the astro-h project - nagoya university · the astro-h project hironori matsumoto (nagoya...
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The ASTRO-H project
Hironori MATSUMOTO (Nagoya University)
On behalf of the ASTRO-H team
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Outline • ASTRO-H System
– Precise Soft X-ray Spectroscopy
• Soft X-ray Telescope (SXT) +Soft X-ray Spectrometer (SXS)
– Hard X-ray Imaging system
• Hard X-ray Telescope (HXT) + Hard X-ray Imager (HXI)
– Soft Gamma-ray
• Soft Gamma-ray Detector (SGD)
– Soft X-ay Imaging
• SXT + Soft X-ray Imager (SXI)
• Athena project
• Summary
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X-ray Universe
Cluster of galaxies hot gas
©SDSS ©RASS
We would overlook real face without X-rays.
Mgal < Mgas
3
Optical X-ray
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ASTRO-H Satellite
weight 2.7t
Launch in FY2015
Japan’s 6th X-ray Astronomical Satellite
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International collaboration More than 160 scientists from Japan/USA/Europe
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SXT + SXS (0.3—12keV)
Soft X-ray Telescope
Soft X-ray
Spectrometer
(X-ray Calorimeter)
f=5.6m
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Principle of X-ray Telescope
Wolter-I Grazing angle optics
“Year ring” of foils
focus X-ray source
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Soft X-ray Telescope (SXT)
SXT-1 FM
203 nested shells
Au-coated Al foils
Total reflection
101.6mm
450mm
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Soft X-ray Spectrometer (SXS)
High-energy resolution even for spatially
extended objects (cf. gratings)
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SXS Energy resolution
Ground Experiment Simulation
SXS
CCD
SXS can distinguish fine structures
Measure physical parameters of plasma directly.
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SXT+SXS vs other gratings
Good for dim objects & high-energy X-rays
Effective Area E resolution
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SXS+SXT
High-energy resolution
for spatially extended
objects for the first time!
Plasma spectroscopy!
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Plasma in the universe T
emp
erat
ure
(K
)
WHIM
cluster
starburst gal
interstellar
gas
supernova
remnant
Earth
magnetoshpere stellar corona
Most can be observed only through X-rays
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Perseus cluster falling down
from outskirts
Feedback
by jets etc.
How chaotic? How much energy stored?
~3e5LY
Active Galactic Nucleus
(Black hole)
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Perseus cluster
~3e5LY
SXS FOV
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Reveal gas dynamics
Theoretical model SXS simulation
Line center bulk motion
Line width turbulence
Line ratio temperature, density etc.
Fe He-like ion
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3.5keV Dark Matter line?
Bulbul et al. 2014
3.5keV line? DM? SXS simulation
But no line was seen in Suzaku data
(Tamura et al. submitted to PASJ)
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Supernova Remnant
~11Ly
Where is the 99% of the total energy?
e.g. Tycho
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Energetics of supernova remnants
Ion expansion speed, temperature
Tycho SNR center
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HXT + HXI (5—80keV)
Hard X-ray Telescope Hard X-ray
Imager
(Si DSD
+ CdTe DSD)
f=12m
Nagoya U. Ux group
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Hard X-ray Imager (HXI)
E<20 keV: Double-sided Si Strip Detector
E>20keV: Double-sided CdTe Strip Detector
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Hard X-ray Telescope 45cm
49
cm
HXT-1 FM
213 nested shells
Pt/C multilayer
Bragg Reflection
E=5—80keV
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SNRs seen with HXI
Clarify the mechanism
of particle acceleration.
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Clusters of galaxies A3667
Radio emission
Relativistic electrons (~GeV) If high E electrons (>TeV) exsist,
hard X-rays can be seen.
(Inverse Compton of CMB)
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SGD (10—600keV)
Soft Gamma-ray
Detector
(Si+CdTe)
Nagoya U.
CR group
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Soft Gamma-ray Detector (SGD)
• Si/CdTe Compton Camera
• Active shield of BGO
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BH binary with jet
Synchrotron
Cyg X-1
GRS1915+105
Polarization will be detected
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SXT + SXI (0.3—12keV)
Soft X-ray Telescope
Soft X-ray
Imager
(X-ray CCD)
f=5.6m
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Soft X-ray Imager (SXI)
Thick depletion layer
~200um
Largest FOV
38min X 38min
Pch X-ray CCD
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Wide energy range (0.3—600keV)
HXI
SGD SXT
HXT
SXI
SXS
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ASTRO-H vs other observatories
suzaku Energy resolution
Energy range
Angular Resolution High-E sensitivity
low-E
sensitivity
ASTRO-H
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ASTRO-H under test
final integration test is now going on!
Mar 6
Micro Vibration Test
May 15
MTM Test
July 10
Delta Thermal Deformtion
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Summary
• ASTRO-H carries four instruments
–SXT + SXS, SXT+SXI, HXT+HXI, SGD
–Wide energy range
–High energy resolution
–High sensitivity in high-E X-rays
–Wide FOV
• Many science topics can be addressed
• ASTRO-H will be launched in FY2015
Visit http://astro-h.isas.jaxa.jp/index.html.en
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Flagship mission in X-ray astronomy
14 2015 16 17 18 19 2020 21 22 23 24 25 26 27 28 29 2030
ASTRO-H(2015~)
Athena(2028~)
Only small/medium
missions eROSITA (2016~),
NICER(2016~) etc.
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Europe Athena project
http://the-athena-x-ray-observatory.eu/
http://www.cosmos.esa.int/web/athena
June 27, 2014
Athena is approved as L2 mission
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ESA cosmic vision (2015-2025)
http://sci.esa.int/cosmic-vision/
Four themes
1) Planets and Life, 2) The Solar System
3) Fundamental Laws, 4) The Universe
ESA missions
L1: JUICE (2020~)
L2: Athena (2028~)
L3: gravitation (2034~)
M1: Solar Orbiter (2017~)
M2: Euclid (2020~)
M3: PLATO (2024~)
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Athena Scientific Objectives
• Hot Universe
– How does ordinary matter assemble into the large scale
structures that we see today?
• Energetic Universe
– How do black holes grow and shape the universe?
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Athena XRT
Wide Field Imager Xray Integral Field Unit
TES calorimeter DEPFET 12m
L2 orbit Ariane V M<5100kg Power~2500W Life>5 yrs
Si Pore Optics
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Hot Universe
Z=2
simulation
How and when was the energy of ICM produced?
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Energetic Universe
Discovery of High-z AGN
How do black holes grow and shape the universe
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Japan’s participation
• 高エネルギー宇宙物理学連絡会(高宇連; High-Energy Astrophysics Association in Japan) supports Athena.
– Athena WG in ISAS
• Chair: H. Matsumoto (Nagoya U.)
• HM joins to the Athena Science Study Team
– Europe (8) + USA(1) + Japan (1; HM)
• Athena team expects to collaborate with Japan
– Japan’s cryogenic technique is the best.
• Suzaku, ASTRO-H, SPICA, …
– Expertise through many successful X-ray missions