korean compact infrared space telescope,...
TRANSCRIPT
MIRIS
D.-H. Lee1, W.-S. Jeong1, Y. Park1, C.H. Ree1, U.-W. Nam1, B. Moon1, S.-J. Park1, S.-M. Cha1, J. Pyo1, J.-H. Park1, K. Seon1, D. Lee1,2, S.-W. Rhee3,
J.-O. Park3, H.M. Lee4, T. Matsumoto4,5, W. Han1 & S. Matsuura5,
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Korean Compact Infrared Space Telescope,
MIRIS
1 KASI, Korea, 2 UST, Korea, 3 KARI, Korea, 4 ASIAA, Taiwan, 5 ISAS/JAXA, Japan
MIRIS
Contents
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1. Satellites for Space Observation in Korea
2. Science & Technology Satellite III
3. Overview of MIRIS Project
4. Development of MIRIS
5. Environment Test
6. Calibration of MIRIS
7. Launch Campaign
MIRIS
Space Observation Program in Korea
■Science & Technology Satellite Seriesl 1st satellite: FIMS (Far-ultraviolet IMaging Spectrograph) (2003)l 2nd Satellite: Observation of Space environment by Korean
Launcher Narol 3rd Satellite: MIRIS (Multipurpose Infrared Imaging System)
(Seon et al. 2011) ST-SAT II
MIRIS
■Primary & Secondary Payloads l MIRIS: first infrared camera in space
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Science & Technology Satellite III
S-band Ant.
X-band Ant.
CSS MIRIS SOCSun-shade
Z X
Y x
y
z
MIRIS SOC
MIRIS
Specifications of MIRIS
■Specifications of Space Observation Cameral Wavelength: 0.9 ~ 2mm − Aperture: 80 mml Detector FOV: 3.67o x 3.67o (Pixel : 51.6 arcsec)
(c.f. Nyq. sampling @ 1.6mm = 4.1 arcsec) → limited by satellite stability
l Telescope & Sensor Temp.: 180K (Passive Cooling), 90Kl Filters (5 filters)
• I (1.05mm), H (1.6mm), blank• Pa a (1.876mm), Pa a Cont
MIRIS
Scientific Objectives (1/3)
■Paa Emission Line Survey : Galactic plane & WIM■ Origin of Warm Ionized Medium
l Previous study of WIM: Photoionization modell Recent study of WIM from FIMS: dust scatteringl Verification of the dust scattering theory
■ Physical properties of interstellar turbulencel Structure of WIMl Comparison between Paa (MIRIS) vs. Ha
• Monte-Carlo simulation§ Uniform dust distribution;
E(B-V) = 0.1§ Point source or Spherical
H II region
MIRIS
Scientific Objectives (2/3)
■Observation of Cosmic Infrared Background (CIB)l CIB from POPIII starsl Spectral peak of CIBl Large scale fluctuation of CIB
Matsumoto et al. 2005
Large-scale structure of CIB from IRTS observation
10
100
0.2 0.4 0.6 0.8 1 3 5
residual_summary
IRTS/NIRS
model by Totani et al. 2001
Totani et al. 2001
Bernstein et al. 2002
DIRBE/COBEWright and Rees 2000 Fazio et al. 2004
Madau and Pozzetti 2000
Cambrecy et al. 2001
Surf
ace b
rightn
ess
(nW
/m2/s
r)
Wavelength (mm)
MIRIS
Parameter Space of CIB
Spitzer / GOODS
Parameter space for MIRIS:
MIRIS
■Zodiacal foregroundl Calibration purpose: 2 orbits /dayl Simultaneous observation of NEP & SEP in 1 orbit l Monitoring of ZL in SEP and NEP: I & H bands ® Revision of ZL Model & Removal of ZL component
Scientific Objectives (3/3)
MIRIS
Optomechanical Design
■Optomechanicsl Outer & Inner partsl Dewar & coolerl Passive cooling: radiator, GFRP
supporter, winston cone baffle, thermal shield
MIRIS11
Optical Design
Specifications
Wavelength 0.9 – 2 um
Aperture 80 mm
Focal ratio f/2
Effective Focal Length
160 mm
Pixel FOV 51.6˝X 51.6˝
Detector FOV 3.67° x 3.67
Telescope Temperature
< 200K
Sensor/Filter Temperature
< 100K
Specifications of sensor
Sensor Model Teledyne PICNIC (MCT)
Pixel Size 40 um X 40 um
Sensor Dimension
256 X 256
Detecting Area 10.2 mm X 10.2 mm
MIRIS
■Thermal analysisl Worst hot & cold cases
in all directions
■FEM analysisl Safety factor > 4
in all directions
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Mechanical & Thermal Analysis
Stress in x direction
MIRIS13
Parts of MIRIS
÷
Radiator
Thermal shield Box
GFRP pipe supporter
Bracket
Auxiliaryplate
Dewar
Cooler Box
Barrel
Winston cone baffle
MIRIS14
Assembly of Dewar
SOC filter SOC filter wheel
SOC dewar
MIRIS
■Confirmation of Passive Cooling : telescope < 200K
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Environmental Test – Passive Cooling
SOC Radiator Cold Plate(Velvet-painted)
MIRIS
l Thermal cycles
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Environmental Test – Thermal/Vacuum Test
Tem
pera
ture
(K)
160
180
200
220
240
260
280
300
320
T0 T1 T2 T3 T4 T5
Time(Hrs)0 10 20 30 40 50 60 70 80 90 100 110 120 130 140 150
Vac
uum
(Tor
r)
1e-71e-61e-51e-41e-31e-21e-11e+01e+11e+21e+31e+4
MIRIS
l Vibration/Shock Profile : MIRIS and E-Boxl Total Integration Dose Test: radiation exposure ~30K rad
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Environmental Test – Vibration/Shock, TID Test
MIRIS
11g rms
E-Box
MIRIS
Calibration - Focus Test
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■Beam profile: Gaussianl System MTF: ~30%
MIRIS
Calibration - Dark Test
■Gaussian: readout noise■Temperature variation: ~3K
l Increase of hot pixels: ~0.26%l Increase of noise < 1 ADUl No difference of dark on
temperature variation
Noise map
0.067 ADU/s
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MIRIS
Calibration - Gain Estimation
■Mean-Variance Testl
l Readout noise (sr) : Gaussian – constantl Photon noise (sp) : Poissonian – increasing
■Mean-Variancel Readout noise ~ 45e-
l 45e- < 50e-
(performance estimation)
signal
Readout noise dominant
Photon noise
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MIRIS
Calibration - Flat Data
■Uniform source by integration sphere■Flat fielding for H & Pa bands
l Deviation: reduction of 50%, 42% for H and Pa cont., respectively
l Flatness < 1%
Before AfterBefore AfterH Pa Cont.
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MIRIS
MLI (Multi-Layer Insulation) Wrapping
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MLI 30 layers
Heat-passplate
Interface plate
MIRIS
Final Functional Test
■ Imaging test : OK■ Operation of filter wheel : OK■ Cooler ON/OFF: OK■ SOH data: OK
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MIRIS
Launch Campaign
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MIRIS
Launch Campaign
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MIRIS
Launch Campaign
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MIRIS
Launch Campaign
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M31
Orion Nebula
Rose Nebula
First Images
MIRIS29
AAQQ&&