the hard x-ray modulation telescope (hxmt) fangjun lu (institute of high energy physics, chinese...
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The Hard X-ray Modulation Telescope (HXMT)
Fangjun Lu (Institute of High Energy Physics, Chinese Academy of Sciences)
On behalf of the HXMT group
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Low Energy X-ray Telescope (LE) (SCD, 1-15KeV,300 cm2)
Medium Energy X-ray Telescope (ME)(SiPIN, 5-30keV,1000 cm2)
Payloads of HXMT
High Energy X-ray Telescope (HE)
( 18 modules, 20-250keV,5000 cm2)
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• HE NaI(Tl)/CsI(Na) Phoswich– Total Detect Area ~5000 cm2
– Energy Range 20~ 250 keV– Energy Resolution ~16% (@60keV)– Continuum Sensitivity ~3.0×10-7 ph cm-2 s-1 keV-1 ,or 0.5 mCrab (3σ@100keV,105s)– Field of View 5.7°x 5.7°– Source Location ≤1 arcmin (20)– Angular Resolution ≤5 arcmin (20)
• ME 5-30 keV, SiPIN, 1000 cm2
(we are optimizing the design of HXMT and may will double the detecting area of ME)• LE 1-15 keV, SCD, 300 cm2
• Mass ~2700 kg (payload ~1100 kg)• Dimension 2.0×2.0×2.8 m3 (L×W×H)• Nominal Mission lifetime 3 years• Orbit Altitude 550km, Inclination 43° • Attitude Three-axis stabilized
Control precision: ±0.25° Stability: 0.005 °/s Measurement accuracy: <0.01°
Characteristics of the HXMT Mission
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Current Status of the HXMT Mission
– Proposed in 1993– 973 Major State Basic Research Project in China since April 2000 (Pre-
Phase A study)• Total about $5M• All the key technical problems for the HE telescope solved.
– Main participating institutions:• Chinese Academy of Sciences• Tsinghua University• Chinese Academy of Space Technology
– PI and Co-PI: Ti-Pei Li and Shuang-Nan Zhang– Selected last year as the first Chinese space astronomy mission for
launch around 2010• Full mission cost about $80M
– We just passed a technical review on this Wednesday, and HXMT is scheduled to enter pre-flight phase (Phase B) next October.
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Configuration of the high energy X-ray telescope
Active Shield
Collimator
Phoswich detector
PMTStructures
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Each module has a field of view (FOV) of 5.7º×1.1º and the long axes of two neighboring FOVs differ by 10º.
Collimator
Shielding Ring
Detector
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The Main Detector system of the HXMT
X-ray
photons
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-2 -1.5 -1 -0.5 0 0.5 1 1.5 2
-2
-1.5
-1
-0.5
0
0.5
1
1.5
2
( )水平方向 度
()
垂直方向度
多 源 成像结果等高图
2mci
2mci 1mci
15.3m观测距离:放射源强度:已标注
( ) 20cm放射源间距 最小值 :0.75对应角度为 度
0.1 成像位置精度: 度
The ground testing system
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The imaging performance of the HXMT
Source Location < 1 arcmin
Angular resolution < 5 arcmin
20 sigma source
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Sensitivity
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Angular Resolution 12’ 5’ 14’
Source Location (20σ) 1’ 1’ 1’
Pointed Sensitivity (mCrab@100 keV, 105s) 3.8 0.5 9
½ Year Survey Sensitivity (mCrab,20-250keV) 2 0.5 1
Observation Capability All sky survey ok good yes
Selected sky deep survey good good bad
Narrow field pointing observation bad good no
Integral/IBIS HXMT/HE Swift/BAT
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Low energy X-ray telescope(2 modules, 300 cm2)
Collimator : fabricated with Electro-deposition or from plates.
FOV of 1°x 6°and 1°x 3°,
Thickness: 5cm.
Material can be Gold-plated copper.
Detector: SCD ( Swept Charge Device ) developed by e2v.
Energy range: 1 - 15 keV, Time resolution :1ms, Spectral resolution:
Working temperature : -30 -0℃
Main Scientific Objectives:( 1 ) Extending the energy coverage to low energy
( 2 ) Multi-wavelength X-ray variability
( 3 ) Absorption column density to AGNs
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Medium Energy x-ray telescope (ME)(2 modules, 1000 cm2)
Collimator: similar to that of LE and defines FOV of 1°×6°.
Detector : covers 5 -30keV, using SiPIN or thin CdZnTe
Main Scientific objectives:( 1 ) Cosmic X-ray background; ( 2 ) Absorption materials surrounding AGNs; ( 3 ) Temporal variability in medium energy X-ray.
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Continuum Sensitivity of ME
HXMT 3sigma in 10^5 s
1.00E-07
1.00E-06
1.00E-05
1.00E-04
1.00E-03
1.00E-02
1.00E-01
1.00E+00
1.00E+01
1 10 100 1000
Ex (keV)
Ph
oto
ns
cm-2
s-1 Crab
HXMT NaI
500u 10^3 cm^2
50u 10^3 cm^2
15u 10^3 cm^2
IBIS-ISGRI
0.1 mCrab@10 keV
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A Possible Fourth Telescope
–ASI of Italy contributes a pair of X-ray focusing telescopes plus X-ray polarimeter (XRT+XPOL) for HXMT.
–People involved:
Enrico Costa, Fabio Muleri, Paolo Soffitta, Ronaldo Bellazzini Alessandro Brez, Gloria Spandre, Vincenzo Cotroneo, Giovanni Pareschi
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From the modulation curve it is derived the polarization degree and angle of the X-ray source.
Bellazzini et al. 2006
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Interface Electronics
Control Electr
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Current design
Sensitive Area of the telescope
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Minimum Detectable Polarization
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Observation modes
• Survey
– All sky scan mode
– 3-axis stabilized anti-earth oriented:
• roll angle=0º , region span=-43º-43º, 66 days
• roll angle=30º , region span=-13º-73º, 66 days
• roll angle=-30º , region span=-73º-13º, 66 days
• Deep scanning observation of selected sky regions
• Pointed observations
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HXMT Sky Survey Observations
The three-phase sky survey of HXMT. In phase (a) the roll angle is β=0°, and the scanned declination range is δ=-43° - 43°, in phase (b) β=30° and δ=-13° - 73°, and in phase (c) β=-30°, δ=-73° - 13°. (d) illustrates the total exposure after the three-phase scan survey.
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HXMT is capable of conducting a deep full sky survey in half a year with a sensitivity of 0.5 mCrab (20-250 keV), and more than 1,000 hard X-ray sources will be detected. The sensitivity around 10 keV is about 0.1 mCrab with ME.
Background fluctuations, all within 3.15 σ Significance distribution of a 0.5 mCrab source, 60% are higher than 3.15σ
Monte-Carlo simulations of the sensitivity of HXMT (for point sources) in a half-year all-sky survey
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Simulated HXMT capability on Galactic diffuse hard X-ray emission.
Model: Strong et al A&A 411, L447(2003), Fig.2
HXMT simulation
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On going hard X-ray survey projects
• The US satellite SWIFT can do hard X-ray all-sky survey. Its survey sensitivity is dominated by systematic errors. For regions in the Galactic Plane (l<45°, 2/3 of the whole sky ) where there are several strong sources always in the BAT FOV, the limiting sensitivity will be ~2 mCrab. For l>45°(1/3 sky), the limiting sensitivity will be ~0.6 mCrab. The final SWIFT hard X-ray catalogue may will contain 200 extragalactic hard X-ray sources (Barthelmy et al. astroph/0507410) .
• Two years of INTEGRAL/IBIS observation has reached ~1 mCrab for regions with the deepest exposures and 209 sources (in which ~50 are active galactic nuclei) have been catalogued.
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The real survey program may will be changed according to how deep the final SWIFT/BAT and INTEGRAL/IBIS survey will be. If they reach a sensitivity of 0.5 mCrab for most of the sky, we may will carry out for example an one-year survey for half sky to improve the sensitivity.
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Small region scan• Deep scan of interesting regions to reach high
sensitivity (such as the lockmann hole region and the Galactic Center region. Theoretically, an one-month’s observation of a region with a radius of 10º can reach a sensitivity limit of 0.1mCrab.
• Periodically scan of the Galactic bulge to study the variations of the Galactic hard X-ray sources.
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Pointed Observations• Study the X-ray variability at multi-wavelength (1-
250 keV) of the X-ray binary systems: QPOs, relations between the hard and soft X-ray components.
• Study the broad band X-ray spectrum of bright AGNs, X-ray binaries, bright SNRs, pulsars, and bright clusters of galaxies.
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BeppoSAX Spectrum of Coma
Simulated HXMT specturm of Coma (105s)
BeppoSAX spectrum of Coma -- 4.5σ detection of non-thermal X-ray emission.
Simulated HXMT spectrum of Coma-- much better constraints on the non-thermal component.
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Simulated HXMT spectrum of Cas A.
Current SNR X-ray specturm. Only up to 30 keV
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Hard X-ray sky survey with highest sensitivity• High precision multi-wavelength X-ray full sky map: diffuse
background and cosmic variance
• Discover highly obscured supermassive BHs and study the
obscuring materials: galaxy formation and evolution
• Discover new types of high energy objects: usual surprises of
new surveys
• Diffuse hard X-ray emission in the Galaxy.
Main advantages and key science of HXMT
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Main advantages and key science of HXMT (II)
High precision pointed observations of high energy objects• Space-time in strong gravitational field: dynamics and radiation
near BH horizons of stellar mass and supermassive BHs
• Equation of state in strong magnetic field: neutron star and its
surface properties
• High energy particle acceleration: AGN, SNR, shock and relativistic
jets
• Large scale structure: through hard X-ray detection of galaxy
clusters
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Bey
ond
Ein
stei
n P
rogr
am
HXMT
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Orbit and Operation
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Constraints on Orbit Design• Operation mode: survey mode requires inclination angle
not less than 25° (sky coverage) and precession speed of the orbital plane not exceeds 0.3 ° /orbit ( ~1/3 of FOV 1.1 ° )
• Low background level: lower inclination angle• Reduce the passage of SAA belt and other radiation belt • Ground station: Beijing Station only• Launch station: Xichang, Taiyuan, Jiuquan• Nominal Lifetime: 3 yrs (height > 500km)
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Final orbit parameters
• Low Earth Orbit
• Height: 550km
• Inclination angle: 43~45°
• Period: ~96min.
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HXMT schedule
2007
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Con-X
XEUS
HXMT
See further (earlier)
and clearer
See inner
Evolution of the whole universe
Survey the local universe
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Thanks!