Search

Your search keyword '"Haba, Y."' showing total 241 results
Start Over Author "Haba, Y."
241 results on '"Haba, Y."'

1. Combined Analysis of X-Ray Spectra of NGC 3227

Author

Newman, J., Tsuruta, S., Liebmann, A. C., Kunieda, H., and Haba, Y.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The 1.5 Seyfert galaxy NGC 3227 has been observed by several X-ray missions. We carried out a combined analysis of the data obtained by more recent major observations of the source: two observations performed by XMM-Newton in 2000 and 2006 and six observations performed by Suzaku in 2008. A unified model, which is consistent with all eight observations by the two satellites with large intensity and spectral changes, was constructed. The model consists of a hard power law withe the spectral index of Gamma Hard = 1.4-1.7, which is interpreted as the Comptonized emission from the corona above an accretion disk. In the high-flux states, an additional soft excess component dominates, which is consistent with a model with either a steeper power law with Gamma Soft = 3.3-3.85, or the warm Comptonization component. These emissions from the central engine are absorbed by a partial covering material and warm absorbers. A reflection component and several emission lines are also present. We examined the relationship between the intrinsic luminosity and the absorbers' physical parameters such as the column density, which suggests that the source expanded significantly during the bright states when the soft excess is greatly enhanced., Comment: 16 pages, 6 tables, and 10 figures

Published
2020
Full Text
View/download PDF

2. Inorbit Performance of the Hard X-ray Telescope (HXT) on board the Hitomi (ASTRO-H) satellite

Author

Matsumoto, H., Awaki, H., Ishida, M., Furuzawa, A., Yamauchi, S., Maeda, Y., Mitsuishi, I., Haba, Y., Hayashi, T., Iizuka, R., Ishibashi, K., Itoh, M., Kunieda, H., Miyazawa, T., Mori, H., Okajima, T., Sugita, S., Tamura., K., and Tawara, Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Hitomi (ASTRO-H) carries two Hard X-ray Telescopes (HXTs) that can focus X-rays up to 80 keV. Combined with the Hard X-ray Imagers (HXIs) that detect the focused X-rays, imaging spectroscopy in the high-energy band from 5 keV to 80 keV is made possible. We studied characteristics of HXTs after the launch such as the encircled energy function (EEF) and the effective area using the data of a Crab observation. The half power diameters (HPDs) in the 5--80 keV band evaluated from the EEFs are 1.59 arcmin for HXT-1 and 1.65 arcmin for HXT-2. Those are consistent with the HPDs measured with ground experiments when uncertainties are taken into account. We can conclude that there is no significant change in the characteristics of the HXTs before and after the launch. The off-axis angle of the aim point from the optical axis is evaluated to be less than 0.5 arcmin for both HXT-1 and HXT-2. The best-fit parameters for the Crab spectrum obtained with the HXT-HXI system are consistent with the canonical values., Comment: 13 pages, 5 figures; the acknowledgment was modified

Published
2018
Full Text
View/download PDF

3. ASTRO-H White Paper - AGN Reflection

Author

Reynolds, C., Ueda, Y., Awaki, H., Gallo, L., Gandhi, P., Haba, Y., Kawamuro, T., LaMassa, S., Lohfink, A., Ricci, C., Tazaki, F., and Zoghbi, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

X-ray observations provide a powerful tool to probe the central engines of active galactic nuclei (AGN). A hard X-ray continuum is produced from deep within the accretion flow onto the supermassive black hole, and all optically thick structures in the AGN (the dusty torus of AGN unification schemes, broad emission line clouds, and the black hole accretion disk) "light up" in response to irradiation by this continuum. This White Paper describes the prospects for probing AGN physics using observations of these X-ray reflection signatures. High-resolution SXS spectroscopy of the resulting fluorescent iron line in type-2 AGN will give us an unprecedented view of the obscuring torus, allowing us to assess its dynamics (through line broadening) and geometry (through the line profile as well as observations of the "Compton shoulder"). The broad-band view obtained by combining all of the ASTRO-H instruments will fully characterize the shape of the underlying continuum (which may be heavily absorbed) and reflection/scattering, providing crucial constraints on models for the Cosmic X-ray Background with a subsequent impact on understanding of supermassive black hole evolution. ASTRO-H will also permit the relativistically broadened reflection spectrum from the inner accretion disk to be robustly studied, even in complex systems with, for example, warm absorption and composite soft excesses. Finally, the HXI will allow the detection and study of reverberation delays between the continuum and the Compton reflection hump from the inner disk., Comment: 20 pages, 14 figures, ASTRO-H White Paper

Published
2014

4. ASTRO-H White Paper - AGN Winds

Author

Kaastra, J. S., Terashima, Y., Kallman, T., Haba, Y., Costantini, E., Gallo, L., Fukazawa, Y., Tombesi, F., Anabuki, N., Awaki, H., Brown, G., di Gesu, L., Ebisawa, K., Ebrero, J., Eckart, M., Hagino, K., Long, K. S., Miller, J., Miyazawa, T., Paltani, S., Reynolds, C., Ricci, C., Sameshima, H., Seta, H., Ueda, Y., and Urry, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

In this white paper we describe the prospects for ASTRO-H for the study of outflows from active galactic nuclei. The most important breakthroughs in this field are expected to arise from the high spectral resolution and sensitivity in the Fe-K band, combined with broad-band sensitivity over the full X-ray band and spectral capabilities also at lower energies. The sensitivity in the Fe-K region allows to extend the absorption measure distribution of the outflow out to the highest ionisation states accessible, where observations with current X-ray missions indicate that most of the outflowing gas is to be found. Due to the high-resolution and sensitivity it will also be able to give the definitive proof for the existence of ultra-fast outflows, and if so, characterise their physical properties in great detail. These ultra-fast outflows carry very large amounts of energy and momentum, and are of fundamental importance for feedback studies. We show how the ASTRO-H observations in general can help to constrain numerical models for outflows. The link to reflection and emission processes is also discussed, as well as the possible relation between outflows and relativistic emission lines. Finally, we discuss the prospects for other related categories of objects like BAL quasars, partially covered sources and Compton thick outflows., Comment: 28 pages, 14 figures, ASTRO-H White Paper

Published
2014

5. The Hard X-ray Polarimeter X-Calibur - Design and Tests

Author

Beilicke, M., Binns, W. R., Buckley, J., Cowsik, R., Dowkontt, P., Garson, A., Guo, Q., Israel, M. H., Lee, K., Krawczynski, H., Baring, M. G., Barthelmy, S., Okajima, T., Schnittman, J., Tueller, J., Haba, Y., Kunieda, H., Matsumoto, H., Miyazawa, T., and Tamura, K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

X-ray polarimetry promises to give new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOCuS grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10-80 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity., Comment: 2011 Fermi Symposium proceedings - eConf C110509

Published
2011

6. Design and tests of the hard X-ray polarimeter X-Calibur

Author

Beilicke, M., Baring, M. G., Barthelmy, S., Binns, W. R., Buckley, J., Cowsik, R., Dowkontt, P., Garson, A., Guo, Q., Haba, Y., Israel, M. H., Kunieda, H., Lee, K., Matsumoto, H., Miyazawa, T., Okajima, T., Schnittman, J., Tamura, K., Tueller, J., and Krawczynski, H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

X-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOCuS grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10-80 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity., Comment: 9 pages, 5 figures, conference proceedings: SPIE 2011 (San Diego)

Published
2011
Full Text
View/download PDF

7. The Evolution of Galaxy Clusters Across Cosmic Time

Author

Arnaud, M., Bohringer, H., Jones, C., McNamara, B., Ohashi, T., Patnaude, D., Arnaud, K., Bautz, M., Blanchard, A., Bregman, J., Chartas, G., Croston, J., David, L., Donahue, M., Fabian, A., Finoguenov, A., Furuzawa, A., Gallagher, S., Haba, Y., Hornschemeier, A., Heinz, S., Kaastra, J., Kapferer, W., Lamer, G., Mahdavi, A., Makishima, K., Matsushita, K., Nakazawa, K., Nulsen, P., Ogle, P., Perlman, E., Ponman, T., Proga, D., Pratt, G., Randall, S., Richards, G., Romer, K., Ruszkowski, M., Schmidt, R., Smith, R., Tananbaum, H., Vrtilek, J., and Worrall, D.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

The large scale structure of the present Universe is determined by the growth of dark matter density fluctuations and by the dynamical action of dark energy and dark matter. While much progress has been made in recent years in constraining the cosmological parameters, and in reconstructing the evolution in the large--scale structure of the dark matter distribution, we still lack an understanding of the evolution of the baryonic component of the Universe. Located at nodes of the cosmic web, clusters of galaxies are the largest collapsed structures in the Universe with total masses up to 10$^{15}$ M$_{\sun}$. Over 80% of their mass resides in the form of dark matter. The remaining mass is composed of baryons, most of which (about 85%) is a diffuse, hot plasma that radiates primarily in X-rays. X-ray observations of the evolving cluster population provide a unique opportunity to address such open and fundamental questions as: How do hot diffuse baryons dynamically evolve in dark matter potentials? How and when was the excess energy which we observe in the intergalactic medium generated? What is the cosmic history of heavy-element production and circulation? Our current knowledge comes primarily from detailed studies of clusters in the relatively nearby Universe (z$<$0.5). Major advances will come from high throughput, high spectral and spatial resolution X-ray observations that measure the thermodynamical properties and metal content of the first low mass clusters emerging at z $\sim$ 2 and directly trace their evolution into today's massive clusters., Comment: Science white paper submitted to the Astro2010 Decadal Survey

Published
2009

8. Suzaku Observation of Two Ultraluminous X-Ray Sources in NGC 1313

Author

Mizuno, T., Miyawaki, R., Ebisawa, K., Kubota, A., Miyamoto, M., Winter, L., Ueda, Y., Isobe, N., Dewangan, G., Done, C., Griffiths, R. E., Haba, Y., Kokubun, M., Kotoku, J., Makishima, K., Matsushita, K., Mushotzky, R. F., Namiki, M., Petre, R., Takahashi, H., Tamagawa, T., and Terashima, Y.

Subjects
Astrophysics
Abstract

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

Published
2006
Full Text
View/download PDF

9. The X-ray variability of the Narrow-Line Seyfert 1 galaxy IRAS 13224-3809 from an XMM-Newton observation

Author

Gallo, L. C., Boller, Th., Tanaka, Y., Fabian, A. C., Brandt, W. N., Welsh, W. F., Anabuki, N., and Haba, Y.

Subjects
Astrophysics
Abstract

We report on the XMM-Newton timing properties of the most X-ray variable, radio-quiet, NLS1 IRAS 13224-3809. IRAS 13224-3809 continues to display the extremely variable behavior that was previously observed with ROSAT and ASCA; however, no giant, rapid flaring events are observed. We detect variations by a factor as high as ~8 during the 64 ks observation, and the variability is persistent throughout the light curve. Dividing the light curve into 9 minute segments we found almost all of the segments to be variable at > 3 sigma. When the time-averaged cross-correlation function is calculated for the 0.3-0.8 keV band with the 3-10 keV band, the cross-correlation profile is skewed indicating a possible smearing of the signal to longer times (soft band leading the hard). A correlation between count rate and hardness ratio is detected in four energy bands. In three cases the correlation is consistent with spectral hardening at lower count rates which can be explained in terms of a partial-covering model. The other band displays the reverse effect, showing spectral hardening at higher count rates. We can explain this trend as a more variable power-law component compared to the soft component. We also detect a delay between the 0.3-1.5 keV count rate and the 0.8-1.5 keV to 0.3-0.8 keV hardness ratio, implying flux induced spectral variability. Such delays and asymmetries in the cross correlation functions could be suggesting reprocessing of soft and hard photons. In general, much of the timing behavior can be attributed to erratic eclipsing behavior associated with the partial covering phenomenon, in addition to intrinsic variability in the source. The variability behavior of IRAS 13224-3809 suggests a complicated combination of effects which we have started to disentangle with this present analysis., Comment: 8 pages including 9 figures. Accepted for publication in MNRAS

Published
2003
Full Text
View/download PDF

10. XMM-Newton spectral properties of the Narrow-Line Seyfert 1 galaxy IRAS 13224--3809

Author

Boller, Th., Tanaka, Y., Fabian, A., Brandt, W. N., Gallo, L., Anabuki, N., Haba, Y., and Vaughan, S.

Subjects
Astrophysics
Abstract

We report on the first XMM-Newton observation of the highly X-ray variable, radio-quiet, Narrow-Line Seyfert 1 galaxy IRAS 13224-3809 obtained during the guaranteed time programme with a 64 ks exposure. The most remarkable spectral feature is a sharp drop, by a factor ~5, in the spectrum at 8 keV. This is a similar, but stronger, feature to that which we found in 1H0707-495. Significant flattening of the hard X-ray spectrum occurs when the source flux decreases. The flattening of the spectrum can be modelled as an increase in the column density of the absorbing material and/or its covering fraction. Below ~ 1.5 keV the spectrum is dominated by a giant soft X-ray excess, and at around ~ 1.2 keV there is a significant absorption feature detected, most probably due to ionized Fe L absorption. The new X-ray spectral properties detected with XMM-Newton in IRAS 13224-3809 support a partial covering interpretation, i.e. the presence of dense material inside the accretion-disc region partially obscuring the emission from the accretion disc. However, the sharpness of the feature, if due to photoelectric absorption, is surprising and may require an alternative explanation. One possibility which does fit the whole spectrum is that it is dominated by ionized reflection rather than absorption. The unusual spectral properties detected with XMM-Newton from Narrow-Line Seyfert 1 galaxies increase the known spectral complexity of active galactic nuclei and should further stimulate a combined theoretical and observational effort to achieve a better understanding of the physics of the innermost regions of AGN., Comment: 5 pages including 7 figures. Accepted for publication in MNRAS Letters

Published
2003
Full Text
View/download PDF

12. Nonuniform plasma meniscus modelling based on backward calculation of negative ion beamlet

Author

Kisaki, M., Nagaoka, K., Slief, J.H., Haba, Y., Nakamoto, R., Tsumori, K., Nakano, H., Ikeda, K., Osakabe, M., Kisaki, M., Nagaoka, K., Slief, J.H., Haba, Y., Nakamoto, R., Tsumori, K., Nakano, H., Ikeda, K., and Osakabe, M.

Abstract

The shape of a plasma meniscus is a key factor to determine the beam focusing. The physics model of the meniscus formation for hydrogen negative ion sources has not been established yet. A backward trajectory calculation based on experimental observation is performed in order to derive the particle information at the meniscus. It is observed that the negative ion density is spatially nonuniform in the direction parallel to the magnets for suppression of co-extracted electrons. A nonuniformity of the negative ion density in the vicinity of the meniscus is taken into account in the forward trajectory calculation. It reveals that the nonuniform negative ion distribution leads to degradation of the beam focusing and the beam splitting in phase space. The importance of the spatial distribution of negative ions on meniscus modelling is discussed with a comparison to uniform extraction model.

Published
2022

13. Ray-Tracing Simulation and In-Orbit Performance of the ASTRO-H Hard X-Ray Telescope (HXT)

Author

Matsumoto, H, Awaki, H, Furuzawa, A, Ishida, M, Kunieda, H, Haba, Y, Hayashi, T, Iizuka, R, Ishibashi, K, Itoh, M, Kosaka, T, Maeda, Y, Mitsuishi, I, Miyazawa, T, Mori, H, Nagano, H, Namba, Y, Ogasaka, Y, Ogi, K, Okajima, T, Sugita, S, Suzuki, Y, Tamura, K, Tawara, Y, Uesugi, K, and Yamauchi, S

Subjects
Astrophysics
Abstract

A ray-trace simulation code for the Hard X-ray Telescope (HXT) on board the Hitomi (ASTRO-H) satellite is beingdeveloped. The half power diameter and effective area simulated based on the code are consistent with groundmeasurements within 10%. The HXT observed the pulsar wind nebula G21.5-0.9 for 105 ksec. We confirmed that theencircled energy function and the half power diameter obtained from the data are consistent with the ground measurements.

Published
2016
Full Text
View/download PDF

15. First Flight of the X-Ray Polarimeter X-Calibur

Author

Beilicke, Matthias, Kislat, F, Guo, Q, Endsley, R, Cowsik, R, Dowkontt, P, Krawczynski, H, Barthelmy, S, Hams, T, Okajima, T, Sasaki, M, De Geronimo, G, Haba, Y, and Saji, S

Subjects
Astrophysics
Abstract

X-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard X-ray polarimeter, X-Calibur, to be used in the focal plane of the balloon-borne InFOCuS grazing incidence X-ray telescope with the goal of observing astrophysical sources. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 20-60 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. A I-day test. flight of the instrument was performed from Ft.Sumner, NM, In fall 2014. The sensitivity, performance and first results form the flight will be presented.

Published
2015
Full Text
View/download PDF

16. Development and characterization of reactively extruded PVC/polystyrene blends

Author

Haba, Y. and Narkis, M.

Subjects
Polymeric composites -- Research, Lubrication and lubricants, Engineering and manufacturing industries, Science and technology
Abstract

PVC/PS blends are obtained through a reactive extrusion--polymerization method by the absorption of a solution of styrene monomer, initiator, and a crosslinking agent in commercial suspension-type porous polyvinyl chloride (PVC) particles, forming a dry-blend with a relatively high monomer content. These PVC/styrene dryblends are reactively polymerized in a twin-screw extruder in the melt state. They do not contain monomer residues as detected by GC. The transparency, fracture surface morphology, thermal stability, rheology and static and dynamic mechanical properties of these blends are compared to physical PVC/PS blends at similar compositions. Owing to the high polymerization temperature (180[degrees]C), short PS chains are formed in the reactive extrusion process. These short chains are dispersed both as a separate phase of ~2 [micro]m particles (recognized by SEM) and also as molecularly dispersed chains enhancing plasticization and compatibilization. The molecularly dispersed short PS chains tend to plasticize the PVC phase, reducing its melt viscosity and glass transition temperature. The content of the short PS chains forming the dispersed separate PS particles is too low for DMTA to detect a separate [T.sub.g]. Thus, reactively extruded PVC/PS blends exhibit single [T.sub.g] transitions at lower temperatures compared with the neat PVC. Migration of the PVC's low-molecular-weight additives (lubricants and thermal stabilizer) to the PS phase is observed in the physical PVC/PS blends, causing antiplasticization of the PS phase. This results in both reduction of the [T.sub.g] and an increase in the thermal stability of the PS phase in the physical PVC/PS blends. Comparing TGA thermograms of reactively extruded and physical PVC/PS indicates that the PS formed in the extruder is different from the commercial PS. This can stem from various chemical reactions that can take place in the studied reactive polymerization process. Polym. Eng. Sci. 44:1473-1483, 2004. [c] 2004 Society of Plastics Engineers., INTRODUCTION Recent decades have seen an increasing demand for new polymeric materials. By blending, new materials can be developed that combine physical and mechanical properties of their components, depending on [...]

Published
2004

20. Design and Tests of the Hard X-Ray Polarimeter X-Calibur

Author

Beilicke, M, Baring, M. G, Barthelmy, S, Binns, W. R, Buckley, J, Cowsik, R, Dowkontt, P, Garson, A, Guo, Q, Haba, Y, Israel, M. H, Kunieda, H, Lee, K, Matsumoto, H, Miyazawa, T, Okajima, T, Schnittman, J, Tamura, K, Tueller, J, and Krawczynski, H

Subjects
Astrophysics
Abstract

X-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOC(mu)S grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10 - 80 keY X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity.

Published
2012

21. Design and Tests of the Hard X-Ray Polarimeter X-Calibur

Author

Beilicke, M, Binns, W. R, Buckley, J, Cowsik, R, Dowkontt, P, Garson, A, Guo, Q, Israel, M. H, Lee, K, Krawczynski, H, Baring, M. G, Barthelmy, S, Okajima, T, Schnittman, J, Tueller, J, Haba, Y, Kunieda, H, Matsumoto, H, Miyazawa, T, and Tamura, K

Subjects
Astrophysics
Abstract

X-ray polarimetry promises to give new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. We designed, built and tested a hard X-ray polarimeter X-Calibur to be used in the focal plane of the InFOC(mu)S grazing incidence hard X-ray telescope. X-Calibur combines a low-Z Compton scatterer with a CZT detector assembly to measure the polarization of 10-80 keV X-rays making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. X-Calibur achieves a high detection efficiency of order unity.

Published
2011

22. Design and tests of the hard X-ray polarimeter X-Calibur

Author

Beilicke, M., Baring, M.G., Barthelmy, S., Binns, W.R., Buckley, J., Cowsik, R., Dowkontt, P., Garson, A., Guo, Q., Haba, Y., Israel, M.H., Kunieda, H., Lee, K., Matsumoto, H., Miyazawa, T., Okajima, T., Schnittman, J., Tamura, K., Tueller, J., and Krawczynski, H.

Published
2012
Full Text
View/download PDF

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

Author

Mizuno, T, Miyawaki, R, Ebisawa, K, Kubota, A, Miyamoto, M, Winter, L, Ueda, Y, Isobe, N, Dewangan, G, Done, C, Griffiths, R. E, Haba, Y, Kokubun, M, Kotoku J, Makishima, K, Matsushita, K, Mushotzky, R. F, Namiki, M, Petre, R, Takahashi, H, Tamagaw, T, and Terashima, Y

Subjects
Astronomy
Abstract

A study was made of two ultraluminous X-ray soures (ULXs) in the nearby face-on, late-type Sb galaxy NGC 1313 using data from Suzaku, the 5th Japanese X-ray satellite. Within the 90 ks observation, both sources named X-1 and X-2 exhibited luminosity change by about 50%. The 0.4-10 keV X-ray luminosity was measured to be 2.5 x 10(exp 40) erg per second and 5.8 x 10 erg per second for X-1 and X-2, respectively, requiring a black hole of 50-200 solar mass in order not to exceed the Eddingtion limit. For X-1: the spectrum exhibited a strong power-law component with a high energy cutoff which is thought to arise from strong Comptonization by a disk corona, suggesting the source was in a very high state. Absorption line features with equivalent widths of 40-80 eV found at 7.0 keV and 7.8 keV in the X-1 spectrum support the presence of a highly ionized plasma and a high mass accretion rate on the system. Oxygen abundance of the NGC 1313 circumstellar matter toward X-1 was found to be subsolar, viz. O/H = (5.0 plus or minus 1.0) x 10(exp -4). The spectrum of X-2 in fainter phase is best represented by a multicolor disk blackbody model with T (sub in) = 1.2-1.3 keV and becomes flatter as the flux increases; the source is interpreted to be in a slim disk state.

Published
2001

29. 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
Full Text
View/download PDF

30. 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
Full Text
View/download PDF

31. 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
Full Text
View/download PDF

32. 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
Full Text
View/download PDF

34. Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster

Author

Aharonian, FA, Akamatsu, H, Akimoto, F, Allen, SW, Angelini, L, Arnaud, KA, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, MW, Blandford, RD, Bulbul, E, Brenneman, LW, Brown, GV, Cackett, EM, Chernyakova, M, Chiao, MP, Coppi, P, Costantini, E, Plaa, JD, Herder, JWD, 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, Gu, L, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, I, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, J, Hornschemeier, AE, Hoshino, A, Hughes, JP, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, S, Inoue, Y, Ishibashi, K, Ishida, M, Ishikawa, K, Ishisaki, Y, Itoh, M, Iwai, M, Iyomoto, N, Kaastra, JS, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, N, Kelley, RL, Khangulyan, D, Kilbourne, CA, King, AL, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, HA, Kubota, A, Kunieda, H, Laurent, P, Lebrun, F, Lee, SH, Leutenegger, MA, Limousin, O, Loewenstein, M, Long, KS, Lumb, DH, Madejski, GM, Maeda, Y, Maier, D, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: clusters: individual (A426), Astrophysics::Galaxy Astrophysics, dark matter
Abstract

© 2017. The American Astronomical Society. All rights reserved. High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E ≈ 3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S xvi (E ≃ 3.44 keV rest-frame) - a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.

Published
2017

35. The quiescent intracluster medium in the core of the Perseus cluster

Author

Aharonian, F, Akamatsu, H, Akimoto, F, Allen, SW, Anabuki, N, Angelini, L, Arnaud, K, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, M, Blandford, R, Brenneman, L, Brown, GV, Bulbul, E, Cackett, E, Chernyakova, M, Chiao, M, Coppi, P, Costantini, E, De Plaa, J, Den Herder, JW, Done, C, Dotani, T, Ebisawa, K, Eckart, M, Enoto, T, Ezoe, Y, Fabian, AC, Ferrigno, C, Foster, A, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, L, Gandhi, P, Giustini, M, Goldwurm, A, Gu, L, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, I, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, J, Hornschemeier, A, Hoshino, A, Hughes, J, Iizuka, R, Inoue, H, Inoue, Y, Ishibashi, K, Ishida, M, Ishikawa, K, Ishisaki, Y, Itoh, M, Iyomoto, N, Kaastra, J, Kallman, T, Kamae, T, Kara, E, Kataoka, J, Katsuda, S, Katsuta, J, Kawaharada, M, Kawai, N, Kelley, R, Khangulyan, D, Kilbourne, C, King, A, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, S, Koyama, K, Kretschmar, P, Krimm, H, Kubota, A, Kunieda, H, Laurent, P, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Hitomi Collaboration, Astrophysics::Galaxy Astrophysics
Abstract

Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling - a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure., Please visit the publisher's website for funding information.

Published
2016

36. Caesiated H- source operation with helium

Author

Tsumori, K., primary, Wada, M., additional, Nakano, H., additional, Kisaki, M., additional, Ikeda, K., additional, Haba, Y., additional, Nagaoka, K., additional, Kamio, S., additional, Fujiwara, Y., additional, and Osakabe, M., additional

Published
2018
Full Text
View/download PDF

39. Caesiated H- Source Operation with Helium.

Author

Tsumori, K., Wada, M., Nakano, H., Kisaki, M., Ikeda, K., Haba, Y., Nagaoka, K., Kamio, S., Fujiwara, Y., and Osakabe, M.

Subjects
CESIUM, HYDROGEN ions, ION sources, COEXTRACTION (Chemistry), DEUTERIUM, ANIONS
Abstract

The consumption rate of cesium (Cs) for negative hydrogen (H-) ion source increases when the source operation gas is changed from hydrogen to deuterium. There was observed a clear indication that a deuterium discharge erodes Cs atoms on the plasma grid (PG) surface to increase work function and the co-extracted electron current. We have proposed a model, that the enhanced sputtering yield of Cs from the PG due to deuterium ions, which carries more kinetic energy to Cs adsorbed on the surface directly or indirectly, is the main reason for this fast dissipation of Cs. Introduction of helium (He) into discharge can verify the enhanced sputtering effect due to the lager mass ions in the source discharge. Comparing the effect due to seeded Cs before and after the He injection into discharge through Cs OES signals as well as the H- density measured with cavity ring-down method, the sputtering/evaporation enhancement due to He is estimated. Neutral atoms and positive ions in the He discharge should cause enhanced sputtering like deuterium, while the system does not generate neutron under the induction of acceleration voltage to diagnose the extracted negative ion beam. Plasma parameters of the H2 and He plasmas are investigated by diagnostics tools installed on NIFS-RNIS (National Institute for Fusion Science, Research and development Negative Ion Source) together with H- density measurement by cavity ring down. Enhanced consumption rate of Cs is compared with proposed sputtering yield data to predict the rate for deuterium operation of negative ion sources. [ABSTRACT FROM AUTHOR]

Published
2018
Full Text
View/download PDF

41. First flight of the X-ray polarimeter X-Calibur

Author

Beilicke, Matthias, primary, Kislat, F., additional, Zajczyk, A., additional, Guo, Q., additional, Endsley, R., additional, Cowsik, R., additional, Dowkontt, P., additional, Krawczynski, H., additional, Barthelmy, S., additional, Hams, T., additional, Okajima, T., additional, Sasaki, M., additional, De Geronimo, G., additional, Haba, Y., additional, and Saji, S., additional

Published
2015
Full Text
View/download PDF

42. PP053-MON: Bone Mineral Density and Bone Metabolism in Gastrectomized Patients with Gastric Cancer – Comparison Between Conventional and Limited Gastrectomies

Author

Fujimura, T., primary, Haba, Y., additional, Higashi, Y., additional, Yamazaki, Y., additional, Watanabe, T., additional, Okamoto, K., additional, Kinoshita, J., additional, Nakamura, K., additional, Oyama, K., additional, Miyashita, T., additional, Tajima, H., additional, Ninomiya, I., additional, Fushida, S., additional, and Ohta, T., additional

Published
2014
Full Text
View/download PDF

45. Design and tests of the hard x-ray polarimeter X-Calibur

Author

Beilicke, M. G., primary, Baring, M., additional, Barthelmy, S., additional, Binns, W. R., additional, Buckley, J., additional, Cowsik, R., additional, Dowkontt, P., additional, Garson, A., additional, Guo, Q., additional, Haba, Y., additional, Israel, M. H., additional, Kislat, F., additional, Kunieda, H., additional, Lee, K., additional, Martin, J., additional, Matsumoto, H., additional, Miyazawa, T., additional, Okajima, T., additional, Schnittman, J., additional, Tamura, K., additional, Tueller, J., additional, and Krawczynski, H., additional

Published
2012
Full Text
View/download PDF

46. The hard X-ray polarimeter X-Calibur

Author

Beilicke, M., primary, Baring, M. G., additional, Barthelmy, S., additional, Binns, W. R., additional, Buckley, J., additional, Cowsik, R., additional, Dowkontt, P., additional, Guo, Q., additional, Haba, Y., additional, Israel, M. H., additional, Kunieda, H., additional, Lee, K., additional, Martin, J., additional, Matsumoto, H., additional, Miyazawa, T., additional, Okajima, T., additional, Schnittman, J., additional, Tamura, K., additional, Tueller, J., additional, and Krawczynski, H., additional

Published
2012
Full Text
View/download PDF

47. Design and tests of the hard x-ray polarimeter X-Calibur

Author

Beilicke, M., primary, Baring, M. G., additional, Barthelmy, S., additional, Binns, W. R., additional, Buckley, J., additional, Cowsik, R., additional, Dowkontt, P., additional, Garson, A., additional, Guo, Q., additional, Haba, Y., additional, Israel, M. H., additional, Kunieda, H., additional, Lee, K., additional, Matsumoto, H., additional, Miyazawa, T., additional, Okajima, T., additional, Schnittman, J., additional, Tamura, K., additional, Tueller, J., additional, and Krawczynski, H., additional

Published
2011
Full Text
View/download PDF

48. In-flight status of the X-ray observatory Suzaku

Author

Dotani, T., primary, Mitsuda, K., additional, Bautz, M., additional, Inoue, H., additional, Kelley, R. L., additional, Koyama, K., additional, Kunieda, H., additional, Makishima, K., additional, Ogawara, Y., additional, Petre, R., additional, Takahashi, T., additional, Tsunemi, H., additional, White, N. E., additional, Anabuki, N., additional, Angelini, L., additional, Arnaud, K., additional, Awaki, H., additional, Bamba, A., additional, Boyce, K., additional, Brown, G. V., additional, Chan, K.-W., additional, Cottam, J., additional, Doty, J., additional, Ebisawa, K., additional, Ezoe, Y., additional, Fabian, A. C., additional, Figueroa, E., additional, Fujimoto, R., additional, Fukazawa, Y., additional, Furusho, T., additional, Furuzawa, A., additional, Gendreau, K., additional, Griffiths, R. E., additional, Haba, Y., additional, Hamaguchi, K., additional, Harrus, I., additional, Hasinger, G., additional, Hatsukade, I., additional, Hayashida, K., additional, Henry, P. J., additional, Hiraga, J. S., additional, Holt, S. S., additional, Hornschemeier, A., additional, Hughes, J. P., additional, Hwang, U., additional, Ishida, M., additional, Ishisaki, Y., additional, Isobe, N., additional, Itoh, M., additional, Iyomoto, N., additional, Kahn, S. M., additional, Kamae, T., additional, Katagiri, H., additional, Kataoka, J., additional, Katayama, H., additional, Kawai, N., additional, Kawaharada, M., additional, Kilbourne, C., additional, Kinugasa, K., additional, Kissel, S., additional, Kitamoto, S., additional, Kohama, M., additional, Kohmura, T., additional, Kokubun, M., additional, Kotani, T., additional, Kotoku, J., additional, Kubota, A., additional, Madejski, G. M., additional, Maeda, Y., additional, Makino, F., additional, Markowitz, A., additional, Matsumoto, C., additional, Matsumoto, H., additional, Matsuoka, M., additional, Matsushita, K., additional, McCammon, D., additional, Mihara, T., additional, Misaki, K., additional, Miyata, E., additional, Mizuno, T., additional, Mori, K., additional, Mori, H., additional, Morii, M., additional, Moseley, H., additional, Mukai, K., additional, Murakami, H., additional, Murakami, T., additional, Mushotzky, R., additional, Nagase, F., additional, Namiki, M., additional, Negoro, H., additional, Nakazawa, K., additional, Nousek, J. A., additional, Okajima, T., additional, Ogasaka, Y., additional, Ohashi, T., additional, Oshima, T., additional, Ota, N., additional, Ozaki, M., additional, Ozawa, H., additional, Parmar, A. N., additional, Pence, W. D., additional, Porter, F. Scott, additional, Reeves, J. N., additional, Ricker, G. R., additional, Sakurai, I., additional, Sanders, W. T., additional, Senda, A., additional, Serlemitsos, P., additional, Shibata, R., additional, Shinozaki, K., additional, Soong, Y., additional, Smith, R., additional, Suzuki, M., additional, Szymkowiak, A. E., additional, Takahashi, H., additional, Takei, Y., additional, Tamagawa, T., additional, Tamura, K., additional, Tamura, T., additional, Tanaka, Y., additional, Tashiro, M., additional, Tawara, Y., additional, Terada, Y., additional, Terashima, Y., additional, Tomida, H., additional, Torii, K., additional, Tsuboi, Y., additional, Tsujimoto, Y., additional, Tsuru, T., additional, Turner, M. J. L., additional, Uchiyama, Y., additional, Ueda, Y., additional, Ueno, S., additional, Ueno, M., additional, Uno, S., additional, Urata, Y., additional, Watanabe, S., additional, Yamamoto, N., additional, Yamaoka, K., additional, Yamasaki, N. Y., additional, Yamashita, K., additional, Yamauchi, M., additional, Yamauchi, S., additional, Yaqoob, T., additional, Yonetoku, D., additional, and Yoshida, A., additional

Published
2007
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results