mid-infrared medium resolution echelle spectrometer (mirmes) itsuki sakon (univ. of tokyo) yuji...
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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 Arm-S 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.
Exploring the process of cosmic recycling among gas, molecules and dust particlesin 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 thesupernovae (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 novae3) 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 shocks4) 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 10m to 40m 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 10-20m and longer wavelength module covering from 20-40m is indispensable. Moreover, accuracy in the absolute flux level and, especially, their relative consistency between the shorter wavelength module covering from 10-20m and longer wavelength module covering from 20-40m is indispensable to obtain the accurate ionic line ratios and profiles of dust band features distributed widely in 10-40m. The SPICA/MIRMES is the instrument that is designed to fulfill those requests given above.
Scientific Targets
Scientific Targets
Key Scientific Targets1. Molecules and dust formation in the ejecta of Core-collapse Supernovae,
Luminous Blue Variables (LBVs) and WR stars
2. Destruction and survival of dust in Supernova remnants (SNRs)
in the Milky Way, Magellanic Clouds, and in Nearby galaxies
3. Molecular Chemistry in the atmosphere of AGB stars and PNe
4. Dust formation in recurrent Novae and Type Ia supernovae
5. Molecules and dust formation in dense clouds with embedded YSOs
6. Cosmic recycling taken place within nearby galaxies
7. Mid-infrared Spectroscopic diagnostics of ISM condition in remote galaxies
8. Mid-infrared spectroscopy of emission lines associated with warm (100-1000K) gas in proto-planetary disks
9. Distribution and physical state of solid materials in proto-planetary disks and dust disks in the main-sequence stars.
Consistency with MRD
1. Multi-epoch MIR spectroscopy of Core-collapse Supernova, LBVs and WR stars
consistent with “Life Cycle of Dust; Objective #1” in MRD.
2. Demonstrating Material Circulation in Supernova remnant
consistent with “Life Cycle of Dust; Objective #3” in MRD.
3. Understanding the Chemistry in the atmosphere of AGB stars and PNe
consistent with “Life Cycle of Dust; Objective #2” in MRD.
4. Measuring the Dust Yields by Nova, Type Ia supernova
consistent with “Life Cycle of Dust; Objective #2” in MRD.
5. Understanding the Dust formation in Dense Interstellar Clouds
consistent with “Life Cycle of Dust; Objective #4” in MRD.
6. Understanding the cosmic recycling taken place within nearby galaxies
consistent with “Life Cycle of Dust; Objective #5” in MRD.
7. MIR Spectroscopic diagnostics of ISM conditions in remote galaxies
consistent with “Extragalactic Science; Objective #3 & #4” in MRD.
8. Mid-infrared spectroscopy of lines emitted from warm gas in protoplanetary disks
consistent with “Planetary System; Objective #2” in MRD.
1. Understanding the role of solid state materials for planet formation.
consistent with “Planetary System; Objective #6” in MRD.
Specification of MIRMES
ARM-S ARM-L
array format Si:As (2k x 2k) 25 m/pix
Si:Sb (1k x 1k) 18 m/pix
Wavelength coverage 10.0m-19.9m 19.9m-35.0m
Spectral resolution (R=/) ~1400 ~750
pixel scale 0.409 (“/pix) 0.413 (“/pix)
Slit width 1”.7 (4.2pixel) 2”.5 (6.1pixel)
FOV size 12” x 8”.5 14” x 12”.5
Arm-S Echelle order min (m) max (m)
4 15.53 19.97 5 12.71 15.53 6 10.75 12.71 7 (9.98) 10.75
※ min and max are defined as the wavelength at which the grating efficiency drops to 40% of the peak
Arm-L Echelle order min (m) max (m)
5 29.4 35.0 6 24.4 29.4 7 21.2 24.4 8 (19.9) 21.2
Optics & Optical Elements
Spectrograph for MIRMES/Arm-S
Si:As detector Array (2k x 2k ; 25um)
Pseudo Slit (60”.8)
30mmCollimator mirrors
Cameramirrors
Optics & Optical Elements
Pseudo Slit (70”)
30mm
Collimator mirrors
Cameramirrors
Spectrograph for MIRMES/Arm-L
Si:Sb detector Array (1k x 1k ; 18um)
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 150MIRMES/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 (parasitic) (active)
Si:As 2K x 2K array x 1 (5K)
4.5K J-T stage ・・・ 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)
Annealing function
for each detectors ・・・ 0 mW N/A mW (TBD)
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 25m flux of 15.5MJy/sr
High-background case; Zodiacal emission modeled by blackbody of Tdust= 268.5K normalized at the 25m 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;
(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
Field-of-View Requirement
FOV size for Arm-S; 12”x8.5”
for Arm-L; 14”x12”.5
- 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
12
”.58”.
5
12”.0
14”.0FOV of Arm-L
FOV of Arm-S
Thermal & Cryogenic Requirement
MIRMES Requirement
Remarksunit parasitic Active Total
1.7K J-T stage parasitic : instrument offactive : ON, incl. parasitic temperature of stage 1.7 K
temperature range requirement K 3KTemp. at detectorSi:Sb 1kX1K x 1
Low temp to reduce dark
temperature stability requirement mK 100mK
Average lift mW 0.0 1.0 1.0
Peak lift mW 0.0 1.0 1.0
4.5K J-T stage
temperature of stage 4.5 K
temperature range requirement K 5.0K Temp. at detector
temperature stability requirement mK 100mK
Average lift mW 0.0 1.0 1.0 Si:As 2kX2K x 1Low temp to reduce dark Peak lift mW 0.0 1.0 1.0
12K 2ST stage
Heat sink for wirePre-Amp at low temp.
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
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
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)
FunctionComponent
#. Pcs.
Power (W)
Power Dissipation
Power (W)
Power Dissipation
Focal-Plane Array 2 9 9 9 9
observing standby
Operation & Observing Mode
Operation; TBD
power data generation rate
(W) (MB/s)
Parasitic 0 0
Active
-standby TBD < 0.01
-observing
single texp=2 (sec) TBD 1.48 ※
single texp=20/60/120/600 (sec) TBD 1.05/0.35/0.18/0.04
step texp=20/60/120/600 (sec) TBD 1.05/0.35/0.18/0.04
-calibration
dark texp=2/20/60/120/600 TBD 1.48/1.05/0.35/0.18/0.04
cal. lamp on texp=2(sec) TBD 1.48※
※4 exposure cycles are 1 unit.
Single mode Parameters; Texp, ncycle
- dithering mode required Step Mapping mode Parameters;
Texp, dstep , nstep, mstep, ncycle
step
off
set
dste
p
/・・・
12
”.58”.
5
12”.0
14”.0FOV of Arm-L
FOV of Arm-S
・・・
nstep
mstep12”.0
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
Test & Verification PlanFMPM
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 testCryogenic 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 testCryogenic temperature vibration testCalibration (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 testCryogenic temperature vibration test
Development Cost
Development Cost (x 1,000 JPY)Optical design(I) 1,000 (Arm-S) + 1,000 (Arm-L) [Photocoding, Cybernet]Structure design(I) 10,000 (Arm-S+Arm-L) [SHI]Optical design(II) 1,000 (Arm-S) + 1,000 (Arm-L) [Photocoding. Cybernet]Structure design(II) 10,000 (Arm-S+Arm-L) [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
Observation Plan to perform Science Targets
1. Multi-epoch MIR spectroscopy of Core-collapse Supernova, LBVs and WR stars
see “Life Cycle of Dust; Objective #1” of MRD in details.
2. Demonstrating Material Circulation in Supernova remnant
see “Life Cycle of Dust; Objective #3” of MRD in details.
3. Understanding the Chemistry in the atmosphere of AGB stars and PNe
see “Life Cycle of Dust; Objective #2” of MRD in details.
4. Measuring the Dust Yields by Nova, Type Ia supernova
see “Life Cycle of Dust; Objective #2” of MRD in details.
5. Understanding the Dust formation in Dense Interstellar Clouds
see “Life Cycle of Dust; Objective #4” of MRD in details.
6. Understanding the cosmic recycling taken place within nearby galaxies
see “Life Cycle of Dust; Objective #5” of MRD in details.
7. MIR Spectroscopic diagnostics of ISM conditions in remote galaxies
see “Extragalactic Science; Objective #3 & #4” of MRD in details.
8. Mid-infrared spectroscopy of lines emitted from warm gas in protoplanetary disks
see “Planetary System; Objective #2” of MRD in details.
1. 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]