| Date: |
December 15, 2008, 13:30 - 15:00 |
| Place: |
Seminar Room at IPMU Prefab. B, Kashiwa Campus of the University of Tokyo |
| Speaker: |
Hiro Tajima (Stanford Linear Accelerator Center) |
| Title: |
"Science and Instrumentation of ASTRO-H Mission: Next Generation X-ray/Gamma-ray Satellite Mission"
![[PDF]](/img/common/point04.gif)
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| Abstract: |
The ASTRO-H mission has been approved in Japan as a successor to the
Suzaku mission. Two major scientific objectives include: study of dark
energy through structure formation history and study of the high-
energy non-thermal Universe (particle acceleration). The instrument
design of the ASTRO-H satellite is optimized to achieve the above
science goals: a high resolution spectrometer (SXS) with an energy
resolution better than 7 eV at iron, two hard X-ray imagers (HXI) with
hard X-ray telescopes (HXTs) to achieve two orders of magnitudes of
sensitivity improvement in the energy range from 10 keV up to 80 keV,
two soft gamma-ray detectors (SGDs) with one order of magnitude better
sensitivity in the 80-300 keV energy band, in addition to a soft X-ray
telescope (SXT)/soft X-ray imager (SXI) for modest spectroscopy/
imaging in the 0.1-10 keV energy band. The continuum sensitivity of
the mission will reach several x10^(-8) photons/s/keV/cm2 in the hard
X-ray region and a few x 10^(-7) photons/s/keV/cm^(2) in the soft
gamma-ray region. Recently, the ASTRO-H mission is approved by as an
official JAXA mission.
I will describe the science of the ASTRO-H mission followed by the
development of Si/CdTe detectors and ASICs (Application Specific
Integrated Circuits) for HXI/SGD.
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