 01 natural sciences, Spacecraft system, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Satellite, 010306 general physics, business, 010303 astronomy & astrophysics
Abstract: The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.
Published: 2016

29. The 2008 October Swift detection of X-ray bursts/outburst from the transient SGR-like AXP 1E 1547.0−5408

Author: G. L. Israel, Neil Gehrels, V. Mangano, P. Romano, Sergio Campana, Lorenzo Stella, Diego Götz, Simone Dall'Osso, Sandro Mereghetti, A. De Luca, Silvia Zane, F. Senziani, Lorella Angelini, David Palmer, Paolo Esposito, Roberto Turolla, Andrea Tiengo, Hans A. Krimm, Rosalba Perna, and Nanda Rea
Subjects: Physics, Swift, X-ray, Flux, Astronomy and Astrophysics, Astrophysics, Spectral line, law.invention, Telescope, Pulsar, Space and Planetary Science, law, Black-body radiation, Transient (oscillation), computer, computer.programming_language
Abstract: We report on the detailed study of the 2008 October outburst from the anomalous X-ray pulsar (AXP) 1E 1547.0-5408 discovered through the Swift/Burst Alert Telescope (BAT) detection of SGR-like short X-ray bursts on 2008 October 3. The Swift/X-ray Telescope (XRT) started observing the source after less than 100 s since the BAT trigger, when the flux (about 6E-11 erg/cm^2/s in the 2-10 keV range) was >50 times higher than its quiescent level. Swift monitored the outbursting activity of 1E 1547.0-5408 on a daily basis for approximately three weeks. This strategy allowed us to find a phase-coherent solution for the source pulsations after the burst, which, besides period and period derivative, requires a positive Period second derivative term (spin-down increase). The time evolution of the pulse shape is complex and variable, with the pulsed fraction increasing from 20% to 50% within the Swift observational window. The XRT spectra can be fitted well by means of a single component, either a power-law (PL) or a blackbody (BB). During the very initial phases of the outburst the spectrum is hard, with a PL photon index about 2 (or kT about 1.4 keV) which steepens to about 4 (or kT about 0.8 keV) within one day from the BAT trigger, though the two components are likely present simultaneously during the first day spectra. An INTEGRAL observation carried out five days after the trigger provided an upper limit of about 2E-11 erg/cm^2/s to the emission of 1E 1547.0-5408 in the 18-60 keV band.
Published: 2010

30. The 7-Steps of the Data Analysis

Author: Yukikatsu Terada, Aya Bamba, Junko S. Hiraga, Naoki Isobe, Aya Kubota, Naomi Ota, Piero Ranalli, Atsushi Senda, Motoko Suzuki, Toru Tamagawa, Yuji Urata, Suzaku Members, Masanobu Ozaki, Ken Ebisawa, Yoshitaka Ishisaki, Hironori Matsumoto, Izumi Yamagishi, Takayuki Tamura, Koji Mukai, Lorella Angelini, Kenji Hamaguchi, and it Suzaku Processing Members
Subjects: Physics, Data profiling, Engineering drawing, Physics and Astronomy (miscellaneous), Process (engineering), Calibration (statistics), Data structure
Abstract: It may seem to be difficult to analyze the Suzaku data, but the data structure and the tools are rather simple. We have constructed the way to process Suzaku FITS data and ftools for over ten years. We have prepared three kinds of manuals to analyze the data; Seven step manual of the XIS and the HXD for beginners, first step manual to walk through the analyses, and the ABC guide as a full manual. In the actual analyses, we have to be careful about events in operation and the limitations in the calibration of instruments. In this paper, the data structure, tools, and manuals with activities of help desks, current status of processing are summarized.
Published: 2007

31. Suzaku observations of cyclotron resonances in binary X-ray pulsars

Author: Hiromitsu Takahashi, F. Nagase, Motoki Nakajima, Yukikatsu Terada, Taro Kotani, Shunji Kitamoto, Motohide Kokubun, Kazuo Makishima, Masaya Suzuki, Lorella Angelini, Sachindra Naik, T. Mihara, Teruaki Enoto, Keisuke Sudoh, Satoshi Sugita, Daisuke Yonetoku, Takayoshi Kohmura, Tadayasu Dotani, and A. Yoshida
Subjects: Physics, Atmospheric Science, Cyclotron, Cyclotron resonance, Aerospace Engineering, Astronomy, Resonance, Astronomy and Astrophysics, Astrophysics, Landau quantization, Luminosity, law.invention, Neutron star, Geophysics, Pulsar, Space and Planetary Science, law, General Earth and Planetary Sciences, Line (formation)
Abstract: Since the typical magnetic field strengths of neutron stars reach 10 12 Gauss, the cyclotron resonance produced by a transition between Landau levels appears in the X-ray band. Systematic measurements of cyclotron absorption features in bright sources have been carried out extensively with Ginga, RXTE, BeppoSAX , and INTEGRAL . The cyclotron resonance phenomena can now be studied with a higher sensitivity over a wider hard X-ray band than before, thanks to the Hard X-ray Detector onboard the fifth Japanese X-ray satellite, Suzaku , launched in July, 2005. Suzaku observed Hercules X-1 mainly for calibration purposes, and successfully confirmed its well-known cyclotron absorption feature. Furthermore, the transient pulsar A0535+262 was observed with Suzaku on 14 September, 2005, in the decay phase of its minor outburst (Finger, M.F. Renewed Activity from A0535+26. The Astronomer’s Telegram, vol. 595, 2005). The cyclotron resonance of A0535+262 was successfully detected in absorption at about 45 keV (Inoue, H., Kunieda, H., White, N., Kelley, R., Mihara, T., Terada, Y., Takahashi, H., Kokubun, M., Makishima, K. Suzaku detection of cyclotron line near 50 keV for A0535+26. The Astronomer’s Telegram vol. 595, 2005; Terada, Y., Mihara, T., Nakajima, M., et al. Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku. ApJL 648, L139–L142, 2006), even though the object was as dim as 30 mCrab at 20 keV. Compared with previous measurements of the same feature achieved at much brighter phases (e.g., Kretschmar, P., Kreykenbohm, I., Pottschmidt, et al. Integral observes possible cyclotron line at 47 keV for 1A0535+262. The Astronomer’s Telegram, vol. 601, 2005; Wilson, C.A., Finger, M.H. RXTE confirms cyclotron line near 50 keV for A0535+26. The Astronomer’s Telegram 605, 2005), the Suzaku results give a new constraint to luminosity-related changes in the resonance energy that are observed in other binary pulsars (Nakajima, M., Mihara, T., Makishima, K., Niko, H. A further study of the luminosity-dependent cyclotron resonance energies of the binary X-ray pulsar 4U 0115+63 with the Rossi X-ray timing explorer. ApJ 646, 1125–1138, 2006).
Published: 2007

32. Suzaku Discovery of Absorption Lines from the Black Hole Transient 4U1630-472

Author: Lorella Angelini, Chris Done, Jean Cottam, Tomonori Yasuda, Taro Kotani, Yasushi Fukazawa, Kazutaka Yamaoka, Shinya Yamada, Hiromitsu Takahashi, Takayoshi Kohmura, Kazuo Makishima, Yoshihiro Ueda, Aya Kubota, Tadayasu Dotani, and Andrew C. Fabian
Subjects: Physics, Physics and Astronomy (miscellaneous), Absorption spectroscopy, Astronomy, Transient (oscillation), Astrophysics
Published: 2007

33. New Identification of the Mixed-Morphology Supernova Remnant G298.6-0.0 with Possible Gamma-ray Association

Author: Makoto Sawada, Yukikatsu Terada, Lorella Angelini, John W. Hewitt, Robert Petre, Yuto Nakano, and Aya Bamba
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Shell (structure), Gamma ray, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, 01 natural sciences, Interstellar medium, Space and Planetary Science, 0103 physical sciences, Thermal, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present an X-ray analysis on the Galactic supernova remnant (SNR) G298.6-0.0 with Suzaku. The X-ray image shows a center-filled structure inside the radio shell, implying this SNR is categorized as a mixed-morphology (MM) SNR. The spectrum is well reproduced by a single temperature plasma model in ionization equilibrium, with a temperature of 0.78 (0.70-0.87) keV. The total plasma mass of 30 solar mass indicates that the plasma has interstellar medium origin. The association with a GeV gamma-ray source 3FGL J1214.0-6236 on the shell of the SNR is discussed, in comparison with other MM SNRs with GeV gamma-ray associations. It is found that the flux ratio between absorption-corrected thermal X-rays and GeV gamma-rays decreases as the MM SNRs evolve to larger physical sizes. The absorption-corrected X-ray flux of G298.6-0.0 and the GeV gamma-ray flux of 3FGL J1214.0-6236 closely follow this trend, implying that 3FGL J1214.0-6236 is likely to be the GeV counterpart of G298.6-0.0., 11 pages, 6 figures, PASJ, in press
Published: 2015

34. Probing the Low‐Luminosity X‐Ray Luminosity Function in Normal Elliptical Galaxies

Author: V. Kalogera, Giuseppina Fabbiano, Ginevra Trinchieri, Lorella Angelini, Andrew J. King, John S. Gallagher, S. E. Zepf, Roger L. Davies, Andreas Zezas, Dong-Woo Kim, and Silvia Pellegrini
Subjects: Physics, Space and Planetary Science, Star formation, Globular cluster, Elliptical galaxy, Binary number, Astronomy and Astrophysics, Astrophysics, Power law, Erg, Galaxy, Luminosity
Abstract: We present the first low-luminosity [LX > (5-10) × 1036 ergs s-1] X-ray luminosity functions (XLFs) of low-mass X-ray binaries (LMXBs) determined for two typical old elliptical galaxies, NGC 3379 and NGC 4278. Because both galaxies contain little diffuse emission from hot ISM and no recent significant star formation (hence no high-mass X-ray binary contamination), they provide two of the best homogeneous sample of LMXBs. With 110 and 140 ks Chandra ACIS S3 exposures, we detect 59 and 112 LMXBs within the D25 ellipses of NGC 3379 and NGC 4278, respectively. The resulting XLFs are well represented by a single power law with a slope (in a differential form) of 1.9 ± 0.1. In NGC 4278, we can exclude the break at LX ∼ 5 × 1037 ergs s -1 that was recently suggested as being a general feature of LMXB XLFs. In NGC 3379, on the other hand, we find a localized excess over the power-law XLF at ∼4 × 1037 ergs s-1, but with a marginal significance of ∼1.6 σ. Because of the small number of luminous sources, we cannot constrain the high-luminosity break (at 5 × 1038 ergs s-1) found in a large sample of early-type galaxies. For our two galaxies, the ratios of the integrated LMXB X-ray luminosities to the optical luminosities differ by a factor of 4, but are consistent with the general trend of a positive correlation between the X-ray-to-optical luminosity ratio and the globular cluster specific frequency. © 2006. The American Astronomical Society. All rights reserved.
Published: 2006

35. Long-term monitoring of the X-ray afterglow of GRB 050408 with Swift/XRT

Author: G. Chincarini, Neil Gehrels, Gianpiero Tagliaferri, Lorella Angelini, V. La Parola, Stefano Covino, P. Boyd, Paolo Giommi, David N. Burrows, D. B. Malesani, Sergio Campana, J. A. Kennea, Milvia Capalbi, Frank Marshall, J. E. Hill, P. Romano, M. Perri, Teresa Mineo, Olivier Godet, V. Mangano, Alberto Moretti, Giancarlo Cusumano, and P. T. O'Brien
Subjects: Physics, Jet (fluid), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, Power law, Rotational energy, Afterglow, Space and Planetary Science, Outflow, Gamma-ray burst, Absorption (electromagnetic radiation)
Abstract: We present observations of the X-ray afterglow of GRB 050408, a gamma-ray burst discovered by HETE-II. Swift began observing the field 42 min after the burst, performing follow-up over a period of 38 d (thus spanning three decades in time).The X-ray light curve showed a steepening with time, similar to many other afterglows. However, the steepening was unusually smooth, over the duration of the XRT observation, with no clear break time. The early decay was too flat to be described in terms of standard models. We therefore explore alternative explanations, such as the presence of a structured afterglow or of long-lasting energy injection into the fireball from the central GRB engine. The lack of a sharp break puts constraints on these two models. In the former case, it may indicate that the angular energy profile of the jet was not a simple power law, while in the second model it implies that injection did not stop abruptly. The late decay may be due either to a standard afterglow (that is, with no energy injection), or to a jetted outflow still being refreshed. A significant amount of absorption was present in the X-ray spectrum, corresponding to a rest-frame Hydrogen column density NH = 1.2 (-0.3,+0.4)*10^22 cm^-2, indicative of a dense environment., Comment: Accepted for publication in A&A; 7 pages, 3 figures
Published: 2006

36. The Modulated Emission of the Ultraluminous X‐Ray Source in NGC 3379

Author: G. Fabbiano, Vicky Kalogera, Andrew J. King, Tassos Fragos, Stephen E. Zepf, Lorella Angelini, Andreas Zezas, Dong-Woo Kim, Roger L. Davies, Silvia Pellegrini, Ginevra Trinchieri, and John S. Gallagher
Subjects: Physics, Stellar population, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), Binary number, Astronomy, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Orbital period, Galaxy, Space and Planetary Science, Modulation (music), Elliptical galaxy, Astrophysics::Galaxy Astrophysics
Abstract: We report recent Chandra observations of the ULX in the elliptical galaxy NGC 3379 that clearly detect two flux variability cycles. Comparing these data with the Chandra observation of ∼5 years ago, we measure a flux modulation with a period of ∼12.6 hr. Moreover, we find that the emission undergoes a correlated spectral modulation, becoming softer at low flux. We argue that our results establish this source as a ULX binary in NGC 3379. Given the old stellar population of this galaxy, the ULX is likely to be a soft transient; however, historical X-ray sampling suggests that the current "on" phase has lasted ∼10yr. We discuss our results in terms of ADC and wind-feedback models. If the flux modulation is orbital, we can constrain the donor mass and orbital period at the onset of mass transfer within 1.15-1.4 Ṁ and 12.5-17 hr, respectively. The duration of the mass transfer phase so far is probably ∼ 1 Gyr, and the binary has been a soft X-ray transient throughout this time. These constraints are insensitive to the mass of the accretor. © 2006. The American Astronomical Society. All rights reserved.
Published: 2006

37. Cyclotron Resonance Energies at a Low X-Ray Luminosity: A0535+262 Observed with Suzaku

Author: Fumiaki Nagase, Atsumasa Yoshida, Lorella Angelini, Koji Mukai, Satoshi Sugita, Sachindra Naik, Hirotaka Takahashi, Tadayasu Dotani, Teruaki Enoto, Shunji Kitamoto, Takaaki Tanaka, Takao Kitaguchi, Motohide Kokubun, Yukikatsu Terada, Richard L. Kelley, Motoki Nakajima, Jean Cottam, Tatehiro Mihara, Yang Soong, Keisuke Sudoh, Naoki Isobe, Mark W. Bautz, Taro Kotani, Sei-ichiro Watanabe, Steve Kissel, John P. Doty, Takayoshi Kohmura, Y. E. Nakagawa, Daisuke Yonetoku, Kazuo Makishima, and M. Suzuki
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Cyclotron resonance, X-ray, FOS: Physical sciences, Resonance, Astronomy and Astrophysics, Astrophysics, Electron cyclotron resonance, Luminosity, Pulsar, Space and Planetary Science, Observatory, Absorption (electromagnetic radiation)
Abstract: 著者人数: 31名, Accepted: 2006-07-28, 資料番号: SA1000375000
Published: 2006

38. Suzaku observation of the black hole transient 4U1630–472: discovery of absorption lines

Author: Hiromitsu Takahashi, Andrew C. Fabian, Taro Kotani, Jean Cottam, Lorella Angelini, Tomonori Yasuda, Yasushi Fukazawa, Kazutaka Yamaoka, Kazuo Makishima, Aya Kubota, Shinya Yamada, Chris Done, Yoshihiro Ueda, Tadayasu Dotani, and Takayoshi Kohmura
Subjects: Physics, Absorption spectroscopy, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Astrophysics, Transient (oscillation)
Abstract: We present the results of six Suzaku observations of the recurrent black hole transient 4U 1630–472 during its decline from its most recent outburst 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.The disk temperature decreases from 1.4 keV to 1.2 keV as the flux decreases by a factor 2, consistent with a constant radius as expected for disk-dominated spectra. All the observations reveal significant absorption lines from highly ionized (H-like and He-like) iron Kα at 7.0 keV and 6.7 keV.The energies of these absorption lines suggest a blue shift with an outflow velocity of ∼1000 km s−1. The H–like iron Kα equivalent width remains approximately constant at ∼30 eV over all the observations, while that of the He–like Kα line increases from 7 eV to 20 eV. Thus the ionization state of the material decreases, as expected from the decline in flux.The data constrain the velocity dispersion of the absorber to 200–2000 km s−1, and the size of the plasma as ∼1010 cm assuming a source distance of 10 kpc.
Published: 2006

39. X-ray flares in the early Swift observations of the possible naked gamma-ray burst 050421

Author: J. A. Kennea, Jay Cummings, P. T. O'Brien, D. C. Morris, Neil Gehrels, J. P. Osborne, A. Moretti, Bing Zhang, David N. Burrows, Michael R. Goad, Lorella Angelini, M. Capalbi, Andrew P. Beardmore, K. L. Page, Olivier Godet, V. Mangano, and Joanne E. Hill
Subjects: Physics, Gamma ray, Flux, Astronomy, Astronomy and Astrophysics, Astrophysics, Radiation, Light curve, Spectral line, law.invention, Space and Planetary Science, law, Emission spectrum, Gamma-ray burst, Flare
Abstract: We present the Swift observations of the faint burst GRB 050421. The X-ray light-curve shows at least two flares: the first flare peaking at ∼110 s after the BAT trigger (To) and the second one peaking at ∼154 s. The first flare presents a flux variation of δF/F peak ∼ 3.7 and a short timescale ratio δt/t peak ∼ 0.07. The second flare is smaller and presents a flux variation of δF/F peak ∼ 1.7 and a short timescale ratio δt/t peak ∼ 0.03. We argue that the mechanism producing these flares is probably late internal shocks. The X-ray light-curve is consistent with a rapid decline with a temporal index α ∼ 3.1, which decays from ∼10 -9 erg cm -2 s -1 at To + 100s to
Published: 2006

40. Swift and XMM-Newton observations of the dark GRB 050326

Author: A. De Luca, N. E. White, Lorella Angelini, A. P. Beardmore, Bing Zhang, Shiho Kobayashi, L. M. Barbier, G. Tagliaferri, James Reeves, A. Cucchiara, G. Chincarini, E. E. Fenimore, Alberto Moretti, Teresa Mineo, M. R. Goad, J. P. Osborne, V. La Parola, D. Malesani, N. Gehrels, Joanne E. Hill, V. Mangano, M. Capalbi, Sergio Campana, Peter Mészáros, S. D. Barthelmy, Andrea Tiengo, C. Pagani, David N. Burrows, P. Banat, L. R. Cominsky, M. Perri, P. Romano, and G. Cusumano
Subjects: Physics, Brightness, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Power law, Redshift, Galaxy, Afterglow, Space and Planetary Science, Gamma-ray burst
Abstract: We present Swift and XMM observations of GRB 050326, detected by Swift-BAT. The fluence was 7.7x10^-6 erg cm^-2 (20-150 keV), and its spectrum was hard, with a power law photon index 1.25. The afterglow light curve did not show any break nor flares between ~1 hr and ~6 d after the burst, and decayed with a slope 1.70. The afterglow spectrum is well fitted by a power-law model, suffering absorption both in the Milky Way and in the host galaxy. The rest-frame Hydrogen column density is significant, N_H_z > 4x10^21 cm^-2, and the redshift of the absorber is z > 1.5. There was good agreement between the Swift-XRT and XMM results. By comparing the prompt and afterglow fluxes, we found that an early break occurred before the XRT observation. The properties of the GRB 050326 afterglow are well described by a spherical fireball expanding in a uniform external medium, so a further steepening is expected at later times. The lack of such a break constrains the jet angle to be >7 deg. Using the redshift constraints provided by the X-ray analysis, we also estimated that the beaming-corrected gamma-ray energy was >3x10^51 erg, at the high end of GRB energies. Despite the brightness in X rays, only deep limits could be placed by Swift-UVOT at optical/UV wavelengths. Thus, this GRB was "truly dark", with the optical-to-X-ray spectrum violating the synchrotron limit. The optical and X-ray observations are consistent either with an absorbed event or with a high-redshift one. To obey the Ghirlanda relation, a moderate/large redshift z>4.5 is required. (abridged)
Published: 2006

41. X-ray flare in XRF 050406: evidence for prolonged engine activity

Author: C. Pagani, J. A. Kennea, Bing Zhang, P. Romano, Gianpiero Tagliaferri, A. M. Parsons, V. Mangano, David N. Burrows, Sergio Campana, Alberto Moretti, Shiho Kobayashi, Neil Gehrels, P. Banat, Guido Chincarini, Olivier Godet, Giancarlo Cusumano, V. La Parola, Milvia Capalbi, J. P. Osborne, J. E. Hill, P. T. O'Brien, Scott Barthelmy, A. P. Beardmore, Peter Mészáros, M. Perri, Dirk Grupe, M. R. Goad, Paolo Giommi, D. C. Morris, A. Falcone, Stefano Covino, Alan A. Wells, Lorella Angelini, K. L. Page, J. A. Nousek, and D. Malesani
Subjects: Physics, Photon, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Light curve, Fluence, Afterglow, law.invention, Space and Planetary Science, law, Erg, Flare
Abstract: We present observations of XRF 050406, the first burst detected by Swift showing a flare in its X-ray light curve. During this flare, which peaks at t_peak ~210s after the BAT trigger, a flux variation of (delta F)/F~6 in a very short time (delta t)/t_peak<, 11 pages, 3 figures, accepted for publication in A&A; added references, corrected typos
Published: 2006

42. Evidence for intrinsic absorption in the Swift X-ray afterglows

Author: Sergio Campana, A. De Luca, Lorella Angelini, Judith Racusin, J. A. Kennea, L. A. Antonelli, Giancarlo Cusumano, C. Pagani, M. Perri, Gianpiero Tagliaferri, Olivier Godet, Milvia Capalbi, Stefano Covino, Teresa Mineo, V. Mangano, J. E. Hill, Paolo Giommi, V. La Parola, Alberto Moretti, Alan A. Wells, David N. Burrows, A. P. Beardmore, P. T. O'Brien, D. C. Morris, J. P. Osborne, Davide Lazzati, P. Romano, Neil Gehrels, G. Chincarini, M. R. Goad, J. A. Nousek, and K. L. Page
Subjects: Swift, Physics, Astrophysics::High Energy Astrophysical Phenomena, Molecular cloud, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Afterglow, Stars, Space and Planetary Science, Ionization, Absorption (electromagnetic radiation), Gamma-ray burst, computer, Astrophysics::Galaxy Astrophysics, computer.programming_language
Abstract: Gamma-ray burst (GRB) progenitors are observationally linked to the death of massive stars. X-ray studies of the GRB afterglows can deepen our knowledge of the ionization status and metal abundances of the matter in the GRB environment. Moreover, the presence of local matter can be inferred through its fingerprints in the X-ray spectrum, i.e. the presence of absorption higher than the Galactic value. A few studies based on BeppoSAX and XMM-Newton found evidence of higher than Galactic values for the column density in a number of GRB afterglows. Here we report on a systematic analysis of 17 GRBs observed by Swift up to April 15, 2005. We observed a large number of GRBs with an excess of column density. Our sample, together with previous determinations of the intrinsic column densities for GRBs with known redshift, provides evidence for a distribution of absorption consistent with that predicted for randomly occurring GRB within molecular clouds., Comment: Accepted for publication on A&A (5 pages and 2 figures)
Published: 2006

43. Swift X-Ray Telescope and Very Large Telescope Observations of the Afterglow of GRB 041223

Author: A. P. Beardmore, Bing Zhang, J. A. Kennea, J. P. Osborne, Shiho Kobayashi, Alberto Moretti, A. F. Abbey, Judith Racusin, M. R. Goad, D. Malesani, Richard Willingale, Joanne E. Hill, P. D'Avanzo, Sergio Campana, P. Giommi, Stefano Covino, J. A. Nousek, Alan A. Wells, L. A. Antonelli, Giancarlo Cusumano, C. Pagani, M. Capalbi, P. T. O'Brien, G. Chincarini, G. Tagliaferri, David N. Burrows, Lorella Angelini, Peter Mészáros, P. Romano, K. L. Page, N. Gehrels, Luigi Stella, D. C. Morris, Burrows, D, Hill, J, Chincarini, G, Tagliaferri, G, Campana, S, Moretti, A, Romano, P, Malesani, D, Racusin, J, Kobayashi, S, Zhang, B, Mészáros, P, O'Brien, P, Willingale, R, Osborne, J, Cusumano, G, Giommi, P, Angelini, L, Abbey, A, Antonelli, L, Beardmore, A, Capalbi, M, Covino, S, D'Avanzo, P, Goad, M, Kennea, J, Morris, D, Pagani, C, Page, K, Stella, L, Nousek, J, Wells, A, and Gehrels, N
Subjects: Physics, Very Large Telescope, Astronomy, Astronomy and Astrophysics, X-ray telescope, GRB, Astrophysics, Afterglow, law.invention, Telescope, Crab Nebula, Space and Planetary Science, law, Spectral energy distribution, Absorption (electromagnetic radiation), Gamma-ray burst
Abstract: GRB 041223 was the first gamma-ray burst detected by the Swift X-Ray Telescope (XRT), beginning 4.6 hr after the burst. The X-ray detection triggered a VLT observation of the optical/near-infrared (NIR) counterpart, located about 1″.1 from the XRT position. The X-ray counterpart faded rapidly, with a power-law index of - 1.72 ± 0.20, with an average unabsorbed X-ray flux of 6.5 × 10-12 ergs cm-2 s-1 in the 0.5-10 keV band for a power-law spectrum of photon index 2.02 ± 0.13 with Galactic absorption. The NIR counterpart was observed at three epochs between 16 and 87 hr after the burst and faded with a power-law index of -1.14 ± 0.08 with a reddening-corrected spectral energy distribution power-law slope of -0.40 ± 0.03. We find that the X-ray and NIR data are consistent with a two-component jet in a wind medium. © 2005. The American Astronomical Society. All rights reserved.
Published: 2005

44. The Infrared Counterpart to the Anomalous X-Ray Pulsar 1RXS J170849-400910

Author: Luigi Stella, R. Perna, Sergio Campana, G. L. Israel, T. Oosterbroek, Roberto Mignani, Stefano Covino, Sandro Mereghetti, Ignacio Negueruela, Lorella Angelini, C. Motch, G. Marconi, and Giuseppe Bono
Subjects: Physics, Telescope, Pulsar, Space and Planetary Science, law, Flux, Astronomy and Astrophysics, Black-body radiation, Astrophysics, X-ray pulsar, law.invention
Abstract: We report the discovery of the likely IR counterpart to the anomalous X-ray pulsar (AXP) 1RXS J170849-400910 based on the Chandra High Resolution Camera (imaging detector) X-ray position and the deep optical/IR observations carried out from ESO telescopes and the Canada-France-Hawaii Telescope during 1999-2002. Within the narrow uncertainty region, we found two relatively faint (K'=20.0 and K'=17.53) IR objects. Based on their color and position in the J-K' versus J-H diagram, only the brighter object is consistent with the known IR properties of the counterparts to other AXPs. No variability was detected for this source, which is similar to what is observed in the case of 4U 0142+614. Like in other AXPs, we found that the IR flux of 1RXS J170849-400910 is higher than expected for a simple blackbody component extrapolated from the X-ray data. If confirmed, this object would be the fourth IR counterpart to a source of the AXP class and would make the IR excess a likely new characteristic of AXPs.
Published: 2003

45. Evidence of a Cyclotron Feature in the Spectrum of the Anomalous X-Ray Pulsar 1RXS J170849−400910

Author: Sandro Mereghetti, G. L. Israel, Stefano Covino, T. Oosterbroek, Sergio Campana, Lorella Angelini, Luigi Stella, and Nanda Rea
Subjects: Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Cyclotron, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Electron, Astrophysics, Anomalous X-ray pulsar, law.invention, Magnetic field, Pulsar, Space and Planetary Science, law, Black-body radiation
Abstract: We report the results of a long observation of the anomalous X-ray pulsar 1RXS J170849-400910 obtained with the BeppoSAX satellite in August 2001. The best-fit phase-averaged spectrum was an absorbed power law plus blackbody model, with photon index Gamma~2.4 and a blackbody temperature of kT_bb~0.4 keV. We confirm the presence of significant spectral variations with the rotational phase of the pulsar. In the spectrum corresponding to the rising part of the pulse we found an absorption-like feature at ~8.1 keV (a significance of 4 sigma), most likely due to cyclotron resonant scattering. The centroid energy converts to a magnetic field of 9x10^11 G and 1.6x10^15 G in the case of electrons and protons, respectively. If confirmed, this would be the first detection of a cyclotron feature in the spectrum of an anomalous X-ray pulsar., Comment: 5 pages, 5 figures. Accepted for publication on ApJ Letters
Published: 2003

46. An [ITAL]XMM-Newton[/ITAL] Observation of 4U 1755−33 in Quiescence: Evidence of a Fossil X-Ray Jet

Author: Lorella Angelini and Nicholas E. White
Subjects: Physics, Jet (fluid), Active galactic nucleus, Field (physics), Astrophysics::High Energy Astrophysical Phenomena, X-ray, Quiescent state, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Luminosity, Black hole, Space and Planetary Science, Low Mass, Astrophysics::Galaxy Astrophysics
Abstract: We report an XMM-Newton observation of the Low mass X-ray Binary (LMXB) and black hole candidate 4U1755-33. This source had been a bright persistent source for at least 25 yrs, but in 1995 entered an extended quiescent phase. 4U1755-33 was not detected with an upper limit to the 2-10 keV luminosity of 5.10^31 erg/s (assuming a distance of 4 kpc) - consistent with the luminosity of other black hole candidates in a quiescent state. An unexpected result is the discovery of a narrow 7' long X-ray jet-like feature centered on the position of 4U1755-33. The spectrum of the jet is similar to that observed from other galactic and extragalactic jets thought to be associated with accreting black holes. The detection of a fossil jet provides additional evidence supporting the black hole candidacy of 4U1755-33. The spectral properties of three bright serendipitous sources in the field are reported and it is suggested these are background active galactic nuclei (AGN).
Published: 2003

47. ChandraandXMMObservations of the Accretion Disk Corona Source 2S 0921−63

Author: Jean Cottam, T. R. Kallman, Bram Boroson, and Lorella Angelini
Subjects: Physics, Accretion disc, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Binary number, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photoionization, Astrophysics, K-line, Accretion (astrophysics), Spectral line
Abstract: We analyze observations of the low-mass X-ray binary (LMXB) 2S 0921-63 obtained with the gratings and CCDs on Chandra and XMM. This object is a high-inclination system showing evidence for an accretion disk corona (ADC). Such a corona has the potential to constrain the properties of the heated accretion disk in this system and other LMXBs by extension. We find evidence for line emission that is generally consistent with that found by previous experiments, although we are able to detect more lines. For the first time in this source, we find that the iron K line has multiple components. We set limits on the line widths and velocity offsets, and we fit the spectra to photoionization models and discuss the implications for ADC models. For the first time in any ADC source we use these fits, together with density constraints based on the O VII line ratio, in order to constrain the flux in the medium-ionization region of the ADC. Under various assumptions about the source luminosity this constrains the location of the emitting region. These estimates, together with estimates for the emission measure, favor a scenario in which the intrinsic luminosity of the source is comparable to what we observe.
Published: 2003

48. Design of the time assignment system for ASTRO-H and its performance before launch

Author: Satoko Kawakami, Lorella Angelini, Masanobu Ozaki, Takashi Kominato, Makoto Tashiro, Taku Inoue, Susumu Kumagai, Kazuyo Mizushima, Tomomi Kouzu, Yukikatsu Terada, Yoshitaka Ishisaki, Sunao Yamaguchi, Hiroki Hihara, Masaru Kasahara, Mina Ogawa, Tadayuki Takahashi, Motohide Kokubun, Shigenobu Sugimoto, Tadayasu Dotani, Hiroaki Mine, Souhei Nakaya, Kaori Iwase, Chikara Natsukari, and M. C. Witthoeft
Subjects: Scientific instrument, Physics, Payload, business.industry, Real-time computing, Astrophysics::Instrumentation and Methods for Astrophysics, Propagation delay, SpaceWire, Software, Assisted GPS, Calibration, Satellite, business, Simulation
Abstract: The ASTRO-H, which will be launched in 2015, is the sixth in a series of Japanese X-ray satellites. It is an international mission led by JAXA in collaboration with NASA and ESA, aiming to observe astrophysical objects in the X-ray band from 0.5 to 600 keV. One of the important scientific goals is to understand physical processes in the extreme environments of active and variable astrophysical objects, such as black holes, neutron stars, binary star, and active galactic nuclei. Therefore, a fast timing capability is a key requirement for the mission. According to numerical estimates of scientific performance, absolute times of X-ray events are required to have an accuracy of 300 µs to achieve minimum scientific goals and an accuracy of 30 µs is desired as a goal. The satellite carries a GPS receiver to get the accurate time information, which is distributed from the central computer on board through the large-and-complex SpaceWire network. Distributions of time information are shared in the same lines used for communications of telemetry and commands, and thus propagation delays and jitters affect the timing accuracy of the payload instruments. Further six items are identified as sources of timing errors and are measured on ground to be used in the calibration by off-line software. The time-assignment tasks in the off-line software packages are designed to be common for all the scientific instruments, although the hardware designs for finer timing resolutions are different by the instruments. Measurements of propagation delays in the flight configuration on ground and in-orbit calibration plans are described. The detail description will be submitted to the IEEE TNS paper in near future. This work demonstrates a good example of care points for space-use instruments in the hardware-and-software designs and calibration measurements in order to achieve a fine timing resolution at the micro second order with the middle-sized satellites using the SpaceWire (IEEE1355) network.
Published: 2014

49. The ASTRO-H X-ray astronomy satellite

Author: Hironori Matsumoto, Yasuharu Sugawara, Hiroshi Tsunemi, Steve Allen, Ikuyuki Mitsuishi, James Pontius, Luigi C. Gallo, Dmitry Khangulyan, Hiroyuki Uchida, Yuichi Terashima, Yoichi Yatsu, Kazutaka Yamaoka, Kiyoshi Hayashida, Makoto Sawada, Peter Shirron, Hirofumi Noda, Andrew C. Fabian, Nicholas E. White, Brian R. McNamara, Dan R. Wilkins, Franco Moroso, Maxim Markevitch, Tadayuki Takahashi, Shin Mineshige, Peter J. Serlemitsos, Stephanie M. LaMassa, Tahir Yaqoob, Richard Mushotzky, Satoshi Sugita, Akihiro Furuzawa, Philipp Azzarello, Atsushi Wada, Yoh Takei, Yoshito Haba, Jun Kataoka, Daisuke Yonetoku, Yoshitaka Ishisaki, Helen Russell, Satoru Katsuda, Hiroaki Takahashi, Knox S. Long, Shinya Nakashima, Meg Urry, Housei Nagano, Chris Baluta, Atsushi Okamoto, Maria Chernyakova, Shin Watanabe, Randall K. Smith, Hans A. Krimm, Samar Safi-Harb, Yuichiro Ezoe, Tsuyoshi Okazaki, Takeshi Go Tsuru, Hiroshi Nakajima, Shin-ichiro Sakai, Katja Pottschmidt, Timothy R. Kallman, Stefan Funk, Kosuke Sato, Naomi Ota, Chikara Natsukari, Kazuo Makishima, Ken Ebisawa, Yasuyuki T. Tanaka, Massimiliano Galeazzi, Tatsuro Kosaka, Mina Ogawa, Jan-Willem den Herder, Atsumasa Yoshida, Joseph Miko, Chris Done, Shin'ichiro Uno, Kosei Ishimura, Hideyuki Mori, Takeshi Nakamori, H. Sameshima, Edward M. Cackett, Francesco Tombesi, Jelle Kaastra, Naoko Iyomoto, Kumi Ishikawa, Takashi Okajima, Yoshihiro Ueda, Hiroyasu Tajima, Mark O. Kimball, Arvind Parmar, Yasuko Shibano, Ryo Iizuka, Masayuki Ohta, Gary A. Sneiderman, Thomas G. Bialas, Toshio Murakami, Masanori Ohno, Christopher S. Reynolds, Masashi Kimura, Yoshiyuki Inoue, Masayuki Ito, Masayoshi Nobukawa, Marshall W. Bautz, Atsushi Harayama, Olivier Limousin, Naohisa Anabuki, Taro Kawano, Maki Shida, Martin Pohl, Saori Konami, Katsuhiro Hayashi, Aya Kubota, Chris Jewell, Yoshitomo Maeda, Steve O' Dell, Yukikatsu Terada, Keiji Ogi, Masanobu Ozaki, Kenji Minesugi, Takahiro Yamada, Edgar Canavan, Hiroki Akamatsu, Katsuji Koyama, Tomomi Watanabe, Marc Audard, Andrew Szymkowiak, Eric J. Miller, Ciro Pinto, Irina Zhuravleva, Shigeo Kawasaki, Jon M. Miller, Grzegorz Madejski, Makoto Tashiro, Ann Hornschemeier, Robert Petre, Koji Mori, Yasunobu Uchiyama, David H. Lumb, Brian D. Ramsey, Alex Koujelev, Shin'ichiro Takeda, Keisuke Shinozaki, Una Hwang, D. Haas, Shiro Ueno, Koji Mukai, Theodore Muench, Shinya Yamada, Masaharu Nomachi, Hiroshi Murakami, Kirk Gilmore, Keith A. Arnaud, Yoichi Sato, Kyoko Matsushita, Yoshiharu Namba, Takuya Miyazawa, Claudio Ricci, Teruaki Enoto, Masahiro Tsujimoto, Ryuichi Fujimoto, Dan McCammon, Daniel S. McGuinness, Abderahmen Zoghbi, Carlo Ferrigno, Motohide Kokubun, Stéphane Paltani, Elisa Costantini, Hiroshi Tomida, Maurice A. Leutenegger, Laura Brenneman, Tsunefumi Mizuno, Keisuke Tamura, Aurora Simionescu, Toru Tamagawa, Paolo De Coppi, Hiroyuki Sugita, Rie Sato, F. Scott Porter, Yusuke Nishioka, Franccois Lebrun, Takanobu Shimada, Yuzuru Tawara, Takayoshi Kohmura, Makoto Yamauchi, Shinya Saito, Jelle de Plaa, Michael J. DiPirro, Poshak Gandhi, Yasushi Fukazawa, Richard L. Kelley, Hirokazu Odaka, Nobuyuki Kawai, Junko S. Hiraga, Frits Paerels, Hiromi Seta, Takao Nakagawa, Rubens Reis, Tetsu Kitayama, Manabu Ishida, Cor P. de Vries, Hiromitsu Takahashi, Kazuhisa Mitsuda, Akio Hoshino, Kazuhiro Nakazawa, Felix Aharonian, Matteo Guainazzi, Meng P. Chiao, Eugenio Ursino, Adam R. Foster, John ZuHone, Hiroyuki Ogawa, John P. Doty, Takayuki Hayashi, Yasuo Tanaka, Junichiro Katsuta, Madoka Kawaharada, Hisamitsu Awaki, Kevin R. Boyce, John P. Hughes, Hiroya Yamaguchi, Ryo Nagino, Lorella Angelini, Philippe Laurent, Michael Loewenstein, Tuneyoshi Kamae, Yang Soong, Takaaki Tanaka, Tadayasu Dotani, Candace Masters, Aya Bamba, Kenji Hamaguchi, Roger Blandford, Kazunori Ishibashi, Takayuki Yuasa, Hideki Uchiyama, Takayuki Tamura, Kazuyuki Hirose, Naoko Iwata, Shunji Kitamoto, Goro Sato, Greg Brown, Shutaro Ueda, Megan E. Eckart, Cynthia Simmons, Takaya Ohashi, Hideyo Kunieda, Lukasz Stawarz, Yohko Tsuboi, Norbert Werner, Fumie Akimoto, Shigeo Yamauchi, Noriko Y. Yamasaki, Nobutaka Bando, Isamu Hatsukade, Caroline A. Kilbourne, and Makoto Asai
Subjects: Physics, Astronautics, X-ray astronomy, Astrophysics::High Energy Astrophysical Phenomena, gamma radiation, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, x-rays, x-ray astronomy, Redshift, Gravitation, satellites, Settore FIS/05 - Astronomia e Astrofisica, spectral resolution, Satellite, equipment and services, Spectral resolution, Astrophysics - Instrumentation and Methods for Astrophysics, galaxy groups and clusters, Instrumentation and Methods for Astrophysics (astro-ph.IM), Galaxy cluster
Abstract: The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions developed by the Institute of Space and Astronautical Science (ISAS), with a planned launch in 2015. The ASTRO-H mission is equipped with a suite of sensitive instruments with the highest energy resolution ever achieved at E > 3 keV and a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. The simultaneous broad band pass, coupled with the high spectral resolution of Delta E < 7 eV of the micro-calorimeter, will enable a wide variety of important science themes to be pursued. ASTRO-H is expected to provide breakthrough results in scientific areas as diverse as the large-scale structure of the Universe and its evolution, the behavior of matter in the gravitational strong field regime, the physical conditions in sites of cosmic-ray acceleration, and the distribution of dark matter in galaxy clusters at different redshifts., 24 pages, 18 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray"
Published: 2014

50. The Discovery of a Second Luminous Low-Mass X-Ray Binary in the Globular Cluster M15

Author: Lorella Angelini and Nicholas E. White
Subjects: Physics, Astrophysics (astro-ph), X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Luminosity, Neutron star, Space and Planetary Science, Globular cluster, Magnitude (astronomy), Cluster (physics), Low Mass
Abstract: We report an observation by the Chandra X-ray Observatory of 4U2127+119, the X-ray source identified with the globular cluster M15. The Chandra observation reveals that 4U2127+119 is in fact two bright sources, separated by 2.7". One source is associated with AC211, the previously identified optical counterpart to 4U2127+119, a low mass X-ray binary (LMXB). The second source, M15-X2, is coincident with a 19th U magnitude blue star that is 3.3" from the cluster core. The Chandra count rate of M15-X2 is 2.5 times higher than that of AC211. Prior to the 0.5" imaging capability of Chandra the presence of two so closely separated bright sources would not have been resolved. The optical counterpart, X-ray luminosity and spectrum of M15-X2 are consistent with it also being an LMXB system. This is the first time that two LMXBs have been seen to be simultaneously active in a globular cluster. The discovery of a second active LMXB in M15 solves a long standing puzzle where the properties of AC211 appear consistent with it being dominated by an extended accretion disk corona, and yet 4U2127+119 also shows luminous X-ray bursts requiring that the neutron star be directly visible. The resolution of 4U2127+119 into two sources suggests that the X-ray bursts did not come from AC211, but rather from M15-X2. We discuss the implications of this discovery for understanding the origin and evolution of LMXBs in GCs as well as X-ray observations of globular clusters in nearby galaxies., Comment: 18 pages, 4 figures, Accepted for publication in Ap J Letters
Published: 2001

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