Download 遠くを見よう→赤外線へ

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
&
Required Specifications
Scientific Targets

Birth and evolution of galaxies in the dust
obscured universe
Cosmic 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 MRD
Resolution of Birth and Evolution of
Galaxies
 Transmigration of Dust in the Universe


MIRACLE covers a part of one of three
Major Objective of the MRD

Studies of Exoplanets and Solar Systems
Specification of Instrument

Wide wavelength coverage: 5-50um

Short (5-26um) and Long (20-38um, 3850um) channel
Wide 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
AKARI view of faint MIR galaxies
a starburst galaxy at zhot=0.6
Ｔａｋａｇｉ et al., 2007, PASJ, 59, S557.
Multi-band imaging is required for SED fitting to reveal the redshift
and physical condition of distant galaxies through the wide field
survey.
Specification of Instrument
Ohyama et al., 2007, PASJ, 59, S441
Low resolution spectroscopy is well fit to reveal
the physical condition of dust and molecule in the ISM.
Concept Study
Current Status
Optics & Optical Elements
Wide field optical system with diffraction limit
performance without lens has been designed.
Detectors
2Kx2K Si:As BIB detector for 5-26um
 1Kx1K Si:Sb BIB detector for 20-38um
 128x128 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 stage
 Detector are placed on 4K and 1.7K
stage
 Detector 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 FOV
 Small 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 detector
 16 bits/pixel
 Maximum 4 detector
 Onboard data storing and compression
 Peak rate 64Mbits/s
 Average rate TBD

Warm Electronics
Heritage from AKARI/IRC-E concept
 Heritage from ASTRO-H hardware (SpW
based system)

Operation & Observing
Mode

Imaging (including slit-less spectroscopy)
Dithering
 Slew to adjacent field


Spectroscopy
Imaging and peak-up
 Dithering
 Step scan
 Slow scan

Development and Test Plan
Key Technical Issues &
TRL

Optics
System high TRL
 Filter (<28um) high TRL
 Filter (>28um) low TRL
 Mirrors high TRL


Detector


AKARI and Spitzer heritage high TRL
Wheels

Slit and Filter AKARI and Planet-C heritage
(high)
Development Plan

書き方を相談する。
Test & Verification Plan

書き方を相談する。
Development Cost

Detector

2Kx2K Si:As
R&D for proto-type 850k$
 Proto-model 200k$/pcsx (2+1)
 Flight-model 500k$/pcs x (2+1)


1Kx1K Si:Sb
R&D for Proto-type 450k$
 Proto-model 350k$/pcs x (2+1)
 Flight-model 500k$/pcs x (2+1)

Development Cost

Optics

System 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 TBD
 Flight-model TBD

Development Cost

Optics

Filters (<30um)
Proto-model TBD
 Flight-model TBD


Filters (>30um)
R&D for Proto-type TBD
 Proto-model TBD
 Flight-model TBD

Development Cost

Mechanics

Wheel (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 TBD
 Flight-model TBD

Development Cost
Structure
 System

Integration
 testing

Control electronics
 Ground sport electronics
 Ground 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 ISAS
 Science

Extra-galactic
 Galactic


Hardware
System
 Detector
 Optics

Summary