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149 results on '"Ken Ebisawa"'

1. Investigation of Nonequilibrium Ionization Plasma during a Giant Flare of UX Arietis Triggered with MAXI and Observed with NICER

Author

Miki Kurihara, Wataru Buz Iwakiri, Masahiro Tsujimoto, Ken Ebisawa, Shin Toriumi, Shinsuke Imada, Yohko Tsuboi, Kazuki Usui, Keith C. Gendreau, and Zaven Arzoumanian

Subjects
Plasma astrophysics, Space plasmas, Astrophysics, QB460-466
Abstract

We detected a giant X-ray flare from the RS CVn–type binary star UX Ari using the Monitor of All-sky X-ray Image on 2020 August 17 and started a series of Neutron star Interior Composition Explorer observations 89 minutes later. For a week, the entire duration of the flare was covered with 32 snapshot observations including the rising phase. The X-ray luminosity reached 2 × 10 ^33 erg s ^−1 , and the entire energy release was ∼10 ^38 erg in the 0.5–8.0 keV band. X-ray spectra characterized by continuum emission with lines of Fe xxv He α and Fe xxvi Ly α were obtained. We found that the temperature peaks before the flux does, which suggests that the period of plasma formation in the magnetic flare loop was captured. Using the continuum information (temperature, flux, and their delay time), we estimated the flare loop size to be ∼3 × 10 ^11 cm and the peak electron density to be ∼4 × 10 ^10 cm ^−3 . Furthermore, using the line ratio of Fe xxv and Fe xxvi , we investigated any potential indications of deviation from collisional ionization equilibrium (CIE). The X-ray spectra were consistent with CIE plasma throughout the flare, but the possibility of an ionizing plasma away from CIE was not rejected in the flux rising phase.

Published
2024
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2. X-Ray Spectral Variations of Circinus X-1 Observed with NICER throughout an Entire Orbital Cycle

Author

Mayu Tominaga, Masahiro Tsujimoto, Ken Ebisawa, Teruaki Enoto, and Kimitake Hayasaki

Subjects
X-ray binary stars, Atomic spectroscopy, Spectroscopy, Ionization, Plasma astrophysics, High energy astrophysics, Astrophysics, QB460-466
Abstract

Circinus X-1 (Cir X-1) is a neutron star binary with an elliptical orbit of 16.6 days. The source is unique for its extreme youth, providing a key to understanding early binary evolution. However, its X-ray variability is too complex to reach a clear interpretation. We conducted the first high-cadence (every 4 hr, on average) observations covering one entire orbit using the NICER X-ray telescope. The X-ray flux behavior can be divided into stable, dip, and flaring phases. The X-ray spectra in all phases can be described by a common model consisting of a partially covered disk blackbody emission and the line features from a highly ionized photoionized plasma. The spectral change over the orbit is attributable to rapid changes of the partial covering medium in the line of sight and gradual changes of the disk blackbody emission. Emission lines of H- and He-like Mg, Si, S, and Fe are detected, most prominently in the dip phase. The Fe emission lines change to absorption in the course of the transition from the dip phase to the flaring phase. The estimated ionization degree indicates no significant changes, suggesting that the photoionized plasma is stable over the orbit. We propose a simple model in which the disk blackbody emission is partially blocked by a local medium in the line of sight that has spatial structures depending on the azimuth of the accretion disk. Emission lines upon the continuum emission are from the photoionized plasma located outside of the blocking material.

Published
2023
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3. Spectral Modeling of the Supersoft X-Ray Source CAL87 Based on Radiative Transfer Codes

Author

Masahiro Tsujimoto, Misaki Mizumoto, Ken Ebisawa, Hirokazu Odaka, and Qazuya Wada

Subjects
X-ray binary stars, High energy astrophysics, Radiative transfer, Astrophysics, QB460-466
Abstract

Supersoft X-ray sources (SSSs) are white dwarf (WD) binaries that radiate almost entirely below ∼1 keV. Their X-ray spectra are often complex when viewed with the X-ray grating spectrometers, where numerous emission and absorption features are intermingled and hard to separate. The absorption features are mostly from the WD atmosphere, for which radiative transfer models have been constructed. The emission features are from the corona surrounding the WD atmosphere, in which incident emission from the WD surface is reprocessed. Modeling the corona requires different solvers and assumptions for the radiative transfer, which has yet to be achieved. We chose CAL87, an SSS in the Large Magellanic Cloud, which exhibits emission-dominated spectra from the corona, as the WD atmosphere emission is assumed to be completely blocked by the accretion disk. We constructed a radiative transfer model for the corona using two radiative transfer codes: xstar for a one-dimensional two-stream solver and MONACO for a three-dimensional Monte Carlo solver. We identified their differences and limitations in comparison to the spectra taken with the Reflection Grating Spectrometer on board the XMM-Newton satellite. We finally obtained a sufficiently good spectral model of CAL87 based on the radiative transfer of the corona plus an additional collisionally ionized plasma. In the coming X-ray microcalorimeter era, it will be required to interpret spectra based on radiative transfer in a wider range of sources than what is presented here.

Published
2023
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4. Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809

Author

Takuya Midooka, Misaki Mizumoto, and Ken Ebisawa

Subjects
Active galactic nuclei, Seyfert galaxies, X-ray astronomy, Astrophysics, QB460-466
Abstract

Recent radiation-magnetohydrodynamic simulations of active galactic nuclei predict the presence of the disk winds, which may become unstable and turn into fragmented clumps far from the central black hole. These inner winds and the outer clumps may be observed as ultrafast outflows (UFOs) and partial absorbers, respectively. However, it is challenging to observationally constrain their origins because of the complicated spectral features and variations. To resolve such degeneracies of the clumpy absorbers and other components, we developed a novel spectral-ratio model fitting technique that estimates the variable absorbing parameters from the ratios of the partially absorbed spectra to the non-absorbed one, canceling the complex non-variable spectral features. We applied this method to the narrow-line Seyfert 1 galaxy IRAS 13224-3809 observed by XMM-Newton in 2016 for ∼1.5 Ms. As a result, we found that the soft spectral variation is mostly caused by changes in the partial covering fraction of the mildly ionized clumpy absorbers, whose outflow velocities are similar to those of the UFO (∼0.2–0.3 c ). Furthermore, the velocities of the clumpy absorbers and UFOs increase similarly with the X-ray fluxes, consistent with the change in the UV-dominant continuum flux. We also discovered a striking correlation between the clump covering fraction and the equivalent width of the UFO absorption lines, which indicates that increasing the outflow in the line of sight leads to more prominent UFOs and more partial absorption. These findings strongly suggest that the clumpy absorbers and the UFO share the same origin, driven by the same UV-dominant continuum radiation.

Published
2023
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5. X-ray Time Lag Evaluation of MAXI J1820+070 with a Differential Cross-correlation Analysis

Author

Tomoki Omama, Masahiro Tsujimoto, Ken Ebisawa, and Misaki Mizumoto

Subjects
Astrostatistics tools, Low-mass x-ray binary stars, X-ray astronomy, Black holes, Stellar accretion disks, Astrostatistics, Astrophysics, QB460-466
Abstract

MAXI J1820+070 is a transient black hole binary discovered on 2018 March 11. The unprecedented rich statistics brought by the NICER X-ray telescope allow detailed timing analyses up to ∼1 kHz uncompromised by photon shot noise. To estimate the time lags, a Fourier analysis was applied, which led to two different conclusions for the system configuration: one supporting a lamp-post configuration with a stable accretion disk extending close to the innermost stable circular orbit and the other supporting a truncated accretion disk contracting with time. Using the same data set, we present the results based on the cross-correlation function (CCF). The CCF is calculated between two different X-ray bands where one side is subtracted from the other side, which we call the differential CCF (dCCF). Soft and hard lags of ∼0.03 and 3 s, respectively, are clearly identified without being diluted by the spectral mixture, demonstrating the effectiveness of the dCCF analysis. The evolution of these lags is tracked, along with spectral changes for the first 120 days since discovery. Both the dCCF and spectral fitting results are interpreted as the soft lag being a reverberation lag between the Comptonized emission and the soft excess emission, and that the hard lag is between the disk blackbody emission and the Comptonized emission. The evolutions of these lags are in line with the picture of a truncated disk contracting with time.

Published
2023
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6. X-Ray and Near-Infrared Spectroscopy of Dim X-Ray Point Sources Constituting the Galactic Ridge X-Ray Emission

Author

Kumiko Morihana, Masahiro Tsujimoto, and Ken Ebisawa

Subjects
Engineering (General). Civil engineering (General), TA1-2040
Abstract

We present the results of X-ray and Near-Infrared observations of the Galactic Ridge X-ray Emission (GRXE). We extracted 2,002 X-ray point sources in the Chandra Bulge Field (l =0°.113, b = 1°.424) down to ~10-14.8 ergscm-2s-1 in 2-8 keV band with the longest observation (900 ks) of the GRXE. Based on X-ray brightness and hardness, we classied the X-ray point sources into three groups: A (hard), B (soft and broad spectrum), and C (soft and peaked spectrum). In order to know populations of the X-ray point sources, we carried out NIR imaging and spectroscopy observation. We identied 11% of X-ray point sources with NIR and extracted NIR spectra for some of them. Based on X-ray and NIR properties, we concluded that non-thermal sources in the group A are mostly active galactic nuclei and the thermal sources are mostly white dwarf binaries such as cataclysmic variables (CVs) and Pre-CVs. We concluded that the group B and C sources are X-ray active stars in flare and quiescence, respectively.

Published
2014
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7. Origin of X-ray Spectral Variation and the Seemingly Broad Iron-Line Spectral Feature in Seyfert Galaxies

Author

Ken Ebisawa, Naoki Iso, Takehiro Miyakawa, and Hajime Inoue

Subjects
Engineering (General). Civil engineering (General), TA1-2040
Abstract

We present systematic X-ray data analysis of the Seyfert galaxies observed by Suzaku to study origin of their hard X-ray (2 - 40 keV) variations. In particular, we examine if the "Variable Partial Covering (VPC) model" proposed by Miyakawa, Ebisawa and Inoue (2012), which was successful to explain spectral variations of MCG{6-30-15, is also valid for other Seyfert galaxies or not. In this model, intrinsic X-ray luminosity of the AGN is not signicantly variable, and most observed flux and spectral variations are caused by change of the geometrical covering fraction of the extended X-ray source by ionized absorbing clouds in the line of sight. We found that the observed flux and spectral variations of 20 targets in addition to MCG{6-30-15 are successfully explained by the VPC model. The transmitted spectral component through the absorbing clouds has a characteristics spectral feature of the ionized iron K-edge, which is considered to be the origin of the seemingly broad iron-line feature commonly observed in Seyfert galaxies. Variation of the partial covering fraction of the constant X-ray luminosity source causes such an anti-correlation between the direct (non-obscured) component and the transmitted (obscured) component, that cancels their variations each other. The cancellation works most effectively at the energy band where intensities of the two components are the closest to each other, namely, just below the iron K-edge. This explains the signicantly small fractional variations in the iron K-energy band, another well-known observational characteristic of Seyfert galaxies.

Published
2014
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10. 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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11. 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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12. 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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13. Simple interpretation of the seemingly complicated X-ray spectral variation of NGC 5548

Author

Takuya Midooka, Ken Ebisawa, Misaki Mizumoto, and Yasuharu Sugawara

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

NGC 5548 is a very well-studied Seyfert 1 galaxy in broad wavelengths. Previous multiwavelength observation campaigns have indicated that its multiple absorbers are highly variable and complex. A previous study applied a two-zone partial covering model with different covering fractions to explain the complex X-ray spectral variation and reported a correlation between one of the covering fractions and the photon index of the power-law continuum. However, it is not straightforward to physically understand such a correlation. In this paper, we propose a model to avoid this unphysical situation; the central X-ray emission region is partially covered by clumpy absorbers composed of double layers. These "double partial coverings" have precisely the same covering fraction. Based on our model, we have conducted an extensive spectral study using the data taken by XMM-Newton, Suzaku, and NuSTAR in the range of 0.3-78 keV for 16 years. Consequently, we have found that the X-ray spectral variations are mainly explained by independent changes of the following three components; (1) the soft excess spectral component below ~1 keV, (2) the cut-off power-law normalization, and (3) the partial covering fraction of the clumpy absorbers. In particular, spectral variations above ~1 keV are mostly explained only by the changes of the partial covering fraction and the power-law normalization. In contrast, the photon index and all the other spectral parameters are not significantly variable., 14 pages, 13 figures, Published in MNRAS

Published
2022

14. Deep near-infrared imaging observation of the faint X-ray point sources constituting the Galactic bulge X-ray emission

Author

Kumiko Morihana, Masahiro Tsujimoto, Ken Ebisawa, and Poshak Gandhi

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Presence of the apparently extended hard (2-10 keV) X-ray emission along the Galactic plane has been known since the early 1980s. With a deep X-ray exposure using the Chandra X-ray Observatory of a slightly off-plane region in the Galactic bulge, most of the extended emission was resolved into faint discrete X-ray sources in the Fe K band (Revnivtsev et al.,2009). The major constituents of these sources have long been considered to be X-ray active stars and magnetic cataclysmic variables (CVs). However, recent works including our NIR imaging and spectroscopic studies (Morihana et al.,2013, 2016) argue that other populations should be more dominant. To investigate this further, we conducted a much deeper NIR imaging observation at the center of the Chandra's exposure field. We have used the MOIRCS on the Subaru telescope, reaching the limiting magnitude of ~18 mag in the J, H, and Ks bands in this crowded region, and identified ~50 % of the X-ray sources with NIR candidate counterparts. We classified the X-ray sources into three groups (A, B, and C) based on their positions in the X-ray color-color diagram and characterized them based on the X-ray and NIR features. We argue that the major populations of the Group A and C sources are, respectively, CVs (binaries containing magnetic or non-magnetic white dwarfs with high accretion rates) and X-ray active stars. The major population of the Group B sources is presumably WD binaries with low mass accretion rates. The Fe K equivalent width in the composite X-ray spectrum of the Group B sources is the largest among the three and comparable to that of the Galactic bulge X-ray emission. This leads us to speculate that there are numerous WD binaries with low mass accretion rates, which are not recognized as CVs, but are the major contributor of the apparently extended X-ray emission., Comment: 14 pages, 10 figures, accepted for publication in PASJ

Published
2022

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

Author

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

Subjects
Data processing, business.industry, Computer science, Mechanical Engineering, FOS: Physical sciences, Astronomy and Astrophysics, Plan (drawing), Pipeline (software), Electronic, Optical and Magnetic Materials, Task (project management), Fiscal year, Space and Planetary Science, Control and Systems Engineering, Agency (sociology), Systems engineering, Data center, Astrophysics - Instrumentation and Methods for Astrophysics, Aerospace, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation
Abstract

XRISM is an X-ray astronomical mission by the JAXA, NASA, ESA and other international participants, that is planned for launch in 2022 (Japanese fiscal year), to quickly restore high-resolution X-ray spectroscopy of astrophysical objects. To enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the instrument teams and the Mission Operations Team. The responsibilities of the SOT are divided into four categories: 1) guest observer program and data distributions, 2) distribution of analysis software and the calibration database, 3) guest observer support activities, and 4) performance verification and optimization activities. As the first step, lessons on the science operations learned from past Japanese X-ray missions are reviewed, and 15 kinds of lessons are identified. Among them, a) the importance of early preparation of the operations from the ground stage, b) construction of an independent team for science operations separate from the instrument development, and c) operations with well-defined duties by appointed members are recognized as key lessons. Then, the team structure and the task division between the mission and science operations are defined; the tasks are shared among Japan, US, and Europe and are performed by three centers, the SOC, SDC, and ESAC, respectively. The SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning, quick-look health checks, pre-pipeline processing, etc., and the SDC covers tasks regarding data calibration processing, maintenance of analysis tools, etc. The data-archive and user-support activities are covered both by the SOC and SDC. Finally, the science-operations tasks and tools are defined and prepared before launch., Comment: 42 pages, 7 figures, 8 table, Accepted for Publication in JATIS (SPIE)

Published
2021

16. X-ray transmission calibration of the gate valve for the x-ray astronomy satellite XRISM

Author

Mayu Tominaga, Manabu Ishida, Shunji Kitamoto, Yoshitomo Maeda, Ken Ebisawa, Takuya Midooka, Nozomi Nakaniwa, and Masahiro Tsujimoto

Subjects
Diffraction, Materials science, Physics::Instrumentation and Detectors, business.industry, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Mechanical Engineering, Astrophysics::Instrumentation and Methods for Astrophysics, Incoherent scatter, Bragg's law, Astronomy and Astrophysics, Gate valve, Synchrotron, Electronic, Optical and Magnetic Materials, law.invention, Optics, Beamline, Space and Planetary Science, Control and Systems Engineering, law, Calibration, business, Instrumentation
Abstract

Resolve onboard the x-ray satellite X-Ray Imaging and Spectroscopy Mission (XRISM) is a cryogenic instrument with an x-ray microcalorimeter in a Dewar. A lid partially transparent to x-rays (called gate valve or GV) is installed at the top of the Dewar along the optical axis. Because observations will be made through the GV for the first few months, the x-ray transmission calibration of the GV is crucial for initial scientific outcomes. We present the results of our ground calibration campaign of the GV, which is composed of a Be window and a stainless steel mesh. For the stainless steel mesh, we measured its transmission using the x-ray beamline at ISAS. For the Be window, we used synchrotron facilities to measure the transmission and modeled the data with (i) photoelectric absorption and incoherent scattering of Be, (ii) photoelectric absorption of contaminants, and (iii) coherent scattering of Be changing at specific energies. We discuss the physical interpretation of the transmission discontinuity caused by the Bragg diffraction in polycrystal Be, which we incorporated into our transmission phenomenological model. We present the x-ray diffraction measurement on the sample to support our interpretation. The measurements and the constructed model meet the calibration requirements of the GV. We also performed a spectral fitting of the Crab nebula observed with Hitomi SXS and confirmed improvements of the model parameters.

Published
2021

17. Long-term X-ray variation of the colliding-wind Wolf–Rayet binary WR 125

Author

Yasuharu Sugawara, Takuya Midooka, and Ken Ebisawa

Subjects
Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Luminosity, Wolf–Rayet star, 0103 physical sciences, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Plasma, X-rays: individual: WR 125, Stars, Space and Planetary Science, stars: Wolf-Rayet, Astrophysics - High Energy Astrophysical Phenomena, binaries: spectroscopic
Abstract

WR 125 is considered as a Colliding Wind Wolf-rayet Binary (CWWB), from which the most recent infrared flux increase was reported between 1990 and 1993. We observed the object four times from November 2016 to May 2017 with Swift and XMM-Newton, and carried out a precise X-ray spectral study for the first time. There were hardly any changes of the fluxes and spectral shapes for half a year, and the absorption-corrected luminosity was 3.0e+33 erg/s in the 0.5 - 10.0 keV range at a distance of 4.1 kpc. The hydrogen column density was higher than that expected from the interstellar absorption, thus the X-ray spectra were probably absorbed by the WR wind. The energy spectrum was successfully modeled by a collisional equilibrium plasma emission, where both the plasma and the absorbing wind have unusual elemental abundances particular to the WR stars. In 1981, the Einstein satellite clearly detected X-rays from WR 125, whereas the ROSAT satellite hardly detected X-rays in 1991, when the binary was probably around the periastron passage. We discuss possible causes for the unexpectedly low soft X-ray flux near the periastron., 5 page, 1 figure, accepted for publication in MNRAS

Published
2019

18. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author

Ludovic Montier, Baptiste Mot, Paolo de Bernardis, Bruno Maffei, Giampaolo Pisano, Fabio Columbro, Jon E. Gudmundsson, Sophie Henrot-Versillé, Luca Lamagna, Joshua Montgomery, Thomas Prouvé, Megan Russell, Giorgio Savini, Samantha Stever, Keith L. Thompson, Masahiro Tsujimoto, Carole Tucker, Benjamin Westbrook, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, Ranajoy Banerji, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Gianluca Morgante, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Gianluca Polenta, Davide Poletti, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), LiteBIRD, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
cosmological model, experimental methods, detector: satellite, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, magnetic field, 02 engineering and technology, LiteBIRD, cosmic microwave background, polarization measurements, space telescopes, 7. Clean energy, 01 natural sciences, law.invention, law, detector: calibration, media_common, Physics, conductivity: thermal, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), inflation: model, experimental equipment, B-mode, cosmic radiation, cryogenics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, cosmic background radiation: detector, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, LiteBIRD, Polarization measurements, Space telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, bolometer: superconductivity, frequency: high, Radio spectrum, tensor scalar: ratio, 010309 optics, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: angular resolution, Astrophysics::Galaxy Astrophysics, Gravitational wave, synchrotron radiation, gravitational radiation: primordial, Astronomy, Physics::History of Physics, optics, detector: sensitivity, 13. Climate action, Sky, Satellite, temperature: stability, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS).

Published
2020

19. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author

Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Lystrup, Makenzie, Hazumi, M, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banjeri, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, and Zonca, A

Subjects
cosmological model, experimental methods, detector: satellite, Physics beyond the Standard Model, Cosmic microwave background, LiteBIRD, cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravi- tational waves, quantum gravity, space telescope, cosmic background radiation: polarization, detector: noise, 02 engineering and technology, 7. Clean energy, 01 natural sciences, expansion: multipole, Cosmology, General Relativity and Quantum Cosmology, B-mode: primordial, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), general relativity, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], B-mode polarization, media_common, Physics, new physics, quantum mechanics, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, BICEP, inflation: model, High Energy Physics - Phenomenology, error: statistical, experimental equipment, cryogenics, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], readout, Astrophysics::Earth and Planetary Astrophysics, dust, control system, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, cosmic inflation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, primordial gravi- tational waves, Cosmic background radiation, space telescope, Lagrangian point, FOS: Physical sciences, LiteBIRD, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, polarization: sensitivity, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Inflation (cosmology), synchrotron radiation, primordial gravitational waves, gravitational radiation: primordial, Astronomy, calibration, Physics::History of Physics, recombination, detector: sensitivity, angular resolution, Sky, quantum gravity, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 µK-arcmin with a typical angular resolution of 0.5◦ at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy.

Published
2020

20. Simulation of the cosmic ray effects for the LiteBIRD satellite observing the CMB B-mode polarization

Author

Mayu Tominaga, T. Ghigna, Hirokazu Ishino, S. Stever, Masahiro Tsujimoto, and Ken Ebisawa

Subjects
Physics, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Lagrangian point, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Spectral line, symbols.namesake, Sky, symbols, Planck, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio), media_common
Abstract

The LiteBIRD satellite is planned to be launched by JAXA in the late 2020s. Its main purpose is to observe the large-scale B-mode polarization in the Cosmic Microwave Background (CMB) anticipated from the Inflation theory. LiteBIRD will observe the sky for three years at the second Lagrangian point (L2) of the Sun-Earth system. Planck was the predecessor for observing the CMB at L2, and the onboard High Frequency Instrument (HFI) suffered contamination by glitches caused by the cosmic-ray (CR) hits. We consider the CR hits can also be a serious source of the systematic uncertainty for LiteBIRD. Thus, we have started a comprehensive end-to-end simulation study to assess impact of the CR hits for the LiteBIRD detectors. Here, we describe procedures to make maps and power spectra from the simulated time-ordered data, and present initial results. Our initial estimate is that $C_l^{BB}$ by CR is $\sim 2 \times 10^{-6}~\mu$K$_{\mathrm{CMB}}^{2}$ in a one-year observation with 12 detectors assuming that the noise is 1~aW/$\sqrt{\mathrm{Hz}}$ for the differential mode of two detectors constituting a polarization pair., Comment: 15 pages, 9 figures, SPIE Proceeding no. 114532H

Published
2020

21. Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD

Author

Mario G. Lattanzi, Carlo Baccigalupi, François Levrier, J. M. Duval, J. Austermann, M. Brilenkov, B. Thorne, Eiichiro Komatsu, D. Rambaud, T. Nagasaki, Peter Shirron, H. Imada, Nozomu Kogiso, Jeff Van Lanen, H. Takakura, T. Kawasaki, Lionel Duband, Ingunn Kathrine Wehus, Y. Hoshino, Tadayasu Dotani, Enrique Martinez-Gonzalez, Tucker Elleflot, S. Beckman, T. Kaga, Shogo Nakamura, A. Kato, Giorgio Savini, S. Bounissou, S. Mandelli, Peter Charles Hargrave, Francois Boulanger, Julien Grain, S. Realini, Reijo Keskitalo, Bruno Maffei, Y. Nagano, Davide Maino, D. Herman, Michael R. Vissers, B. Mot, R. Banerji, N. Katayama, James A. Beall, Johannes Hubmayr, Tomotake Matsumura, Shugo Oguri, G. Patanchon, S. Basak, S. Takakura, Créidhe O'Sullivan, Massimo Gervasi, Y. Takase, S. Stever, A. Carones, Raphael Flauger, F. J. Casas, T. de Haan, Yasuhiro Murata, T. Prouvé, Douglas Scott, P. Vielva, Toshiya Namikawa, Mayu Tominaga, Yuki Sakurai, Luca Lamagna, Eric Hivon, S. Nerval, Ken Ebisawa, Noriko Y. Yamasaki, Julian Borrill, Shingo Kashima, Hajime Sugai, M. De Petris, R. Nagata, Ted Kisner, D. W. Curtis, A. Mennella, P. de Bernardis, Alexandre E. Adler, Misao Sasaki, Jiansong Gao, Kam Arnold, K. Ganga, T. Ghigna, Kazunori Kohri, Ben Westbrook, R. Aurlien, T. Toda, Yasuhiro Takeda, U. Fuskeland, Alessandro Gruppuso, Giuseppe Puglisi, A. Ritacco, I. Kreykenbohm, C. Leloup, M. A. Dobbs, Jochen Weller, Joel N. Ullom, Chao-Lin Kuo, M. Migliaccio, Charles A. Hill, E. Allys, Nicola Vittorio, T. Yoshida, R. Takaku, Thomas Essinger-Hileman, Alessandro Paiella, J. Aumont, Berend Winter, Junji Yumoto, Yutaka Terao, Aritoki Suzuki, T. Hasebe, Toshiyuki Nishibori, A. Cukierman, P. Campeti, Y. Hirota, Alan J. Kogut, Josquin Errard, S. Sugiyama, L. P. L. Colombo, Anthony Challinor, Yohei Kobayashi, A. Kushino, Gemma Luzzi, Makoto Nagai, M. Sandri, Christopher Raum, Giuseppe D'Alessandro, Masashi Hazumi, Masaya Hasegawa, Renée Hlozek, Silvia Masi, Joseph Seibert, F. Piacentini, J. A. Murphy, Greg Jaehnig, Jose Alberto Rubino-Martin, Davide Poletti, Michael L. Brown, Blake D. Sherwin, Daniela Paoletti, Joshua Montgomery, F. Columbro, Gianluca Morgante, J. Bermejo, M. Tomasi, Haruki Nishino, P. Diego-Palazuelos, Hirokazu Ishino, T. Iida, Kazuhisa Mitsuda, Haruyuki Sakurai, Keith L. Thompson, Javier Cubas, Neil Trappe, Keisuke Shinozaki, Adrian T. Lee, Hiroyuki Ohsaki, Martina Gerbino, D. Herranz, M. Tsuji, Marco Bersanelli, Nadia Dachlythra, M. Russell, E. Gjerløw, Maresuke Shiraishi, E. de la Hoz, Eric V. Linder, Graeme Smecher, Eric R. Switzer, Erminia Calabrese, G. Roudil, Mario Zannoni, T. Maciaszek, L. Pagano, D. Auguste, Frank Grupp, Kosei Ishimura, Fabrizio Villa, Kuniaki Konishi, I. S. Ohta, G. Signorelli, J. Bonis, A. Tartari, Jun-ichi Suzuki, R. B. Barreiro, J. F. Cliche, M. Maki, Douglas H Beck, Ricardo Genova-Santos, A. J. Banday, M. Galloway, T. L. Svalheim, Fabio Finelli, L. A. Montier, H. K. Eriksen, Nicoletta Krachmalnicoff, Karen C. Cheung, Cristian Franceschet, Matthieu Tristram, V. Chan, G. Polenta, Clive Dickinson, N. W. Halverson, Kiyotomo Ichiki, Yuji Chinone, Mathieu Remazeilles, Giampaolo Pisano, Jon E. Gudmundsson, J. Peloton, M. Reinecke, Shannon M. Duff, Carole Tucker, Y. Minanmi, Gene C. Hilton, Martin Bucher, P. A. R. Ade, G. Vermeulen, K. Komatsu, Norio Okada, Thibaut Louis, Sophie Henrot-Versille, Edward J. Wollack, Paolo Natoli, Hideo Ogawa, Jörn Wilms, E. Taylor, Andrea Zonca, Makoto Hattori, Radek Stompor, Masahiro Tsujimoto, Yutaro Sekimoto, Marcin Gradziel, H. Thommesen, Zmuidzinas, Jonas, Sekimoto, Y, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minanmi, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Osaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Tambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique de l'ENS (LPTENS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Hautes Energies (LPTHE), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -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 des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Laboratoire de Physique Théorique de l'ENS [École Normale Supérieure] (LPTENS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, FOS: Physical sciences, 7. Clean energy, cryogenic telescope, law.invention, Cosmic microwave background, Entrance pupil, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, millimeter-wave polarization, space program, Settore FIS/05 - Astronomia e Astrofisica, law, Angular resolution, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Stray light, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Lens (optics), Cardinal point, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of $-56$ dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34--161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view ($18^\circ \times 9^\circ$) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90$^\circ$ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at $5\,$K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented., Comment: 21 pages, 14 figures

Published
2020

22. Nature of the warm absorber outflow in NGC 4051

Author

Misaki Mizumoto and Ken Ebisawa

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Emission spectrum, Spectral resolution, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Line-of-sight, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, galaxies: Seyfert, Space and Planetary Science, X-rays: individual: NGC 4051, Outflow, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Narrow-line Seyfert 1 galaxy NGC 4051 is known to exhibit significant X-ray spectral/flux variations and have a number of emission/absorption features. X-ray observations have revealed that these absorption features are blueshifted, which indicates that NGC 4051 has warm absorber outflow. In order to constrain physical parameters of the warm absorber outflow, we analyze the archival data with the longest exposure taken by XMM-Newton in 2009. We calculate the root-mean-square (RMS) spectra with the grating spectral resolution for the first time. The RMS spectra have a sharp peak and several dips, which can be explained by variable absorption features and non-variable emission lines; a lower-ionized warm absorber (WA1: $\log\xi = 1.5,\, v=-650\,\mathrm{km\,s}^{-1}$) shows large variability, whereas higher-ionized warm absorbers (WA2: $\log\xi= 2.5,\,v=-4100\,\mathrm{km\,s}^{-1}$, WA3: $\log\xi= 3.4,\, v=-6100\,\mathrm{km\,s}^{-1}$) show little variability. WA1 shows the maximum variability at a timescale of $\sim10^4$~s, suggesting that the absorber locates at $\sim10^3$ times of the Schwarzschild radius. The depth of the absorption features due to WA1 and the observed soft X-ray flux are anti-correlated in several observational sequences, which can be explained by variation of partial covering fraction of the double-layer blobs that are composed of the Compton-thick core and the ionized layer ($=$WA1). WA2 and WA3 show little variability and presumably extend uniformly in the line of sight. The present result shows that NGC 4051 has two types of the warm absorber outflows; the static, high-ionized and extended line-driven disk winds, and the variable, low-ionized and clumpy double-layer blobs., Comment: Accepted for MNRAS. Sorry for broken hyperref (citation of references is broken). Please find the published version

Published
2017

23. X-ray reverberation lags of the Fe–K line due to AGN disc winds

Author

Kouichi Hagino, Ken Ebisawa, Chris Done, Misaki Mizumoto, Hirokazu Odaka, and Masahiro Tsujimoto

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Active galactic nucleus, Line-of-sight, 010308 nuclear & particles physics, Scattering, Event horizon, black hole physics, galaxies: active, Solid angle, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Xrays: individual: 1H 0707-495, Ark 564, 01 natural sciences, K-line, galaxies: Seyfert, Spectral line, X-rays: galaxies, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Line (formation)
Abstract

Short X-ray reverberation lags are seen across a broad Fe-K energy band in more than twenty active galactic nuclei (AGNs). This broad iron line feature in the lag spectrum is most significant in super-Eddington sources such as Ark 564 ($L/L_{\rm Edd}\sim 1$) and 1H 0707--495 ($L/L_{\rm Edd}\gtrsim 10$). The observed lag timescales correspond to very short distances of several $R_g/c$, so that they have been used to argue for extremely small `lamp-post' coronae close to the event horizon of rapidly spinning black holes. Here we show for the first time that these Fe-K short lags are more likely to arise from scattering in a highly-ionised wind, launched at $\sim 50\,R_g$, rotating and outflowing with a typical velocity of $0.2c$. We show that this model can simultaneously fit the time-averaged energy spectra and the short-timescale lag-energy spectra of both 1H 0707--495 and Ark 564. The Fe-K line in 1H 0707--495 has a strong P-Cygni-like profile, which requires that the wind solid angle is large and that our line of sight intercepts the wind. By contrast the lack of an absorption line in the energy spectrum of Ark 564 requires rather face-on geometry, while the weaker broad Fe-K emission in the energy and lag-energy spectra argue for a smaller solid angle of the wind. This is consistent with theoretical predictions that the winds get stronger when the sources are more super-Eddington, supporting the idea of AGN feedback via radiation pressure driven winds., Comment: 11 pages, 10 figures, accepted for publication in MNRAS

Published
2019

24. The CALorimetric Electron Telescope (CALET) on the international space station: Results from the first two years on orbit

Author

A. M. Messineo, G. Castellini, A. Sulaj, N. Tateyama, F. Stolzi, Paolo Papini, G. A. de Nolfo, Shunsuke Ozawa, Seiya Ueno, P. Brogi, L. Pacini, Nicola Mori, J. E. Suh, Y. Katayose, Holger Motz, T. G. Guzik, V. Pal'shin, Satoshi Sugita, P. Spillantini, Katsuaki Kasahara, S. Yanagita, K. Hibino, Nobuyuki Hasebe, Chihiro Kato, Y. Kawakubo, Shoji Torii, Ryuho Kataoka, Hideyuki Fuke, Roberta Sparvoli, S. Bonechi, John Mitchell, Henric Krawczynski, N. Cannady, Shoko Miyake, G. Bigongiari, John Krizmanic, M. H. Israel, Kazutaka Yamaoka, A. Shiomi, Kazuoki Munakata, E. Vannuccini, Y. Shimizu, Atsumasa Yoshida, J. F. Ormes, M. Bongi, Yoichi Asaoka, Wataru Ishizaki, Yukio Uchihori, Maria Grazia Bagliesi, H. Tomida, T. Hams, J. Nishimura, Emanuele Berti, Kenji Yoshida, M. Ichimura, T. Lomtadze, G. Collazuol, Toshio Terasawa, Katsuaki Asano, H. Murakami, C. Checchia, Yoshiki Tsunesada, W. R. Binns, Kazunori Kohri, K. Sakai, V. Di Felice, Alexander Moiseev, J. Kataoka, A. Bruno, A. V. Penacchioni, T. Tamura, Manami Sasaki, J. H. Buckley, O. Adriani, Kunihito Ioka, T. Sakamoto, Masato Takita, Y Akaike, I. Takahashi, S. B. Ricciarini, Michael Cherry, Masaki Mori, Satoshi Nakahira, K. Mori, P. Maestro, Brian Rauch, M. Takayanagi, John P. Wefel, Norita Kawanaka, F. Palma, Ken Ebisawa, S. Okuno, and P. S. Marrocchesi

Subjects
History, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, astro-ph.HE, International Space stations, 01 natural sciences, 7. Clean energy, Education, law.invention, Telescope, Positron, law, 0103 physical sciences, International Space Station, Gamma-ray observations, 010306 general physics, 010303 astronomy & astrophysics, Settore FIS/01, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, Cosmic ray electrons, Gravitational wave, Gamma rays, Astronomy, LIGO, Computer Science Applications, Particle acceleration, Astrophysics - High Energy Astrophysical Phenomena, Telescopes
Abstract

The CALorimetric Electron Telescope (CALET) is a high-energy astroparticle physics space experiment installed on the International Space Station (ISS), developed and operated by Japan in collaboration with Italy and the United States. The CALET mission goals include the investigation of possible nearby sources of high-energy electrons, of the details of galactic particle acceleration and propagation, and of potential signatures of dark matter. CALET measures the cosmic-ray electron + positron flux up to 20 TeV, gamma-rays up to 10 TeV, and nuclei with Z=1 to 40 up to 1,000 TeV for the more abundant elements during a long-term observation aboard the ISS. Starting science operation in mid-October 2015, CALET performed continuous observation without major interruption with close to 20 million triggered events over 10 GeV per month. Based on the data taken during the first two-years, we present an overview of CALET observations: uses w/o major interruption 1) Electron + positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation including a characterization of on-orbit performance. Results of the electromagnetic counterpart search for LIGO/Virgo gravitational wave events are discussed as well., 10 pages, 10 figures, a contribution to the proceedings of 26th Extended European Cosmic Ray Symposium, 6-10 July 2018, Russia, which summarizes our recent publications such as arXiv:1712.01711, arXiv:1712.01757, arXiv:1803.05834, arXiv:1806.09728, and arXiv:1807.01435

Published
2019

25. 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

26. Variabiity of the X-ray broad iron spectral features in active galactic nuclei and black-hole binaries

Author

Misaki Mizumoto, Hajime Inoue, Masahiro Tsujimoto, and Ken Ebisawa

Subjects
Physics, Active galactic nucleus, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Mode (statistics), Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Black hole, Amplitude, Space and Planetary Science, 0103 physical sciences, Reflection (physics), Calibration, 010303 astronomy & astrophysics
Abstract

The “broad iron spectral features” are often seen in X-ray spectra of active galactic nuclei (AGN) and black-hole binaries (BHB). These features may be explained either by the “relativistic disc reflection” scenario or the “partial covering” scenario: It is hardly possible to determine which model is valid from time-averaged spectral analysis. Thus, X-ray spectral variability has been investigated to constrain spectral models. To that end, it is crucial to study iron structure of BHBs in detail at short time-scales, which is, for the first time, made possible with the Parallel-sum clocking (P-sum) mode of XIS detectors on board of Suzaku. This observational mode has a time-resolution of 7.8 ms as well as a CCD energyresolution. We have carried out systematic calibration of the P-sum mode, and investigated spectral variability of the BHB GRS 1915+105. Consequently, we found that the spectral variability of GRS 1915+105 does not show iron features at sub-seconds. This is totally different from variability of AGN such as 1H0707–495, where the variation amplitude significantly drops at the iron K-energy band. This difference can be naturally explained in the framework of the “partial covering” scenario. (© 2016 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

Published
2016

27. Discovery of the Black Hole X-Ray Binary Transient MAXI J1348–630

Author

Megumi Shidatsu, Yasuharu Sugawara, Ken Ebisawa, Mayu Tominaga, Motoki Oeda, Tatehiro Mihara, Nobuyuki Kawai, Mutsumi Sugizaki, Satoshi Nakahira, Yoshihiro Ueda, and Hitoshi Negoro

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, General Relativity and Quantum Cosmology, Space and Planetary Science, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Transient (oscillation), Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

We report the first half-year monitoring of the new Galactic black hole candidate MAXI J1348-630, discovered on 2019 January 26 with the Gas Slit Camera (GSC) on-board MAXI. During the monitoring period, the source exhibited two outburst peaks, where the first peak flux (at T=14 day from the discovery of T =0) was ~4 Crab (2-20 keV) and the second one (at T =132 day) was ~0.4 Crab (2-20 keV). The source exhibited distinct spectral transitions between the high/soft and low/hard states and an apparent "q"-shape curve on the hardness-intensity diagram, both of which are well-known characteristics of black hole binaries. Compared to other bright black hole transients, MAXI J1348-630 is characterized by its low disk-temperature (~0.75 keV at the maximum) and high peak flux in the high/soft state. The low peak-temperature leads to a large innermost radius that is identified as the Innermost Stable Circular Orbit (ISCO), determined by the black hole mass and spin. Assuming the empirical relation between the soft-to-hard transition luminosity (Ltrans) and the Eddington luminosity (LEdd), Ltrans/LEdd ~ 0.02, and a face-on disk around a non-spinning black hole, the source distance and the black hole mass are estimated to be D ~ 4 kpc and ~7 (D/4 kpc) Mo, respectively. The black hole is more massive if the disk is inclined and the black hole is spinning. These results suggest that MAXI J1348-630 may host a relatively massive black hole among the known black hole binaries in our Galaxy., Comment: 7 pages, 5 figures, accepted by ApJL

Published
2020

28. Can the relativistic light-bending model explain X-ray spectral variations of Seyfert galaxies?

Author

Misaki Mizumoto, Ken Ebisawa, Norita Kawanaka, Shin Mineshige, Masahiro Tsujimoto, and Kotaro Moriyama

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, galaxies: individual (IRAS 13224-3809), Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, galaxies: Seyfert, Spectral line, Galaxy, X-rays: galaxies, Amplitude, Rotating black hole, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Schwarzschild radius, Line (formation)
Abstract

Many Seyfert galaxies are known to exhibit Fe-K broad emission line features in their X-ray energy spectra. The observed lines have three distinct features; (1) the line profiles are skewed and show significant low-energy tails, (2) the Fe-K band have low variability, which produces a broad and deep dip in the root-mean-square (rms) spectra, and (3) photons in this band have time lags behind those in the adjacent energy bands with amplitudes of several $R_g/c$, where $R_g$ is the gravitational radius. The "relativistic light bending model" is proposed to explain these observed features, where a compact X-ray source (lamp post) above an extreme Kerr black hole illuminates the innermost area of the accretion disc. In this paper, we critically examine the relativistic light bending model by computing the rms spectra and the lag features using a ray-tracing technique, when a lamp post moves vertically on the black hole spin axis. As a result, we found that the observed deep rms dip requires that the iron is extremely overabundant ($\gtrsim10$ solar), whereas the observed lag amplitude is consistent with the normal iron abundance. Furthermore, disappearance of the lag in the high-flux state requires a source height as high as $\sim40\,R_g$, which contradicts the relativistically broad emission line feature. Our simulations agree with the data that the reverberation feature moves to lower frequencies with larger source height, however, if this scenario is correct, the simulations predict detection of a clear Fe-K lag at low frequencies, which is not constrained in the data. Therefore, we conclude that the relativistic light bending model may not explain the characteristic Fe-K spectral variations in Seyfert galaxies., Comment: 17 pages, 15 figures, accepted by PASJ

Published
2018

29. 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

30. 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

31. 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

32. 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

33. 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

34. X線衛星代替機における科学運用の計画概要

Author

Terada, Yukikatsu, Tashiro, S. Makoto, Takahashi, Hiromitsu, Mizuno, Tsunefumi, Tamura, Takayuki, Uno, Shin'ichiro, Kubota, Aya, Nakazawa, Kazuhiro, Watanabe, Shin, Iizuka, Ryo, Uchiyama, Hideki, Ken, Ebisawa, Ohno, Masanori, Nobukawa, Masayoshi, Shidatsu, Megumi, Ota, Naomi, Katsuda, Satoru, Yamauchi, Shigeo, Nakashima, Shinya, Kitaguchi, Takao, Sugawara, Yasuharu, Fukazawa, Yasushi, Tanaka, Yasuyuki, Tsuboi, Yohko, and Terashima, Yuichi

Abstract

第18回宇宙科学シンポジウム (2018年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 18th Space Science Symposium (January 9-10, 2018. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 25名, 資料番号: SA6000118167, レポート番号: P-134

Published
2018

35. X-ray short-time lags in the Fe-K energy band produced by scattering clouds in active galactic nuclei

Author

Hirokazu Odaka, Chris Done, Ken Ebisawa, Masahiro Tsujimoto, Misaki Mizumoto, and Kouichi Hagino

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Reverberation, Photon, Active galactic nucleus, 010308 nuclear & particles physics, Scattering, Event horizon, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies: active, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, K-line, galaxies: Seyfert, X-rays: galaxies, Space and Planetary Science, 0103 physical sciences, Electronic band structure, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Schwarzschild radius, Astrophysics::Galaxy Astrophysics
Abstract

X-rays illuminating the accretion disc in active galactic nuclei give rise to an iron K line and its associated reflection spectrum which are lagged behind the continuum variability by the light-travel time from the source to the disc. The measured lag timescales in the iron band can be as short as $\sim R_g/c$, where $R_g$ is the gravitational radius, which is often interpreted as evidence for a very small continuum source close to the event horizon of a rapidly spinning black hole. However, the short lags can also be produced by reflection from more distant material, because the primary photons with no time-delay dilute the time-lags caused by the reprocessed photons. We perform a Monte-Carlo simulation to calculate the dilution effect in the X-ray reverberation lags from a half-shell of neutral material placed at $100\,R_g$ from the central source. This gives lags of $\sim2\,R_g/c$, but the iron line is a distinctly narrow feature in the lag-energy plot, whereas the data often show a broader line. We show that both the short lag and the line broadening can be reproduced if the scattering material is outflowing at $\sim0.1c$. The velocity structure in the wind can also give shifts in the line profile in the lag-energy plot calculated at different frequencies. Hence we propose that the observed broad iron reverberation lags and shifts in profile as a function of frequency of variability can arise from a disc wind at fairly large distances from the X-ray source., Comment: 12 pages, accepted for publication in MNRAS

Published
2018
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36. 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

37. Energy Dependent Intensity Variation of the Persistent X-ray Emission of Magnetars Observed with Suzaku

Author

Yujin E. Nakagawa, Teruaki Enoto, and Ken Ebisawa

Subjects
Energy dependent, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, X-rays: stars, Astrophysics, Poisson distribution, Magnetar, 01 natural sciences, Root mean square, symbols.namesake, stars: magnetars, pulsars: general, 0103 physical sciences, Thermal, Variation (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), X-ray, Astronomy and Astrophysics, Intensity (physics), Space and Planetary Science, symbols, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Emission mechanism of the magnetars is still controversial while various observational and theoretical studies have been made. In order to investigate mechanisms of both the persistent X-ray emission and the burst emission of the magnetars, we have proposed a model that the persistent X-ray emission consists of numerous micro-bursts of various sizes. If this model is correct, intensity Root Mean Square (RMS) variations of the persistent emission exceed the values expected from the Poisson distribution. Using $Suzaku$ archive data of 11 magnetars (22 observations), the RMS intensity variations were calculated from 0.2 keV to 70 keV. As a result, we found significant excess RMS intensity variations from all the 11 magnetars. We suppose that numerous mircro-bursts constituting the persistent X-ray emission cause the observed variations, suggesting that the persistent X-ray emission and the burst emission have identical emission mechanisms. In addition, we found that the RMS intensity variations clearly increase toward higher energy bands for 4 magnetars (6 observations). The energy dependent RMS intensity variations imply that the soft thermal component and the hard X-ray component are emitted from different regions far apart from each other., Comment: 21 pages, 4 figures, 2 tables, Accepted for publication in PASJ

Published
2018
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38. 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

39. SMILES observations of mesospheric ozone during the solar eclipse

Author

Yousuke Yamashita, Makoto Suzuki, Ken Ebisawa, Koji Imai, Masato Shiotani, Kenshi Takahashi, Hideharu Akiyoshi, and Takashi Imamura

Subjects
Ozone, Analytical expressions, Solar eclipse, Radiation, Atmospheric sciences, Mesosphere, Atmosphere, chemistry.chemical_compound, Geophysics, chemistry, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, General Earth and Planetary Sciences, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Eclipse
Abstract

The Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) successfully observed vertical distributions of ozone (O3) concentration in the middle atmosphere during the annular solar eclipse that occurred on 15 January 2010. In the mesosphere, where the photochemical lifetime of O3 is relatively short (approximately 100 s), altitude-dependent changes in O3 concentration under reduced solar radiation and their temporal variations were clearly observed as a function of the eclipse obscuration. This study reports the vertical distributions of mesospheric O3 during a solar eclipse event and analyzes theoretically the eclipse-induced changes. We show that simple analytical expressions for O3 concentration, which assume that O3 and O are in a photochemically steady state, can be used to describe the O3 concentration under reduced solar radiation. The SMILES data obtained during the eclipse provide a unique opportunity to test our current understanding of mesospheric O3 photochemistry.

Published
2015

40. X-Ray and Near-Infrared Spectroscopy of Dim X-Ray Point Sources Constituting the Galactic Ridge X-Ray Emission

Author

Masahiro Tsujimoto, Ken Ebisawa, and Kumiko Morihana

Subjects
Physics, Brightness, Active galactic nucleus, Galactic ridge, Near-infrared spectroscopy, White dwarf, Astronomy, Astrophysics, Stars, lcsh:TA1-2040, Bulge, General Earth and Planetary Sciences, lcsh:Engineering (General). Civil engineering (General), Spectroscopy, General Environmental Science
Abstract

We present the results of X-ray and Near-Infrared observations of the Galactic Ridge X-ray Emission (GRXE). We extracted 2,002 X-ray point sources in the Chandra Bulge Field (l =0°.113, b = 1°.424) down to ~10-14.8 ergscm-2s-1 in 2-8 keV band with the longest observation (900 ks) of the GRXE. Based on X-ray brightness and hardness, we classied the X-ray point sources into three groups: A (hard), B (soft and broad spectrum), and C (soft and peaked spectrum). In order to know populations of the X-ray point sources, we carried out NIR imaging and spectroscopy observation. We identied 11% of X-ray point sources with NIR and extracted NIR spectra for some of them. Based on X-ray and NIR properties, we concluded that non-thermal sources in the group A are mostly active galactic nuclei and the thermal sources are mostly white dwarf binaries such as cataclysmic variables (CVs) and Pre-CVs. We concluded that the group B and C sources are X-ray active stars in flare and quiescence, respectively.

Published
2014

41. Origin of X-ray Spectral Variation and the Seemingly Broad Iron-Line Spectral Feature in Seyfert Galaxies

Author

Naoki Iso, Hajime Inoue, Takehiro Miyakawa, and Ken Ebisawa

Subjects
Physics, Line-of-sight, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral component, Galaxy, Luminosity, lcsh:TA1-2040, Ionization, General Earth and Planetary Sciences, Electronic band structure, lcsh:Engineering (General). Civil engineering (General), Astrophysics::Galaxy Astrophysics, General Environmental Science, Line (formation)
Abstract

We present systematic X-ray data analysis of the Seyfert galaxies observed by Suzaku to study origin of their hard X-ray (2 - 40 keV) variations. In particular, we examine if the "Variable Partial Covering (VPC) model" proposed by Miyakawa, Ebisawa and Inoue (2012), which was successful to explain spectral variations of MCG{6-30-15, is also valid for other Seyfert galaxies or not. In this model, intrinsic X-ray luminosity of the AGN is not signicantly variable, and most observed flux and spectral variations are caused by change of the geometrical covering fraction of the extended X-ray source by ionized absorbing clouds in the line of sight. We found that the observed flux and spectral variations of 20 targets in addition to MCG{6-30-15 are successfully explained by the VPC model. The transmitted spectral component through the absorbing clouds has a characteristics spectral feature of the ionized iron K-edge, which is considered to be the origin of the seemingly broad iron-line feature commonly observed in Seyfert galaxies. Variation of the partial covering fraction of the constant X-ray luminosity source causes such an anti-correlation between the direct (non-obscured) component and the transmitted (obscured) component, that cancels their variations each other. The cancellation works most effectively at the energy band where intensities of the two components are the closest to each other, namely, just below the iron K-edge. This explains the signicantly small fractional variations in the iron K-energy band, another well-known observational characteristic of Seyfert galaxies.

Published
2014

42. IVOA Recommendation: HiPS - Hierarchical Progressive Survey

Author

Daniel Durand, Felix Sharipov, Jesus Salgado, Ken Ebisawa, Laurent Michel, Mark Allen, Pierre Fernique, Thomas Boch, and Tom Donaldson

Subjects
ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), GeneralLiterature_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, ComputingMethodologies_COMPUTERGRAPHICS
Abstract

This document presents HiPS, a hierarchical scheme for the description, storage and access of sky survey data. The system is based on hierarchical tiling of sky regions at finer and finer spatial resolution which facilitates a progressive view of a survey, and supports multi-resolution zooming and panning. HiPS uses the HEALPix tessellation of the sky as the basis for the scheme and is implemented as a simple file structure with a direct indexing scheme that leads to practical implementations.

Published
2017

43. A Systematic X-ray Study of the Dwarf Novae Observed with Suzaku

Author

Takayuki Hayashi, Qazuya Wada, Ken Ebisawa, and Masahiro Tsujimoto

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, binaries: close, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), X-ray, FOS: Physical sciences, Quiescent state, X-rays: stars, Astronomy and Astrophysics, Astrophysics, Plasma, Cooling flow, 01 natural sciences, Spectral line, Boundary layer, Space and Planetary Science, 0103 physical sciences, novae, cataclysmic variables, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, stars: dwarf novae, Line (formation)
Abstract

Accepted: 2016-11-08, 資料番号: SA1160293000

Published
2016

44. Origin of the Characteristic X-ray Spectral Variations of IRAS 13224$-$3809

Author

Ken Ebisawa, Misaki Mizumoto, Hiroaki Sameshima, and Hiroki Yamasaki

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Line-of-sight, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, galaxies: Seyfert, Galaxy, Spectral line, Root mean square, X-rays: galaxies, Characteristic X-ray, Space and Planetary Science, 0103 physical sciences, Absorption (electromagnetic radiation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Optical depth
Abstract

The Narrow-line Seyfert 1 galaxy (NLS1) IRAS 13224$-$3809 is known to exhibit significant X-ray spectral variation, a sharp spectral drop at $\sim$ 7 keV, strong soft excess emission, and a hint of iron L-edge feature, which is very similar to the NLS1 1H 0707$-$495. We have proposed the "Variable Double Partial Covering (VDPC) model" to explain the energy spectra and spectral variability of 1H 0707$-$495 (Mizumoto, Ebisawa and Sameshima 2014, PASJ, 66, 122). In this model, the observed flux/spectral variations below 10 keV within a $\sim$day are primarily caused by change of the partial covering fraction of patchy clouds composed by double absorption layers in the line of sight. In this paper, we apply the VDPC model to IRAS 13224$-$3809. Consequently, we have found that the VDPC model can explain the observed spectral variations of IRAS 13224$-$3809 in the 0.5$-$10 keV band. In particular, we can explain the observed Root Mean Square (RMS) spectra (energy dependence of the fractional flux variation) in the entire 0.5$-$10 keV band. In addition to the well-known significant drop in the iron K-band, we have found intriguing iron L-peaks in the RMS spectra when the iron L-edge is particularly deep. This feature, which is also found in 1H 0707$-$495, is naturally explained with the VDPC model, such that the RMS variations increase at the energies where optical depths of the partial absorbers are large. The absorbers have a larger optical depth at the iron L-edge than in the adjacent energy bands, thus a characteristic iron L-peak appears. On the other hand, just below the iron K-edge, the optical depth is the lowest and the RMS spectrum has a broad dip., Comment: 18 pages, 10 figures, Accepted for PASJ

Published
2016
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45. 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

47. MAXI GSC Monitoring of the Crab Nebula and Pulsar during the GeV Gamma-Ray Flare in 2010 September

Author

Tatehiro Mihara, Mitsuhiro Kohama, Yohko Tsuboi, Motoki Nakajima, Hiroshi Tomida, Kousuke Sugimori, Hitoshi Negoro, Kazuo Hiroi, Fumitoshi Suwa, Nobuyuki Kawai, Ryuichi Usui, Megumi Shidatsu, Yoshihiro Ueda, Takayuki Yamamoto, Satoshi Eguchi, Kyohei Yamazaki, Takanori Matsumura, Arata Daikyuji, Yujin E. Nakagawa, Tetsuya Sootome, Kazutaka Yamaoka, Satoshi Nakahira, Hiroshi Tsunemi, Shiro Ueno, Masashi Kimura, Mikio Morii, Masaki Ishikawa, H. Ozawa, Mutsumi Sugizaki, Akiko Uzawa, Ken Ebisawa, Kazuyoshi Kawasaki, Hiroki Kitayama, Atsumasa Yoshida, Masaru Matsuoka, Naoki Isobe, and Motoko Serino

Subjects
Physics, Crab Nebula, Pulsar, Space and Planetary Science, law, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Pulse (physics), Flare, law.invention
Abstract

著者人数: 37名, Accepted: 2011-07-20, 資料番号: SA1003146000

Published
2011

48. The Astronomical Data Sonification Project 2: Experimental production of sound-based data plot software 'splot'

Author

Shin'ichiro, Uno, Sho, Sotoya, Akira, Miura, Ken, Ebisawa, 原著論文, Original, 日本福祉大学健康科学部, エー・アンド・アイ システム株式会社, and 宇宙航空研究開発機構宇宙科学研究所

Subjects
音声化，科学衛星，マルチメディア，視覚障害
Abstract

We are developing a sound-based, interactive, data-plotting program to enable the visually impaired to turn astronomical data into meaningful sounds. The sonification software, called "splot", would be available to any scientist to analyze data. Splot reads ASCII data files containing various plotting commands and other data, and then outputs sounds corresponding to the data instead of plotting to a display or a printer. Input data for splot is partially compatible with "qdp", a data-plotting program developed by NASA HEASARC. In this paper, we report the status of development. In the current version, splot only sonifies a one-dimensional histogram and thus remains an experimental production. Before releasing this software, we must extend its functions for a suitable field test and construct a data-analysis environment for the visually impaired.

Published
2011

49. X-Ray Studies of HESS J1809-193 with Suzaku

Author

Aya Bamba, Ken Ebisawa, Takayasu Anada, and Tadayasu Dotani

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Energy loss, Photon, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Electron, Pulsar wind nebula, Synchrotron emission, Pulsar, Space and Planetary Science, Energy spectrum, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Suzaku observed the region including HESS J1809-193, one of the TeV unidentified (unID) sources, and confirmed existence of the extended hard X-ray emission previously reported by ASCA, as well as hard X-ray emission from the pulsar PSR J1809-1917 in the region. One-dimensional profile of the diffuse emission is represented with a Gaussian model with the best-fit sigma of 7+-1 arcmin. The diffuse emission extends for at least 21 pc (at the 3sigma level, assuming the distance of 3.5 kpc), and has a hard spectrum with the photon index of Gamma ~1.7. The hard spectrum suggests the pulsar wind nebula (PWN) origin, which is also strengthened by the hard X-ray emission from PSR J1809-1917 itself. Thanks to the low background of Suzaku XIS, we were able to investigate spatial variation of the energy spectrum, but no systematic spectral change in the extended emission is found. These results imply that the X-ray emitting pulsar wind electrons can travel up to 21 pc from the pulsar without noticeable energy loss via synchrotron emission., Comment: 12 pages, 25 figures, PASJ, in press

Published
2010

50. Iron Emission Lines on the Galactic Ridge Observed with Suzaku

Author

Ezoe Yuichiro, Shigeo Yamauchi, Hiromitsu Takahashi, Yasuo Tanaka, Hironori Matsumoto, Ken Ebisawa, Katsuji Koyama, and Noriko Y. Yamasaki

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Galactic ridge, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy, X-rays: stars, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic plane, X-rays: ISM, Galaxy: disk, X-rays: spectra, Space and Planetary Science, Emission spectrum, Disc, X-rays: diffuse background, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

In order to elucidate origin of the Galactic Ridge X-ray Emission, we analyzed Suzaku data taken at various regions along the Galactic plane and studied their Fe-K emission line features. Suzaku resolved the Fe line complex into three narrow lines at ~6.4 keV,~6.7 keV and ~6.97 keV, which are K-lines from neutral (or low-ionized), He-like, and H-like iron ions, respectively. The 6.7 keV line is clearly seen in all the observed regions and its longitudinal distribution is consistent with that determined from previous observations. The 6.4 keV emission line was also found in various Galactic plane regions (b~0). Differences in flux ratios of the 6.4 keV/6.7 keV and 6.97 keV/6.7 keV lines between the Galactic plane and the Galactic center regions are studied and its implication is discussed., Comment: Accepted for publication in PASJ Suzaku 3rd special issue

Published
2009

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