The ASTRO-H X-ray Astronomy Satellite

Abstract

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions developed by the Institute of Space and Astronautical Science (ISAS), with a planned launch in 2015. The ASTRO-H mission is equipped with a suite of sensitive instruments with the highest energy resolution ever achieved at E > 3 keV and a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. The simultaneous broad band pass, coupled with the high spectral resolution of Delta E < 7 eV of the micro-calorimeter, will enable a wide variety of important science themes to be pursued. ASTRO-H is expected to provide breakthrough results in scientific areas as diverse as the large-scale structure of the Universe and its evolution, the behavior of matter in the gravitational strong field regime, the physical conditions in sites of cosmic-ray acceleration, and the distribution of dark matter in galaxy clusters at different redshifts.

24 pages, 18 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray"

References in corpus (4)

• The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission
• The Si/CdTe semiconductor Compton camera of the ASTRO-H Soft Gamma-ray Detector (SGD)
• Soft Gamma-ray Detector for the ASTRO-H Mission
• Multiwavelength Astronomy and CTA: X-rays

Cited by in corpus (26)

• The Quiescent Intracluster Medium in the Core of the Perseus Cluster
• Hitomi constraints on the 3.5 keV line in the Perseus galaxy cluster
• Sterile neutrino dark matter: A tale of weak interactions in the strong coupling epoch
• The dust sublimation radius as an outer envelope to the bulk of the narrow Fe Kalpha line emission in Type 1 AGN
• Physical Origins of Gas Motions in Galaxy Cluster Cores: Interpreting Hitomi Observations of the Perseus Cluster
• An optically-thick disk wind in GRO J1655-40?
• X-ray Spectral Model of Reprocessing by Smooth and Clumpy Molecular Tori in Active Galactic Nuclei with the MONACO framework
• What Do the Hitomi Observations Tell Us About the Turbulent Velocities in the Perseus Cluster? Probing the Velocity Field with Mock Observations
• Dark Matter Velocity Spectroscopy
• Simulating Astro-H Observations of Sloshing Gas Motions in the Cores of Galaxy Clusters
• Deep morphological and spectral study of the SNR RCW 86 with Fermi-LAT
• Broad-band High-Energy Resolution Hard X-ray Spectroscopy using Transition Edge Sensors at SPring-8
• Search for gas bulk motions in eight nearby clusters of galaxies with Suzaku
• Fe-K Line Time variability and Ni abundance of Distant Reflector in Seyfert Galaxies
• Thermal X-ray emission from a baryonic jet: a self-consistent multicolour spectral model
• The Nonstandard Properties of a "Standard" PWN: Unveiling the Mysteries of PWN G21.5-0.9 Using its IR and X-ray emission
• Accretion disk winds in active galactic nuclei: X-ray observations, models, and feedback
• The complex circumnuclear environment of the broad-line radio galaxy 3C 390.3 revealed by Chandra HETG
• The sign of active galactic nucleus quenching in a merger remnant with radio jets
• The Co-Evolution of a Magnetized Intracluster Medium and Hot Galactic Coronae: Magnetic Field Amplification and Turbulence Generation
• Hard X-ray/Soft gamma-ray experiments and missions: overview and prospects
• Study of the Polarimetric Performance of a Si/CdTe Semiconductor Compton Camera for the Hitomi Satellite
• Gamma-ray Diagnostics of r-process Nucleosynthesis in the Remnants of Galactic Binary Neutron-Star Mergers
• Measurements of the Soft Gamma-ray Emission from SN2014J with Suzaku
• The impact of improved plasma diagnostics on modeling the X-ray Universe
• CHEERS: Future perspectives for abundance measurements in clusters with XMM-Newton