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STSAT-3 UN BSSW, June 2008 KASI Compact Wide-Field Survey IR Space Telescope Design Wonyong Han Korea Astronomy & Space Science Institute (KASI)
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STSAT-3 UN BSSW, June 2008 KASI
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STSAT-3 UN BSSW, June 2008 KASI - Korea Sci & Tech Satellite (STSAT) began 1999 - Korea Sci & Tech Satellite (STSAT) began 1999 - FIMS : KASI developedFIMS,Main Payload of STSAT-1, - FIMS : KASI developed FIMS, Main Payload of STSAT-1, in collaboration with KAIST & UC Berkeley in collaboration with KAIST & UC Berkeley - STSAT-1 (FIMS) Launched in 2003 - STSAT-1 (FIMS) Launched in 2003 - FIMS Science Results were Published on ApJL in 2006 - FIMS Science Results were Published on ApJL in 2006 - STSAT-3 Program started in 2007 - STSAT-3 Program started in 2007 - KASI Proposal, MIRIS was Chosen as Main Payload - KASI Proposal, MIRIS was Chosen as Main Payload - MIRIS is small wide-field IR Space Telescope - MIRIS is small wide-field IR Space Telescope [ M ulti-purpose I nfra- R ed I maging S ystem ] [ M ulti-purpose I nfra- R ed I maging S ystem ] Introduction
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STSAT-3 UN BSSW, June 2008 KASI FIMS Heritage ApJL, 2006, Vol 644, Special Issue - First results from the FIMS Mission - 9 papers published including Instruments & System Performances Total diffuse intensity map of the sky for the SPEAR/FIMS L-band (1360-1730 A) observations. Evident features include the Galactic plane, the Sco-Cen association, and the LMC.
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STSAT-3 UN BSSW, June 2008 KASI MIRIS : Scientific Goal (1/3) Galactic Plane Survey (1/2) Origin of the Warm Ionized Medium (WIM) –Challenge to the current paradigm of the Ionization theory –Test the effect of Dust scattering for the WIM observation Observation : Pa survey –Pa (MIRIS) vs. H (Ground-based) : Scattering difference Hαmap from a ground-based survey
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STSAT-3 UN BSSW, June 2008 KASI Scientific Goal (2/3) Galactic Plane Survey (2/2) Physical Properties of Turbulence in the Galaxy –Survey the physical parameters of turbulence in the Galaxy –Derive Magnetic field strength from the structure characteristics of turbulence Observation : Pa survey –Pa (MIRIS) vs. H (Ground-based) : Extinction difference Measurement of the turbulence structure Turbulence model
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STSAT-3 UN BSSW, June 2008 KASI Scientific Goal (3/3) Cosmic Infrared Background (CIB) Observation Origin of the Near-IR CIB –Test the hypothesis of the Pop III origin –Confirm the degree-scale fluctuation suggested by IRTS & AKARI and reveal its nature Observation : I & H-band –I-band (no Pop III) vs. H-band (Pop III expected) Matsumoto et al. 2005 Spectral bump suspected to be redshifted from the Pop III Ly-cutoff Degree-scale fluctuation in the power spectrum from IRTS
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STSAT-3 UN BSSW, June 2008 KASI MIRIS System Design
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STSAT-3 UN BSSW, June 2008 KASI STSAT-3 Layout Space Observation Camera Earth Observation Camera Secondary Payload, COMIS Sun Avoidance = ±90 degree Earth Avoidance = ±30 degree Sun Avoidance = ±30 degree Star Tracker
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STSAT-3 UN BSSW, June 2008 KASI Space Observation Camera (SOC) MIRIS Layout Controller box Nadir Flight direction X(Roll) Z(Yaw) Y(Pitch)
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STSAT-3 UN BSSW, June 2008 KASI MIRIS Specifications Space Obs. Camera (SOC)Earth Obs. Camera (EOC) Wavelength0.9 – 2 um3 – 5 um Aperture80 mm100 mm Focal ratiof/2f/5 Pixel FOV51.6 arcsec Detector FOV3.67 o x 3.67 o Ground pixel size42 m @700km Swath width13.4 km @700km SensorTeledyne PICNICi3 system FilterFilter Wheel (6 filters)Band pass filter Telescope Temp180-200 K (passive cooling)300 K Sensor Temp77 K PerformanceMTF > 60%MTF > 20%
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STSAT-3 UN BSSW, June 2008 KASI MIRIS Operation Concept ModeTest (3 months)1 st Year2 nd Year Bus Test 10 orbits/day (1 month) (if needed) Space Observation -Galactic Plane -Cosmic Background -Calibration (1 month) 4 orbits/day 2 orbits/day 6 orbits/day 2 orbits/day User time (if needed) Earth Observation (1 month) 2 orbits/day Regular Test & Emergency Observation 6 orbits/day Ground Contact4 orbits/day
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STSAT-3 UN BSSW, June 2008 KASI SOC Layout Cooler Lens Detector Baffle Radiator
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STSAT-3 UN BSSW, June 2008 KASI SOC Optics
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STSAT-3 UN BSSW, June 2008 KASI SOC Filter System Purpose IDCWL (um)FWHM (um) Cosmic Infrared Background I1.050.3 H1.60.8 Galactic Plane Survey Pa alpha1.8760.0188 Pa alpha cont 11.840.0184 Pa alpha cont 21.920.0192 Dark & ShutterBlank
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STSAT-3 UN BSSW, June 2008 KASI Performance of SOC Optics Field (degree) RMS spot size (um) 0.00012.4 0.89510.8 1.79012.0 2.61224.0
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STSAT-3 UN BSSW, June 2008 KASI SOC Structure (1/2)
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STSAT-3 UN BSSW, June 2008 KASI SOC Structure (2/2)
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STSAT-3 UN BSSW, June 2008 KASI Passive Cooling for SOC (1/2)
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STSAT-3 UN BSSW, June 2008 KASI Passive Cooling for SOC (1/2) Temperature profile during one orbit (1) The telescope can be cooled below the goal temperature of 200K (2) The detector can be cooled below the goal temperature of 80K
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STSAT-3 UN BSSW, June 2008 KASI MIRIS Eelectronics
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STSAT-3 UN BSSW, June 2008 KASI MIRIS Electronics Box
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STSAT-3 UN BSSW, June 2008 KASI SOC Electronics Q1Q2 Q3Q4 AMPADC PATTERN GENERATOR 4 channel VIDEO Siganal Processing IMAGE DATA DECODER AMPADC AMPADC AMPADC FPGA MEMEORY IMAGE BUFFER CONTROL COMMAND MMS GSE DSP UNIT PICNIC 256 256 ARRAY BIAS CLOCK FIFO SOC READOUT UNIT
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STSAT-3 UN BSSW, June 2008 KASI SOC Detector - HgCdTe Astronomical Wide Area Infrared Imager (PICNIC) - 256 256 IR FPA HgCdTe/Al 2 O 3 (MBE) ParameterSpecificationGoal Format256 256 Pixel Pitch (μm)40 Fill Factor90 Quantum Efficiency(77K) @2.3 μm55%75% Long wavelength cutoff (μm)2.5 Short wavelength cut on (μm).9 Read noise: multiple sample (e - @ 77K)< 40< 20 Dark current (e-/s @ 77K)< 2< 0.2 Well capacity(e-, V b = 0.5V)150,000200,000 Yield(working pixels)> 95%> 99% Temperature77K
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STSAT-3 UN BSSW, June 2008 KASI MIRIS Operation
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STSAT-3 UN BSSW, June 2008 KASI Plan for Galactic Plan Survey 6°
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STSAT-3 UN BSSW, June 2008 KASI Plan for Galactic Plan Survey
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STSAT-3 UN BSSW, June 2008 KASI Plan for the CIB Observation 10 o x10 o deep field @ NEP 50%(1.84 o ) overlap mosaic for uniform sensitivity Best in October & November
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STSAT-3 UN BSSW, June 2008 KASI Thank you whan@kasi.re.kr
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