Mid-InfRAred Camera wo LEns (MIRACLE) for SPICA
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Mid-InfRAred Camera wo LEns (MIRACLE) for SPICA Takehiko Wada and team MIRACLE
description
Mid-InfRAred Camera wo LEns (MIRACLE) for SPICA. Takehiko Wada and team MIRACLE. Outline. Scientific target and Required Specification Current status of Conceptual Study System Resource Requirement Development plan Observing plan. Scientific Objectives/Targets & - PowerPoint PPT Presentation
Transcript of Mid-InfRAred Camera wo LEns (MIRACLE) for SPICA
Mid-InfRAred Camera wo LEns (MIRACLE) for SPICA
Takehiko Wada
and
team MIRACLE
Outline
Scientific target and Required Specification
Current status of Conceptual StudySystem Resource RequirementDevelopment planObserving plan
Scientific Objectives/Targets&
Required Specifications
Scientific Targets
Birth and evolution of galaxies in the dust obscured universeCosmic star formation history large scale structure and galaxy evolution
Formation and evolution of dust in the universe Interstellar medium in the Milky way and
near-by galaxies
Consistency with MRD
MIRACLE is the key device for two of three Major Objective of the MRDResolution of Birth and Evolution of
GalaxiesTransmigration of Dust in the Universe
MIRACLE covers a part of one of three Major Objective of the MRDStudies of Exoplanets and Solar Systems
Specification of Instrument
Wide wavelength coverage: 5-50umShort (5-26um) and Long (20-38um, 38-
50um) channelWide field of view: 4x4arcsec (6x6 goal)Multi-band imaging: 6 filters (18 goal)Low resolution spectroscopy: R=5-200
Specification of Instrument
Wide and contiguous wavelength coverage (5-38um) is required to reveal the redshift and star-formation activity in the dust obscured galaxies in the range of redshift z=0-4
Specification of Instrument
Wide field of view is required for superior mapping speed in wavelength shorter than 20um compare to the JWST/MIRI
Specification of Instrument
Wide field of view is required to cover the proto-cluster and the
surrounding region at the redshift z>1
Specification of Instrument
Multi-band imaging is required for SED fitting to reveal the redshift and physical condition of distant galaxies through the wide field survey.
Ｔａｋａｇｉ et al., 2007, PASJ, 59, S557.
AKARI view of faint MIR galaxiesa starburst galaxy at zhot=0.6
Specification of Instrument
Low resolution spectroscopy is well fit to reveal
the physical condition of dust and molecule in the ISM.
Ohyama et al., 2007, PASJ, 59, S441
Concept StudyCurrent Status
Optics & Optical Elements
Wide field optical system with diffraction limit performance without lens has been designed.
Detectors
2Kx2K Si:As BIB detector for 5-26um1Kx1K Si:Sb BIB detector for 20-38um128x128 Si:X BIB detector for 38-50um
Heritage of AKARI/IRC and Spitzer/IRS.
Developments for JWST/MIRI, SOFIA, and FIDTAP.
Volume & Structure
えをはりつける
Thermal Design
Optics are placed on 4K stageDetector are placed on 4K and 1.7K
stageDetector power of mW Parasitic thermal input of mW
Expected Performance
Telescope diffraction limited image quality cover 6x6 arcmin. FOV
Natural background limited sensitivityえ
Resource Requirements
Field-of-View Requirement
6x6 arcmin FOVSmall telescope distortion (inside 9
arcmin from the center)Two set of FOV (for Short and Long
channel)
Thermal & Cryogenic Requirement
4K stage for optics (small power)4K stage for Short channel detector (xx
mW)1.7K stage for Long channel detector (xx
mW)20K stage for buffer amp (xx mW)
Pointing / Attitude control Requirement
Xx arcsec stability for x00 sec (for shortest wavelength)
Xx arcsec absolute pointing (for cross-slit direction)
Xx arcsec relative pointing (for slit maping)
Quick pointing slew for xx arcmin (dithering observation)
Structural Requirement
No special requirement
Data Generation Rate & Data Handling Requirement
1 M pixel/s sampling for each detector16 bits/pixelMaximum 4 detectorOnboard data storing and compressionPeak rate 64Mbits/sAverage rate TBD
Warm Electronics
Heritage from AKARI/IRC-E conceptHeritage from ASTRO-H hardware (SpW
based system)
Operation & Observing Mode
Imaging (including slit-less spectroscopy)DitheringSlew to adjacent field
Spectroscopy Imaging and peak-upDitheringStep scanSlow scan
Development and Test Plan
Key Technical Issues & TRL
OpticsSystem high TRLFilter (<28um) high TRLFilter (>28um) low TRLMirrors high TRL
Detector AKARI and Spitzer heritage high TRL
WheelsSlit and Filter AKARI and Planet-C heritage (high)Grating wheel (mid TRL)
Development Plan
書き方を相談する。
Test & Verification Plan
書き方を相談する。
Development Cost
Detector2Kx2K Si:As
R&D for proto-type 850k$Proto-model 200k$/pcsx (2+1)Flight-model 500k$/pcs x (2+1)
1Kx1K Si:SbR&D for Proto-type 450k$Proto-model 350k$/pcs x (2+1)Flight-model 500k$/pcs x (2+1)
Development Cost
OpticsSystem design
R&D for Proto-type 500 万円Proto-model 500 万円Flight-model 500 万円
Mirrors and support R&D for Proto-type TBD 万円Proto-model TBDFlight-model TBD
Development Cost
OpticsFilters (<30um)
Proto-model TBDFlight-model TBD
Filters (>30um)R&D for Proto-type TBDProto-model TBDFlight-model TBD
Development Cost
MechanicsWheel (filter and slit)
R&D for Proto-type 500 万円Proto-model 500 万円Flight-model 500 万円
Grating wheel R&D for Proto-type TBD 万円Proto-model TBDFlight-model TBD
Development Cost
StructureSystem
Integration testing
Control electronicsGround sport electronicsGround sport software
Observing Program
Observation Plan to perform Science Targets
何を書いたらよいか聞く
Outline of Ground Data Processing
Similar to AKARI/IRC
Organization & Structure for Development
Core ISASScience
Extra-galacticGalactic
HardwareSystemDetectorOptics
Summary
