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ASTRO-H
Quick Reference
(http://astro-h.isas.jaxa.jp/ahqr.pdf)
ASTRO-H Science Office
<[email protected]>
Contents
I. Overview
IV. Figures of Merit
1. ASTRO-H mission
2. Spacecraft & Components
3. Parameters
1.
2.
3.
4.
II. Telescopes
V. Case Studies
1. SXT
2. HXT
1. Black holes
2. Supernova remnants
3. Clusters of galaxies
III. Instruments
1.
2.
3.
4.
Effective area
Limiting sensitivity
Energy resolution
FoV & Grasp
SXS
SXI
HXI
SGD
Further information
Releases
2010-08-18 For A-H 1st Summer School
(N. Ota, M. Tsujimoto)
2010-11-09 HXI & SGD updates (H. Takahashi)
1
I. Overview
I-1. ASTRO-H Mission
Overview
ASTRO-H is an international X-ray observatory, which is the 6th in the series of the X-ray
observatories from Japan. It is currently planned to be launched in the fiscal year 2013 with
an H-IIA rocket from the Tanegashima Space Center, Kagoshima, Japan.
Launch site
Tanegashima Space Center
Launch vehicle
JAXA HII-A rocket
Orbit Altitude
550 km
Orbit Type
Approximate circular orbit
Orbit Inclination
< 31 degrees
Orbit Period
96 minutes
Total Length
14 m
Mass
< 2.6 metric ton
Mission life
> 3 years
Fig. 1 Artist's drawings of
the ASTRO-H satellite.
Scientific objectives
●
Revealing the large-scale structure and its evolution of the Universe
●
Understanding the extreme conditions in the Universe
●
Exploring the diverse phenomena of non-thermal Universe
●
Elucidating dark matter and dark energy
Key technologies
The ambitious scientific goals are made possible with many novel technologies developed
for ASTRO-H, including
1. An X-ray micro-calorimeter detector which enables high resolution (5 eV) spectroscopic
observations between 0.3 and 12 keV.
2. Hard X-ray telescopes to provide X-ray images and spectra to 80 keV.
3. Detectors allowing observations over an extremely large energy range of 0.3-600 keV.
Fig. 2 Scientific instruments onboard the ASTRO-H satellite and energy coverage.
2
I. Overview
I-2. Spacecraft & Components
3
I. Overview
I-3. Parameters
Table 1 Properties of ASTRO-H telescopes (current best estimate)
Properties
SXT
HXT
Diameter (cm)
45
45
Focal length (m)
5.6
12
No. of nested shells
203
213
Reflector coating
Aeff (cm2)
HPD (arcmin)
2
FoV (arcmin )
multilayer
Al (0.03 µm)
+ PET(5 µm)
(0.2 µm)
HXT
279/312
338
(@0.5/6keV)
(@30keV)
1.3
1.7
22.2 /19.8
2
6.42/5.32
(@0.5/6 keV) (@30/50keV)
Stray-light
reduction rate
>99 (@30'
>99 (@15'-
off-axis)
25' off-axis)
Thermal shield
70
92
transmission (%)
(@0.5keV)
(@5 keV)
Al (0.03 µm)
+ polyimide
SXT
2
Pt/C
Au
Thermal shield
Properties
Table 2 Properties of ASTRO-H instruments (current best estimate)
SGD
SGD
(photo-abs)
(Compton)
300
150
20
(@0.5/6 keV)
(@30 keV)
(@30 keV)
(@100 keV)
0.3-12.0
0.4-12.0
5-80
10-600
40-600
1.3
1.3
1.7
N/A
N/A
Properties
SXS
SXI
HXI
Effective area
50/225
214/360
(cm2)
(@0.5/6 keV)
Energy range (keV)
Angular resolution
in HPD (arcmin)
Field of view
(arcmin2)
Energy resolution
in FWHM (eV)
33x33 (<150 keV)
3.05x3.05
38x38
9x9
600x600
(>150 keV)
5
33x33 (<150 keV)
600x600
(>150 keV)
150
< 2000
2000
4000
(@6 keV)
(@60 keV)
(@40 keV)
(@40 keV)
several x 10-5
several x 10-5
several x 10-5
Timing resolution (s)
8x10-5
4
Instrumental background
2x10-3/0.7x10-3
0.1/0.1
(/s/keV/FoV)
(@0.5/6 keV)
(@0.5/6 keV)
6x10-3/2x10-4
(@10/50 keV)1
2x10-3/4x10-5
(@10/50 keV)2
1
4 layers, 21 layer
1x10-4/1x10-5
(@100/600
keV)
4
II. Telescopes
II-1. Soft X-ray Telescopes
Basics ASTRO-H has two identical Soft X-ray Telescopes (SXTs). One is for SXS (SXT-S) and
the other for SXI (SXT-I). SXT is a similar in concept to the X-Ray Telescope (XRT) of Suzaku
(table 1). It is composed of 203 thin reflector shells tightly nested confocally and coaxially. A
conical approximation of Wolter-I type optics is used.
Table 1 Comparison of ASTRO-H/SXT and Suzaku/XRT
No. of
telescope
Focal
length
(m)
Diameter
(cm)
No. of
nested
shells
HPD
(arcmin)
SXT
2
5.6
45
203
1.3
560
425
XRT-I
4
4.75
40
175
2.0
470
320
Aeff
(cm2)*1
Aeff is the on-axis effective area (mirror only) at 0.5 & 6 keV. Source extraction of r=∞, or 100% photons are
encircled. The value for one unit for XRT-I.
*1
Technology Three different thicknesses of Al substrates (152, 229,
and 305 μm) are used, in which the outer shells use the thicker
substrates. This is intended for achieving a large collecting area with
a better imaging quality than Suzak/XRT. The considerably better
HPD than XRT (table 1) is realized by fixing the reflectors to support
bars with adhesive. Stray light, or contaminating X-rays from outside
of the field of view, is reduced by a stray-light baffle, which consists
of coaxially-nested cylindrical aluminum blades placed above each
reflector. A thermal shield is attached in front of the pre-collimator to
stabilize the thermal environment of the SXT. The shield is made of
Al-coated Polyimide film to ensure a large effective
Fig. 1 Schematic view of SXT. The blue and red parts
area in the soft energy band.
are the mirror housing and pre-collimator, respectively.
Performance
Fig. 2 Effective area (mirror only) as a function
of energy at on-axis and some off-axis angles.
Source extraction from a r=1.8' circle (78%
encircled energy fraction).
Fig. 3 Encircled effective area, representing the
sharpness of an image at several energies at
on-axis and some off-axis angles.
5
II. Telescopes
II-2. Hard X-ray Telescopes
Basics ASTRO-H has two identical Hard X-ray Telescopes and the HXIs, with an HXI at the
focus of each HXT. The global structure is very similar to that of SXTs, but the focal length,
the reflector length, and the reflector coating are optimized for hard (> 10 keV) X-ray
imaging. It is composed of 213 nested sets of conically approximated thin-foil Wolter-I type
reflectors.
Technology The surface of the reflector is coated
with a stack of depth-graded Pt/C multi-layer, which
reflects hard X-ray photons by Bragg reflection
(fig. 1). The mirrors are fabricated by the replication
Fig. 1 Schematic view of a Bragg reflection.
method, in which a depth-graded Pt/C multi-layer
is sputtered onto the smooth surface of a glass tube and
transferred to a conically shaped aluminum substrate with epoxy glue.
The “pre-collimator”, or the stray-light baffle, is mounted atop the HXT.
The thermal shield is integrated on top of the pre-collimator to
keep the HXT temperature within a specific range.
Performance The current best estimate of the HPD is ~1.7'.
The effective area is plotted vs. energy (fig. 3) and off-axis
angle (fig. 4). Other performance parameters are being
characterized now.
Fig. 3 HXT on-axis effective area (one unit) with an
interfacial roughness of 3(black), 4(red) and 5
Å(green). The blue points indicate the 1st and 2nd level
requirements.
Fig. 2 Schematic view of HXT.
Fig. 4 The vignetting function at 10 keV (black), 30
keV (red) and 50 keV (green) calculated by the raytracing simulator for the ideal reflector case. The
interfacial roughness is 3 Å assumed.
6
III. Instruments
III-1. Soft X-ray Spectrometer
Basics The Soft X-ray Spectrometer (SXS) is equipped with an X-ray microcalorimeter array
of 6x6 pixels at the focus of the Soft X-ray Telescope (SXT), which is capable of nondispersive high-resolution (∆E~5 eV) spectroscopy and limited imaging of 3x3 field of view in
the soft X-ray (0.3-12 keV) band with a large effective area.
Technology The detector measures the temperature rise upon
each incident X-ray photon, achieving an unprecedented energy
resolution. The thermometer is made of HgTe absorbers of a 8µm
HgTe
thickness on micro-machined, ion-implanted Si wafer. The anticoincidence Si semiconductor detector enables rejection of
background events. The mK temperature in the dewar is achieved
by the cooling system comprised of adiabatic demagnetization
refrigerators, He coolants, and mechanical coolers. The cooling
Fig. 1 Concept of X-ray micro-calorimetry.
system allows redundancy and cryogenic-free operation.
The filter wheel provides a suite of attenuation filters to enhance the dynamic range of the
SXS. The modulated X-ray source is planned for accurate response calibration.
Performance Since the SXS is a non-dispersive spectrometer, it can be used to obtain highresolution spectra of both point and extended sources (fig. 3). The effective area of >200
cm2 at the Fe K-band is considerably larger than any other high-resolution spectrometers.
The imaging capability is limited as the HPD is comparable to the FoV (fig. 2).
Fig. 2 Pixel layout. The array encompasses
~74% of photons of a point source at the center.
Fig. 3 Simulated spectrum of Centaurus cluster.
CCD
µ-calorimeter
Fig. 4 Grade definition. Calorimeter resolution
(∆E<10 eV) is obtained only for high-res (HR)
and med-res (MR) events.
Observation modes SXS has only one observation
mode. All X-ray events are graded (fig 4). The digital
processor is capable of handling only 250/s ~ 150
mCrab (“PSP limit”). For bright sources,
it is beneficial to intentionally Fig. 5 Filter selection.
reduce the incoming photons
open
using filters (fig. 5) and/or
25µm
50µm
Be
Be
disabling center pixels
dominated by LR events.
25%
ND
open
OBF
Fig. 6 Incident vs. observed rate.
7
III. Instruments
III-2. Soft X-ray Imager
Basics The Soft X-ray Imager (SXI) is equipped with X-ray CCD devices placed at the focal
plane of the Soft X-ray Telescope (SXT-I). The SXI has an imaging-spectroscopic capability of
a wide field (38 arcmin2) and a medium energy resolution (E/∆E~40@6keV) at the soft X-ray
band (0.4-12 keV). The SXI is a successor of the XIS onboard the Suzaku observatory.
Table 1 Comparison of ASTRO-H/SXI and Suzaku/XIS.
No. of
CCD
No. of
telescope
Layout
Pixel
scale
Format
(one
CCD)
FoV
(sq.arc
min)*1
SXI
4
1
2x2
array
1.74”
640x
640
38x38
XIS
4
4
4 coaligned
1.04”
1024x
1024
18x18
*1
Grasp
(cm2
arcdeg2)
Frame
time
(s)
Illumin
ation
Type
Depl.
layer
(µm)
214
360
40
4
BIx4
p-chan
200
240
950
35
8
FIx3,
BIx1
n-chan
80 (FI),
45 (BI)
Aeff
(cm )
2 *2
FoV for the 2x2 array for SXI. *2Aeff is the on-axis effective area at 0.5 & 6 keV. Four CCDs combined for XIS.
Technology Mechanical coolers will be used to keep the
device temperature at -120 C. The p-channel CCD will have a
thick depletion layer to extend the hard-band coverage. The
thick depletion layer also leads to a significant background
reduction above ~7 keV compared to the same BI CCD in
Suzaku/XIS. The BI devices is more resistant than the FI
devices to micro-meteorite hits, which made a part of the XIS
dysfunctional. The design is underway to suppress
contamination accumulation on the CCD chips. Onboard
calibration source is under discussion.
Fig 1. Schematic view.
Performance The 2x2 CCD array covers a very large FoV. The nominal position is placed at
the center of SXS FoV, which is 4.'3 offset from the SXI center. A gap of ~20” is between the
chips. Similarly to XIS, the background level of SXI is expected to be low and stable,
benefiting from the low-earth orbit of the satellite.
Fig 3. Redistribution of 55Fe source
measured with a proto-type CCD.
Fig 2. Layout of SXI array and SXS FoV.
Observation mode Several CCD clocking mode (partial read and stacking) will be supported
for the main purpose of mitigating CCD pile-up. The detail is under discussion.
8
III. Instruments
III-3. Hard X-ray Imager
Basics The Hard X-ray Imager (HXI) is the detector assembly that comprises the hard X-ray
imaging system with the Hard X-ray Telescope (HXT). ASTRO-H has two identical HXT-HXI
systems. The HXI is equipped with multi-layered imaging devices, enabling hard X-ray
imaging and spectroscopic observations.
Technology The detector assembly consists of
four-layers of double-sided Si strip detectors
(DSSD; 0.5 mm) and one layer of CdTe doublesided strip detector (CdTe DSD; 0.5-1 mm) at
the bottom (fig. 1). Soft X-rays (<30 keV) are
absorbed by the DSSD, while hard X-rays (2080 keV) penetrate the DSSD and are captured
by the newly developed CdTe DSD. The total
thickness of the DSSD amounts to 2 mm,
which is comparable to the HXD-PIN onboard
Suzaku. The fast timing response of both DSSD
and CdTe DSD detectors allows us to place the
entire detector assembly at the bottom of a
very deep well of the active BGO shield, which
works as a veto counter.
Fig. 1 Schematic view of HXI.
Performance The combination of HXI + HXT will obtain images and spectra at 10 -70 keV.
The HXI has good energy resolution (fig. 2), and low-level of background due to the use of a
BGO active shield. Since each event is read out separately with good time resolution, the HXI
can observe bright sources without pile-up.
DSSD
CdTe DSD
ALL
(4-layer DSSD
+ 1-layer CdTe)
DSSD
Top 1-layer
Fig. 2 Energy spectra of DSSD (left) and CdTe
DSD (right) detectors with 241Am source.
Fig. 3 Detection efficiency of 1layer (0.5 mm-thick) DSSD (black)
and all (4-layer DSSD + 1-layer
CdTe DSD) of the HXI (red).
Observation mode The HXI has only one mode. For data reduction, observers may select
events in the following way depending on source fluxes, images (point/diffuse source) and
spectra.
- Normal (bright/hard) sources : Events detected with all of the HXI detectors.
- Faint/soft sources : Events with only the top 1-layer DSSD. Soft X-rays tend to be
detected by the top layer, while the background distributes over the entire detectors,
especially the CdTe DSD.
III. Instruments
III-4. Soft γ-ray Detector
Basics The SGD is a non-imaging soft gamma-ray detector covering a 10—600 keV
energy range at x10 better sensitivity than the Suzaku HXD at 300 keV. It outperforms
any previous soft γ-ray instruments in background rejection capability by adopting a new
concept of narrow-FoV Compton telescope. SGD also has a polarimeteric capability.
Technology A Compton telescope is made up of a stack of Si pad detectors and CdTe
pixel detectors, which drastically reduces the background and thus improves the
sensitivity. The telescope is mounted at the bottom of a well-type active shield. Incident
photons of E>40 keV sometimes interact twice in the stacked detector; once by Compton
scattering in the stack of Si pad detectors and another by photoelectric absorption in the
CdTe detector (“Compton mode”). With the Compton kinematics, the energy and direction
(as a cone in the sky) of each incident γ-ray are derived from the locations and energies of
the two interactions. Events from the collimator FoV are selected (narrow FoV Compton
telescope).
Fig. 1 Schematic views of the SGD (left,
middle) and a Compton camera unit (right).
The SGD has 6 Compton camera units in total.
Performance SGD uniquely performs highly sensitive observations at several hundred
keV with a good energy resolution. Each event is read out separately with good time
resolution. For Compton events, the SGD has the capability to study the polarization of
soft gamma-rays.
Fig. 2 Effective area of the Compton mode of
the SGD.
Fig. 3 Estimated SGD background level of the
Compton mode (Red). The neutron background
component (green) and the activation background
component (blue) are also shown.
Observation mode The SGD has only one mode. For data reduction, the following event
selection is recommended depending on source flux.
- Normal sources : Events detected with the Compton mode.
- Bright sources : Events with the photo-absorption mode as well as the Compton mode.
9
10
IV. Figures of Merit
IV-1. Effective Area
Fig. 1 On-axis effective area of all ASTRO-H telescopes &
detectors, SXT-I+SXI, SXT-S+SXS, HXT+HXI (2 units).
Fig. 2 SXT-S+SXS on-axis effective area with filter: the
open filter(red), optical blocking filter(black), 25μm/50μm
Be filter (green/blue).
Fig. 3 On-axis effective area of ASTRO-H, Suzaku (XIS-BI+XIS-2FI, HXD), Chandra (ACIS-S), XMM
(PN+MOS1+MOS2), and NuSTAR.
IV. Figures of Merit
IV-2. Limiting Sensitivity
Fig. 1 3σ sensitivity targets for the SXI, HXI, and SGD for continuum emissions from point source (the upper
panel) and extended sources (the bottom panel) assuming an exposure time of 100 ks, and comparison with
other hard X-ray instruments (Tajima et al. 2010 Proc. of SPIE).
11
12
IV. Figures of Merit
IV-3. Energy Resolution
(i) Strong line: FOM ~ √A
(ii) Weak line: FOM ~ √(A/ΔE)
(iii) Strong line: FOM ~ √(A E2/ΔE2)
(iv) Weak line: FOM ~ √(A E2/ΔE3)
(v) Strong line: FOM ~ √(A E4/ΔE4)
(vi) Weak line: FOM ~ √(A E4/ΔE5)
Fig. 1 Figures of merit (FOM) for (i) detection of strong line, (ii) detection of weak line, (iii) velocity
of strong line, (iv) velocity of weak line, (v) broadening of strong line, (vi) broadening of weak line.
IV. Figures of Merit
IV-4. FoV and Grasp
Fig. 1 Field of views of the ASTRO-H instruments, SXS, SXI, HXI (the red boxes). Chandra ACIS-I and
XMM are also shown for comparison. The background image is the Coma cluster taken with ROSAT
(credit: ROSAT/MPE/S. L. Snowden).
Fig. 2 Grasp vs on-axis effective area at 7 keV of SXT-I+SXI, SXT-S+SXS. Suzaku XIS, Chandra
ACIS-I, XMM PN are also shown for comparison.
13
14
V. Case Studies
V-1. Black Holes
ASTRO-H provides an unprecedented view of the motions and extreme physical conditions of
matter near the event horizon. This will help us unravel how black holes grow by accreting
gas and simultaneously shape their environments via the intense radiation fields and
powerful, sometimes relativistic, matter outflows that accompany this accretion.
Gaseous winds driven from black hole disks can carry away a substantial fraction of the gas
that would otherwise accrete onto the central black hole. Such winds are hot, and most easily
detected in the Fe K band via absorption lines. As shown in fig. 1, the superior resolution of
SXS in the Fe K band enables the unambiguous detection of weak and narrow lines from a
wind. We will be able to use these to precisely determine the radius at which the wind is
launched and the mass outflow rate carried by it. This will give us strong constraints on the
driving mechanism of the wind and its feedback on the accretion flow as well as the black
hole’s environment.
logNH=23.7
24
24.7
25
Instrumental BGD limit
Fig. 1 A simulated spectrum of the black hole GRO
J1655-40 with a 100ks SXS observation. The model is
based on a prior Chandra observation.
Fig. 2 Simulated HXI spectra of heavily obscured AGN
with different absorbing columns (NH) for an exposure
of 100ks (300ks for logNH=25). The continuum is
assumed to be a power-law of photon index 1.9 with an
intrinsic 2-10 keV flux of 1x10-11 erg/s/cm2 (based on
Swift J0601.9-8636, Ueda et al. 2007).
ASTRO-H will also give us key observations to investigate the co-evolution of supermassive
black holes and their host galaxies.
Recent observations imply the existence of a large number of Active Galactic Nuclei (AGN)
that are heavily obscured by the gas and dust surrounding their supermassive black holes.
Some are identified as a "new type" of AGN, so deeply buried in dense tori of gas that they
show little emission in soft X-ray and visible light. While this has made such objects
extremely difficult to detect and observe, this highly obscured activity may in fact represent
the dominant phase of supermassive black hole growth. Understanding this phase is thus
key to understanding the correlated evolution of the black hole and its host galaxy. As
shown in fig. 2, the high sensitivity for hard X-rays provided by HXI allows precise spectral
studies of even very obscured AGN. ASTRO-H will provide us with a large AGN sample to
pursue systematic studies of the true AGN population, unbiased by obscuration effects, and
to measure the co-evolution of supermassive black holes with their host galaxies.
15
V. Case Studies
V-2. Supernova Remnants
The high resolution X-ray spectroscopy provided by SXS will be particularly ground-breaking
for supernova remnants (SNRs) because they are extended objects with rich emission-line
spectra from a wide range of different elements (carbon through nickel). To determine the
element abundances reliably, measurements of the relative strengths of a number of lines
from each elemental species are required. Accurate element abundances provide constraints
to test the explosion mechanisms of supernovae and to explore their environments.
Gas motions of the rapidly expanding supernova ejecta and swept-up interstellar and/or
circumstellar medium may also be measured by SXS by their Doppler shifts. Gas moving
toward or away from us will show shifts in the energies of the emission lines. Velocity
measurements are needed to understand how SNRs evolve, based on their age and the
detailed properties of the explosion, the ejecta, and ambient medium.
Fig. 1 Simulated spectra of the iron K-shell
complex from the inner region of the Tycho
SNR with an exposure of 100 ks with SXS.
The ion temperature is assumed to be 30
billion degrees (black) or negligible (green).
Red- and blue-shifted lines from the fast
moving gas can be readily resolved with SXS.
Particle acceleration is receiving much
attention at present, but the origin of
cosmic rays is still unclear 100 years
after their discovery. Young SNRs with
shock speeds of several 1000 km/s are
among the best candidates to accelerate
cosmic rays up to the knee around 10 15
eV (the highest energy accessible to
Galactic accelerators). The combination
of ASTRO-H's hard X-ray imaging
capability and high spectral resolution
will provide information to understand
crucial aspects of shock acceleration in
SNRs such as the maximum energy of
the accelerated particles, the conditions
at the acceleration sites, and the
acceleration efficiency.
Fig. 2 Simulated 100ks
HXI image of the SN
1006 NE shell.
16
V. Case Studies
V-3. Clusters of Galaxies
The dominant baryonic matter component in galaxy clusters is hot intergalactic gas, heated
by shocks during violent cluster mergers. By observing its emission lines with calorimetric
energy resolution, the SXS will be able to detect turbulence and gas flows generated during
such mergers, which may persist for billions of years. Understanding kinematics of the cluster
gas is of great importance for the physics of cluster formation and for “precision cosmology”.
In bright cluster cores, the SXS will be able to resolve a tangle of lines from different ions,
while the low-background SXI will map the gas temperatures far in the cluster outskirts.
Intracluster shocks and turbulence are believed to produce ultra-relativistic cosmic rays,
which create faint radio synchrotron halos and “relics”. The HXI will detect non-thermal
emission from the brightest relics, vastly enhancing our understanding of cosmic ray
generation.
Simulated spectra below give a sample of measurements that will push ASTRO-H capabilities
to the limit. In a low surface brightness region of a nearby merging cluster A3667, the SXS
will be able to detect turbulence with a Mach number (the speed of the flow compared to the
speed of sound) as low as M=0.2. For the bright radio relic in A3667, believed to trace an
outlying shock front, the HXI will disentangle thermal emission from the intra-cluster gas
(observed by XMM) and Inverse Compton emission from ultra-relativistic electrons, producing
the first unbiased estimate of the energy in cosmic rays and the cluster magnetic field.
HXI spectrum of the relic in A3667
HXI
IC (assuming B=1μG)
T=5 keV
radio contours
(synchrotron emission)
100 ks
A3667
z=0.05
SXS spectrum of a low-brightness region
Chandra image
(thermal emission)
SXS
500 kpc
17
Further Information
Web pages
●
ASTRO-H <http://astro-h.isas.jaxa.jp/>
References
●
●
●
●
●
●
●
[ASTRO-H] Takahashi et al. 2010, Proc. of SPIE
[SXS] Mitsuda et al. 2010, Proc. of SPIE
[SXI] Tsunemi et al. 2010, Proc. of SPIE
[HXI] Kokubun et al. 2010, Proc. of SPIE
[SGD] Tajima et al. 2010, Proc. of SPIE
[SXT] Serlemitsos et al. 2010, Proc. of SPIE
[HXT] Kunieda et al. 2010, Proc. of SPIE
Mailing lists
●
●
●
ASTRO-H collaboration (all members) <[email protected]>
Science office <[email protected]>
Calibration & Software board <[email protected]>
Points of Contact
(Questions specific to sub-systems)
[SXS] Naomi Ota (Nara Women's U.) <[email protected]>
[SXI] Nasayoshi Nobukawa (Kyoto U.) <[email protected]>
[HXI] Hiromitsu Takahashi (Hiroshima U.) <[email protected]>
[SGD] Hiromitsu Takahashi (Hiroshima U.) <[email protected]>
[SXT] Yoshito Haba (Nagoya U.) <[email protected]>
[HXT] Yoshito Haba (Nagoya U.) <[email protected]>
Science Task Force Leaders
Stars & WDs : Jelle Kaastra (SRON)
Compact objects : Jon M. Miller (Michigan)
Particle acceleration : Felix Aharonian (DIAS)
Supermassive black holes and their environments : Chris Reynolds (Maryland)
Cluster dynamics and evolution : Maxim Markevitch (Harvard/CfA)
Chemical evolution : John P. Huges (Rutgers)
Feedback phenomena : Andy Fabian (Cambridge)
Cosmology and GRBs : Tetsu Kitayama (Toho)
Radiation processes : Frits Paerels (Columbia)
Multi-wavelength follow-up and transients : Paolo Coppi (Yale)