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Mid-InfraRed Medium Resolution
Echelle Spectrometer (MIRMES)
Itsuki Sakon (Univ. of Tokyo)
Yuji Ikeda(Photocoding)
Naofumi Fujishiro(Cybernet)
Hirokazu Kataza (ISAS/JAXA)
Takashi Onaka (Univ. of Tokyo),
SPICA pre-project team
Outline
The Mid-Infrared Medium-Resolution Eschelle Spectrometer
(MIRMES) is one of the focal plane instrument onboard SPICA
mission in the pre-project phase. It is designed particularly for
measuring the intensity and the profile of lines from ionized gas and
molecules as well as the detailed spectral structure of dust band
features of various compositions in the wavelengths continuously from
10 to 40 micron with moderately high spectral resolution power that is
almost comparable to that of SAFARI in the far-infrared.
MIRMES consists of two channels; Arm-S covers the wavelengths
from 10.3 to 19.9 micron with the resolution power of R~1200 and
Arm-L covers from 19.9 to 36.0 micron with R~750. They share the
same field of view by means of a beamsplitter. The FOV size for ArmS and –L is 12” x 8”.5 for Arm-S and 14” x 12”.5 for Arm-L. The FOV
is split into 5 rows by using the integral field spectroscopy (IFU) unit.
Scientific Objectives/Targets
& Required Specifications
Scientific Targets
Exploring the process of cosmic recycling among gas, molecules and dust particles
in the context of chemical evolution history of the universe is one of the most important
objective of the SPICA mission. Particularly, the following observational approaches are
crucial to achieve this objective;
1) infrared spectroscopic diagnostics of the composition and the properties of dust and
molecules formed in the mass loss winds from the evolved massive stars including the
supernovae (SNe), Wolf-Rayet (WR) stars, and Luminous Blue Variables (LBVs)
2) infrared spectroscopic diagnostics of the composition and the properties of dust and
molecules formed in the mass loss wind from low- to intermediate-mass evolved stars
including post-Asymptotic Giant Branch (AGB) stars, Planetary Nebulae (PNe) and novae
3) infrared spectroscopic diagnostics of the composition and the properties of molecules
synthesized in the atmosphere of evolved low- to intermediate-mass stars・infrared
spectroscopic analysis of SN remnants in the Milky Way and in nearby galaxies to
understand how much fraction of newly condensed dust in the SN ejecta is destroyed
and how much of them survives the shocks
4) infrared spectroscopy of dense molecular clouds with embedded young stellar object
to identify the infrared bands of iron sulfide grains and to systematically understand the
role of cold dense molecular clouds as the site of dust synthesis and the grain growth
Scientific Targets
5) Infrared spectroscopy of various ISM structures in nearby galaxies to demonstrate the
cosmic recycling among ionic gas, molecules, and dust particles on a galactic scale.
6) Infrared spectroscopic diagnostics of ISM properties of remote galaxies, which provide
us unique physical parameter space in terms of metallicity and morphology.
All these observational approaches require spectroscopic abilities covering thoroughly
from 10mm to 40mm with moderately high (R>1000) spectral resolution power in order to
measure the intensity and profiles of ionic lines, molecular lines and various dust band
features in this wavelength regime. In addition, observations of time-varying objects such
as supernovae, LBVs, WRs and novae are indispensable to achieve our scientific purpose,
simultaneous operation of shorter wavelength module covering from 10-20mm and longer
wavelength module covering from 20-40mm is indispensable. Moreover, accuracy in the
absolute flux level and, especially, their relative consistency between the shorter
wavelength module covering from 10-20mm and longer wavelength module covering
from 20-40mm is indispensable to obtain the accurate ionic line ratios and profiles of dust
band features distributed widely in 10-40mm. The SPICA/MIRMES is the instrument that
is designed to fulfill those requests given above.
Scientific Targets
Key Scientific Targets
1.
2.
3.
4.
5.
6.
7.
8.
9.
Molecules and dust formation in the ejecta of Core-collapse Supernovae,
Luminous Blue Variables (LBVs) and WR stars
Destruction and survival of dust in Supernova remnants (SNRs)
in the Milky Way, Magellanic Clouds, and in Nearby galaxies
Molecular Chemistry in the atmosphere of AGB stars and PNe
Dust formation in recurrent Novae and Type Ia supernovae
Molecules and dust formation in dense clouds with embedded YSOs
Cosmic recycling taken place within nearby galaxies
Mid-infrared Spectroscopic diagnostics of ISM condition in remote galaxies
Mid-infrared spectroscopy of emission lines associated with warm (1001000K) gas in proto-planetary disks
Distribution and physical state of solid materials in proto-planetary disks
and dust disks in the main-sequence stars.
Consistency with MRD
1.
2.
3.
4.
5.
6.
7.
8.
9.
Multi-epoch MIR spectroscopy of Core-collapse Supernova, LBVs and WR stars
 consistent with “Life Cycle of Dust; Objective #1” in MRD.
Demonstrating Material Circulation in Supernova remnant
 consistent with “Life Cycle of Dust; Objective #3” in MRD.
Understanding the Chemistry in the atmosphere of AGB stars and PNe
 consistent with “Life Cycle of Dust; Objective #2” in MRD.
Measuring the Dust Yields by Nova, Type Ia supernova
 consistent with “Life Cycle of Dust; Objective #2” in MRD.
Understanding the Dust formation in Dense Interstellar Clouds
 consistent with “Life Cycle of Dust; Objective #4” in MRD.
Understanding the cosmic recycling taken place within nearby galaxies
 consistent with “Life Cycle of Dust; Objective #5” in MRD.
MIR Spectroscopic diagnostics of ISM conditions in remote galaxies
 consistent with “Extragalactic Science; Objective #3 & #4” in MRD.
Mid-infrared spectroscopy of lines emitted from warm gas in protoplanetary disks
 consistent with “Planetary System; Objective #2” in MRD.
Understanding the role of solid state materials for planet formation.
 consistent with “Planetary System; Objective #6” in MRD.
Specification of MIRMES
ARM-L
ARM-S
array format
Si:As (2k x 2k)
25 mm/pix
Si:Sb (1k x 1k)
18 mm/pix
Wavelength coverage
10.0mm-19.9mm
19.9mm-35.0mm
Spectral resolution (R=l/Dl)
~1400
pixel scale
0.409 (“/pix)
0.413 (“/pix)
Slit width
1”.7 (4.2pixel)
2”.5 (6.1pixel)
12” x 8”.5
FOV size
Arm-S
Echelle order lmin (mm) lmax (mm)
4
5
6
7
~750
15.53
12.71
10.75
(9.98)
19.97
15.53
12.71
10.75
14” x 12”.5
Arm-L
Echelle order lmin (mm)
5
6
7
8
29.4
24.4
21.2
(19.9)
lmax (mm)
35.0
29.4
24.4
21.2
※ lmin and lmax are defined as the wavelength at which the grating efficiency drops to 40% of the peak
Specification of Instrument
Echelle Formats on detector arrays of Arm-S and Arm-L
Concept Study
Current Status
Optics & Optical Elements
Fore-Optics for MIRMES
Image Slicer (with 5 slitlets)
side view
top view
Optics & Optical Elements
Spectrograph for MIRMES/Arm-S
Camera
mirrors
Pseudo Slit
(60”.8)
Collimator mirrors
30mm
Si:As detector Array
(2k x 2k ; 25um)
Optics & Optical Elements
Spectrograph for MIRMES/Arm-L
Camera
mirrors
Si:Sb detector Array
(1k x 1k ; 18um)
Pseudo Slit
(70”)
30mm
Collimator mirrors
Detectors
MIRMES/Arm-S (TBD; same as that used for MIRACLE)
Si:As 2kx2k (Raytheon)
Pixel pitch; 25um/pix
Dark current; 0.1e/sec
Full well; 1.0x106 (electron/pix)
Thermal output; 1mW
Quantum Efficiency; N/A
MIRMES/Arm-L (TBD; same as that used for MIRACLE)
Si:Sb 1kx1k (DRS)
Pixel pitch; 18um/pix
Dark current; 1e/sec
Full well; 1.0x106 (electron/pix)
Thermal output; 1mW
Quantum Efficiency; N/A
Volume & Structure
Total Volume
MIRMES/Arm-S;
300 x 300 x 150
MIRMES/Arm-L;
200 x 250 x 150
(in units of mm)
Thermal Design
-No driving modules in MIRMES
-Calibration lamp & shutter for dark measurements are shared with MIRACLE
Detectors
Si:As 2K x 2K array x 1 (5K)
4.5K J-T stage ・・・
(parasitic)
(active)
0 mW
1 mW
(TBD)
Si:Sb 1K x 1K array x 1 (3K)
1.7K J-T stage ・・・
0 mW
1 mW
(TBD)
Wire (20K) 12K 2ST stage ・・・
1 mW
50 mW
(TBD)
0 mW
N/A mW
(TBD)
Annealing function
for each detectors
・・・
Expected Performance
Assumptions;
-Surface Brightness of the Background
dominated by zodiacal emission
(cf. Reach et al. (2003));
Low-background case; Zodiacal emission
modeled by blackbody of Tdust= 274.0K
normalized at the 25mm flux of 15.5MJy/sr
High-background case; Zodiacal emission
modeled by blackbody of Tdust= 268.5K
normalized at the 25mm flux of 79.42MJy/sr
-Spatial scale of 1 pixel in the sky;
0”.409 for Arm-S, 0”.413 for Arm-L
-Effective area of the primary mirror;
p(3.0/2)2 x 0.8 [m2]
-Slit Width;
1”.7 (4.2pix) for Arm-S, 2”.5 (6.1pix) for Arm-L
-Effective Image Size;
1”.7 (4.2pix) for Arm-S, 2”.5 (6.1pix) for Arm-L
-Optical System Efficiency (including filters,
mirror transmittance, beamsplitter, etc.);
0.3 for Arm-S, 0.3 for Arm-L
-Dark Current;
0.1[e/sec] for Si:As 2Kx2K array (Arm-S),
1.0[e/sec] for Si:Sb 1Kx1K array(Arm-L)
-Readout Noise;
10[e] for Arm-S, 20[e] for Arm-L
-Maximum lamp time per exposure; 600 [sec]
-Minimum lamp time per exposure; 2 [sec]
-Full well per pixel;
1.0x106[e/pix] for Arm-S
1.0x106[e/pix] for Arm-L
-Linearity warranty;
0.5 x full well
-Maximum encircled energy fraction
in a central pixel for a point source;
0.12 for Arm-S, 0.06 for Arm-L
Expected Performance
SPICA/MIRMES Sensitivity for point sources
Expected Performance
SPICA/MIRMES Sensitivity for diffuse sources
Expected Performance
SPICA/MIRMES Saturation for point sources
Resource Requirements
Field-of-View Requirement
FOV of Arm-L
FOV of Arm-S
12”.5
FOV size for Arm-S; 12”x8.5”
for Arm-L; 14”x12”.5
8”.5
14”.0
12”.0
- Arm-S and Arm–L share the same field of view by means of a
beam splitter installed in the fore-optics.
- Each FOV is divided into 5 slitlets with image slicer.
- The size of each slitlet;
12” x 1”.7 for Arm-S
14” x 2”.5 for Arm-L
Thermal & Cryogenic
Requirement
MIRMES
Requirement
unit
parasitic
Active
Total
1.7K J-T stage
temperature of stage
temperature range requirement
temperature stability requirement
Remarks
parasitic : instrument off
active : ON, incl. parasitic
1.7 K
K
3K
mK
100mK
Average lift
mW
0.0
1.0
1.0
Peak lift
mW
0.0
1.0
1.0
Temp. at detector
Si:Sb 1kX1K x 1
Low temp to reduce dark
4.5K J-T stage
temperature of stage
temperature range requirement
temperature stability requirement
4.5 K
K
5.0K
mK
100mK
Temp. at detector
Average lift
mW
0.0
1.0
1.0
Peak lift
mW
0.0
1.0
1.0
Si:As 2kX2K x 1
Low temp to reduce dark
12K 2ST stage
temperature of stage
12K
temperature range requirement
K
20K
temperature stability requirement
K
1K
Average lift
mW
1.0
50.0
Peak lift
mW
1.0
50.0
Heat sink for wire
Pre-Amp at low temp.
stage
Pointing / Attitude control
Requirement
Requested pointing/attitude control accuracy; 0”.425
The widths of slitlet of Arms-S and –L are 1.7” and 2.5”, respectively.
The pointing accuracy corresponding to the ¼ of the width of slitlet
is requested; 1”.7 x 0.25 ~ 0”.425 for Arm-S
2”.5 x 0.25 ~ 0”.625 for Arm-L
Structural Requirement
TBD
Data Generation Rate & Data
Handling Requirement
Simultaneous readout of data of Arms-S and -L
1 pixel = 16bit(=2Byte), 2K x 2K pixels = 8.4MB (Arm-S), 1K x 1K pixels = 2.1MB (Arm-L)
(1) The case of longest ramp time (texp=600 sec)
If we try to downlink the data sampled before and after the reset,
the data generation rate becomes; 10.5(MB) x 2 / 600(sec) = 35KBps
(2) The case of shortest ramp time (texp=2.0)
If we try to downlink the data sampled before and after the reset,
the data generation rate becomes; 10.5(MB) x 2 / 2(sec) = 10.5MBps
If we calculate the differential between data sampled before and after the reset, integrate
4 exposures, and downlink only the result, the data generation rate becomes;
18bit /16bit x (8.4MB +2.1MB) / 2(sec) / 4 = 1.48MBps (preferred)
Onboard computer that can handle the image operation is requested
Warm Electronics
TBD
(common among MIRACLE, MIRMES and MIRHES)
Function
Component
#.
Pcs.
Power
(W)
Power
Dissipation
Power
(W)
observing
Focal-Plane Array
2
9
9
Power
Dissipation
standby
9
9
Operation & Observing
Mode
12”.0
Operation; TBD
Parasitic
Active
-standby
-observing
single texp=2 (sec) ※
single texp=20/60/120/600 (sec)
step texp=20/60/120/600 (sec)
-calibration
dark texp=2/20/60/120/600
cal. lamp on texp=2(sec) ※
※4 exposure cycles are 1 unit.
power
(W)
0
data generation rate
(MB/s)
0
TBD
< 0.01
mstep
nstep
TBD
TBD
TBD
1.48
1.05/0.35/0.18/0.04
1.05/0.35/0.18/0.04
TBD
TBD
1.48/1.05/0.35/0.18/0.04
1.48
/
FOV of Arm-L
FOV of Arm-S
12”.0
step offset
- dithering mode required
dstep
12”.5
Single mode
Parameters; Texp, ncycle
8”.5
14”.0
Step Mapping mode Parameters;
Texp, dstep , nstep, mstep, ncycle
Development and Test Plan
Key Technical Issues &
TRL
SPICA/MIRMES
-optics design(I)；
almost completed.
Volume reduction is under consideration
-structure design(I); starting analyses with SHI (~ 30 Apr. 2010)
-optics design(II);
Not yet (scheduled from 1st May 2010 ~)
-structure design(II); Not yet (scheduled from 1st May 2010 ~)
-beam splitter / filter; starting analyses with JDS Uniphase (Feb. 2010 ~)
-slice mirror;
starting analyses of manufacturing the slice mirror
- detector/ electric design; common with MIRACLE
Development Plan
FM
PM
Test & Verification Plan
MIRMES Prototype Model(PM) test & Verification (2013/6—2014/6)
Room temperature optical source test (optical alignment check)
Cryogenic temperature infrared source test (infrared alignment check, detector electric circuit test)
Room temperature vibration test
Cryogenic temperature vibration test
MIRMES Flight Model(FM) test & Verification (2015/1—2015/9)
Room temperature optical source test (optical alignment check)
Cryogenic temperature infrared source test (infrared alignment check, detector electric circuit test)
Room temperature vibration test
Cryogenic temperature vibration test
Calibration (wavelength, flux)
MIRMES FM combination test with MIRACLE (2015/9—2016/3)
Room temperature optical source test (optical alignment check)
Cryogenic temperature infrared source test (infrared alignment check, detector circuit test)
Room temperature vibration test
Cryogenic temperature vibration test
Development Cost
Development Cost (x 1,000 JPY)
Optical design(I)
1,000 (Arm-S) + 1,000 (Arm-L)
Structure design(I) 10,000 (Arm-S+Arm-L)
Optical design(II)
1,000 (Arm-S) + 1,000 (Arm-L)
Structure design(II) 10,000 (Arm-S+Arm-L)
[Photocoding, Cybernet]
[SHI]
[Photocoding. Cybernet]
[SHI]
Detector, Detector Circuits; common development system with MIRACLE
primary investment 200,000
Si:As 2Kx2K 100,000 x 2 (FM + PM) [Laytheon]
Si:Sb 1Kx1K 100,000 x 2 (FM + PM) [DRS]
Beamsplitter, filter; 1 sample test 2,000 x 5 (TBD; negotiation with JDS
Uniphase)
Slice mirror;
2,000 x 2 (FM + PM)
Mirror; common development system with MIRACLE
PM x 2 + FM; 1,000,000 (TBD; negotiation with SHI)
Test & Verification; 100,000
Observing Program
Observation Plan to
perform Science Targets
1.
2.
3.
4.
5.
6.
7.
8.
9.
Multi-epoch MIR spectroscopy of Core-collapse Supernova, LBVs and WR stars
 see “Life Cycle of Dust; Objective #1” of MRD in details.
Demonstrating Material Circulation in Supernova remnant
 see “Life Cycle of Dust; Objective #3” of MRD in details.
Understanding the Chemistry in the atmosphere of AGB stars and PNe
 see “Life Cycle of Dust; Objective #2” of MRD in details.
Measuring the Dust Yields by Nova, Type Ia supernova
 see “Life Cycle of Dust; Objective #2” of MRD in details.
Understanding the Dust formation in Dense Interstellar Clouds
 see “Life Cycle of Dust; Objective #4” of MRD in details.
Understanding the cosmic recycling taken place within nearby galaxies
 see “Life Cycle of Dust; Objective #5” of MRD in details.
MIR Spectroscopic diagnostics of ISM conditions in remote galaxies
 see “Extragalactic Science; Objective #3 & #4” of MRD in details.
Mid-infrared spectroscopy of lines emitted from warm gas in protoplanetary disks
 see “Planetary System; Objective #2” of MRD in details.
Understanding the role of solid state materials for planet formation.
 see “Planetary System; Objective #6” of MRD in details.
Outline of Ground Data
Processing
All the procedures used for the data processing of MIRMES
are generally same as those of Subaru/COMICS.
The data reduction pipeline and contribution softwares are
prepared during the performance verification phase.
The calibration datasets (monitoring standard star, flat
fielding, ) are taken regularly (say, once a month) to check
the stability of the on-orbit performance.
Organization & Structure
for Development
※Detector, electric circuit, mirrors; common with MIRACLE team
General: I. Sakon (Univ. of Tokyo), H.Kataza (ISAS/JAXA),
T. Onaka (Univ. of Tokyo) [adviser]
Optical Design：Y. Ikeda (Photocoding)・N.Fujishiro (CYBERNET.Co.)
Structural Design：Sumitomo Heavy Industry (SHI)
Detector：T. Wada, H.Kataza (ISAS/JAXA)・technical staff 1
Electric Circuit： technical staff 2
Test and Verification of MIRMES (including development of beam splitter,
filters, and slice mirrors, experiments and performance test)：
I. Sakon (Univ. of Tokyo), 1-2 graduate school students, technical staff 3
Sciene Discussion：I.Sakon, T.Onaka (Univ. of Tokyo), Y.Okada (Univ. of
Cologne), H.Kaneda (Nagoya University), T. Nozawa (IPMU), T. Kozasa
(Hokkaido Univ.), M. Matsuura (University College London) [TBD]
Summary