MIRACLE
Mid-InfRAred Camera without LEnsz

Mid-IR Imaging Camera & low-res. spectroscopic capabilityzWide-Field with high spatial resolution via Silicon BIB detector array (Si:As 2Kx2K,Si:Sb1Kx1K,Si:X 128x128)

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Continuous coverage at 5-38μm by 2 channels (MIRACLE-S : 526μm, MIRACLE-L : 20-38μm)
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Cluster of Galaxies / entire nearby galaxy in aSingle Shotλ/∆λ＝5 (Imaging) 200(Spec.)zz

E.g. Star-formation activity upto z=4 by using PAH features at 8μm

FoV： 5’x5’ Imaging, 5’ long slit forspectroscopyz FoVs of MIRACLE-S & -L areseparated
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Reflective optics : broad-band, high efficiency, low probability of ghost
Observing Efficiency: superior than JWST

Useful for PAH, Graphite, H2O ice

Angular resolution: diffraction limited(0.35”@5um)

MIRACLE on IOBMIRHESMid-IR High-resolution Echelle Spectrograph
Overview Compact high-dispersion spectrograph with Imersion Grating
consisting of Short-mode (S-mode)、Long-mode (L-mode)

OpticsS-modeSpecifications
S-modeL-modeWavelength

4-8 μm

12-18 μm(R= λ/Δλ )~30,000~30,000

Slit width

0.72”

1.20”

Slit length

3.5”

6.0”

Dispersion element

ZnSe Imersion Grating

CdTe Imersion Grating

Detector array

2k x 2k Si:As (25 μm/pix)

2k x 2k Si:As (25 μm/pix)

pixel scale0.29”/pix0.48”/pix

L-modeSensitivity ＊600s exposure, RN=10e-, Dark 0.1e-/s, Zodi background(high/low)

S-mode Point source

L-mode Point Source

S-mode Diffuse

L-mode Diffuse

・Japanese-led (U. Tokyo/IoA, Kyoto-Sngyo Univ./ISAS）

・High-blaze Echelle grating is also under consideration for L-mode2MIRMES
Mid-IR Medium-resolution Echelle Spectrograph
Simultaneous IFU using both Arm-S & Arm-L ( Image slicer )
ARM-L

ARM-S

Si:As (2k x 2k :25 μm/pix) Si:Sb (1k x 1k:18 μm/pix)array format
Wavelength coverage

10.0μm-20.0μm

19.5μm-36.1μm

Spectral resolution (R=λ/Δλ)~1490@13μm~680@27.8μm

pixel scale

0.403 (“/pix)

0.485 (“/pix)

Slit width

1”.2 x 5 slice2”.5 x 5 slice

FOV size12” x 6”.012” x 12”.5Arm-S
Echelle order λmin (μm) λmax (μm)
456715.53
12.71
10.75(9.98)

19.97
15.53
12.71
10.75

Arm-LEchelle order λmin (μm)
5678

29.5
25.0
21.7
19.5

λmax (μm)
36.1
29.5
25.0
21.7

※ λmin and λmax are defined as the wavelength at which the grating efficiency drops to 40% of the peak
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SPICA coronagraph instrument (SCI)High‐dynamic range coronagraph inthe mid‐IR
Key Observing programs
Jupiter‐like exoplanets
Monitoring of planet transit

Wavelength (λ)

Long channlel 5<λ<27μm
Short channel ~1<λ<5μm(coronagraph mode at λ>3.5μm)

Coronagraph method

Binary pupil mask

Observation Mode

Coronagraph Imaging/spectroscopy
or Non- coronagraphImaging/spectroscopy (simultaneoususe of Short/long channels)

Contrast

6th order of magnitude

Spectral Reolution~20, ~200 in spectroscopy mode

Filter bands in imaging
modeBand-pass filters at both Short, longchannels

Inner working angle

3.3 λ/D

Detector array

Si:As (long channel),InSb (short channel)

FoV

1’ x 1’

Simultaneous use of short/longOptimization of pixel size
covers the whole SED of exoplanets

Wavefront control via deformablemirrorsHigh‐accuracy attitude control
C‐TTM（tip‐tilt mirrors), C‐FPC(Guide sensor)

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FPC (Focal Plane Camera)
Proposed Korean Contribution of one of Focal Plane Instrument, consisting twocameras:
FPC‐GFPC‐S

Focal Plane Guide Camera, a part of AOCS for high‐accuracy attitude control
Pointing Stability 0.036 arcsec（3σ） @ 0.5 Hz、Control Accuracy: 0.02 arcsec (0‐P)
Near‐IR (0.8 – 5 μm) imaging & spectrometer for Astronomical purposes
Wide‐field & high throughput compared with JWST
Back‐up system for FPC‐GKASI (Korean Astronomy and Space Science Institute) will lead the development,
assembly & test

FPC‐GOptics
Detector array
Field‐of‐View
Pixel Scale
Read‐out Speed
Wavelength range
Wavelength Resolution
Sensitivity
Operating Temperature
Heat dissp. at 4.5K stage
Cold Mass

FPC‐S

refractive optics with lens
1K x 1K InSb
5 arcmin
0.3 arcsec
2 sec
100 ‐‐ 600 sec
I band (0.8 μm)
0.8 – 5 μm
R=5R= 5 – 50
single channel
5 wide band filters + 3 LVF
21.5 mag (AB), 5σ
26.3 mag (AB), 100 sec, R=5Structure 4.5 K, Detector at 10 K
< 1 mW< 1 mW~ 5 Kg~7Kg