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Brief Overview of China’s Future Space X-ray Astronomy Program. Shuang-Nan Zhang Center for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences. Outline. Approved missions: launch within the next 5 years Hard X-ray Modulation Telescope (HXMT) - PowerPoint PPT Presentation
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Brief Overview of China’s Future Space X-ray Astronomy Program
Shuang-Nan Zhang
Center for Particle AstrophysicsInstitute of High Energy PhysicsChinese Academy of Sciences
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Outline• Approved missions: launch within the next 5 years
– Hard X-ray Modulation Telescope (HXMT)– Space Variable Object Monitor (SVOM): China-France
collaboration (Barret’s Talk)– Gamma-ray burst polarimeter (POLAR): China-Europe
collaboration on China’s Spacelab• In mission definition and technology development phase:
launch within next ~10 years– X-ray Timing and Polarization mission (XTP)
• Proposed onboard China’s Space Station: launch around 2021-2022– Optical/UV/X-ray All-Sky Monitor
Payload Cabin
Platform Cabin
Chinese Academy of Sciences, Tsinghua UniversityChinese Academy of Space Technology
HXMT is a collaboration between:
Payloads onboard HXMT
LE:S
CD
,384 cm2
HE: NaI/CsI 5000 cm2
Size ： 1900×1600×1000 mm3
ME
:Si-P
IN,952 cm
2
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A sunshading board will be set so that the LE and ME instruments can work at low temperatures
The Sun
LE
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High Energy X-ray Instrument
HXMT/HE Components assembly• The 18 main collimated phoswich detectors• Charged-particle anticoincidence plates (6 pieces up side +12
lateral side)• Particle Monitor detectors• Calibration detectors (automatic gain control)
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The Field of View configuration of HE
1 Blind Module2 Modules of 5.7 °× 5.7 °
15 Modules of 1.1 ° × 5.7 °
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16 Si-PIN (0.56 cm2 each) pixels will be in one package and 2 packages read by a RENA-3 asic.
Detector: Si-PIN
Energy coverage: 5-30 keV
Detecting area: ~950 cm2 (1728 pixels)
Sensitivity: 0.5 mCrab
Field of view: 1°×4°,4 °×4°, blind field
Energy resolution: < 1.5 [email protected]
Work temperature: -20~-40 for Si-PIN℃
Time resolution: 40 μs
Mass: 105kg
Power dissipation: 130 W
2×2CCD236 16 cm2
The low energy instrument (LE)
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FOVs of an LE module
The Hard X-ray Modulation Telescope @ EAMA-7
Charge flow
Real & dummy outputs in gap
Schematic map of a CCD236 (e2v)
Detector: SCD
Energy coverage: 1-15 keV
Detecting area: ~384 cm2 (96 chips)
Sensitivity: 0.5 mCrab
Field of view: 1.5°×6°,4 °×6°, blind field
60 °×3°(48cm2),
Energy resolution: <150 eV@6keV
Work temperature: -40~-80 for SCD℃
Time resolution: 1 ms
Mass: 105 kg
Power dissipation: 130 W
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Detectors LE: SCD, 384 cm2;ME : Si-PIN, 952 cm2
HE : NaI/CsI, 5000 cm2
Energy Range LE: 1-15 keV;ME: 5-30 keV;HE: 20-250 keV
Time Resolution HE: 25μs; ME: 20μs;LE: 1ms
Energy Resolution LE: 2.5% @ 6 keV ME: 8% @ 17.8 keV HE: 19% @ 60 keV
Field of View of one module
LE: 6°×1.5°; 6°×4°; 60°×3°; blind;ME: 4°×1°; 4°×4°; blind;HE: 5.7°×1.1°; 5.7°×5.7° ； blind
Source Location <1' (20σ source)
Characteristics of the HXMT Mission
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Sensitivity (3σ, in 105s)
LE: 4.4×10-5 cts cm-2s-1 keV–1 (@6keV)ME: 2.6×10-5 cts cm-2s-1 keV–1 (@20keV)HE: 3×10-7 cts cm-2s-1 keV–1 (@100keV)
Orbit Altitude: ~550 km ; Inclination: ~43°
Attitude Three-axis stabilizedControl precision: ±0.1°Measurement accuracy: ±0.01°
Data Rate LE: 3 Mbps; ME: 3 Mbps; HE: 300 kbps
Payload Mass ~1000 kg
Nominal Lifetime 4 years
Working Mode Scan survey, pointed observation
Scientific objectives of pointed observations
• X-ray Binaries
– Broadband X-ray variability, especially the QPO properties of BH
binaries at energy higher than 20 keV;
– Broadband spectral characteristics and state transitions
• Cyclotron Resonance Features (CRF) close to the neutron star
surface;
• Broadband spectrum of bright AGN: reflecting components and
high energy cut off;
Observation modes
• Scanning Sky Survey mode
• Deep scanning observations of selected sky regions (such as the Galactic center region)
• Pointed observations
Status of HXMT
Full-funding decision: March 2011• Phase-B (pre-flight module): 2011.6-2012.12• Phase-C (flight module): 2013.1-2014.6 • Launch: ~2015
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Outline• Approved missions: launch within the next 5 years
– Hard X-ray Modulation Telescope (HXMT)– Space Variable Object Monitor (SVOM): China-France
collaboration (Barret’s Talk)– Gamma-ray burst polarimeter (POLAR): China-Europe
collaboration on China’s Spacelab• In mission definition and technology development phase:
launch within next ~10 years– X-ray Timing and Polarization mission (XTP)
• Proposed onboard China’s Space Station: launch around 2021-2022– Optical/UV/X-ray All-Sky Monitor
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GRB prompt emission polarization: a last observables of GRBs•Different GRB models
– E-M Model: well defined, moderate Plin ~ 50%
– Fireball Model: high values excluded Plin ~ 10-20 %
– Cannon ball Model: full range possible Plin = 0 - 100%
•Probe quantum gravity (???): – Amelino-Camelia G., 2000, Nature,
408, 661– Piran T, 2005, Lect. Notes Phys, 669,
351– Fan, Y-Z; Wei, D-M; Xu, D. 2007,
MNRAS, 376, 1857See papers discussing various GRB models: T. Piran, A. Dar, M. Lyutikov, D. Eichler, G. Ghisellini, D. Lazzatti, M. Medvedev, E. Rossi etc.
From M. Lyutikov, 2003
Gamma-ray burst polarization experiment onboard China’s Spacelab: POLAR
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Gamma-ray burst polarization experiment onboard China’s Spacelab: POLAR
• Onboard China’s spacelab TG-2: launch time 2012-13
• A China-led international collaboration (Switzerland, France, Poland)
• FOV of POLAR: ~½ sky
Tian-Gong 天宫Palace in Heaven
Plastic scintillator stacks
Instrument concept proposed by N. Produit, et al., NIM (2005)
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POLAR capability summary
0 10 20 30 40 50 60 70 80 90 1000
20
40
60
80
100
120
140
160
180
Minimum Detectable Polarization with 3σ (%)
Num
ber
of
GR
Bs (
N <
MD
P)
One year observation of POLAR
TS2/DM2 FOV = 2π
0 10 20 30 40 50 60 70 80 90 1000
20
40
60
80
100
120
140
160
180
Minimum Detectable Polarization with 3σ (%)
Num
ber
of
GR
Bs (
N <
MD
P)
One year observation of POLAR
TS2/DM2 FOV = 2π
•10 GRBs per year down to 8%, or •60 GRBs per year down to 30%, or 100
GRBs per year down to 50%
polarization,
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Outline• Approved missions: launch within the next 5 years
– Hard X-ray Modulation Telescope (HXMT)– Space Variable Object Monitor (SVOM): China-France
collaboration (Barret’s Talk)– Gamma-ray burst polarimeter (POLAR): China-Europe
collaboration on China’s Spacelab• In mission definition and technology development phase:
launch within next ~10 years– X-ray Timing and Polarization mission (XTP)
• Proposed onboard China’s Space Station: launch around 2021-2022– Optical/UV/X-ray All-Sky Monitor
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X-ray Timing and Polarization (XTP) mission
• Key Science: Matter under extreme conditions
• Precise Light curve: Neutron Star equation of state, BH basic parameters, formation and growth …
• Polarization of X-ray: Radiation mechanism…• Diffuse X-ray emission, hot gas distribution in Galaxy• …
• Main Requirement: large effective area & high counting rate
• The most accurate light curve and polarization observation at 1-30 keV
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HERO concept: High Energy Replicated Optics – Small Aperture, Short Focal Length and Shallow Grazing Incidence
Using small mirror array to achieve large collection area at hard X-ray (>10 keV): technically more feasible than single large mirror.
Ramsey et al, SPIE 2000
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Bepicolombo soft X-ray (<10 keV) MPO telescope: short focal length & lightweight
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XTP Mission Concept
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XTP (Possible) Instruments
High-energy Collimated Array (1-100 keV)
Low-energy Collimated Array (0.5-15 keV)
High-energy Focused Array (1-100 keV)
All Sky Monitor (5-300 keV) Polarization Observation
Telescope (2-10 keV)
Low-energy Focused (0.5-10 keV)
4 m focal
length
SDD/CZT
SDD/CZT
CCD
SCD
GEM
CZT
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有效载荷初步方案LFA: Low energy X-ray Focusing telescope Array 0.5-10 keVMicro-pore Optics (MPO) mirrors, mDEPFET detectors
MPO光学原理
矩形微通道排列 环形微通道排列
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High energy X-ray Focusing telescope Array (HFA): 1-100 keV
Double conical nested mirrors SDD+CZT composite detector
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Low energy x-ray Collimated detector Array (LCA): 0.5-15 keV
一个 LCA模块示意图 LIGA made collimator: 30μm thickness each layer
SCD: e2V
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HCA: High energy X-ray Collimated detector Array 1-100 keV
HCA composite detector
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POT: Polarization Observation Telescopes 2-10 keV
掠射望远镜可通过国际合作由意大利 INAF研制，图示为意大利原为HXMT设计的多层掠射镜的装配图。
GEM-TPC: 0.25-30 keV
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ASM: All-Sky Monitor
FOV~2Sr, 4-300 keV, 1000cm2, 6400 × 4mm×4mm CdZnTe
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Energy Range, Weight, FOV & Angular Resolution
HFA ： 1-100 keV, 480 kg, 1°×1°, 1’LFA ： 0.5-10 keV, 170 kg, 1°×1°, 1’HCA ： 1-100 keV, 500 kg, 2°×2°LCA ： 0.5-15 keV, 400 kg, 2°×2°ASM ： 4-300 keV, 100 kg, 2 SrPOT ： 2-10 keV, 110 kg, 22’ ×22’Total satellite mass: 3210 kg
Geometrical Area
HFA: 5000 cm2 (1-6 keV), 2800 cm2@30 keVLFA ： 7400 cm2@1 keVHCA: 15000 cm2 (6-30 keV)LCA: 15000 cm2 (1-6 keV)
Energy Resolution150 [email protected] keV4 keV@30 keV
Timing Resolution 10 μs
XTP Basic Parameters
May choose near-earth orbit or L2 orbit, depending on available launcher (money)
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Outline• Approved missions: launch within the next 5 years
– Hard X-ray Modulation Telescope (HXMT)– Space Variable Object Monitor (SVOM): China-France
collaboration (Barret’s Talk)– Gamma-ray burst polarimeter (POLAR): China-Europe
collaboration on China’s Spacelab• In mission definition and technology development phase:
launch within next ~10 years– X-ray Timing and Polarization mission (XTP)
• Proposed onboard China’s Space Station: launch around 2021-2022– Optical/UV/X-ray All-Sky Monitor
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OUVX-ASM Mission Conceptzenith
Motion of spacecraft
FOV of X-ASM
FOV of OUV-ASM
One X-ray ASM Module
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Summary on China’s Future Space X-ray Astronomy Program
• Approved missions– Hard X-ray Modulation Telescope (HXMT): 2014-2015– Space Variable Object Monitor (SVOM): China-France
collaboration (Barret’s Talk) ~2015– Gamma-ray burst polarimeter (POLAR): China-Europe
collaboration on China’s Spacelab 2012-2013• In mission definition and technology development phase
– X-ray Timing and Polarization mission (XTP) ~2020• Proposed onboard China’s Space Station
– Optical/UV/X-ray All-Sky Monitor ~2021-2022
