Author: "Maxim Markevitch" - Searchworks@Jio Institute Digital Library Search Results

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169 results on '"Maxim Markevitch"'

1. XRISM Spectroscopy of the Fe Kα Emission Line in the Seyfert Active Galactic Nucleus NGC 4151 Reveals the Disk, Broad-line Region, and Torus

Author: XRISM Collaboration, Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Xin Xiang, Takeo Minezaki, Margaret Buhariwalla, Dimitra Gerolymatou, and Scott Hagen
Subjects: High energy astrophysics, High-luminosity active galactic nuclei, Accretion, Astrophysical black holes, Astrophysics, QB460-466
Abstract: We present an analysis of the first two XRISM/Resolve spectra of the well-known Seyfert-1.5 active galactic nucleus (AGN) in NGC 4151, obtained in 2023 December. Our work focuses on the nature of the narrow Fe K _α emission line at 6.4 keV, the strongest and most common X-ray line observed in AGN. The total line is found to consist of three components. Even the narrowest component of the line is resolved with evident Fe K _α _,1 (6.404 keV) and K _α _,2 (6.391 keV) contributions in a 2:1 flux ratio, fully consistent with neutral gas with negligible bulk velocity. Subject to the limitations of our models, the narrowest and intermediate-width components are consistent with emission from optically thin gas, suggesting that they arise in a disk atmosphere and/or wind. Modeling the three line components in terms of Keplerian broadening, they are readily associated with (1) the inner wall of the “torus,” (2) the innermost optical “broad-line region” (or “X-ray BLR”), and (3) a region with a radius of r ≃ 100 GM / c ^2 that may signal a warp in the accretion disk. Viable alternative explanations of the broadest component include a fast-wind component and/or scattering; however, we find evidence of variability in the narrow Fe K _α line complex on timescales consistent with small radii. The best-fit models are statistically superior to simple Voigt functions, but when fit with Voigt profiles the time-averaged lines are consistent with a projected velocity broadening of FWHM $\,=\,{1600}_{-200}^{+400}\,\mathrm{km}\,{{\rm{s}}}^{-1}$ . Overall, the resolution and sensitivity of XRISM show that the narrow Fe K line in AGN is an effective probe of all key parts of the accretion flow, as it is currently understood. We discuss the implications of these findings for our understanding of AGN accretion, future studies with XRISM, and X-ray-based black hole mass measurements.
Published: 2024
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2. On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies

Author: Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski, and Maxim Markevitch
Subjects: Intracluster medium, Galaxy clusters, X-ray astronomy, Astrophysics, QB460-466
Abstract: The intracluster medium of the Perseus Cluster exhibits spiral-shaped X-ray surface brightness discontinuities known as “cold fronts,” which simulations indicate are caused by the sloshing motion of the gas after the passage of a subcluster. Recent observations of Perseus have shown that these fronts extend to large radii. In this work, we present simulations of the formation of sloshing cold fronts in Perseus using the AREPO magnetohydrodynamics code, to produce a plausible scenario for the formation of the large front at a radius of 700 kpc. Our simulations explore a range of subcluster masses and impact parameters. We find that low-mass subclusters cannot generate a cold front that can propagate to such a large radius, and that small impact parameters create too much turbulence, which leads to the disruption of the cold front before it reaches such a large distance. Subclusters that make only one core passage produce a stable initial front that expands to large radii, but without a second core passage of the subcluster, other fronts are not created at a later time in the core region. We find a small range of simulations with subclusters with mass ratios of R ∼ 1:5 and an initial impact parameter of θ ∼ 20°–25° that not only produce the large cold front but a second set in the core region at later times. These simulations indicate that the “ancient” cold front is ∼6–8.5 Gyr old. For the simulations providing the closest match with observations, the subcluster has completely merged into the main cluster.
Published: 2024
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3. Mapping the Imprints of Stellar and Active Galactic Nucleus Feedback in the Circumgalactic Medium with X-Ray Microcalorimeters

Author: Gerrit Schellenberger, Ákos Bogdán, John A. ZuHone, Benjamin D. Oppenheimer, Nhut Truong, Ildar Khabibullin, Fred Jennings, Annalisa Pillepich, Joseph Burchett, Christopher Carr, Priyanka Chakraborty, Robert Crain, William Forman, Christine Jones, Caroline A. Kilbourne, Ralph P. Kraft, Maxim Markevitch, Daisuke Nagai, Dylan Nelson, Anna Ogorzalek, Scott Randall, Arnab Sarkar, Joop Schaye, Sylvain Veilleux, Mark Vogelsberger, Q. Daniel Wang, and Irina Zhuravleva
Subjects: Circumgalactic medium, Stellar feedback, Active galactic nuclei, Astrophysics, QB460-466
Abstract: The Astro2020 Decadal Survey has identified the mapping of the circumgalactic medium (CGM; the gaseous plasma around galaxies) as a key objective. We explore the prospects for characterizing the CGM in and around nearby galaxy halos with a future large-grasp X-ray microcalorimeter. We create realistic mock observations from hydrodynamical simulations (EAGLE, IllustrisTNG, and Simba) that demonstrate a wide range of potential measurements, which will address the open questions in galaxy formation and evolution. By including all background and foreground components in our mock observations, we show why it is impossible to perform these measurements with current instruments, such as X-ray CCDs, and why only microcalorimeters will allow us to distinguish the faint CGM emission from the bright Milky Way (MW) foreground emission lines. We find that individual halos of MW mass can, on average and depending on star formation rate, be traced out to large radii, around R _500 , and for larger galaxies even out to R _200 , using prominent emission lines, such as O vii , or O viii . Furthermore, we show that emission-line ratios for individual halos can reveal the radial temperature structure. Substructure measurements show that it will be possible to relate azimuthal variations to the feedback mode of the galaxy. We demonstrate the ability to construct temperature, velocity, and abundance ratio maps from spectral fitting for individual galaxy halos, which reveal rotation features, active galactic nucleus outbursts, and enrichment.
Published: 2024
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4. Properties of the Line-of-sight Velocity Field in the Hot and X-Ray-emitting Circumgalactic Medium of Nearby Simulated Disk Galaxies

Author: John A. ZuHone, Gerrit Schellenberger, Anna Ogorzałek, Benjamin D. Oppenheimer, Jonathan Stern, Ákos Bogdán, Nhut Truong, Maxim Markevitch, Annalisa Pillepich, Dylan Nelson, Joseph N. Burchett, Ildar Khabibullin, Caroline A. Kilbourne, Ralph P. Kraft, Paul E. J. Nulsen, Sylvain Veilleux, Mark Vogelsberger, Q. Daniel Wang, and Irina Zhuravleva
Subjects: Disk galaxies, X-ray observatories, N-body simulations, AGN host galaxies, Astrophysics, QB460-466
Abstract: The hot, X-ray-emitting phase of the circumgalactic medium of massive galaxies is believed to be the reservoir of baryons from which gas flows onto the central galaxy and into which feedback from active galactic nuclei and stars inject mass, momentum, energy, and metals. These effects shape the velocity fields of the hot gas, which can be observed via the Doppler shifting and broadening of emission lines by X-ray integral field units. In this work, we analyze the gas kinematics of the hot circumgalactic medium of Milky Way–mass disk galaxies from the TNG50 simulation with synthetic observations to determine how future instruments can probe this velocity structure. We find that the hot phase is often characterized by outflows from the disk driven by feedback processes, radial inflows near the galactic plane, and rotation, although in some systems the velocity field is more disorganized and turbulent. With a spectral resolution of ∼1 eV, fast and hot outflows (∼200–500 km s ^−1 ) can be measured, depending on the orientation of the galaxy on the sky. The rotation velocity of the hot phase (∼100–200 km s ^−1 ) can be measured using line shifts in edge-on galaxies, and is slower than that of colder gas phases but similar to stellar rotation velocities. By contrast, the slow inflows (∼50–100 km s ^−1 ) are difficult to measure in projection with these other components, but may be detected in multicomponent spectral fits. We find that the velocity measured is sensitive to which emission lines are used. Measuring these flows will constrain theories of how the gas in these galaxies evolves.
Published: 2024
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5. Circumgalactic Medium on the Largest Scales: Detecting X-Ray Absorption Lines with Large-area Microcalorimeters

Author: Ákos Bogdán, Ildar Khabibullin, Orsolya E. Kovács, Gerrit Schellenberger, John ZuHone, Joseph N. Burchett, Klaus Dolag, Eugene Churazov, William R. Forman, Christine Jones, Caroline Kilbourne, Ralph P. Kraft, Erwin Lau, Maxim Markevitch, Dan McCammon, Daisuke Nagai, Dylan Nelson, Anna Ogorzalek, Benjamin D. Oppenheimer, Arnab Sarkar, Yuanyuan Su, Nhut Truong, Sylvain Veilleux, Stephan Vladutescu-Zopp, and Irina Zhuravleva
Subjects: Circumgalactic medium, Disk galaxies, Galaxy evolution, High resolution spectroscopy, X-ray astronomy, X-ray observatories, Astrophysics, QB460-466
Abstract: The circumgalactic medium (CGM) plays a crucial role in galaxy evolution as it fuels star formation, retains metals ejected from the galaxies, and hosts gas flows in and out of galaxies. For Milky Way–type and more-massive galaxies, the bulk of the CGM is in hot phases best accessible at X-ray wavelengths. However, our understanding of the CGM remains largely unconstrained due to its tenuous nature. A promising way to probe the CGM is via X-ray absorption studies. Traditional absorption studies utilize bright background quasars, but this method probes the CGM in a pencil beam, and, due to the rarity of bright quasars, the galaxy population available for study is limited. Large-area, high spectral resolution X-ray microcalorimeters offer a new approach to exploring the CGM in emission and absorption. Here, we demonstrate that the cumulative X-ray emission from cosmic X-ray background sources can probe the CGM in absorption. We construct column density maps of major X-ray ions from the Magneticum simulation and build realistic mock images of nine galaxies to explore the detectability of X-ray absorption lines arising from the large-scale CGM. We conclude that the O VII absorption line is detectable around individual massive galaxies at the 3 σ –6 σ confidence level. For Milky Way–type galaxies, the O VII and O VIII absorption lines are detectable at the ∼ 6 σ and ∼ 3 σ levels even beyond the virial radius when coadding data from multiple galaxies. This approach complements emission studies, does not require additional exposures, and will allow for probing the baryon budget and the CGM at the largest scales.
Published: 2023
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6. Line Emission Mapper Probing Physics of Cosmic Ecosystems

Author: Ralph Kraft, Maxim Markevitch, Caroline Kilbourne, Joseph S. Adams, Hiroki Akamatsu, Mohammadreza Ayromlou, Simon R. Bandler, Douglas A. Bennett, Anil Bhardwaj, Veronica Biff, Dennis Bodewits, Ákos Bogdán, Massimiliano Bonamente, Stefano Borgani, Graziella Branduardi-Raymont, Joel N. Bregman, Joseph N. Burchett, Jenna Cann, Jenny Carter, Priyanka Chakraborty, Eugene Churazov, Robert A. Crain, Renata Cumbee, Romeel Davé, Michael DiPirro, Klaus Dolag, W. Bertrand Doriese, Jeremy Drake, William Dunn, Megan Eckart, Edmund Hodges-Kluck, Amir Jahromi, Richard L. Kelley, Maurice Leutenegger, François Mernier, Michela Negro, Anna Ogorzałek, Ryan W. Pfeifle, Frederick S. Porter, Kazuhiro Sakai, Stephen J. Smith, Kimberly Weaver, and William W. Zhang
Subjects: Instrumentation and Photography, Astrophysics
Abstract: The Line Emission Mapper (LEM) is an X-ray Probe for the 2030s that will answer the outstanding questions of the Universe’s structure formation. It will also provide transformative new observing capabilities for every area of astrophysics, and to heliophysics and planetary physics as well. LEM’s main goal is a comprehensive look at the physics of galaxy formation, including stellar and black-hole feedback and flows of baryonic matter into and out of galaxies. These processes are best studied in X-rays; as emphasized by the 2020 Decadal Survey, emission-line mapping is the pressing need in this area. LEM will use a large microcalorimeter array/IFU (that builds on Athena XIFU technology developments), covering a 30 × 300 field with 1000 angular resolution, to map the soft Xray line emission from objects that constitute galactic ecosystems. These include supernova remnants, star-forming regions, superbubbles, galactic outflows (such as the Fermi/eROSITA bubbles in the Milky Way and their analogs in other galaxies), the Circumgalactic Medium in the Milky Way and other galaxies, and the Intergalactic Medium at the outskirts and beyond the confines of galaxies and clusters. LEM’s 1–2 eV spectral resolution in the 0.2–2 keV band will make it possible to disentangle the faintest emission lines in those objects from the bright Milky Way foreground, providing groundbreaking measurements of the physics of these plasmas, from temperatures, densities, chemical composition to gas dynamics. While the mission is optimized to provide critical observations that will push our understanding of galaxy formation, LEM will provide transformative capability for all classes of astrophysical objects, from the Earth’s magnetosphere, planets and comets to the interstellar medium and X-ray binaries in nearby galaxies, AGN, and cooling gas in galaxy clusters. In addition to pointed observations, LEM will perform a shallow all-sky survey that will dramatically expand the discovery space.
Published: 2022
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7. Chandra and XMM–Newton observations of A2256: cold fronts, merger shocks, and constraint on the IC emission

Author: Chong Ge, Ruo-Yu Liu, Ming Sun, Heng Yu, Lawrence Rudnick, Jean Eilek, Frazer Owen, Sarthak Dasadia, Mariachiara Rossetti, Maxim Markevitch, Tracy E Clarke, Thomas W Jones, Simona Ghizzardi, Tiziana Venturi, Alexis Finoguenov, and Dominique Eckert
Published: 2020
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8. Resonant scattering of the OVII X-ray emission line in the circumgalactic medium of TNG50 galaxies

Author: Dylan Nelson, Chris Byrohl, Anna Ogorzalek, Maxim Markevitch, Ildar Khabibullin, Eugene Churazov, Irina Zhuravleva, Akos Bogdan, Priyanka Chakraborty, Caroline Kilbourne, Ralph Kraft, Annalisa Pillepich, Arnab Sarkar, Gerrit Schellenberger, Yuanyuan Su, Nhut Truong, Stephan Vladutescu-Zopp, and Nastasha Wijers
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: We study the impact of resonantly scattered X-ray line emission on the observability of the hot circumgalactic medium (CGM) of galaxies. We apply a Monte Carlo radiative transfer post-processing analysis to the high-resolution TNG50 cosmological magnetohydrodynamical galaxy formation simulation. This allows us to model the resonant scattering of OVII(r) X-ray photons within the complex, multi-phase, multi-scale CGM. The resonant transition of the OVII He-like triplet is one of the brightest, and most promising, X-ray emission lines for detecting the hot CGM and measuring its physical properties. We focus on galaxies with stellar masses 10 < log(M*/Msun) < 11 at z ~ 0. After constructing a model for OVII(r) emission from the central galaxy as well as from CGM gas, we forward model these intrinsic photons to derive observable surface brightness maps. We find that scattering significantly boosts the observable OVII(r) surface brightness of the extended and diffuse CGM. This enhancement can be large -- an order of magnitude on average at a distance of 200 projected kpc for high-mass M* = 10^10.7 Msun galaxies. The enhancement is larger for lower mass galaxies, and can even reach a factor of 100, across the extended CGM. Galaxies with higher star formation rates, AGN luminosities, and central OVII(r) luminosities all have larger scattering enhancements, at fixed stellar mass. Our results suggest that next-generation X-ray spectroscopic missions including XRISM, LEM, ATHENA, and HUBS -- which aim to detect the hot CGM in emission -- could specifically target halos with significant enhancements due to resonant scattering., Published in MNRAS. See https://www.lem-observatory.org/ and https://www.tng-project.org/ for more details; 2023MNRAS.522.3665N
Published: 2023

9. An ALMA+ACA measurement of the shock in the Bullet Cluster

Author: Luca Di Mascolo, Tony Mroczkowski, Eugene Churazov, Maxim Markevitch, Kaustuv Basu, Tracy E. Clarke, Mark Devlin, Brian S. Mason, Scott W. Randall, Erik D. Reese, Rashid Sunyaev, and Daniel R. Wik
Subjects: Astronomy, Astrophysics
Abstract: Context: The thermal Sunyaev-Zeldovich (SZ) effect presents a relatively new tool for characterizing galaxy cluster merger shocks, traditionally studied through X-ray observations. Widely regarded as the “textbook example” of a cluster merger bow shock, the western, most-prominent shock front in the Bullet Cluster (1E0657-56) represents the ideal test case for such an SZ study. Aims: We aim to characterize the shock properties using deep, high-resolution interferometric SZ effect observations in combination with priors from an independent X-ray analysis. Methods: Our analysis technique relies on the reconstruction of a parametric model for the SZ signal by directly and jointly fitting data from the Atacama Large Millimeter/submillimeter Array (ALMA) and Atacama Compact Array (ACA) in Fourier space. Results: The ALMA+ACA data are primarily sensitive to the electron pressure difference across the shock front. To estimate the shock Mach number M, this difference can be combined with the value for the upstream electron pressure derived from an independent Chandra X-ray analysis. In the case of instantaneous electron-ion temperature equilibration, we find M = 2.08 (+0.12,−0.12), in ≈ 2.4σ tension with the independent constraint from Chandra, M(X)= 2.74 ± 0.25. The assumption of purely adiabatic electron temperature change across the shock leads to M = 2.53 (+0.33,−0.25), in better agreement with the X-ray estimate M(X) = 2.57 ± 0.23 derived for the same heating scenario. Conclusion: We have demonstrated that interferometric observations of the thermal SZ effect provide constraints on the properties of the shock in the Bullet Cluster that are highly complementary to X-ray observations. The combination of X-ray and SZ data yields a powerful probe of the shock properties, capable of measuring M and addressing the question of electron-ion equilibration in cluster shocks. Our analysis is however limited by systematics related to the overall cluster geometry and the complexity of the post-shock gas distribution. To overcome these limitations, a simultaneous, joint-likelihood analysis of SZ and X-ray data is needed.
Published: 2019
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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. Substructures in the core of Abell 2319

Author: Aurora Simionescu, Norbert Werner, Maxim Markevitch, Yuto Ichinohe, and Q. H. S. Wang
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Brightness, 010308 nuclear & particles physics, Front (oceanography), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, 01 natural sciences, Core (optical fiber), Galaxies: clusters: individual: Abell 2319, Cold front, Space and Planetary Science, X-rays: galaxies: clusters, 0103 physical sciences, Cluster (physics), Ophiuchus, Astrophysics - High Energy Astrophysical Phenomena, Galaxies: clusters: intracluster medium, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract: We analysed the deep archival Chandra observations of the high-temperature galaxy cluster Abell 2319 to investigate the prominent cold front in its core. The main sharp arc of the front shows wiggles, or variations of the radius of the density jump along the arc. At the southern end of the arc is a feature that resembles a Kelvin-Helmholtz (KH) eddy, beyond which the sharp front dissolves. These features suggest that KH instabilities develop at the front. Under this assumption, we can place an upper limit on the ICM viscosity that is several times below the isotropic Spitzer value. Other features include a split of the cold front at its northern edge, which may be another KH eddy. There is a small pocket of hot, less-dense gas inside the cold front, which may indicate a `hole' in the front's magnetic insulation layer that lets the heat from the outer gas to penetrate inside the front. Finally, a large concave brightness feature southwest of the cluster core can be caused by the gasdynamic instabilities. We speculate that it can also be an inner boundary of a giant AGN bubble, similar to that in Ophiuchus. If the latter interpretation is supported by better radio data, this could be a remnant of another extremely powerful AGN outburst., Accepted for publication in MNRAS
Published: 2021

14. Surface brightness discontinuities in radio halos

Author: Andrea Botteon, Maxim Markevitch, Reinout J. van Weeren, Gianfranco Brunetti, and Timothy W. Shimwell
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Dynamical motions in the ICM can imprint distinctive features on X-ray images that map the thermal emission from galaxy clusters, such as sharp surface brightness discontinuities due to shocks and cold fronts. The gas dynamics during cluster mergers may also drive large-scale turbulence in the ICM, which in turn generates extended synchrontron sources known as radio halos. Surface brightness edges have been found numerous times in the thermal gas of clusters based on X-ray observations. In contrast, edges in radio halos have only been observed in a handful of cases. Our goal is to search for new radio surface brightness discontinuities in the ICM. We inspected the images of the Bullet Cluster and the other 25 radio halos reported in the MeerKAT Galaxy Cluster Legacy Survey. To aid the identification of surface brightness discontinuities, we applied a gradient-filtering edge-detection method to the radio images. We find that the adopted filtering technique is helpful in identifying surface brightness edges in radio images, allowing us to identify at least one gradient in half of the radio halos studied. For the Bullet Cluster, we find excellent agreement between the locations of the 4 radio discontinuities detected and the X-ray edges. This similarity informs us that there is substantial interplay between thermal and nonthermal components in galaxy clusters. This interplay is likely due to the frozen-in ICM magnetic field, which mediates the advection of cosmic rays while being dragged by thermal gas flows. We conclude that radio halos are shaped by dynamical motions in the ICM and that they often display surface brightness discontinuities, which appear to be co-located with edges in the thermal gas emission. Our results demonstrate that new and future generations of radio telescopes will provide a complementary approach to X-rays to efficiently detect shocks and cold fronts in the ICM., v2: Matches accepted version in A&A (minor changes, added two new figures) corrected by language editor. Abstract abridged to meet arXiv requirements
Published: 2023

15. Chandra and XMM-Newton observations of A2256: cold fronts, merger shocks, and constraint on the IC emission

Author: Mariachiara Rossetti, Dominique Eckert, Ruo-Yu Liu, Lawrence Rudnick, Chong Ge, Sarthak Dasadia, Tracy E. Clarke, Tiziana Venturi, Ming Sun, Thomas W Jones, Simona Ghizzardi, Heng Yu, Alexis Finoguenov, Maxim Markevitch, Frazer N. Owen, Jean A. Eilek, USA, and Department of Physics
Subjects: DYNAMICS, galaxies: clusters: individual: Abell 2256, galaxies: clusters: intracluster medium, SUBSTRUCTURE, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio relics, 0103 physical sciences, Cluster (physics), Surface brightness, 010303 astronomy & astrophysics, ABELL 2256, TEMPERATURE, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Center (category theory), Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Cold front, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, Astrophysics - High Energy Astrophysical Phenomena, GALAXY CLUSTERS, RADIO RELICS, INTERGALACTIC MEDIUM
Abstract: We present the results of deep Chandra and XMM-Newton observations of a complex merging galaxy cluster Abell 2256 (A2256) that hosts a spectacular radio relic (RR). The temperature and metallicity maps show clear evidence of a merger between the western subcluster (SC) and the primary cluster (PC). We detect five X-ray surface brightness edges. Three of them near the cluster center are cold fronts (CFs): CF1 is associated with the infalling SC; CF2 is located in the east of the PC; and CF3 is to the west of the PC core. The other two edges at cluster outskirts are shock fronts (SFs): SF1 near the RR in the NW has Mach numbers derived from the temperature and the density jumps, respectively, of $M_T=1.62\pm0.12$ and $M_\rho=1.23\pm0.06$; SF2 in the SE has $M_T=1.54\pm0.05$ and $M_\rho=1.16\pm0.13$. In the region of the RR, there is no evidence for the correlation between X-ray and radio substructures, from which we estimate an upper limit for the inverse-Compton emission, and therefore set a lower limit on the magnetic field ($\sim$ 450 kpc from PC center) of $B>1.0\ \mu$G for a single power-law electron spectrum or $B>0.4\ \mu$G for a broken power-law electron spectrum. We propose a merger scenario including a PC, an SC, and a group. Our merger scenario accounts for the X-ray edges, diffuse radio features, and galaxy kinematics, as well as projection effects., Comment: 15 pages, 12 figures, MNRAS in press
Published: 2020

16. Status of x-ray imaging and spectroscopy mission (XRISM)

Author: Yutaka Fujita, Koji Mukai, Peter Shirron, Kumiko K. Nobukawa, Toshiaki Takeshima, Isamu Hatsukade, Richard F. Mushotzky, Brian J. Williams, Greg Brown, Hirofumi Noda, Brian Comber, Maria Diaz-Trigo, Manabu Ishida, Brian R. McNamara, Takahiro Sasaki, M. Ohno, Iurii Babyk, Richard L. Kelley, Sayuri Iga, Hiroshi Nakajima, Yuusuke Uchida, Hiroya Yamaguchi, Caroline A. Kilbourne, Takeshi Go Tsuru, Kosuke Sato, Tsunefumi Mizuno, Ryo Iizuka, Irina Zhuravleva, Shogo B. Kobayashi, Hironori Matsumoto, Matthew Holland, K. Matsuzaki, Makoto Sawada, Laura Brenneman, Susumu Yasuda, Shinya Yamada, Makoto Tashiro, Hirokazu Odaka, Yoshihiro Ueda, Keiichi Yanagase, Hiroki Akamatsu, Yasuharu Sugawara, Akihiro Furuzawa, Nobutaka Bando, Akio Hoshino, Koji Mori, Misaki Mizumoto, Lia Corrales, Katsuhiro Hayashi, Yasushi Fukazawa, Hideki Uchiyama, Hironori Maejima, Robert Petre, Yoshitaka Ishisaki, Teruaki Enoto, Mina Ogawa, Kenichi Toda, Natalie Hell, Shin'ichiro Uno, Tessei Yoshida, Thomas G. Bialas, Maurice A. Leutenegger, Masayuki Ohta, Yang Soong, Elisa Costantini, Kenji Hamaguchi, Shunji Kitamoto, Takafumi Horiuchi, Leslie Hartz, Luigi C. Gallo, Edmund Hodges-Kluck, Renata Cumbee, Yusuke Nishioka, Toshiki Sato, Paul P. Plucinsky, Katja Pottschmidt, Aya Kubota, Ehud Behar, Tom Lockard, Masanobu Ozaki, Kenji Minesugi, Ann Hornschemeier, T. R. Jaffe, Aurora Simionescu, Kazutaka Yamaoka, Stéphane Paltani, Keisuke Tamura, Chris Done, Makoto Yamauchi, Kouichi Hagino, Kosei Ishimura, Akihide Kobayashi, Eric J. Miller, Carlo Ferrigno, Hiromitsu Takahashi, Hiromi Seta, Nathalie Gorter, Cor P. de Vries, Michael J. Sampson, A. E. Szymkowiak, Mark O. Kimball, Gary A. Sneiderman, Dan McCammon, Meng P. Chiao, S. Eguchi, Randall K. Smith, Naoki Ishihama, Yohko Tsuboi, Jon M. Miller, Erin Kara, Takayoshi Kohmura, Timothy R. Kallman, Takashi Okajima, Kenichiro Nigo, Jan-Willem den Herder, Shigeo Yamauchi, Kazunori Someya, Maxim Markevitch, Yuto Ichinohe, M. C. Witthoeft, Yukikatsu Terada, Nasa Yoshioka, Edgar Canavan, Jelle Kaastra, Takao Kitaguchi, Masahiro Tsujimoto, Hideto Nakamura, Shinji Mitani, Hiroyuki Uchida, Masayoshi Nobukawa, R. Sato, Atsushi Tanimoto, Junko S. Hiraga, Keisuke Shinozaki, Yuichiro Ezoe, Hiroshi Tsunemi, Brian McLaughlin, Yasuko Shibano, Ikuyuki Mitsuishi, Matteo Guainazzi, Lillian Reichenthal, Yuichi Terashima, Kumi Ishikawa, Naomi Ota, Chikara Natsukari, Joseph Miko, Kiyoshi Hayashida, M. Loewenstein, Connor Martz, Tahir Yaqoob, D. Eckert, Ryuichi Fujimoto, Johannes Dercksen, Hiroshi Murakami, Hiroshi Tomida, Ken Ebisawa, Rob Wolfs, Martin Grim, Tomomi Watanabe, Marc Audard, Keisuke Sugawara, Yoh Takei, Megan E. Eckart, Takaya Ohashi, Atsushi Okamoto, Noriko Y. Yamasaki, Shin Watanabe, Yoshitomo Maeda, Shuhei Shigeto, Yoshitaka Arai, Maki Shida, Hisamitsu Awaki, Muzi Li, Takaaki Tanaka, Tadayasu Dotani, David Hawthorn, Jacco Vink, Joy Henegar-Leon, Rozenn Boissay-Malaquin, Kazuhiro Nakazawa, Aya Bamba, Megumi Shidatsu, Satoru Katsuda, Liyi Gu, Kyoko Matsushita, Toru Tamagawa, F. Scott Porter, Michael J. DiPirro, Steven Kenyon, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Sun sensor, Cardinal point, Spacecraft, Robustness (computer science), Computer science, business.industry, Survivability, Control reconfiguration, Field of view, Aerospace engineering, business, Fault detection and isolation
Abstract: The X-Ray Imaging and Spectroscopy Mission (XRISM) is the successor to the 2016 Hitomi mission that ended prematurely. Like Hitomi, the primary science goals are to examine astrophysical problems with precise highresolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. XRISM carries a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly and a co-aligned X-ray CCD camera that covers the same energy band over a large field of view. XRISM utilizes Hitomi heritage, but all designs were reviewed. The attitude and orbit control system were improved in hardware and software. The number of star sensors were increased from two to three to improve coverage and robustness in onboard attitude determination and to obtain a wider field of view sun sensor. The fault detection, isolation, and reconfiguration (FDIR) system was carefully examined and reconfigured. Together with a planned increase of ground support stations, the survivability of the spacecraft is significantly improved.
Published: 2020

17. Digging up a dinosaur in a galaxy cluster

Author: Maxim Markevitch
Subjects: Digging, Astronomy, Geology, Galaxy cluster
Published: 2020

18. Discovery of a giant radio fossil in the Ophiuchus galaxy cluster

Author: Simona Giacintucci, Tracy Clarke, Melanie Johnston-Hollitt, Maxim Markevitch, Daniel R. Wik, and Q. H. S. Wang
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Asymmetry, Radio spectrum, 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Astronomy and Astrophysics, Observable, Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Ophiuchus, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Ophiuchus galaxy cluster exhibits a curious concave gas density discontinuity at the edge of its cool core. It was discovered in the Chandra X-ray image by Werner and collaborators, who considered a possibility of it being a boundary of an AGN-inflated bubble located outside the core, but discounted this possibility because it required much too powerful an AGN outburst. Using low-frequency (72-240 MHz) radio data from MWA GLEAM and GMRT, we found that the X-ray structure is, in fact, a giant cavity in the X-ray gas filled with diffuse radio emission with an extraordinarily steep radio spectrum. It thus appears to be a very aged fossil of the most powerful AGN outburst seen in any galaxy cluster ($pV\sim 5\times 10^{61}$ erg for this cavity). There is no apparent diametrically opposite counterpart either in X-ray or in the radio. It may have aged out of the observable radio band because of the cluster asymmetry. At present, the central AGN exhibits only a weak radio source, so it should have been much more powerful in the past to have produced such a bubble. The AGN is currently starved of accreting cool gas because the gas density peak is displaced by core sloshing. The sloshing itself could have been set off by this extraordinary explosion if it had occurred in an asymmetric gas core. This dinosaur may be an early example of a new class of sources to be uncovered by low-frequency surveys of galaxy clusters., Comment: 18 pages, 12 figures, accepted for publication in ApJ
Published: 2020
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19. How merger-driven gas motions in galaxy clusters can turn AGN bubbles into radio relics

Author: John ZuHone, Paul Nulsen, Maxim Markevitch, Rainer Weinberger, and Kristian Ehlert
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Front (oceanography), FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Plasma, Astrophysics, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio relics, Space and Planetary Science, Intracluster medium, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Radio relics in galaxy clusters are extended synchrotron sources produced by cosmic-ray electrons in the $\mu$G magnetic field. Many relics are found in the cluster periphery and have a cluster-centric, narrow arc-like shape, which suggests that the electrons are accelerated or re-accelerated by merger shock fronts propagating outward in the intracluster plasma. In the X-ray, some relics do exhibit such shocks at the location of the relic, but many do not. We explore the possibility that radio relics trace not the shock fronts but the shape of the underlying distribution of seed relativistic electrons, lit up by a recent shock passage. We use magnetohydrodynamic simulations of cluster mergers and include bubbles of relativistic electrons injected by jets from the central AGN or from an off-center radio galaxy. We show that the merger-driven gas motions (a) can advect the bubble cosmic rays to very large radii, and (b) spread the relativistic seed electrons preferentially in tangential direction -- along the gravitational equipotential surfaces -- producing extended, filamentary or sheet-like regions of intracluster plasma enriched with aged cosmic rays, which resemble radio relics. Once a shock front passes across such a region, the sharp radio emission edges would trace the sharp boundaries of these enriched regions rather than the front. We also show that these elongated cosmic ray features are naturally associated with magnetic fields stretched tangentially along their long axis, which could help explain the high polarization of relics., Comment: 18 pages, 13 figures, accepted by ApJ
Published: 2020
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20. Editorial to the Topical Collection on Clusters of Galaxies: Physics and Cosmology

Author: Jelle Kaastra, Maxim Markevitch, Maurizio Falanga, Marcus Brüggen, A. M. Bykov, and F. B. S. Paerels
Subjects: Physics, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Galaxy, Cosmology
Published: 2019

21. Expanding the Sample of Radio Minihalos in Galaxy Clusters

Author: Tracy Clarke, Simona Giacintucci, V. Cuciti, Rossella Cassano, Maxim Markevitch, Tiziana Venturi, and Ruta Kale
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Sample (material), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Positive correlation, 01 natural sciences, Luminosity, Cold front, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, 0105 earth and related environmental sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Radio minihalos are diffuse synchrotron sources of unknown origin found in the cool cores of some galaxy clusters. We use GMRT and VLA data to expand the sample of minihalos by reporting three new minihalo detections (A 2667, A 907 and PSZ1 G139.61+24.20) and confirming minihalos in five clusters (MACS J0159.8-0849, MACS J0329.6-0211, RXC J2129.6+0005, AS 780 and A 3444). With these new detections and confirmations, the sample now stands at 23, the largest sample to date. For consistency, we also reanalyze archival VLA 1.4 GHz observations of 7 known minihalos. We revisit possible correlations between the non-thermal emission and the thermal properties of their cluster hosts. Consistently with our earlier findings from a smaller sample, we find no strong relation between the minihalo radio luminosity and the total cluster mass. Instead, we find a strong positive correlation between the minihalo radio power and X-ray bolometric luminosity of the cool core (r, 37 pages, 16 figures, 8 tables, accepted for publication in The Astrophysical Journal
Published: 2019

22. An ALMA+ACA measurement of the shock in the Bullet Cluster

Author: Rashid Sunyaev, Eugene Churazov, Erik D. Reese, Tony Mroczkowski, Maxim Markevitch, Brian Mason, Daniel R. Wik, Luca Di Mascolo, Scott W. Randall, Mark J. Devlin, Tracy Clarke, Kaustuv Basu, Di Mascolo, L., Mroczkowski, T., Churazov, E., Markevitch, M., Basu, K., Clarke, T. E., Devlin, M., Mason, B. S., Randall, S. W., Reese, E. D., Sunyaev, R., and Wik, D. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Cosmic background radiation, FOS: Physical sciences, Context (language use), Galaxies: clusters: individual: 1E 0657-56, Galaxies: clusters: intracluster medium, Astrophysics, clusters: individual: 1E 0657-56 [Galaxies], clusters: intracluster medium [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Submillimeter Array, 010104 statistics & probability, 0103 physical sciences, Cluster (physics), Bow shock (aerodynamics), 0101 mathematics, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astronomy and Astrophysics, Galaxy, Shock (mechanics), Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The thermal Sunyaev-Zeldovich (SZ) effect presents a relatively new tool for characterizing galaxy cluster merger shocks, traditionally studied through X-ray observations. Widely regarded as the "textbook example" of a cluster merger bow shock, the western shock front in the Bullet Cluster (1E0657-56) represents the ideal test case for such an SZ study. We aim to reconstruct a parametric model for the shock SZ signal by directly and jointly fitting deep, high-resolution interferometric data from the Atacama Large Millimeter/submillimeter Array (ALMA) and Atacama Compact Array (ACA) in Fourier space. The ALMA+ACA data are primarily sensitive to the electron pressure difference across the shock front. To estimate the shock Mach number $M$, this difference can be combined with the value for the upstream electron pressure derived from an independent Chandra X-ray analysis. In the case of instantaneous electron-ion temperature equilibration, we find $M=2.08^{+0.12}_{-0.12}$, in $\approx 2.4\sigma$ tension with the independent constraint from Chandra, $M_X=2.74\pm0.25$. The assumption of purely adiabatic electron temperature change across the shock leads to $M=2.53^{+0.33}_{-0.25}$, in better agreement with the X-ray estimate $M_X=2.57\pm0.23$ derived for the same heating scenario. We have demonstrated that interferometric observations of the SZ effect provide constraints on the properties of the shock in the Bullet Cluster that are highly complementary to X-ray observations. The combination of X-ray and SZ data yields a powerful probe of the shock properties, capable of measuring $M$ and addressing the question of electron-ion equilibration in cluster shocks. Our analysis is however limited by systematics related to the overall cluster geometry and the complexity of the post-shock gas distribution. To overcome these limitations, a joint analysis of SZ and X-ray data is needed., Comment: 9 pages (including appendices), 5 figures, and 1 table; accepted for publication in A&A
Published: 2019

23. 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

24. Concept of the X-ray Astronomy Recovery Mission

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

25. 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

26. Bow shock in merging cluster A520: the edge of the radio halo and the electron-ion equilibration timescale

Author: Simona Giacintucci, Qian H. S. Wang, and Maxim Markevitch
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Shock (fluid dynamics), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Electron, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Mach number, Radio halo, Space and Planetary Science, 0103 physical sciences, symbols, Electron temperature, Bow shock (aerodynamics), Adiabatic process, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We studied the prominent bow shock in the merging galaxy cluster A520 using a deep Chandra X-ray observation and archival VLA radio data. This shock is a useful diagnostic tool, owing to its clear geometry and relatively high Mach number. At the "nose" of the shock, we measure a Mach number of $M=2.4_{-0.2}^{+0.4}$. The shock becomes oblique away from the merger axis, with the Mach number falling to $\simeq$1.6 around 30$^{\circ}$ from the nose. The electron temperature immediately behind the shock nose is consistent with that from the Rankine-Hugoniot adiabat, and is higher (at a 95% confidence) than expected for adiabatic compression of electrons followed by Coulomb electron-proton equilibration, indicating the presence of equilibration mechanisms faster than Coulomb collisions. This is similar to an earlier finding for the Bullet cluster. We also combined four archival VLA datasets to obtain a better image of the cluster's giant radio halo at 1.4 GHz. An abrupt edge of the radio halo traces the shock front, and no emission is detected in the pre-shock region. If the radio edge were due only to adiabatic compression of relativistic electrons in pre-shock plasma, we would expect a pre-shock radio emission detectable in this radio dataset; however, an interferometric artifact dominates the uncertainty, so we cannot rule this model out. Other interesting features of the radio halo include a peak at the remnant of the cool core, suggesting that the core used to have a radio minihalo, and a peak marking a possible region of high turbulence., 13 pages, 6 figures (v1: revised submission accepted by ApJ; v2: fixed typos, better quality for image figures)
Published: 2018

27. 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

28. 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

29. A Deep X-Ray Look At Abell 2142 --- Viscosity Constraints From Kelvin-Helmholtz Eddies, A Displaced Cool Peak That Makes A Warm Core, And A Possible Plasma Depletion Layer

Author: Maxim Markevitch and Q. D. Wang
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Brightness, 010308 nuclear & particles physics, Front (oceanography), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gravitational potential, Viscosity, Cold front, Amplitude, Space and Planetary Science, 0103 physical sciences, Brightest cluster galaxy, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We analyzed 200 ks of Chandra ACIS observations of the merging galaxy cluster A2142 to examine its prominent cold fronts in detail. We find that the southern cold front exhibits well-developed Kelvin-Helmholtz (KH) eddies seen in the sky plane. Comparing their wavelength and amplitude with those in hydrodynamic simulations of cold fronts in viscous gas, and estimating the gas tangential velocity from centripetal acceleration, we constrain the effective viscosity to be at most 1/5 of Spitzer isotropic viscosity, but consistent with full Braginskii anisotropic viscosity for magnetized plasma. While the northwestern front does not show obvious eddies, its shape and the structure of its brightness profile suggest KH eddies seen in projection. The southern cold front continues in a spiral to the center of the cluster, ending with another cold front only 12 kpc from the gas density peak. The cool peak itself is displaced ~30 kpc from the BCG (the biggest such offset among centrally-peaked clusters), while the X-ray emission on a larger scale is still centered on the BCG, indicating that the BCG is at the center of the gravitational potential and the cool gas is sloshing in it. The specific entropy index of the gas in the peak ($K\approx49$ keV cm$^2$) makes A2142 a rare "warm core"; apparently the large displacement of the cool peak by sloshing is the reason. Finally, we find a subtle narrow, straight channel with a 10% drop in X-ray brightness, aligned with the southern cold front --- possibly a plasma depletion layer in projection., Comment: 15 pages, 6 figures. Submitted to ApJ
Published: 2018
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30. 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

31. 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

32. 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

33. Another shock for the Bullet cluster, and the source of seed electrons for radio relics

Author: Shea Brown, Bryan Gaensler, Luigina Feretti, Melanie Johnston-Hollitt, Maxim Markevitch, Raghav Srinivasan, Timothy W. Shimwell, and Craig S. Lage
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Shock wave, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Shock (mechanics), Radio relics, Relativistic plasma, Space and Planetary Science, Intracluster medium, Surface brightness, Bow shock (aerodynamics), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: With Australia Telescope Compact Array observations, we detect a highly elongated Mpc-scale diffuse radio source on the eastern periphery of the Bullet cluster 1E0657-55.8, which we argue has the positional, spectral and polarimetric characteristics of a radio relic. This powerful relic (2.3+/-0.1 x 10^25 W Hz^-1) consists of a bright northern bulb and a faint linear tail. The bulb emits 94% of the observed radio flux and has the highest surface brightness of any known relic. Exactly coincident with the linear tail we find a sharp X-ray surface brightness edge in the deep Chandra image of the cluster -- a signature of a shock front in the hot intracluster medium (ICM), located on the opposite side of the cluster to the famous bow shock. This new example of an X-ray shock coincident with a relic further supports the hypothesis that shocks in the outer regions of clusters can form relics via diffusive shock (re-)acceleration. Intriguingly, our new relic suggests that seed electrons for reacceleration are coming from a local remnant of a radio galaxy, which we are lucky to catch before its complete disruption. If this scenario, in which a relic forms when a shock crosses a well-defined region of the ICM polluted with aged relativistic plasma -- as opposed to the usual assumption that seeds are uniformly mixed in the ICM -- is also the case for other relics, this may explain a number of peculiar properties of peripheral relics., 10 pages, 9 figures, 1 table, accepted for publication in MNRAS
Published: 2015

34. 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

35. Occurrence of radio minihalos in a mass-limited sample of galaxy clusters

Author: Maxim Markevitch, Tiziana Venturi, Gianfranco Brunetti, Simona Giacintucci, Rossella Cassano, and Tracy Clarke
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Galaxy groups and clusters, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Halo, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Radio astronomy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the occurrence of radio minihalos --- diffuse radio sources of unknown origin observed in the cores of some galaxy clusters --- in a statistical sample of 58 clusters drawn from the Planck Sunyaev-Zel'dovich cluster catalog using a mass cut ($M_{500}>6\times 10^{14} M_{\odot}$). We supplement our statistical sample with a similarly-sized non-statistical sample mostly consisting of clusters in the ACCEPT X-ray catalog with suitable X-ray and radio data, which includes lower-mass clusters. Where necessary (for 9 clusters), we reanalyzed the Very Large Array archival radio data to determine if a mihinalo is present. Our total sample includes all 28 currently known and recently discovered radio minihalos, including 6 candidates. We classify clusters as cool-core or non-cool core according to the value of the specific entropy floor in the cluster center, rederived or newly derived from the Chandra X-ray density and temperature profiles where necessary (for 27 clusters). Contrary to the common wisdom that minihalos are rare, we find that almost all cool cores - at least 12 out of 15 (80%) - in our complete sample of massive clusters exhibit minihalos. The supplementary sample shows that the occurrence of minihalos may be lower in lower-mass cool-core clusters. No minihalos are found in non-cool-cores or "warm cores". These findings will help test theories of the origin of minihalos and provide information on the physical processes and energetics of the cluster cores., 34 pages, accepted for publication in ApJ. Added a section "Definition of a minihalo" and an appendix "Radio size and average surface brigthtness of minihalos and halos"
Published: 2017

36. In-flight verification of the calibration and performance of the ASTRO-H (Hitomi) Soft X-Ray Spectrometer

Author: Hideyuki Mori, Satoshi Sugita, Shinya Yamada, Dan McCammon, Ryuichi Fujimoto, Megan E. Eckart, Yoshitaka Ishisaki, Manabu Ishida, Cor P. de Vries, Sho Kurashima, Maurice A. Leutenegger, Richard L. Kelley, Naomichi Kikuchi, Peter J. Serlemitsos, Nozomi Nakaniwa, Yoh Takei, Kosuke Sato, Jan-Willem den Herder, Noriko Y. Yamasaki, Hiromi Seta, Gregory V. Brown, Kazuhisa Mitsuda, Meng P. Chiao, Kevin R. Boyce, Gary A. Sneiderman, Caroline A. Kilbourne, Maxim Markevitch, Masahiro Tsujimoto, Yoshitomo Maeda, Shu Koyama, Toshiki Sato, Yuzuru Tawara, F. Scott Porter, Matteo Guainazzi, Yang Soong, Stéphane Paltani, Takayuki Hayashi, Makoto Tashiro, D. Haas, Tomomi Watanabe, Marc Audard, Andrew Szymkowiak, Robert Petre, Makoto Sawada, Takashi Okajima, Akihiro Furuzawa, and Ryo Iizuka
Subjects: Physics, Spectrometer, Physics::Instrumentation and Detectors, business.industry, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 01 natural sciences, law.invention, Telescope, Optics, Pulsar, Observatory, law, 0103 physical sciences, Calibration, Spectral resolution, 010306 general physics, business, 010303 astronomy & astrophysics, Remote sensing
Abstract: The Soft X-ray Spectrometer (SXS) onboard the Astro-H (Hitomi) orbiting x-ray observatory featured an array of 36 silicon thermistor x-ray calorimeters optimized to perform high spectral resolution x-ray imaging spectroscopy of astrophysical sources in the 0.3-12 keV band. Extensive pre- flight calibration measurements are the basis for our modeling of the pulse-height-energy relation and energy resolution for each pixel and event grade, telescope collecting area, detector efficiency, and pulse arrival time. Because of the early termination of mission operations, we needed to extract the maximum information from observations performed only days into the mission when the onboard calibration sources had not yet been commissioned and the dewar was still coming into thermal equilibrium, so our technique for reconstructing the per-pixel time-dependent pulse-height-energy relation had to be modified. The gain scale was reconstructed using a combination of an absolute energy scale calibration at a single time using a fiducial from an onboard radioactive source, and calibration of a dominant time-dependent gain drift component using a dedicated calibration pixel, as well as a residual time-dependent variation using spectra from the Perseus cluster of galaxies. The energy resolution was also measured using the onboard radioactive sources. It is consistent with instrument-level measurements accounting for the modest increase in noise due to spacecraft systems interference. We use observations of two pulsars to validate our models of the telescope area and detector efficiency, and to derive a more accurate value for the thickness of the gate valve Be window, which had not been opened by the time mission operations ceased. We use observations of the Crab pulsar to refine the pixel-to-pixel timing and validate the absolute timing.
Published: 2016

37. Searching for the 3.5 keV Line in the Stacked Suzaku Observations of Galaxy Clusters

Author: M. Loewenstein, Maxim Markevitch, Scott W. Randall, Esra Bulbul, Randall K. Smith, Adam R. Foster, Eric L. Miller, and Mark W. Bautz
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Andromeda Galaxy, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Galactic Center, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Redshift, Galaxy groups and clusters, Space and Planetary Science, 0103 physical sciences, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Line (formation), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a detailed study of the stacked Suzaku observations of 47 galaxy clusters, spanning a redshift range of 0.01-0.45, to search for the unidentified 3.5 keV line. This sample provides an independent test for the previously detected line. We detect only a 2sigma-significant spectral feature at 3.5 keV in the spectrum of the full sample. When the sample is divided into two subsamples (cool-core and non-cool core clusters), cool-core subsample shows no statistically significant positive residuals at the line energy. A very weak (2sigma-confidence) spectral feature at 3.5 keV is permitted by the data from the non-cool core clusters sample. The upper limit on a neutrino decay mixing angle from the full Suzaku sample is consistent with the previous detections in the stacked XMM-Newton sample of galaxy clusters (which had a higher statistical sensitivity to faint lines), M31, and Galactic Center at a 90% confidence level. However, the constraint from the present sample, which does not include the Perseus cluster, is in tension with previously reported line flux observed in the core of the Perseus cluster with XMM-Newton and Suzaku., ApJ in press, 9 pages, 3 figures
Published: 2016

38. The Efficiency of Magnetic Field Amplification at Shocks by Turbulence

Author: S. Peng Oh, Suoqing Ji, Mateusz Ruszkowski, and Maxim Markevitch
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Field strength, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Vorticity, 01 natural sciences, Magnetic field, Supernova, Radio relics, Space and Planetary Science, 0103 physical sciences, Physics::Space Physics, Magnetohydrodynamics, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Dynamo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Turbulent dynamo field amplification has often been invoked to explain the strong field strengths in thin rims in supernova shocks ($\sim 100 \, \mu$G) and in radio relics in galaxy clusters ($\sim \mu$G). We present high resolution MHD simulations of the interaction between pre-shock turbulence, clumping and shocks, to quantify the conditions under which turbulent dynamo amplification can be significant. We demonstrate numerically converged field amplification which scales with Alfv\'en Mach number, $B/B_0 \propto {\mathcal M}_{\rm A}$, up to ${\mathcal M}_{\rm A} \sim 150$. This implies that the post-shock field strength is relatively independent of the seed field. Amplification is dominated by compression at low ${\mathcal M}_{\rm A}$, and stretching (turbulent amplification) at high ${\mathcal M}_{\rm A}$. For high $\mathcal{M}_{\rm A}$, the $B$-field grows exponentially and saturates at equipartition with turbulence, while the vorticity jumps sharply at the shock and subsequently decays; the resulting field is orientated predominately along the shock normal (an effect only apparent in 3D and not 2D). This agrees with the radial field bias seen in supernova remnants. By contrast, for low $\mathcal{M}_{\rm A}$, field amplification is mostly compressional, relatively modest, and results in a predominantly perpendicular field. The latter is consistent with the polarization seen in radio relics. Our results are relatively robust to the assumed level of gas clumping. Our results imply that the turbulent dynamo may be important for supernovae, but is only consistent with the field strength, and not geometry, for cluster radio relics. For the latter, this implies strong pre-existing $B$-fields in the ambient cluster outskirts., Comment: 15 pages, 11 figures, published version on MNRAS
Published: 2016

39. Radial Profile of the 3.5 keV Line Out to R200 in the Perseus Cluster

Author: Michael McDonald, Oleg Ruchayskiy, Esra Bulbul, Eric J. Miller, Mark W. Bautz, Adam R. Foster, Randall K. Smith, Maxim Markevitch, Dmytro Iakubovskyi, Jeroen Franse, Alexey Boyarsky, M. Loewenstein, and Scott W. Randall
Subjects: Physics, Brightness, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Galaxy groups and clusters, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Emission spectrum, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract: The recent discovery of the unidentified emission line at 3.5 keV in galaxies and clusters has attracted great interest from the community. As the origin of the line remains uncertain, we study the surface brightness distribution of the line in the Perseus cluster since that information can be used to identify its origin. We examine the flux distribution of the 3.5 keV line in the deep Suzaku observations of the Perseus cluster in detail. The 3.5 keV line is observed in three concentric annuli in the central observations, although the observations of the outskirts of the cluster did not reveal such a signal. We establish that these detections and the upper limits from the non-detections are consistent with a dark matter decay origin. However, absence of positive detection in the outskirts is also consistent with some unknown astrophysical origin of the line in the dense gas of the Perseus core, as well as with a dark matter origin with a steeper dependence on mass than the dark matter decay. We also comment on several recently published analyses of the 3.5 keV line.
Published: 2016

40. A STRONG MERGER SHOCK in ABELL 665

Author: Gabriele Giovannini, Andrea Morandi, Valentina Vacca, Ming Sun, Craig L. Sarazin, Sarthak Dasadia, Maxim Markevitch, Federica Govoni, Daniel R. Wik, Luigina Feretti, Dasadia, S., Sun, M., Sarazin, C., Morandi, A., Markevitch, M., Wik, D., Feretti, L., Giovannini, G., Govoni, F., and Vacca, V.
Subjects: Shock wave, shock wave, Astrophysics::High Energy Astrophysical Phenomena, radio continuum: general, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Galaxy groups and clusters, 0103 physical sciences, galaxies: clusters: individual (Abell 665), 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Front (oceanography), Astronomy and Astrophysics, Astronomy and Astrophysic, X-rays: galaxies: cluster, Shock (mechanics), Cold front, Radio halo, Mach number, galaxies: clusters: general, Space and Planetary Science, symbols, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Deep (103 ks) \chandra\ observations of Abell 665 have revealed rich structures in this merging galaxy cluster, including a strong shock and two cold fronts. The newly discovered shock has a Mach number of $M$ = 3.0 $\pm$ 0.6, propagating in front of a cold disrupted cloud. This makes Abell~665 the second cluster where a strong merger shock of $M \approx$ 3 has been detected, after the Bullet cluster. The shock velocity from jump conditions is consistent with (2.7 $\pm$ 0.7) $\times$ 10$^3$ km sec$^{-1}$. The new data also reveal a prominent southern cold front, with potentially heated gas ahead of it. Abell 665 also hosts a giant radio halo. There is a hint of diffuse radio emission extending to the shock at the north, which needs to be examined with better radio data. This new strong shock provides a great opportunity to study the re-acceleration model with the X-ray and radio data combined., Accepted for publication in ApJL
Published: 2016

41. 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

42. Searching for decaying dark matter in deep XMM-Newton observation of the Draco dwarf spheroidal

Author: Esra Bulbul, Oleg Ruchayskiy, Andrii Neronov, Alexey Boyarsky, Jeroen Franse, Dominique Eckert, Maxim Markevitch, Dmytro Iakubovskyi, and Denys Malyshev
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Dwarf galaxy problem, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, dark matter, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Hot dark matter, Astronomy, Astronomy and Astrophysics, galaxies: dwarf, Galaxy, Dwarf spheroidal galaxy, Dark matter halo, High Energy Physics - Phenomenology, Space and Planetary Science, Dark galaxy, Astrophysics - High Energy Astrophysical Phenomena, line: identification
Abstract: We present results of a search for the 3.5 keV emission line in our recent very long (~ 1.4 Ms) XMM-Newton observation of the Draco dwarf spheroidal galaxy. The astrophysical X-ray emission from such dark matter-dominated galaxies is faint, thus they provide a test for the dark matter origin of the 3.5 keV line previously detected in other massive, but X-ray bright objects, such as galaxies and galaxy clusters. We do not detect a statistically significant emission line from Draco; this constrains the lifetime of a decaying dark matter particle to tau > (7-9) x 10^27 s at 95% CL (combining all three XMM-Newton cameras; the interval corresponds to the uncertainty of the dark matter column density in the direction of Draco). The PN camera, which has the highest sensitivity of the three, does show a positive spectral residual (above the carefully modeled continuum) at E = 3.54 +/- 0.06 keV with a 2.3 sigma significance. The two MOS cameras show less-significant or no positive deviations, consistently within 1 sigma with PN. Our Draco limit on tau is consistent with previous detections in the stacked galaxy clusters, M31 and the Galactic Center within their 1-2 sigma uncertainties, but is inconsistent with the high signal from the core of the Perseus cluster (which has itself been inconsistent with the rest of the detections). We conclude that this Draco observation does not exclude the dark matter interpretation of the 3.5 keV line in those objects., 10 pages, 5 figures. Accepted by MNRAS
Published: 2015

43. Structures and components in galaxy clusters: observations and models

Author: A. M. Bykov, E. M. Churazov, Jelle Kaastra, William R. Forman, J. de Plaa, Maxim Markevitch, Chiara Ferrari, and U. Klein
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Relativistic plasma, Space and Planetary Science, Halo, Spectroscopy, Astrophysics - High Energy Astrophysical Phenomena, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Clusters of galaxies are the largest gravitationally bounded structures in the Universe dominated by dark matter. We review the observational appearance and physical models of plasma structures in clusters of galaxies. Bubbles of relativistic plasma which are inflated by supermassive black holes of AGNs, cooling and heating of the gas, large scale plasma shocks, cold fronts, non-thermal halos and relics are observed in clusters. These constituents are reflecting both the formation history and the dynamical properties of clusters of galaxies. We discuss X-ray spectroscopy as a tool to study the metal enrichment in clusters and fine spectroscopy of Fe X-ray lines as a powerful diagnostics of both the turbulent plasma motions and the energetics of the non-thermal electron populations. The knowledge of the complex dynamical and feedback processes is necessary to understand the energy and matter balance as well as to constrain the role of the non-thermal components of clusters., 55 pages, 24 pages
Published: 2015

44. CORE GAS SLOSHING IN ABELL 1644

Author: William R. Forman, Ryan Johnson, Christine Jones, Maxim Markevitch, and Gary Wegner
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Slosh dynamics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Potential energy, Electromagnetic radiation, Galaxy, Cold front, Space and Planetary Science, Surface brightness, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an analysis of a 72 ks Chandra observation of the double cluster Abell 1644 (z=0.047). The X-ray temperatures indicate the masses are M500=2.6+/-0.4 x10^{14} h^{-1} M_sun for the northern subcluster and M500=3.1+/-0.4 x10^{14} h^{-1} M_sun for the southern, main cluster. We identify a sharp edge in the radial X-ray surface brightness of the main cluster, which we find to be a cold front, with a jump in temperature of a factor of ~3. This edge possesses a spiral morphology characteristic of core gas sloshing around the cluster potential minimum. We present observational evidence, supported by hydrodynamic simulations, that the northern subcluster is the object which initiated the core gas sloshing in the main cluster at least 700 Myr ago. We discuss reheating of the main cluster's core gas via two mechanisms brought about by the sloshing gas: first, the release of gravitational potential energy gained by the core's displacement from the potential minimum, and second, a dredging inwards of the outer, higher entropy cluster gas along finger-shaped streams. We find the available gravitational potential energy is small compared to the energy released by the cooling gas in the core., Comment: 13 pages, 9 figures, Accepted for publication in The Astrophysical Journal, 1/9/2010
Published: 2010

45. Comparative analysis of the diffuse radio emission in the galaxy clusters A1835, A2029, and Ophiuchus

Author: Matteo Murgia, L. Feretti, G. B. Taylor, Maxim Markevitch, Gabriele Giovannini, Federica Govoni, Ettore Carretti, Murgia M., Govoni F., Markevitch M., Feretti L., Giovannini G., Taylor G.B., and Carretti E.
Subjects: Physics, Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Radio halo, Space and Planetary Science, Emissivity, Ophiuchus, Halo, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We recently performed a study of a sample of relaxed, cooling core galaxy clusters with deep Very Large Array observations at 1.4 GHz. We find that in the central regions of A1835, A2029, and Ophiuchus the dominant radio galaxy is surrounded by a diffuse low-brightness radio emission that takes the form of a mini-halo. Here we present the results of the analysis of the extended diffuse radio emission in these mini-halos. In order to investigate the morphological properties of the diffuse radio emission in clusters of galaxies we propose to fit their azimuthally averaged brightness profile with an exponential, obtaining the central brightness and the e-folding radius from which the radio emissivity can be calculated. We investigate the radio properties of the mini-halos in A1835, A2029, and Ophiuchus in comparison with the radio properties of a representative sample of mini-halos and halos already known in the literature. We find that radio halos can have quite different length-scales but their emissivity is remarkably similar from one halo to the other. In contrast, mini-halos span a wide range of radio emissivity. Some of them, like the Perseus mini-halos, are characterized by a radio emissivity which is more than 100 times greater than that of radio halos. On the other hand, the new mini-halos in cooling core clusters analyzed in this work, namely A2029, Ophiuchus, and A1835, have a radio emissivity which is much more typical of halos in merging clusters rather than similar to that of the other mini-halos previously known., 17 pages, 11 figures, A&A in press. For a version with high quality figures, see http://erg.ca.astro.it/preprints/mini_halo_2/
Published: 2009

46. A MULTIPLY IMAGED LUMINOUS INFRARED GALAXY BEHIND THE BULLET CLUSTER (1E0657-56)

Author: Christine Jones, Dennis Zaritsky, Anthony H. Gonzalez, Marusa Bradac, D. Clowe, and Maxim Markevitch
Subjects: Luminous infrared galaxy, Physics, Stellar mass, Infrared, Strong gravitational lensing, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Luminosity, Photometry (optics), Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present evidence for a Spitzer-selected luminous infrared galaxy (LIRG) behind the Bullet Cluster. The galaxy, originally identified in IRAC photometry as a multiply imaged source, has a spectral energy distribution consistent with a highly extincted (A_V~3.3), strongly star-forming galaxy at z=2.7. Using our strong gravitational lensing model presented in Bradac et al. (2006), we find that the magnifications are 10 to 50 for the three images of the galaxy. The implied infrared luminosity is consistent with the galaxy being a LIRG, with a stellar mass of M_*~2e11 M_Sun and a star formation rate of ~90 M_Sun/yr. With lensed fluxes at 24 microns of 0.58 mJy and 0.39 mJy in the two brightest images, this galaxy presents a unique opportunity for detailed study of an obscured starburst with star fomation rate comparable to that of L* galaxies at z>2.
Published: 2009

47. Constraints on the Self‐Interaction Cross Section of Dark Matter from Numerical Simulations of the Merging Galaxy Cluster 1E 0657−56

Author: Maxim Markevitch, Scott W. Randall, Anthony H. Gonzalez, Douglas Clowe, and Marusa Bradac
Subjects: Physics, Cold dark matter, Space and Planetary Science, Self-interacting dark matter, Dark matter, Sigma, Strongly interacting massive particle, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Weak gravitational lensing, Galaxy cluster
Abstract: (Abridged) We compare recent results from X-ray, strong lensing, weak lensing, and optical observations with numerical simulations of the merging galaxy cluster 1E0657-56. X-ray observations reveal a bullet-like subcluster with a prominent bow shock, while lensing results show that the positions of the total mass peaks are consistent with the centroids of the collisionless galaxies (and inconsistent with the X-ray brightness peaks). Previous studies, based on older observational datasets, have placed upper limits on the self-interaction cross-section of dark matter per unit mass, sigma/m, using simplified analytic techniques. In this work, we take advantage of new, higher-quality observational datasets by running N-body simulations of 1E0657-56 that include the effects of self-interacting dark matter, and comparing the results with observations. Furthermore, the recent data allow for a new independent method of constraining sigma/m, based on the non-observation of an offset between the bullet subcluster mass peak and galaxy centroid. This new method places an upper limit (68% confidence) of sigma/m < 1.25 cm^2/g. If we make the assumption that the subcluster and the main cluster had equal mass-to-light ratios prior to the merger, we derive our most stringent constraint of sigma/m < 0.7 cm^2/g, which comes from the consistency of the subcluster's observed mass-to-light ratio with the main cluster's, and with the universal cluster value, ruling out the possibility of a large fraction of dark matter particles being scattered away due to collisions. Our limit is a slight improvement over the previous result from analytic estimates, and rules out most of the 0.5 - 5cm^2/g range invoked to explain inconsistencies between the standard collisionless cold dark matter model and observations.
Published: 2008

48. Complex X-ray morphology of Abell 3128: a distant cluster behind a disturbed cluster

Author: Maxim Markevitch, E. M. Churazov, Norbert Werner, Hans Boehringer, R. A. Burenin, Jelle Kaastra, and Alexis Finoguenov
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Type-cD galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, K-line, Galaxy, Redshift, Space and Planetary Science, Supercluster, Cluster (physics), Surface brightness, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract: We present here the results of a detailed study of the X-ray properties of the cluster of galaxies Abell 3128 (z=0.06), based on the analysis of deep (100 ks) XMM-Newton data. The most obvious feature of the X-ray morphology of A3128 is the presence of two X-ray peaks separated by ~12'. By detecting the redshifted Fe K line, we find that the Northeast (NE) X-ray peak observed toward A3128 is a distant luminous cluster of galaxies at redshift z=0.44. Our subsequent optical spectroscopic observation of a distant radio bright galaxy in the centre of the NE X-ray peak with the Magellan telescope also revealed a redshift of z=0.44, confirming the association of the galaxy with the cluster seen in X-rays. We detect a gravitational arc around the galaxy. The properties of this galaxy indicate that it is the cD galaxy of the cluster in the background. The properties of the Southwest X-ray peak suggest that it is the core of a group merging with A3128 along our line of sight. Based on 2D maps of thermodynamic properties of the intra-cluster medium determined after subtracting a model for the background cluster, we conclude that an enhanced surface brightness region at a distance of ~2.8' from the centre of the galaxy distribution is the centre of the gravitational potential of the cluster A3128. The unrelaxed nature of A3128 can be attributed to its location in the high density environment of the Horologium-Reticulum supercluster., Comment: accepted for publication in A&A
Published: 2007

49. Discovery of a giant radio halo in a new Planck galaxy cluster PLCKG171.9-40.7

Author: Maxim Markevitch, Daniel R. Wik, Ruta Kale, Simona Giacintucci, Tiziana Venturi, Simona Giacintucci, Ruta Kale, Daniel R. Wik, Tiziana Venturi, and Maxim Markevitch
Subjects: Physics, Giant Metrewave Radio Telescope, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio spectrum, galaxies: clusters: general, galaxies: clusters: individual (PLCKG171.9-40.7), intergalactic medium, radio continuum: general, X-rays: galaxies: clusters, Galaxy groups and clusters, Radio halo, Space and Planetary Science, Halo, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the discovery of a giant radio halo in a new, hot, X-ray luminous galaxy cluster recently found by Planck, PLCKG171.9-40.7. The radio halo was found using Giant Metrewave Radio Telescope observations at 235 MHz and 610 MHz, and in the 1.4 GHz data from a NRAO Very Large Array Sky Survey pointing that we have reanalyzed. The diffuse radio emission is coincident with the cluster X-ray emission, has an extent of ~1 Mpc and a radio power of ~5x 10^24 W/Hz at 1.4 GHz. Its integrated radio spectrum has a slope of alpha~1.8 between 235 MHz and 1.4 GHz, steeper than that of a typical giant halo. The analysis of the archival XMM-Newton X-ray data shows that the cluster is hot (~10 keV) and disturbed, consistent with X-ray selected clusters hosting radio halos. This is the first giant radio halo discovered in one of the new clusters found by Planck., 9 pages, 8 figures and 4 tables. Corrected Figure 7. Matches ApJ published version
Published: 2013

50. Mapping the Gas Turbulence in the Coma Cluster: Predictions for Astro-H

Author: Irina Zhuravleva, Maxim Markevitch, and John ZuHone
Subjects: Physics, Turbulent diffusion, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Turbulence, Spectral density, Velocity dispersion, FOS: Physical sciences, Astronomy and Astrophysics, Coma (optics), 01 natural sciences, Computational physics, Space and Planetary Science, 0103 physical sciences, Coma Cluster, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Astro-H will be able for the first time to map gas velocities and detect turbulence in galaxy clusters. One of the best targets for turbulence studies is the Coma cluster, due to its proximity, absence of a cool core, and lack of a central active galactic nucleus. To determine what constraints Astro-H will be able to place on the Coma velocity field, we construct simulated maps of the projected gas velocity and compute the second-order structure function, an analog of the velocity power spectrum. We vary the injection scale, dissipation scale, slope, and normalization of the turbulent power spectrum, and apply measurement errors and finite sampling to the velocity field. We find that even with sparse coverage of the cluster, Astro-H will be able to measure the Mach number and the injection scale of the turbulent power spectrum--the quantities determining the energy flux down the turbulent cascade and the diffusion rate for everything that is advected by the gas (metals, cosmic rays, etc.). Astro-H will not be sensitive to the dissipation scale or the slope of the power spectrum in its inertial range, unless they are outside physically motivated intervals. We give the expected confidence intervals for the injection scale and the normalization of the power spectrum for a number of possible pointing configurations, combining the structure function and velocity dispersion data. Importantly, we also determine that measurement errors on the line shift will bias the velocity structure function upward, and show how to correct this bias., Comment: 18 pages, 13 figures. Matches published ApJ version, except that it fixes an error in the left panel of Figure 5 that is being addressed in an ApJ erratum
Published: 2015
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