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1. PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

Author

Miller, M. C., Lamb, F. K., Dittmann, A. J., Bogdanov, S., Arzoumanian, Z., Gendreau, K. C., Guillot, S., Harding, A. K., Ho, W. C. G., Lattimer, J. M., Ludlam, R. M., Mahmoodifar, S., Morsink, S. M., Ray, P. S., Strohmayer, T. E., Wood, K. S., Enoto, T., Foster, R., Okajima, T., Prigozhin, G., and Soong, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Nuclear Theory
Abstract

Neutron stars are not only of astrophysical interest, but are also of great interest to nuclear physicists, because their attributes can be used to determine the properties of the dense matter in their cores. One of the most informative approaches for determining the equation of state of this dense matter is to measure both a star's equatorial circumferential radius $R_e$ and its gravitational mass $M$. Here we report estimates of the mass and radius of the isolated 205.53 Hz millisecond pulsar PSR J0030+0451 obtained using a Bayesian inference approach to analyze its energy-dependent thermal X-ray waveform, which was observed using the Neutron Star Interior Composition Explorer (NICER). This approach is thought to be less subject to systematic errors than other approaches for estimating neutron star radii. We explored a variety of emission patterns on the stellar surface. Our best-fit model has three oval, uniform-temperature emitting spots and provides an excellent description of the pulse waveform observed using NICER. The radius and mass estimates given by this model are $R_e = 13.02^{+1.24}_{-1.06}$ km and $M = 1.44^{+0.15}_{-0.14}\ M_\odot$ (68%). The independent analysis reported in the companion paper by Riley et al. (2019) explores different emitting spot models, but finds spot shapes and locations and estimates of $R_e$ and $M$ that are consistent with those found in this work. We show that our measurements of $R_e$ and $M$ for PSR J0030$+$0451 improve the astrophysical constraints on the equation of state of cold, catalyzed matter above nuclear saturation density., Comment: 49 pages, 16 figures, part of The Astrophysical Journal Letters focus issue on the Neutron Star Interior Composition Explorer

Published
2019
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3. NICER Observes the Effects of an X-Ray Burst on the Accretion Environment in Aql X-1

Author

Keek, L., Arzoumanian, Z., Bult, P., Cackett, E. M., Chakrabarty, D., Chenevez, J., Fabian, A. C., Gendreau, K. C., Guillot, S., Güver, T., Homan, J., Jaisawal, G. K., Lamb, F. K., Ludlam, R. M., Mahmoodifar, S., Markwardt, C. B., Miller, J. M., Prigozhin, G., Soong, Y., Strohmayer, T. E., and Wolff, M. T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Accretion disks around neutron stars regularly undergo sudden strong irradiation by Type I X-ray bursts powered by unstable thermonuclear burning on the stellar surface. We investigate the impact on the disk during one of the first X-ray burst observations with the Neutron Star Interior Composition Explorer (NICER) on the International Space Station. The burst is seen from Aql X-1 during the hard spectral state. In addition to thermal emission from the neutron star, the burst spectrum exhibits an excess of soft X-ray photons below 1 keV, where NICER's sensitivity peaks. We interpret the excess as a combination of reprocessing by the strongly photoionized disk and enhancement of the pre-burst persistent flux, possibly due to Poynting Robertson drag or coronal reprocessing. This is the first such detection for a short sub-Eddington burst. As these bursts are observed frequently, NICER will be able to study how X-ray bursts affect the disk and corona for a range of accreting neutron star systems and disk states., Comment: 6 pages, 5 figures, published by ApJ Letters

Published
2018
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5. In-orbit performance of the soft X-ray imaging system aboard Hitomi (ASTRO-H)

Author

Nakajima, H., Maeda, Y., Uchida, H., Tanaka, T., Tsunemi, H., Hayashida, K., Tsuru, T. G., Dotani, T., Nagino, R., Inoue, S., Ozaki, M., Tomida, H., Natsukari, C., Ueda, S., Mori, K., Yamauchi, M., Hatsukade, I., Nishioka, Y., Sakata, M., Beppu, T., Honda, D., Nobukawa, M., Hiraga, J. S., Kohmura, T., Murakami, H., Nobukawa, K. K., Bamba, A., Doty, J. P., Iizuka, R., Sato, T., Kurashima, S., Nakaniwa, N., Asai, R., Ishida, M., Mori, H., Soong, Y., Okajima, T., Serlemitsos, P., Tawara, Y., Mitsuishi, I., Ishibashi, K., Tamura, K., Hayashi, T., Furuzawa, A., Sugita, S., Miyazawa, T., Awaki, H., Miller, E. D., and Yamaguchi, H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the in-orbit performance of the soft X-ray imaging system consisting of the Soft X-ray Telescope and the Soft X-ray Imager aboard Hitomi. Verification and calibration of imaging and spectroscopic performance are carried out making the best use of the limited data of less than three weeks. Basic performance including a large field of view of 38'x38' is verified with the first light image of the Perseus cluster of galaxies. Amongst the small number of observed targets, the on-minus-off pulse image for the out-of-time events of the Crab pulsar enables us to measure a half power diameter of the telescope as about 1.3'. The average energy resolution measured with the onboard calibration source events at 5.89 keV is 179 pm 3 eV in full width at half maximum. Light leak and cross talk issues affected the effective exposure time and the effective area, respectively, because all the observations were performed before optimizing an observation schedule and parameters for the dark level calculation. Screening the data affected by these two issues, we measure the background level to be 5.6x10^{-6} counts s^{-1} arcmin^{-2} cm^{-2} in the energy band of 5-12 keV, which is seven times lower than that of the Suzaku XIS-BI., Comment: Accepted for publication in PASJ. 17 pages, 18 figures

Published
2017
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6. ASTRO-H White Paper - Low-mass X-ray Binaries

Author

Done, C., Tsujimoto, M., Cackett, E., Herder, J. W. den, Dotani, T., Enoto, T., Ferrigno, C., Kallman, T., Kohmura, T., Laurent, P., Miller, J., Mineshige, S., Mori, H., Nakazawa, K., Paerels, F., Sakurai, S., Soong, Y., Sugita, S., Takahashi, H., Tamagawa, T., Tanaka, Y., Terada, Y., and Uno, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

There is still 10-20% uncertainty on the neutron star (NS) mass-radius relation. These uncertainties could be reduced by an order of magnitude through an unambiguous measure of M/R from the surface redshift of a narrow line, greatly constraining the Equation of State for ultra-dense material. It is possible that the SXS on ASTRO-H can detect this from an accreting neutron star with low surface velocity in the line of sight i.e. either low inclination or low spin. Currently there is only one known low inclination LMXB, Ser X-1, and one known slow spin LMXB, J17480-2446 in Terzan 5. Ser X-1 is a persistent source which is always in the soft state (banana branch), where the accreting material should form a equatorial belt around the neutron star. A pole-on view should then allow the NS surface to be seen directly. A 100 ks observation should allow us to measure M/R if there are any heavy elements in the photosphere at the poles. Conversely, J17480-2446 in Terzan 5 is a transient accretion powered millisecond pulsar, where the accreting material is collimated onto the magnetic pole in the hard (island) state (L_x < 0.1 L_Edd). The hotspot where the shock illuminates the NS surface is clearly seen in this state. A 100 ks ToO observation of this (or any other similarly slow spin system) in this state, may again allow the surface redshift to be directly measured. (abstract continues), Comment: 19 pages, 7 figures, ASTRO-H White Paper

Published
2014

7. Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku

Author

Terada, Y., Mihara, T., Nakajima, M., Suzuki, M., Isobe, N., Makishima, K., Takahashi, H., Enoto, T., Kokubun, M., Kitaguchi, T., Naik, S., Dotani, T., Nagase, F., Tanaka, T., Watanabe, S., Kitamoto, S., Sudoh, K., Yoshida, A., Nakagawa, Y., Sugita, S., Kohmura, T., Kotani, T., Yonetoku, D., Angelini, L., Cottam, J., Mukai, K., Kelley, R., Soong, Y., Bautz, M., Kissel, S., and Doty, J.

Subjects
Astrophysics
Abstract

The binary X-ray pulsar A0535+262 was observed with the Suzaku X-ray observatory, on 2005 September 14 for a net exposure of 22 ksec. The source was in a declining phase of a minor outburst, exhibiting 3--50 keV luminosity of about $3.7 \times 10^{35}$ ergs s$^{-1}$ at an assumed distance of 2 kpc. In spite of the very low source intensity (about 30 mCrab at 20 keV), its electron cyclotron resonance was detected clearly with the Suzaku Hard X-ray Detector, in absorption at about 45 keV. The resonance energy is found to be essentially the same as those measured when the source is almost two orders of magnitude more luminous. These results are compared with the luminosity-dependent changes in the cyclotron resonance energy, observed from 4U 0115+63 and X 0331+53., Comment: 12 pages, 4 figures, accepted to ApJL, high resolution version is available from http://cosmic.riken.jp/terada/01work/paper/a0535_suzaku2006.pdf

Published
2006
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8. Resolve Instrument on X-ray Astronomy Recovery Mission (XARM)

Author

Ishisaki, Y., Ezoe, Y., Yamada, S., Ichinohe, Y., Fujimoto, R., Takei, Y., Yasuda, S., Ishida, M., Yamasaki, N. Y., Maeda, Y., Tsujimoto, M., Iizuka, R., Koyama, S., Noda, H., Tamagawa, T., Sawada, M., Sato, K., Kitamoto, S., Hoshino, A., Brown, G. V., Eckart, M. E., Hayashi, T., Kelley, R. L., Kilbourne, C. A., Leutenegger, M. A., Mori, H., Okajima, T., Porter, F. S., Soong, Y., McCammon, D., Szymkowiak, A. E., and The XARM Resolve Team

Published
2018
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9. A Broad Band and Large Area X-Ray Omni Sky Monitor (BLOSM)

Author

Zhang, W., Petre, R., Peele, A. N., Jahoda, K., Marshall, F. E., Soong, Y., and White, N. E.

Subjects
Astrophysics
Abstract

We present a conceptual design for a new X-ray all sky monitor (ASM). Compared with previous ASMs, its salient features are: (1) it has a focusing capability that increases the signal to background ratio by a factor of 3; (2) it has a broad-band width: 200 eV to 15 keV; (3) it has a large X-ray collection area: ~100 square cm; (4) it has a duty cycle of nearly 100%, and (5) it can measure the position of a new source with an accuracy of a few minutes of arc. These features combined open up an opportunity for discovering new phenomena as well as monitoring existing phenomena with unprecedented coverage and sensitivity., Comment: 9 pages (figures and tables embedded), uses aas2pp4, Contributed paper to "All-Sky X-ray Observations in the Next Decade -- A workshop for ASM and GRB missions in the X-ray Band," March 3-5, 1997, Wako, Saitama, Japan

Published
1997

10. InFOCμS hard X-ray imaging telescope

Author

Tueller, J., Krimm, H. A., Okajima, T., Barthelmy, S. D., Owens, S. M., Serlemitsos, P. J., Soong, Y., Chan, K. -W., Ogasaka, Y., Shibata, R., Tamura, K., Furuzawa, A., Tawara, Y., Kunieda, H., Yamashita, K., and von Ballmoos, Peter, editor

Published
2006
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13. The X-Ray Polarimeter Instrument on Board the Polarimeter for Relativistic Astrophysical X-Ray Sources (PRAXyS) Mission

Author

Hill, J. E, Black, J. K, Jahoda, K, Tamagawa, T, Iwakiri, W, Kitaguchi, T, Kubota, M, Kaaret, P, Mccurdy, R, Miles, D. M, Okajima, T, Soong, Y, Olsen, L, Sparr, L, Mosely, S. J, and Nolan, D

Subjects
Astrophysics
Abstract

The Polarimeter for Relativistic Astrophysical X-ray Sources (PRAXyS) is one of three Small Explorer (SMEX) missions selected by NASA for Phase A study. The PRAXyS observatory carries an X-ray Polarimeter Instrument (XPI) capable of measuring the linear polarization from a variety of high energy sources, including black holes, neutron stars, and supernova remnants. The XPI is comprised of two identical mirror-Time Projection Chamber (TPC) polarimeter telescopes with a system effective area of 124 sq cm at 3 keV, capable of photon limited observations for sources as faint as 1 mCrab. The XPI is built with well-established technologies. This paper will describe the performance of the XPI flight mirror with the engineering test unit polarimeter

Published
2016
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17. Triboelectrostatic Separation of Mineral Matter from Slovakian Coals

Author

Schehl R. R., Marchant S., Turèániová ¼., Balá P., Link T. A., Schoffstall M. R., and Soong Y.

Subjects
triboelectrostatic separation, Slovak steam coal, ash content, Mining engineering. Metallurgy, TN1-997, Geology, QE1-996.5
Abstract

V èlánku sú diskutované niektoré technické aspekty triboelektrostatickej separácie a výs-ledky aplikácie tohto postupu pri úprave troch typov uhlia, konkrétne energetického uhlia z Cíg¾a, Handlovej a Novák. Bolo zistené, e úèinnos separácie ve¾mi úzko závisí na druhu separovan uhlia. Prvé výsledky preukázali súvislos medzi úèinnosou separácie obsahom popola v uhlí.

Published
1998

19. Resolve Instrument on X-ray Astronomy Recovery Mission (XARM)

Author

Yasuda, S., Brown, G. V., Eckart, M. E., Hayashi, T., Kelley, R. L., Kilbourne, C. A., Leutenegger, M. A., Porter, F. S., Soong, Y., McCammon, D., Szymkowiak, A. E., The, XARM Resolve Team, Ishisaki, Yoshitaka, Ezoe, Yuichiro, Yamada, Shinya, Ichinohe, Yuto, Fujimoto, Ryuichi, Takei, Yoh, Ishida, Manabu, Yamasaki, Noriko Y., Maeda, Yoshitomo, Tsujimoto, Masahiro, Iizuka, Ryo, Koyama, Shu, Noda, Hirofumi, Tamagawa, Toru, Sawada, Makoto, Sato, K., Kitamoto, Shunji, Hoshino, Akio, Mori, Hideyuki, and Okajima, Takashi

Subjects
Physics, X-ray astronomy, Spectrometer, Cryogenic detector, Astronomy, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, law.invention, 010309 optics, Telescope, Microcalorimeter, law, 0103 physical sciences, Focal length, General Materials Science, Orbit (control theory), 010303 astronomy & astrophysics
Abstract

著者人数: 31名ほか, Accepted: 2018-04-07, 資料番号: SA1180344000

Published
2018
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20. InFOCμS Hard X-ray Imaging Telescope

Author

Tueller, J., Krimm, H. A., Okajima, T., Barthelmy, S. D., Owens, S. M., Serlemitsos, P. J., Soong, Y., Chan, K.-W., Ogasaka, Y., Shibata, R., Tamura, K., Furuzawa, A., Tawara, Y., Kunieda, H., and Yamashita, K.

Published
2005
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24. PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter

Author

Miller, M. C., primary, Lamb, F. K., additional, Dittmann, A. J., additional, Bogdanov, S., additional, Arzoumanian, Z., additional, Gendreau, K. C., additional, Guillot, S., additional, Harding, A. K., additional, Ho, W. C. G., additional, Lattimer, J. M., additional, Ludlam, R. M., additional, Mahmoodifar, S., additional, Morsink, S. M., additional, Ray, P. S., additional, Strohmayer, T. E., additional, Wood, K. S., additional, Enoto, T., additional, Foster, R., additional, Okajima, T., additional, Prigozhin, G., additional, and Soong, Y., additional

Published
2019
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25. Development of the ASTRO-H Soft X-ray Telescope (SXT): Engineering Model Performance

Author

Okajima, Takashi, Serlemitsos, P. J, and Soong, Y

Subjects
Astronomy
Abstract

The X-ray astronomy satellite ASTRO-H, being developed under the collaboration among JAXA, NASA's GSFC and ESA, will have two Soft X-ray Telescopes (SXTs), among other instuments onboard, with a sensitive energy band below 12 keV. One is for an X-ray micorocalorimeter detector and the other for a X-ray CCD detector. The SXT uses a conically approximated Wolter I grazing incidence optic implemented by thin aluminum foil substrates with thickness of 0.152, 0.229, and 0.305 mm. It is similar to the Suzaku XRT, but with larger diameter (45 cm) and longer focal length (5.6 m). Goal of the angular resolution and effective area are 1 arcmin and 390 cm$A2$ at 6 keV, respectively. We made serveral improvements from Suzaku to ASTRO-H, such as thicker substrates, more forming mandrels, thinner epoxy layer for replication, stiffer housings, precise alignment bars, etc. With all these changes, we have fabricated the engineering test unit of the SXT. In this paper, we will discuss all the changes made, their effects, and report X-ray performance of the SXT test unit. An angular resolution of the test unit was measured at new Goddard X-ray calibration facility (100 m X-ray beamline) and was found to be 1.1 arcmin. We will also discuss further improvements toward the flight unit to be delivered to JAXA in 2012.

Published
2011

34. NICER Observes the Effects of an X-Ray Burst on the Accretion Environment in Aql X-1

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Chakrabarty, Deepto, Prigozhin, Gregory, Keek, L., Arzoumanian, Z., Bult, P., Cackett, E. M., Chenevez, J., Fabian, A. C., Gendreau, K. C., Guillot, S., Güver, T., Homan, J., Jaisawal, G. K., Lamb, F. K., Ludlam, R. M., Mahmoodifar, S., Markwardt, C. B., Miller, J. M., Soong, Y., Strohmayer, T. E., Wolff, M. T., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Chakrabarty, Deepto, Prigozhin, Gregory, Keek, L., Arzoumanian, Z., Bult, P., Cackett, E. M., Chenevez, J., Fabian, A. C., Gendreau, K. C., Guillot, S., Güver, T., Homan, J., Jaisawal, G. K., Lamb, F. K., Ludlam, R. M., Mahmoodifar, S., Markwardt, C. B., Miller, J. M., Soong, Y., Strohmayer, T. E., and Wolff, M. T.

Abstract

Accretion disks around neutron stars regularly undergo sudden strong irradiation by Type-I X-ray bursts powered by unstable thermonuclear burning on the stellar surface. We investigate the impact on the disk during one of the first X-ray burst observations with the Neutron Star Interior Composition Explorer (NICER) on the International Space Station. The burst is seen from Aql X-1 during the hard spectral state. In addition to thermal emission from the neutron star, the burst spectrum exhibits an excess of soft X-ray photons below 1 keV, where NICER's sensitivity peaks. We interpret the excess as a combination of reprocessing by the strongly photoionized disk and enhancement of the pre-burst persistent flux, possibly due to Poynting-Robertson drag or coronal reprocessing. This is the first such detection for a short sub-Eddington burst. As these bursts are observed frequently, NICER will be able to study how X-ray bursts affect the disk and corona for a range of accreting neutron star systems and disk states. Key words: accretion, accretion disks – stars: individual (Aql X-1) – stars: neutron – X-rays: binaries – X-rays: bursts, National Science Foundation (U.S.) (Grant PHY-1430152), United States. National Aeronautics and Space Administration

Published
2019

37. Production and Performance of the InFOCmicronS 20-40 keV Graded Multilayer Mirror

Author

Berendse, F, Owens, S. M, Serlemitsos, P. J, Tueller, J, Chan, K.-W, Soong, Y, Krimm, H, Baumgartner, W. H, Tamura, K, Okajima, T, Tawara, Y, and White, Nicholas E

Subjects
Astronomy
Abstract

The International Focusing Optics Collaboration for micron Crab Sensitivity (InFOC micronS) balloon-borne hard x-ray incorporates graded multilayer technology to obtain significant effective area at energies previously inaccessible to x-ray optics. The telescope mirror consists of 2040 segmented thin aluminum foils coated with replicated Pt/C multilayers. A sample of these foils was scanned using a pencil-beam reflectometer to determine, multilayer quality. The results of the reflectometer measurements demonstrate our capability to produce large quantity of foils while maintaining high-quality multilayers with a mean Nevot-Croce interface roughness of 0.5nm. We characterize the performance of the complete InFOC micronS telescope with a pencil beam raster scan to determine the effective area and encircled energy function of the telescope. The effective area of the complete telescope is 78, 42 and 22 square centimeters at 20 30 and 40 keV. respectively. The measured encircled energy fraction of the mirror has a half-power diameter of 2.0 plus or minus 0.5 arcmin (90% confidence). The mirror successfully obtained an image of the accreting black hole Cygnus X-1 during a balloon flight in July, 2001. The successful completion and flight test of this telescope demonstrates that graded-multilayer telescopes can be manufactured with high reliability for future x-ray telescope missions such as Constellation-X.

Published
2002

38. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi*

Author

Aharonia, F., Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M. W., Blandford, R., Brenneman, L. W., Brown, G. V., Bulbul, E., Cackett, E. M., Canning, R. E. A., Chernyakova, M., Chiao, M. P., Coppi, P. S., Costantini, E., Plaa, J., Vries, C. P., Den Herder, J. -W, Done, C., Dotani, T., Ebisawa, K., Eckart, M. E., Enoto, T., Ezoe, Y., Fabian, A. C., Ferrigno, C., Foster, A. R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L. C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I. M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J. S., Hornschemeier, A., Hoshino, A., Hughes, J. P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, S., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R. L., Kilbourne, C. A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H. A., Kubota, A., Kunieda, H., Laurent, P., Lee, S. -H, Leutenegger, M. A., Limousin, O., Loewenstein, M., Long, K. S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Kyoko Matsushita, Mccammon, D., Mcnamara, B. R., Mehdipour, M., Miller, E. D., Miller, J. M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R. F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K. K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F. S., Pottschmidt, K., Reynolds, C. S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P. J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R. K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Amagawa, T. T., Tamura, T., Tanaka, K., Tanaka, T., Tanaka, Y., Tanaka, Y. T., Tashiro, M. S., Tawara, Y., Terada, Y., Erashima, Y. T., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T. G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C. M., Ursino, E., Wang, Q. H. S., Watanabe, S., Werner, N., Wilkins, D. R., Williams, B. J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N. Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., 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), 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, 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, Active galactic nucleus, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], individual (NGC 1275) [galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: individual, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: individual (Perseus) [galaxies], 01 natural sciences, Intracluster medium, 0103 physical sciences, Emission spectrum, Brightest cluster galaxy, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Settore FIS/05, 010308 nuclear & particles physics, Velocity gradient, RCUK, Velocity dispersion, Astronomy and Astrophysics, Redshift, ST/J003697/2, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, Electron temperature, galaxies: clusters [X-rays], ST/L00075X/1, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: Hitomi Collaboration 197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; 林, 佑; 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 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.), Accepted: 201710-31, 資料番号: SA1170334000

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

Author

Hitomi, C, Aharonian, F, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hell, N, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Raassen, Ajj, 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), 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), 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
FOS: Physical sciences, Astrophysics, X-rays: general, 01 natural sciences, Measure (mathematics), X-ray, nickel, benchmark, iron, Settore FIS/05 - Astronomia e Astrofisica, general [X-rays], excited state, 0103 physical sciences, data analysis [methods], Calibration, Emission spectrum, Sensitivity (control systems), cluster, dielectric, 010306 general physics, 010303 astronomy & astrophysics, Collisional excitation, plasma, instrumentation: spectrographs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Resolution (electron density), temperature, resolution, Astronomy and Astrophysics, Plasma, calibration, sensitivity, methods: data analysis, recombination, 13. Climate action, Space and Planetary Science, spectral, data management, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, spectrographs [instrumentation]
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: 2017-12-13, 資料番号: SA1170337000

Published
2018
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40. Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sato, T, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, 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), 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 ), 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), 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
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], observational [methods], FOS: Physical sciences, Astrophysics, 01 natural sciences, individual objects (N 132 D) [ISM], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Spectral resolution, 010306 general physics, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Line (formation), ISM: supernova remnants, instrumentation: spectrographs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], individual (N 132 D) [X-rays], Astronomy and Astrophysics, X-rays: individual (N 132 D), Redshift, Interstellar medium, Supernova, ISM: individual object (N 132 D), 13. Climate action, Space and Planetary Science, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], spectrographs [instrumentation]
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, 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 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.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-06, 資料番号: SA1170341000

Published
2018
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41. Hitomi X-ray studies of giant radio pulses from the Crab pulsar

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, Oo, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Oshimizu, K, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Terasawa, T, Sekido, M, Takefuji, K, Kawai, E, Misawa, H, Tsuchiya, F, Yamazaki, R, Kobayashi, E, Kisaka, S, Aoki, T, 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
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetosphere, X-rays: stars, Astrophysics, 01 natural sciences, Article, Radio observatory, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, pulsars: individual (B0531+21), 010306 general physics, 010303 astronomy & astrophysics, stars [radio continuum], stars [X-rays], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, X-ray, Astronomy and Astrophysics, Pulse (physics), Space and Planetary Science, individual (B0531+21) [pulsars], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], radio continuum: stars, Phase width
Abstract

著者人数: Hitomi Collaboration 203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）, Number of authors: Hitomi Collaboration 203 (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.), Accepted: 2017-07-27, 資料番号: SA1170340000

Published
2018
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