Current Status of SPICA
Focal Plane Instruments
October 19, 2009
Hideo Matsuhara (ISAS/JAXA) & FPI team
MIRACLE
(Mid-InfRAred Camera w/o LEns)

MIRACLE is a mid-IR instrument with imaging
and low-resolution spectroscopy consisting of
two channels:
2K x 2K
• Filter-wheel : imaging band (R~5) &
spectroscopy with grism/prism (R~100)
MIRACLE Optics
Rear-optics camera
Telescope Focus
Final image
Fore-optics
collimator
Rear-optics
collimator
Re-imaging focus
Fore-optics camera
MIRMES
(MIR Medium-Resolution Spectrometer)


Wavelengths: 16-38mm, 2 channels (Si:As x 1, Si:Sb x 1)
Image slicer, Spectral resolution 700-1000
ARM-S
ARM-L
Wavelength coverage
10.32 mm - 19.35mm
19.22 mm - 36.04mm
Spectral resolution
(R=l/Dl)
~1500
~900
pixel scale
0.37”
0.72”
slit width
1.11” (3 pixel)
3.6” (5 pixel)
FOV size
12.95” x 5.55”
25.2” x 18.0”
(35pixel x 3 pixel x
5rows)
(35pixel x 5 pixel x
5rows)
MIRHES
(MIR High-Resolution Spectrometer)
Short(S)-mode
Long(L)-mode
Wavelength
coverage
Spectral
resolution
(R=l/Dl)
4 – 8mm
12 – 18mm
30,000
20,000 – 30,000
Slit width
0.72”
1.20”
Slit length
3.5”
6.0”
Dispersion
element
ZeSe immersion
grating
KRS5
immersion
grating
Cross disperser
Reflective
reflective
MIRHES
S-mode
MIRACLE/MIRMES/MIRHES:
Current Progress

MIRACLE




Optics design mostly fixed:
Short-wave ch. Detector format is now 2K x 2K (Raytheon
IBC)
Mid-IR filter (long-wave ch.) development is underway
SHI will design :



Pointing control :


Slit-mapping is under consideration, which will relax the absolute
pointing requirement
MIRMES



Structure
Moving mechanism (Filter Wheel, slit changer)
Spectrometer concept has been fixed, Optical design
underway
Beam splitter is a key issue
MIRHES

R&D of Immersing grating for long-wave ch.
SCI : SPICA Coronagraph
Insturment

A mid-IR coronagraph instrument with
both imaging & low-res. spectroscopic
capability.
 Major goal : direct imaging &
spectroscopy at 3.5-27mm
 Coronagraph method


Binary-shaped pupil mask (baseline)
Contrast > 10-6


Field of View: 1.0 x 1.0 arcmin2
Spectral resolution : 20-200

Current status :


Draft optical, structure design finished
improved Tip-tilt design
SAFARI
SPICA Far-infrared
Instrument

Leaded by SAFARI consortium in Europe
 Imaging Fourier-transform spectrometer
covering 35-210mm
 FOV : 2 x 2 arcmin2
 Wavelength resolution

2000 at 100 mm is maximum
SAFARI Design
@Phase-A1 conclusion
Current cold mass : 38.8kg (22% margin to 50kg allocation)
BLISS
(Background-Limited Infrared-Submm Spectrograph)
Proposed by US
AO for conceptual study released by NASA (due 2nd
Nov.)
 Wavelength: 38-430 mm,
 Spectral resolution R=700
 Grating spectrometer, 5 channel, 4200 bolometers at
50mK


FPC (Focal-Plane Finding Camera)



Korean-leading instrument, with participation of NAOJ
FPC-G : guidance sensor for the Attitude control System
to stabilize the attitude with an accuracy of 0.05”
FPC-S: science camera for 2.5-5 mm imaging
Cold stage heat generation

Assumption:



Baseline : No parallel mode
Any observations will be executed by using single
FPI, excluding FPC-G
Current Status
<15mW＠4.5K for any observation mode
 Exceeds [email protected] (baseline allocation
for 1.7K stage) but less than 10mW

14
Heat load (max/average)
@4.5K stage (09/08/31)Ｔ
15
Heat load (max/average)
@1.7K stage (09/08/31)
16
FPI Mass (@ESA CV)
FPI
MIRACLE
MIRMES
MIRHES
SCI
FPC
SAFARI
BLISS
IOB, FPI cover
Total
Weight
(kg)
comment
60.0
with 20% margin
30.0
10.0
50.0
30.0 (optional FPI)
50.0 with 20% margin
200 excluding BLISS
FOV allocation
Pick Off Mirrors
FPI footprint on IOB
Folding Mirror Module

If the pick-off mirror for each FPI belongs to the cold
hardware volume of the FPI, assembling of the whole
FPIs on IOB is really difficult
 We decide to consider a common pick-off module
(PoM) separated from each FPI, but mechanically I/F
to IOB


There may need a hole in the center of PoM, for the
optical test of STA?


PoM is a subsystem of IOBA
May be an issue for SCI’s pick-off location
Important alignment issue for MIRACLE,MIRHES, SCI


They request “co-focus” : stringent accuracy requirements
in their back-focus location
How can we achieve this?
ICS-FPI

ICS (interface control specification) document should
be prepared for SRR



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Following issues should be prepared by 5th Nov. (or so)

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I/F with STA (mechanical/optical), CRYO (thermal), BM
(bus module: electrical), AOCS (pointing control I/F)
MIRACLE, MIRMES, MIRHES & SCI will be put in ICS-FPI
Dedicated ICS for SAFARI, BLISS, FPC
Operation mode
Observing mode
Warm electronics power/heat in each operating mode
(observation/standby)
``Urgently” required info.:

Cold Weight, Volume, outer shape … necessary for the
design of whole FPI assembly
FPI SELECTION PROCESS
Japanese-lead instruments

MIRACLE




Instrument Proposal / Concept study report will be
released by Jan. 2010 (may be delayed)
Refereeing / Reviewing in Jan-March 2010 (may be
delayed) by a Japanese Selection committee
Decision of the Selection will be authorized by JAXA
MIRMES, MIRHES, SCI



Instrument Proposal / Concept study report will be
released by Apr. 2010
Refereeing / Reviewing in Apr-July 2010 by a Japanese
Selection committee
Decision of the Selection will be authorized by JAXA
Oversea-based instruments

SAFARI




BLISS

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

Leaded by European SAFARI consortium
Result of Concept study will be reviewed by ESA
Also JAXA’s review expected before SDR
Leaded by US under NASA AO
Participation critically depends on the Decadal Survey
report
Selection will be decided by discussion between JAXA
and NASA
FPC



Leaded by Korean consortium (w/ participation of NAOJ)
FPC-G (mandatory) , FPC-S (optional)
Review & selection of the specifications will be decided
by discussion between JAXA and Korean consortium